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overflow: hidden; text-overflow: ellipsis; -webkit-line-clamp: 3; -webkit-box-orient: vertical; }</style><div class="col-xs-12 clearfix"><div class="u-floatLeft"><h1 class="PageHeader-title u-m0x u-fs30">Star Formation</h1><div class="u-tcGrayDark">3,877 Followers</div><div class="u-tcGrayDark u-mt2x">Recent papers in <b>Star Formation</b></div></div></div></div></div></div><div class="TabbedNavigation"><div class="container"><div class="row"><div class="col-xs-12 clearfix"><ul class="nav u-m0x u-p0x list-inline u-displayFlex"><li class="active"><a href="https://www.academia.edu/Documents/in/Star_Formation">Top Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_Formation/MostCited">Most Cited Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_Formation/MostDownloaded">Most Downloaded Papers</a></li><li><a href="https://www.academia.edu/Documents/in/Star_Formation/MostRecent">Newest Papers</a></li><li><a class="" href="https://www.academia.edu/People/Star_Formation">People</a></li></ul></div><style type="text/css">ul.nav{flex-direction:row}@media(max-width: 567px){ul.nav{flex-direction:column}.TabbedNavigation li{max-width:100%}.TabbedNavigation li.active{background-color:var(--background-grey, #dddde2)}.TabbedNavigation li.active:before,.TabbedNavigation li.active:after{display:none}}</style></div></div></div><div class="container"><div class="row"><div class="col-xs-12"><div class="u-displayFlex"><div class="u-flexGrow1"><div class="works"><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_20063279" data-work_id="20063279" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/20063279/From_Globular_Clusters_to_Tidal_Dwarfs_Structure_Formation_in_Tidal_Tails">From Globular Clusters to Tidal Dwarfs: Structure Formation in Tidal Tails</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Star clusters can be found in galaxy mergers, not only in central regions, but also in the tidal debris. In both the Eastern and Western tidal tails of NGC 3256 there are dozens of young star clusters, confirmed by their blue colors and... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_20063279" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Star clusters can be found in galaxy mergers, not only in central regions, but also in the tidal debris. In both the Eastern and Western tidal tails of NGC 3256 there are dozens of young star clusters, confirmed by their blue colors and larger concentration index as compared to sources off of the tail. Tidal tails of other galaxy pairs do not have such widespread cluster formation, indicating environmental influences on the process of star formation or the packaging of the stars.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/20063279" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="e80d4a541ce00ccb75314872e8629a4b" rel="nofollow" data-download="{"attachment_id":41157148,"asset_id":20063279,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/41157148/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="41039535" href="https://independent.academia.edu/KKnierman">K. Knierman</a><script data-card-contents-for-user="41039535" type="text/json">{"id":41039535,"first_name":"K.","last_name":"Knierman","domain_name":"independent","page_name":"KKnierman","display_name":"K. Knierman","profile_url":"https://independent.academia.edu/KKnierman?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_20063279 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="20063279"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 20063279, container: ".js-paper-rank-work_20063279", }); });</script></li><li class="js-percentile-work_20063279 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 20063279; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_20063279"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_20063279 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="20063279"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 20063279; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=20063279]").text(description); $(".js-view-count-work_20063279").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_20063279").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="20063279"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="962097" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Clusters">Star Clusters</a>, <script data-card-contents-for-ri="962097" type="text/json">{"id":962097,"name":"Star Clusters","url":"https://www.academia.edu/Documents/in/Star_Clusters?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1789202" rel="nofollow" href="https://www.academia.edu/Documents/in/Concentration_Index">Concentration Index</a><script data-card-contents-for-ri="1789202" type="text/json">{"id":1789202,"name":"Concentration Index","url":"https://www.academia.edu/Documents/in/Concentration_Index?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=20063279]'), work: {"id":20063279,"title":"From Globular Clusters to Tidal Dwarfs: Structure Formation in Tidal Tails","created_at":"2016-01-06T10:46:31.324-08:00","url":"https://www.academia.edu/20063279/From_Globular_Clusters_to_Tidal_Dwarfs_Structure_Formation_in_Tidal_Tails?f_ri=4363","dom_id":"work_20063279","summary":"Star clusters can be found in galaxy mergers, not only in central regions, but also in the tidal debris. In both the Eastern and Western tidal tails of NGC 3256 there are dozens of young star clusters, confirmed by their blue colors and larger concentration index as compared to sources off of the tail. Tidal tails of other galaxy pairs do not have such widespread cluster formation, indicating environmental influences on the process of star formation or the packaging of the stars.","downloadable_attachments":[{"id":41157148,"asset_id":20063279,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":41039535,"first_name":"K.","last_name":"Knierman","domain_name":"independent","page_name":"KKnierman","display_name":"K. Knierman","profile_url":"https://independent.academia.edu/KKnierman?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":962097,"name":"Star Clusters","url":"https://www.academia.edu/Documents/in/Star_Clusters?f_ri=4363","nofollow":true},{"id":1789202,"name":"Concentration Index","url":"https://www.academia.edu/Documents/in/Concentration_Index?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_30923679" data-work_id="30923679" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/30923679/Search_for_glycine_in_the_solar_type_protostar_IRAS_16293_2422">Search for glycine in the solar type protostar IRAS 16293-2422</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We report the first search for line emission from one of the simplest amino acids, glycine, from a solar type protostar, IRAS16293-2422. Previous searches for glycine have been carried out on bright massive star formation regions, so far... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_30923679" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We report the first search for line emission from one of the simplest amino acids, glycine, from a solar type protostar, IRAS16293-2422. Previous searches for glycine have been carried out on bright massive star formation regions, so far without success. Recent observations show that although less luminous, solar type protostars also harbor complex molecules and may even be more favorable than massive protostars for the formation and survival of complex molecules.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/30923679" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="0d2ce42b51ac30dcf7ee7dbeb79a8744" rel="nofollow" data-download="{"attachment_id":51348878,"asset_id":30923679,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/51348878/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="58864405" href="https://independent.academia.edu/BertrandLefloch">Bertrand Lefloch</a><script data-card-contents-for-user="58864405" type="text/json">{"id":58864405,"first_name":"Bertrand","last_name":"Lefloch","domain_name":"independent","page_name":"BertrandLefloch","display_name":"Bertrand Lefloch","profile_url":"https://independent.academia.edu/BertrandLefloch?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_30923679 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="30923679"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 30923679, container: ".js-paper-rank-work_30923679", }); 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$(".js-view-count[data-work-id=30923679]").text(description); $(".js-view-count-work_30923679").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_30923679").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="30923679"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">3</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a>, <script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="585573" rel="nofollow" href="https://www.academia.edu/Documents/in/Amino_Acid_Profile">Amino Acid Profile</a><script data-card-contents-for-ri="585573" type="text/json">{"id":585573,"name":"Amino Acid Profile","url":"https://www.academia.edu/Documents/in/Amino_Acid_Profile?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=30923679]'), work: {"id":30923679,"title":"Search for glycine in the solar type protostar IRAS 16293-2422","created_at":"2017-01-14T02:59:33.018-08:00","url":"https://www.academia.edu/30923679/Search_for_glycine_in_the_solar_type_protostar_IRAS_16293_2422?f_ri=4363","dom_id":"work_30923679","summary":"We report the first search for line emission from one of the simplest amino acids, glycine, from a solar type protostar, IRAS16293-2422. Previous searches for glycine have been carried out on bright massive star formation regions, so far without success. Recent observations show that although less luminous, solar type protostars also harbor complex molecules and may even be more favorable than massive protostars for the formation and survival of complex molecules.","downloadable_attachments":[{"id":51348878,"asset_id":30923679,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":58864405,"first_name":"Bertrand","last_name":"Lefloch","domain_name":"independent","page_name":"BertrandLefloch","display_name":"Bertrand Lefloch","profile_url":"https://independent.academia.edu/BertrandLefloch?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":585573,"name":"Amino Acid Profile","url":"https://www.academia.edu/Documents/in/Amino_Acid_Profile?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_58509101" data-work_id="58509101" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/58509101/A_Constant_Bar_Fraction_out_to_Redshift_z_1_in_the_Advanced_Camera_for_Surveys_Field_of_the_Tadpole_Galaxy">A Constant Bar Fraction out to Redshift z ∼ 1 in the Advanced Camera for Surveys Field of the Tadpole Galaxy</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Bar-like structures were investigated in a sample of 186 disk galaxies larger than 0.5 arcsec that are in the I-band image of the Tadpole galaxy taken with the Hubble Space Telescope Advanced Camera for Surveys. We found 22 clear cases of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_58509101" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Bar-like structures were investigated in a sample of 186 disk galaxies larger than 0.5 arcsec that are in the I-band image of the Tadpole galaxy taken with the Hubble Space Telescope Advanced Camera for Surveys. We found 22 clear cases of barred galaxies, 21 galaxies with small bars that appear primarily as isophotal</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/58509101" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="4f2c6760d0d51b76ab06a327bae408cd" rel="nofollow" data-download="{"attachment_id":72885236,"asset_id":58509101,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/72885236/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="33305432" href="https://vassar.academia.edu/DebraElmegreen">Debra Elmegreen</a><script data-card-contents-for-user="33305432" type="text/json">{"id":33305432,"first_name":"Debra","last_name":"Elmegreen","domain_name":"vassar","page_name":"DebraElmegreen","display_name":"Debra Elmegreen","profile_url":"https://vassar.academia.edu/DebraElmegreen?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_58509101 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="58509101"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 58509101, container: ".js-paper-rank-work_58509101", }); });</script></li><li class="js-percentile-work_58509101 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 58509101; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_58509101"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_58509101 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="58509101"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 58509101; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=58509101]").text(description); $(".js-view-count-work_58509101").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_58509101").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="58509101"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">10</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a><script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=58509101]'), work: {"id":58509101,"title":"A Constant Bar Fraction out to Redshift z ∼ 1 in the Advanced Camera for Surveys Field of the Tadpole Galaxy","created_at":"2021-10-16T17:43:32.574-07:00","url":"https://www.academia.edu/58509101/A_Constant_Bar_Fraction_out_to_Redshift_z_1_in_the_Advanced_Camera_for_Surveys_Field_of_the_Tadpole_Galaxy?f_ri=4363","dom_id":"work_58509101","summary":"Bar-like structures were investigated in a sample of 186 disk galaxies larger than 0.5 arcsec that are in the I-band image of the Tadpole galaxy taken with the Hubble Space Telescope Advanced Camera for Surveys. We found 22 clear cases of barred galaxies, 21 galaxies with small bars that appear primarily as isophotal","downloadable_attachments":[{"id":72885236,"asset_id":58509101,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":33305432,"first_name":"Debra","last_name":"Elmegreen","domain_name":"vassar","page_name":"DebraElmegreen","display_name":"Debra Elmegreen","profile_url":"https://vassar.academia.edu/DebraElmegreen?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":188982,"name":"High redshift galaxies and quasars","url":"https://www.academia.edu/Documents/in/High_redshift_galaxies_and_quasars?f_ri=4363"},{"id":246370,"name":"Clusters of Galaxies","url":"https://www.academia.edu/Documents/in/Clusters_of_Galaxies?f_ri=4363"},{"id":398159,"name":"Cold Dark Matter","url":"https://www.academia.edu/Documents/in/Cold_Dark_Matter?f_ri=4363"},{"id":526858,"name":"Size Effect","url":"https://www.academia.edu/Documents/in/Size_Effect?f_ri=4363"},{"id":1181250,"name":"Hubble Space Telescope Images","url":"https://www.academia.edu/Documents/in/Hubble_Space_Telescope_Images?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_34936461" data-work_id="34936461" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/34936461/On_the_abundances_of_GRO_J1655_40">On the abundances of GRO J1655-40</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Context. The detection of overabundances of α-elements and lithium in the secondary star of a black-hole binary provides important insights about the formation of a stellar-mass black-hole. α-enhancement might theoretically also be the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_34936461" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Context. The detection of overabundances of α-elements and lithium in the secondary star of a black-hole binary provides important insights about the formation of a stellar-mass black-hole. α-enhancement might theoretically also be the result of pollution by the nucleosynthesis occurring during an outburst, or through spallation by the jet. Aims. We study the abundances, and their possible variations with time, in the secondary star of the runaway black-hole binary GRO J1655-40, in order to understand their origin. Methods. We present a detailed comparison between a Keck spectrum obtained in 1998 found in the literature, archival VLT-UVES data taken in 2004 and new VLT-UVES spectra obtained early 2006. We carefully determine the equivalent widths of different α-elements (Mg, O, Ti, S and Si) with their associated uncertainty. We use the well-studied comparison star HD 156098 as well as synthetic spectra to match the spectrum of GRO J1655-40 in order to determine the abundances of these elements. Results. We see no significant variations of equivalent widths with time. Our fit using HD 156098 reveals that there is significant overabundance of oxygen in all our spectra, but no overabundances of any of the other α-elements. Finally, we do not detect the lithium line at 6707 Å. Conclusions. We show that there is no detected pollution in GRO J1655-40 after the burst in 2005. Moreover, we argue that uncertainties in the equivalent widths were previously underestimated by a factor of ∼3. Consequently, our results challenge the existence of general overabundances of α-elements observed in this galactic black-hole binary, and thus the accepted interpretation that they are of supernova origin. The physical cause of the overabundance of oxygen remains unclear.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/34936461" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="2cad52229c603eced74a3682fb9da2d1" rel="nofollow" data-download="{"attachment_id":54798228,"asset_id":34936461,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/54798228/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="441099" href="https://saao.academia.edu/EricDepagne">Eric Depagne</a><script data-card-contents-for-user="441099" type="text/json">{"id":441099,"first_name":"Eric","last_name":"Depagne","domain_name":"saao","page_name":"EricDepagne","display_name":"Eric Depagne","profile_url":"https://saao.academia.edu/EricDepagne?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_34936461 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="34936461"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 34936461, container: ".js-paper-rank-work_34936461", }); 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$(".js-view-count[data-work-id=34936461]").text(description); $(".js-view-count-work_34936461").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_34936461").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="34936461"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">11</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4536" rel="nofollow" href="https://www.academia.edu/Documents/in/X-ray_Binaries">X-ray Binaries</a>, <script data-card-contents-for-ri="4536" type="text/json">{"id":4536,"name":"X-ray Binaries","url":"https://www.academia.edu/Documents/in/X-ray_Binaries?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4751" rel="nofollow" href="https://www.academia.edu/Documents/in/Black_Holes">Black Holes</a>, <script data-card-contents-for-ri="4751" type="text/json">{"id":4751,"name":"Black Holes","url":"https://www.academia.edu/Documents/in/Black_Holes?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a><script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=34936461]'), work: {"id":34936461,"title":"On the abundances of GRO J1655-40","created_at":"2017-10-23T14:34:05.123-07:00","url":"https://www.academia.edu/34936461/On_the_abundances_of_GRO_J1655_40?f_ri=4363","dom_id":"work_34936461","summary":"Context. The detection of overabundances of α-elements and lithium in the secondary star of a black-hole binary provides important insights about the formation of a stellar-mass black-hole. α-enhancement might theoretically also be the result of pollution by the nucleosynthesis occurring during an outburst, or through spallation by the jet. Aims. We study the abundances, and their possible variations with time, in the secondary star of the runaway black-hole binary GRO J1655-40, in order to understand their origin. Methods. We present a detailed comparison between a Keck spectrum obtained in 1998 found in the literature, archival VLT-UVES data taken in 2004 and new VLT-UVES spectra obtained early 2006. We carefully determine the equivalent widths of different α-elements (Mg, O, Ti, S and Si) with their associated uncertainty. We use the well-studied comparison star HD 156098 as well as synthetic spectra to match the spectrum of GRO J1655-40 in order to determine the abundances of these elements. Results. We see no significant variations of equivalent widths with time. Our fit using HD 156098 reveals that there is significant overabundance of oxygen in all our spectra, but no overabundances of any of the other α-elements. Finally, we do not detect the lithium line at 6707 Å. Conclusions. We show that there is no detected pollution in GRO J1655-40 after the burst in 2005. Moreover, we argue that uncertainties in the equivalent widths were previously underestimated by a factor of ∼3. Consequently, our results challenge the existence of general overabundances of α-elements observed in this galactic black-hole binary, and thus the accepted interpretation that they are of supernova origin. The physical cause of the overabundance of oxygen remains unclear.","downloadable_attachments":[{"id":54798228,"asset_id":34936461,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":441099,"first_name":"Eric","last_name":"Depagne","domain_name":"saao","page_name":"EricDepagne","display_name":"Eric Depagne","profile_url":"https://saao.academia.edu/EricDepagne?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4536,"name":"X-ray Binaries","url":"https://www.academia.edu/Documents/in/X-ray_Binaries?f_ri=4363","nofollow":true},{"id":4751,"name":"Black Holes","url":"https://www.academia.edu/Documents/in/Black_Holes?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":47598,"name":"Cosmology","url":"https://www.academia.edu/Documents/in/Cosmology?f_ri=4363"},{"id":61603,"name":"Uncertainty","url":"https://www.academia.edu/Documents/in/Uncertainty?f_ri=4363"},{"id":235060,"name":"Black Hole","url":"https://www.academia.edu/Documents/in/Black_Hole?f_ri=4363"},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=4363"},{"id":864382,"name":"Jet","url":"https://www.academia.edu/Documents/in/Jet?f_ri=4363"},{"id":2504124,"name":"Nucleosynthesis","url":"https://www.academia.edu/Documents/in/Nucleosynthesis?f_ri=4363"},{"id":2719759,"name":"Spallation","url":"https://www.academia.edu/Documents/in/Spallation?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4202212" data-work_id="4202212" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4202212/Stellar_Populations_and_the_Star_Formation_Histories_of_LSB_Galaxies_I_Optical_and_H_alpha_Imaging">Stellar Populations and the Star Formation Histories of LSB Galaxies: I. Optical and H-alpha Imaging</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">This paper presents optical and Hα imaging for a large sample of LSB galaxies selected from the PSS-II catalogs . As noted in previous work, LSB galaxies span a range of luminosities (−10 > M V > −20) and sizes (0.3 kpc < R V 25 < 10... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4202212" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">This paper presents optical and Hα imaging for a large sample of LSB galaxies selected from the PSS-II catalogs . As noted in previous work, LSB galaxies span a range of luminosities (−10 > M V > −20) and sizes (0.3 kpc < R V 25 < 10 kpc), although they are consistent in their irregular morphology. Their Hα luminosities (L(Hα) range from 10 36 to 10 41 ergs s −1 (corresponding to a range in star formation, using canonical prescriptions, from 10 −5 to 1 M yr −1 ). Although their optical colors are at the extreme blue edge for galaxies, they are similar to the colors of dwarf galaxies (van Zee 2001) and gas-rich irregulars . However, their star formation rates per unit stellar mass are a factor of ten less than other galaxies of the same baryonic mass, indicating that they are not simply quiescent versions of more active star forming galaxies. This paper presents the data, reduction techniques and new philosophy of data storage and presentation. Later papers in this series will explore the stellar population and star formation history of LSB galaxies using this dataset. arXiv:1109.2360v1 [astro-ph.CO] 11 Sep 2011 -2 -4449 (Huchra et al. 1983). The advent of newer all-sky surveys in the 1980's/90's demonstrated the importance of low surface brightness (LSB) galaxies to the galaxy population, and opened up a wider range of irregular late-type galaxies for study. Although initial suggestions were that LSB galaxies dominate the total galaxy population of the Universe over their higher surface brightness (HSB) cousins, it was later found to be untrue , Hayward, Irwin & Bergman 2005. Nonetheless, LSB galaxies offer a new avenue for the study of galaxy evolution, having low stellar densities and recent star formation rates. Their study, as a class of galaxies, has merit for stellar population work.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4202212" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="13a05772030ac1b1a0bb2666c0cfc4a1" rel="nofollow" data-download="{"attachment_id":31695943,"asset_id":4202212,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31695943/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="1005476" href="https://cambridge.academia.edu/TamelaMaciel">Tamela Maciel</a><script data-card-contents-for-user="1005476" type="text/json">{"id":1005476,"first_name":"Tamela","last_name":"Maciel","domain_name":"cambridge","page_name":"TamelaMaciel","display_name":"Tamela Maciel","profile_url":"https://cambridge.academia.edu/TamelaMaciel?f_ri=4363","photo":"https://0.academia-photos.com/1005476/1071423/6708788/s65_tamela.maciel.png"}</script></span></span></li><li class="js-paper-rank-work_4202212 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4202212"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4202212, container: ".js-paper-rank-work_4202212", }); 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$(".js-view-count[data-work-id=4202212]").text(description); $(".js-view-count-work_4202212").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4202212").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4202212"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">4</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="47599" rel="nofollow" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a>, <script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="587957" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_History">Star formation History</a>, <script data-card-contents-for-ri="587957" type="text/json">{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2509238" rel="nofollow" href="https://www.academia.edu/Documents/in/Integral_Field_Spectroscopy">Integral Field Spectroscopy</a><script data-card-contents-for-ri="2509238" type="text/json">{"id":2509238,"name":"Integral Field Spectroscopy","url":"https://www.academia.edu/Documents/in/Integral_Field_Spectroscopy?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4202212]'), work: {"id":4202212,"title":"Stellar Populations and the Star Formation Histories of LSB Galaxies: I. Optical and H-alpha Imaging","created_at":"2013-08-08T21:02:50.076-07:00","url":"https://www.academia.edu/4202212/Stellar_Populations_and_the_Star_Formation_Histories_of_LSB_Galaxies_I_Optical_and_H_alpha_Imaging?f_ri=4363","dom_id":"work_4202212","summary":"This paper presents optical and Hα imaging for a large sample of LSB galaxies selected from the PSS-II catalogs . As noted in previous work, LSB galaxies span a range of luminosities (−10 \u003e M V \u003e −20) and sizes (0.3 kpc \u003c R V 25 \u003c 10 kpc), although they are consistent in their irregular morphology. Their Hα luminosities (L(Hα) range from 10 36 to 10 41 ergs s −1 (corresponding to a range in star formation, using canonical prescriptions, from 10 −5 to 1 M yr −1 ). Although their optical colors are at the extreme blue edge for galaxies, they are similar to the colors of dwarf galaxies (van Zee 2001) and gas-rich irregulars . However, their star formation rates per unit stellar mass are a factor of ten less than other galaxies of the same baryonic mass, indicating that they are not simply quiescent versions of more active star forming galaxies. This paper presents the data, reduction techniques and new philosophy of data storage and presentation. Later papers in this series will explore the stellar population and star formation history of LSB galaxies using this dataset. arXiv:1109.2360v1 [astro-ph.CO] 11 Sep 2011 -2 -4449 (Huchra et al. 1983). The advent of newer all-sky surveys in the 1980's/90's demonstrated the importance of low surface brightness (LSB) galaxies to the galaxy population, and opened up a wider range of irregular late-type galaxies for study. Although initial suggestions were that LSB galaxies dominate the total galaxy population of the Universe over their higher surface brightness (HSB) cousins, it was later found to be untrue , Hayward, Irwin \u0026 Bergman 2005. Nonetheless, LSB galaxies offer a new avenue for the study of galaxy evolution, having low stellar densities and recent star formation rates. Their study, as a class of galaxies, has merit for stellar population work.","downloadable_attachments":[{"id":31695943,"asset_id":4202212,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":1005476,"first_name":"Tamela","last_name":"Maciel","domain_name":"cambridge","page_name":"TamelaMaciel","display_name":"Tamela Maciel","profile_url":"https://cambridge.academia.edu/TamelaMaciel?f_ri=4363","photo":"https://0.academia-photos.com/1005476/1071423/6708788/s65_tamela.maciel.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363","nofollow":true},{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363","nofollow":true},{"id":2509238,"name":"Integral Field Spectroscopy","url":"https://www.academia.edu/Documents/in/Integral_Field_Spectroscopy?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_6353792" data-work_id="6353792" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/6353792/Evolution_and_Nucleosynthesis_in_Low_Mass_Asymptotic_Giant_Branch_Stars_II_Neutron_Capture_and_the_s_Process">Evolution and Nucleosynthesis in Low-Mass Asymptotic Giant Branch Stars. II. Neutron Capture and the s-Process</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">New models of thermally pulsing asymptotic giant branch (TP-AGB) stars of low mass and solar chemical composition are presented, namely, Z \ 0.02, and Y \ 0.28. The inÑuence of 1 ¹ M/M _ ¹ 3, various parameters (such as the initial core... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_6353792" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">New models of thermally pulsing asymptotic giant branch (TP-AGB) stars of low mass and solar chemical composition are presented, namely, Z \ 0.02, and Y \ 0.28. The inÑuence of 1 ¹ M/M _ ¹ 3, various parameters (such as the initial core mass, the envelope mass, the mass-loss rate, the opacity, and the mixing length) on the properties of the models is discussed in detail. Our main Ðndings are the following :</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/6353792" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="215c9877fb665d5f794d9037bd31772a" rel="nofollow" data-download="{"attachment_id":48904802,"asset_id":6353792,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/48904802/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="9920134" href="https://cineca.academia.edu/ClaudioArlandini">Claudio Arlandini</a><script data-card-contents-for-user="9920134" type="text/json">{"id":9920134,"first_name":"Claudio","last_name":"Arlandini","domain_name":"cineca","page_name":"ClaudioArlandini","display_name":"Claudio Arlandini","profile_url":"https://cineca.academia.edu/ClaudioArlandini?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_6353792 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="6353792"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 6353792, container: ".js-paper-rank-work_6353792", }); 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$(".js-view-count[data-work-id=6353792]").text(description); $(".js-view-count-work_6353792").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_6353792").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="6353792"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">11</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="716" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium">Interstellar Medium</a>, <script data-card-contents-for-ri="716" type="text/json">{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a><script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=6353792]'), work: {"id":6353792,"title":"Evolution and Nucleosynthesis in Low-Mass Asymptotic Giant Branch Stars. II. Neutron Capture and the s-Process","created_at":"2014-03-09T23:17:34.347-07:00","url":"https://www.academia.edu/6353792/Evolution_and_Nucleosynthesis_in_Low_Mass_Asymptotic_Giant_Branch_Stars_II_Neutron_Capture_and_the_s_Process?f_ri=4363","dom_id":"work_6353792","summary":"New models of thermally pulsing asymptotic giant branch (TP-AGB) stars of low mass and solar chemical composition are presented, namely, Z \\ 0.02, and Y \\ 0.28. The inÑuence of 1 ¹ M/M _ ¹ 3, various parameters (such as the initial core mass, the envelope mass, the mass-loss rate, the opacity, and the mixing length) on the properties of the models is discussed in detail. Our main Ðndings are the following :","downloadable_attachments":[{"id":48904802,"asset_id":6353792,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":9920134,"first_name":"Claudio","last_name":"Arlandini","domain_name":"cineca","page_name":"ClaudioArlandini","display_name":"Claudio Arlandini","profile_url":"https://cineca.academia.edu/ClaudioArlandini?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":230832,"name":"Nuclear Reactions","url":"https://www.academia.edu/Documents/in/Nuclear_Reactions?f_ri=4363"},{"id":309434,"name":"Solar System","url":"https://www.academia.edu/Documents/in/Solar_System?f_ri=4363"},{"id":550856,"name":"AGB stars","url":"https://www.academia.edu/Documents/in/AGB_stars?f_ri=4363"},{"id":772972,"name":"Chemical Composition","url":"https://www.academia.edu/Documents/in/Chemical_Composition?f_ri=4363"},{"id":963709,"name":"Mass Loss","url":"https://www.academia.edu/Documents/in/Mass_Loss?f_ri=4363"},{"id":1993786,"name":"Cumulant","url":"https://www.academia.edu/Documents/in/Cumulant?f_ri=4363"},{"id":2504124,"name":"Nucleosynthesis","url":"https://www.academia.edu/Documents/in/Nucleosynthesis?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_14495755" data-work_id="14495755" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/14495755/When_is_star_formation_episodic_A_delay_differential_equation_negative_feedback_model">When is star formation episodic? A delay differential equation `negative feedback' model</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We introduce a differential equation for star formation in galaxies that incorporates negative feedback with a delay. When the feedback is instantaneous, solutions approach a self-limiting equilibrium state. When there is a delay, even... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_14495755" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We introduce a differential equation for star formation in galaxies that incorporates negative feedback with a delay. When the feedback is instantaneous, solutions approach a self-limiting equilibrium state. When there is a delay, even though the feedback is negative, the solutions can exhibit cyclic and episodic solutions. We find that periodic or episodic star formation only occurs when two conditions</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/14495755" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="65a24ed2fd8966787b2b94d413567f97" rel="nofollow" data-download="{"attachment_id":38329089,"asset_id":14495755,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/38329089/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="33442227" href="https://rochester.academia.edu/AliceCQuillen">Alice C. Quillen</a><script data-card-contents-for-user="33442227" type="text/json">{"id":33442227,"first_name":"Alice C.","last_name":"Quillen","domain_name":"rochester","page_name":"AliceCQuillen","display_name":"Alice C. Quillen","profile_url":"https://rochester.academia.edu/AliceCQuillen?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_14495755 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="14495755"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 14495755, container: ".js-paper-rank-work_14495755", }); });</script></li><li class="js-percentile-work_14495755 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 14495755; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_14495755"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_14495755 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="14495755"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 14495755; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=14495755]").text(description); $(".js-view-count-work_14495755").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_14495755").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="14495755"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a>, <script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="51901" rel="nofollow" href="https://www.academia.edu/Documents/in/Time-Delay_Systems">Time-Delay Systems</a>, <script data-card-contents-for-ri="51901" type="text/json">{"id":51901,"name":"Time-Delay Systems","url":"https://www.academia.edu/Documents/in/Time-Delay_Systems?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="84487" rel="nofollow" href="https://www.academia.edu/Documents/in/Delay_Differential_Equation">Delay Differential Equation</a><script data-card-contents-for-ri="84487" type="text/json">{"id":84487,"name":"Delay Differential Equation","url":"https://www.academia.edu/Documents/in/Delay_Differential_Equation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=14495755]'), work: {"id":14495755,"title":"When is star formation episodic? A delay differential equation `negative feedback' model","created_at":"2015-07-29T14:04:43.464-07:00","url":"https://www.academia.edu/14495755/When_is_star_formation_episodic_A_delay_differential_equation_negative_feedback_model?f_ri=4363","dom_id":"work_14495755","summary":"We introduce a differential equation for star formation in galaxies that incorporates negative feedback with a delay. When the feedback is instantaneous, solutions approach a self-limiting equilibrium state. When there is a delay, even though the feedback is negative, the solutions can exhibit cyclic and episodic solutions. We find that periodic or episodic star formation only occurs when two conditions","downloadable_attachments":[{"id":38329089,"asset_id":14495755,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":33442227,"first_name":"Alice C.","last_name":"Quillen","domain_name":"rochester","page_name":"AliceCQuillen","display_name":"Alice C. Quillen","profile_url":"https://rochester.academia.edu/AliceCQuillen?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":51901,"name":"Time-Delay Systems","url":"https://www.academia.edu/Documents/in/Time-Delay_Systems?f_ri=4363","nofollow":true},{"id":84487,"name":"Delay Differential Equation","url":"https://www.academia.edu/Documents/in/Delay_Differential_Equation?f_ri=4363","nofollow":true},{"id":110294,"name":"Negative Feedback","url":"https://www.academia.edu/Documents/in/Negative_Feedback?f_ri=4363"},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363"},{"id":174781,"name":"Oscillations","url":"https://www.academia.edu/Documents/in/Oscillations?f_ri=4363"},{"id":679783,"name":"Boolean Satisfiability","url":"https://www.academia.edu/Documents/in/Boolean_Satisfiability?f_ri=4363"},{"id":765146,"name":"Differential equation","url":"https://www.academia.edu/Documents/in/Differential_equation?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_20953653" data-work_id="20953653" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/20953653/Deuterium_astration_in_the_local_disc_and_beyond">Deuterium astration in the local disc and beyond</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Estimates of the interstellar deuterium abundance span a wide range of values. Until recently, it was customary to adopt the abundance of deuterium measured in the Local Bubble as representative of the local one. Now, it is becoming... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_20953653" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Estimates of the interstellar deuterium abundance span a wide range of values. Until recently, it was customary to adopt the abundance of deuterium measured in the Local Bubble as representative of the local one. Now, it is becoming unclear whether the true local deuterium abundance is significantly higher or lower than this value, depending on the interpretation given to current data. It is important to deal with the issue of the deuterium variation and see whether it challenges our current understanding of the Galaxy evolution. To this aim, we study the evolution of deuterium in the framework of successful models for the chemical evolution of the Milky Way able to reproduce the majority of the observational constraints for the solar neighbourhood and for the Galactic disc. We show that, in the framework of our models, the lowest D/H values observed locally cannot be explained in terms of simple astration processes occurring during the Galaxy evolution. Indeed, the combination of a mild star formation and a continuous infall of unprocessed gas required to fit all the available observational data allows only a modest variation of the deuterium abundance from its primordial value. Therefore, we suggest that depletion of deuterium on to dust grains is the most likely physical mechanism proposed so far to explain the observed dispersion in the local data.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/20953653" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="9064f9761e99af5c6c16dbf4a1473d09" rel="nofollow" data-download="{"attachment_id":41643709,"asset_id":20953653,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/41643709/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="42211319" href="https://units.academia.edu/FrancescaMatteucci">Francesca Matteucci</a><script data-card-contents-for-user="42211319" type="text/json">{"id":42211319,"first_name":"Francesca","last_name":"Matteucci","domain_name":"units","page_name":"FrancescaMatteucci","display_name":"Francesca Matteucci","profile_url":"https://units.academia.edu/FrancescaMatteucci?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_20953653 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="20953653"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 20953653, container: ".js-paper-rank-work_20953653", }); });</script></li><li class="js-percentile-work_20953653 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 20953653; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_20953653"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_20953653 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="20953653"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 20953653; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=20953653]").text(description); $(".js-view-count-work_20953653").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_20953653").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="20953653"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="14920" rel="nofollow" href="https://www.academia.edu/Documents/in/Chemical_Evolution">Chemical Evolution</a>, <script data-card-contents-for-ri="14920" type="text/json">{"id":14920,"name":"Chemical Evolution","url":"https://www.academia.edu/Documents/in/Chemical_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="97563" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_evolution">Galaxy evolution</a>, <script data-card-contents-for-ri="97563" type="text/json">{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="162319" rel="nofollow" href="https://www.academia.edu/Documents/in/Milky_Way">Milky Way</a><script data-card-contents-for-ri="162319" type="text/json">{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=20953653]'), work: {"id":20953653,"title":"Deuterium astration in the local disc and beyond","created_at":"2016-01-27T08:24:17.433-08:00","url":"https://www.academia.edu/20953653/Deuterium_astration_in_the_local_disc_and_beyond?f_ri=4363","dom_id":"work_20953653","summary":"Estimates of the interstellar deuterium abundance span a wide range of values. Until recently, it was customary to adopt the abundance of deuterium measured in the Local Bubble as representative of the local one. Now, it is becoming unclear whether the true local deuterium abundance is significantly higher or lower than this value, depending on the interpretation given to current data. It is important to deal with the issue of the deuterium variation and see whether it challenges our current understanding of the Galaxy evolution. To this aim, we study the evolution of deuterium in the framework of successful models for the chemical evolution of the Milky Way able to reproduce the majority of the observational constraints for the solar neighbourhood and for the Galactic disc. We show that, in the framework of our models, the lowest D/H values observed locally cannot be explained in terms of simple astration processes occurring during the Galaxy evolution. Indeed, the combination of a mild star formation and a continuous infall of unprocessed gas required to fit all the available observational data allows only a modest variation of the deuterium abundance from its primordial value. Therefore, we suggest that depletion of deuterium on to dust grains is the most likely physical mechanism proposed so far to explain the observed dispersion in the local data.","downloadable_attachments":[{"id":41643709,"asset_id":20953653,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":42211319,"first_name":"Francesca","last_name":"Matteucci","domain_name":"units","page_name":"FrancescaMatteucci","display_name":"Francesca Matteucci","profile_url":"https://units.academia.edu/FrancescaMatteucci?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":14920,"name":"Chemical Evolution","url":"https://www.academia.edu/Documents/in/Chemical_Evolution?f_ri=4363","nofollow":true},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363","nofollow":true},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363","nofollow":true},{"id":1196781,"name":"Solar Neighbourhood","url":"https://www.academia.edu/Documents/in/Solar_Neighbourhood?f_ri=4363"},{"id":1706299,"name":"Local Bubble","url":"https://www.academia.edu/Documents/in/Local_Bubble?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_19289093 coauthored" data-work_id="19289093" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/19289093/AMAZE">AMAZE</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We present initial results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z>3 by means of deep near-IR spectroscopy. Gas metallicities are measured, for an initial sample of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_19289093" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present initial results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z>3 by means of deep near-IR spectroscopy. Gas metallicities are measured, for an initial sample of nine star forming galaxies at z∼3.5, by means of optical nebular lines redshifted into the near-IR. Stellar masses are accurately determined by using Spitzer-IRAC data, which sample the rest-frame near-IR stellar light in these distant galaxies. When compared with previous surveys, the mass-metallicity relation inferred at z∼3.5 shows an evolution much stronger than observed at lower redshifts. The evolution is prominent even in massive galaxies, indicating that z∼3 is an epoch of major action in terms of star formation and metal enrichment also for massive systems. There are also indications that the metallicity evolution of low mass galaxies is stronger relative to high mass systems, an effect which can be considered the chemical version of the galaxy downsizing. The mass-metallicity relation observed at z∼3.5 is difficult to reconcile with the predictions of some hierarchical evolutionary models. Such discrepancies suggest that at z>3 galaxies are assembled mostly with relatively un-evolved sub-units, i.e. small galaxies with low star formation efficiency. The bulk of the star formation and metallicity evolution probably occurs once small galaxies are already assembled into bigger systems.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/19289093" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="b09bb0e79ce6a315eb447940206d4ecd" rel="nofollow" data-download="{"attachment_id":42226930,"asset_id":19289093,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/42226930/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="39545396" href="https://units.academia.edu/SilviaBallero">Silvia K Ballero</a><script data-card-contents-for-user="39545396" type="text/json">{"id":39545396,"first_name":"Silvia","last_name":"Ballero","domain_name":"units","page_name":"SilviaBallero","display_name":"Silvia K Ballero","profile_url":"https://units.academia.edu/SilviaBallero?f_ri=4363","photo":"https://0.academia-photos.com/39545396/10882007/12144254/s65_silvia.ballero.jpg"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-19289093">+3</span><div class="hidden js-additional-users-19289093"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://units.academia.edu/FrancescaMatteucci">Francesca Matteucci</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/AndreaGrazian">Andrea Grazian</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://inaf.academia.edu/LauraSilva">Laura Silva</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-19289093'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-19289093').html(); 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container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_19289093 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="19289093"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 19289093; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=19289093]").text(description); $(".js-view-count-work_19289093").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_19289093").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="19289093"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a>, <script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a>, <script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="188982" rel="nofollow" href="https://www.academia.edu/Documents/in/High_redshift_galaxies_and_quasars">High redshift galaxies and quasars</a><script data-card-contents-for-ri="188982" type="text/json">{"id":188982,"name":"High redshift galaxies and quasars","url":"https://www.academia.edu/Documents/in/High_redshift_galaxies_and_quasars?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=19289093]'), work: {"id":19289093,"title":"AMAZE","created_at":"2015-12-01T06:07:07.907-08:00","url":"https://www.academia.edu/19289093/AMAZE?f_ri=4363","dom_id":"work_19289093","summary":"We present initial results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z\u003e3 by means of deep near-IR spectroscopy. Gas metallicities are measured, for an initial sample of nine star forming galaxies at z∼3.5, by means of optical nebular lines redshifted into the near-IR. Stellar masses are accurately determined by using Spitzer-IRAC data, which sample the rest-frame near-IR stellar light in these distant galaxies. When compared with previous surveys, the mass-metallicity relation inferred at z∼3.5 shows an evolution much stronger than observed at lower redshifts. The evolution is prominent even in massive galaxies, indicating that z∼3 is an epoch of major action in terms of star formation and metal enrichment also for massive systems. There are also indications that the metallicity evolution of low mass galaxies is stronger relative to high mass systems, an effect which can be considered the chemical version of the galaxy downsizing. The mass-metallicity relation observed at z∼3.5 is difficult to reconcile with the predictions of some hierarchical evolutionary models. Such discrepancies suggest that at z\u003e3 galaxies are assembled mostly with relatively un-evolved sub-units, i.e. small galaxies with low star formation efficiency. The bulk of the star formation and metallicity evolution probably occurs once small galaxies are already assembled into bigger systems.","downloadable_attachments":[{"id":42226930,"asset_id":19289093,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":39545396,"first_name":"Silvia","last_name":"Ballero","domain_name":"units","page_name":"SilviaBallero","display_name":"Silvia K Ballero","profile_url":"https://units.academia.edu/SilviaBallero?f_ri=4363","photo":"https://0.academia-photos.com/39545396/10882007/12144254/s65_silvia.ballero.jpg"},{"id":42211319,"first_name":"Francesca","last_name":"Matteucci","domain_name":"units","page_name":"FrancescaMatteucci","display_name":"Francesca Matteucci","profile_url":"https://units.academia.edu/FrancescaMatteucci?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":37774842,"first_name":"Andrea","last_name":"Grazian","domain_name":"independent","page_name":"AndreaGrazian","display_name":"Andrea Grazian","profile_url":"https://independent.academia.edu/AndreaGrazian?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":1120980,"first_name":"Laura","last_name":"Silva","domain_name":"inaf","page_name":"LauraSilva","display_name":"Laura Silva","profile_url":"https://inaf.academia.edu/LauraSilva?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":188982,"name":"High redshift galaxies and quasars","url":"https://www.academia.edu/Documents/in/High_redshift_galaxies_and_quasars?f_ri=4363","nofollow":true},{"id":448421,"name":"IR Spectroscopy","url":"https://www.academia.edu/Documents/in/IR_Spectroscopy?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_69346844" data-work_id="69346844" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/69346844/Superclusters_of_galaxies_in_the_2dF_redshift_survey_3_The_properties_of_galaxies_in_superclusters">Superclusters of galaxies in the 2dF redshift survey. 3. The properties of galaxies in superclusters</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Context. Superclusters are the largest systems in the Universe to give us information about the very early Universe. Our present series of papers is devoted to the study of the properties of superclusters of galaxies from the 2dF Galaxy... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_69346844" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Context. Superclusters are the largest systems in the Universe to give us information about the very early Universe. Our present series of papers is devoted to the study of the properties of superclusters of galaxies from the 2dF Galaxy Redshift survey. Aims. We use catalogues of superclusters of galaxies from the 2dF Galaxy Redshift Survey to compare the properties of rich and poor superclusters. In particular, we study the properties of galaxies (spectral types, colours, and luminosities) in superclusters. Methods. We compare the distribution of densities in rich and poor superclusters, and the properties of galaxies in high and lowdensity regions of rich superclusters, in poor superclusters, and in the field. In superclusters and in the field, we also compare the properties of galaxies in groups, and the properties of those galaxies which do not belong to any group. Results. We show that in rich superclusters the values of the luminosity density smoothed on a scale of 8 h −1 Mpc are higher than in poor superclusters: the median density in rich superclusters is δ ≈ 7.5 and in poor superclusters δ ≈ 6.0. Rich superclusters contain high-density cores with densities δ > 10, while in poor superclusters such high-density cores are absent. The properties of galaxies in rich and poor superclusters and in the field are different: the fraction of early type, passive galaxies in rich superclusters is slightly higher than in poor superclusters, and is the lowest among the field galaxies. Most importantly, in high-density cores of rich superclusters (δ > 10), there is an excess of early type, passive galaxies in groups and clusters, as well as among those which do not belong to any group. The main galaxies of superclusters have a rather limited range of absolute magnitudes. The main galaxies of rich superclusters have higher luminosities than those of poor superclusters and of groups in the field. Conclusions. Our results show that both the local (group/cluster) environments and global (supercluster) environments influence galaxy morphologies and their star formation activity.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/69346844" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="e59d3ba0e60150cb2fd9dc82c6f02969" rel="nofollow" data-download="{"attachment_id":79478690,"asset_id":69346844,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/79478690/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="35571483" href="https://ut-ee.academia.edu/ESaar">E. Saar</a><script data-card-contents-for-user="35571483" type="text/json">{"id":35571483,"first_name":"E.","last_name":"Saar","domain_name":"ut-ee","page_name":"ESaar","display_name":"E. Saar","profile_url":"https://ut-ee.academia.edu/ESaar?f_ri=4363","photo":"https://0.academia-photos.com/35571483/136546297/126000149/s65_e..saar.jpg"}</script></span></span></li><li class="js-paper-rank-work_69346844 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="69346844"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 69346844, container: ".js-paper-rank-work_69346844", }); });</script></li><li class="js-percentile-work_69346844 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 69346844; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_69346844"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_69346844 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="69346844"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 69346844; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=69346844]").text(description); $(".js-view-count-work_69346844").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_69346844").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="69346844"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="7936" rel="nofollow" href="https://www.academia.edu/Documents/in/Quantum_Mechanics">Quantum Mechanics</a>, <script data-card-contents-for-ri="7936" type="text/json">{"id":7936,"name":"Quantum Mechanics","url":"https://www.academia.edu/Documents/in/Quantum_Mechanics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="47598" rel="nofollow" href="https://www.academia.edu/Documents/in/Cosmology">Cosmology</a>, <script data-card-contents-for-ri="47598" type="text/json">{"id":47598,"name":"Cosmology","url":"https://www.academia.edu/Documents/in/Cosmology?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1276871" rel="nofollow" href="https://www.academia.edu/Documents/in/Astronomy_and_Astrophysics-1">Astronomy & Astrophysics</a><script data-card-contents-for-ri="1276871" type="text/json">{"id":1276871,"name":"Astronomy \u0026 Astrophysics","url":"https://www.academia.edu/Documents/in/Astronomy_and_Astrophysics-1?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=69346844]'), work: {"id":69346844,"title":"Superclusters of galaxies in the 2dF redshift survey. 3. The properties of galaxies in superclusters","created_at":"2022-01-24T04:46:01.291-08:00","url":"https://www.academia.edu/69346844/Superclusters_of_galaxies_in_the_2dF_redshift_survey_3_The_properties_of_galaxies_in_superclusters?f_ri=4363","dom_id":"work_69346844","summary":"Context. Superclusters are the largest systems in the Universe to give us information about the very early Universe. Our present series of papers is devoted to the study of the properties of superclusters of galaxies from the 2dF Galaxy Redshift survey. Aims. We use catalogues of superclusters of galaxies from the 2dF Galaxy Redshift Survey to compare the properties of rich and poor superclusters. In particular, we study the properties of galaxies (spectral types, colours, and luminosities) in superclusters. Methods. We compare the distribution of densities in rich and poor superclusters, and the properties of galaxies in high and lowdensity regions of rich superclusters, in poor superclusters, and in the field. In superclusters and in the field, we also compare the properties of galaxies in groups, and the properties of those galaxies which do not belong to any group. Results. We show that in rich superclusters the values of the luminosity density smoothed on a scale of 8 h −1 Mpc are higher than in poor superclusters: the median density in rich superclusters is δ ≈ 7.5 and in poor superclusters δ ≈ 6.0. Rich superclusters contain high-density cores with densities δ \u003e 10, while in poor superclusters such high-density cores are absent. The properties of galaxies in rich and poor superclusters and in the field are different: the fraction of early type, passive galaxies in rich superclusters is slightly higher than in poor superclusters, and is the lowest among the field galaxies. Most importantly, in high-density cores of rich superclusters (δ \u003e 10), there is an excess of early type, passive galaxies in groups and clusters, as well as among those which do not belong to any group. The main galaxies of superclusters have a rather limited range of absolute magnitudes. The main galaxies of rich superclusters have higher luminosities than those of poor superclusters and of groups in the field. Conclusions. Our results show that both the local (group/cluster) environments and global (supercluster) environments influence galaxy morphologies and their star formation activity.","downloadable_attachments":[{"id":79478690,"asset_id":69346844,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":35571483,"first_name":"E.","last_name":"Saar","domain_name":"ut-ee","page_name":"ESaar","display_name":"E. Saar","profile_url":"https://ut-ee.academia.edu/ESaar?f_ri=4363","photo":"https://0.academia-photos.com/35571483/136546297/126000149/s65_e..saar.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":7936,"name":"Quantum Mechanics","url":"https://www.academia.edu/Documents/in/Quantum_Mechanics?f_ri=4363","nofollow":true},{"id":47598,"name":"Cosmology","url":"https://www.academia.edu/Documents/in/Cosmology?f_ri=4363","nofollow":true},{"id":1276871,"name":"Astronomy \u0026 Astrophysics","url":"https://www.academia.edu/Documents/in/Astronomy_and_Astrophysics-1?f_ri=4363","nofollow":true},{"id":3443535,"name":"High density","url":"https://www.academia.edu/Documents/in/High_density?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_33641931" data-work_id="33641931" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/33641931/IAC_STAR_A_Code_for_Synthetic_Color_Magnitude_Diagram_Computation">IAC-STAR: A Code for Synthetic Color-Magnitude Diagram Computation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The code IAC-star is presented. It generates synthetic HR and colormagnitude diagrams (CMDs) and is mainly aimed to star formation history studies in nearby galaxies. Composite stellar populations are calculated on a star by star basis,... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_33641931" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The code IAC-star is presented. It generates synthetic HR and colormagnitude diagrams (CMDs) and is mainly aimed to star formation history studies in nearby galaxies. Composite stellar populations are calculated on a star by star basis, by computing the luminosity, effective temperature and gravity of each star by direct bi-logarithmic interpolation in the metallicity and age grid of a library of stellar evolution tracks. Visual (broad band and HST) and infrared magnitudes are also provided for each star after applying bolometric corrections. The Padua and Teramo (Pietrinferni et al. 2004) stellar evolution libraries and various bolometric corrections libraries are used in the current version. A variety of star formation rate functions, initial mass functions and chemical enrichment laws are allowed and binary stars can be computed. Although the main motivation of the code is the computation of synthetic CMDs, it also provides integrated masses, luminosities and magnitudes as well as surface brightness fluctuation luminosities and magnitudes for the total synthetic stellar population, and therefore it can also be used for population synthesis research.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/33641931" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="131b05ad53964428316c08d208605e4a" rel="nofollow" data-download="{"attachment_id":53653741,"asset_id":33641931,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/53653741/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="884430" href="https://girona.academia.edu/CarmeTimonedaGallart">Carme Timoneda-Gallart</a><script data-card-contents-for-user="884430" type="text/json">{"id":884430,"first_name":"Carme","last_name":"Timoneda-Gallart","domain_name":"girona","page_name":"CarmeTimonedaGallart","display_name":"Carme Timoneda-Gallart","profile_url":"https://girona.academia.edu/CarmeTimonedaGallart?f_ri=4363","photo":"https://0.academia-photos.com/884430/19168933/19114978/s65_carme.timoneda-gallart.jpg"}</script></span></span></li><li class="js-paper-rank-work_33641931 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="33641931"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 33641931, container: ".js-paper-rank-work_33641931", }); 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$(".js-view-count[data-work-id=33641931]").text(description); $(".js-view-count-work_33641931").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_33641931").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="33641931"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="712" rel="nofollow" href="https://www.academia.edu/Documents/in/Stellar_Evolution">Stellar Evolution</a>, <script data-card-contents-for-ri="712" type="text/json">{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="335361" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared">Infrared</a>, <script data-card-contents-for-ri="335361" type="text/json">{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="587957" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_History">Star formation History</a><script data-card-contents-for-ri="587957" type="text/json">{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=33641931]'), work: {"id":33641931,"title":"IAC-STAR: A Code for Synthetic Color-Magnitude Diagram Computation","created_at":"2017-06-25T03:49:52.066-07:00","url":"https://www.academia.edu/33641931/IAC_STAR_A_Code_for_Synthetic_Color_Magnitude_Diagram_Computation?f_ri=4363","dom_id":"work_33641931","summary":"The code IAC-star is presented. It generates synthetic HR and colormagnitude diagrams (CMDs) and is mainly aimed to star formation history studies in nearby galaxies. Composite stellar populations are calculated on a star by star basis, by computing the luminosity, effective temperature and gravity of each star by direct bi-logarithmic interpolation in the metallicity and age grid of a library of stellar evolution tracks. Visual (broad band and HST) and infrared magnitudes are also provided for each star after applying bolometric corrections. The Padua and Teramo (Pietrinferni et al. 2004) stellar evolution libraries and various bolometric corrections libraries are used in the current version. A variety of star formation rate functions, initial mass functions and chemical enrichment laws are allowed and binary stars can be computed. Although the main motivation of the code is the computation of synthetic CMDs, it also provides integrated masses, luminosities and magnitudes as well as surface brightness fluctuation luminosities and magnitudes for the total synthetic stellar population, and therefore it can also be used for population synthesis research.","downloadable_attachments":[{"id":53653741,"asset_id":33641931,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":884430,"first_name":"Carme","last_name":"Timoneda-Gallart","domain_name":"girona","page_name":"CarmeTimonedaGallart","display_name":"Carme Timoneda-Gallart","profile_url":"https://girona.academia.edu/CarmeTimonedaGallart?f_ri=4363","photo":"https://0.academia-photos.com/884430/19168933/19114978/s65_carme.timoneda-gallart.jpg"}],"research_interests":[{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true},{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363","nofollow":true},{"id":1181250,"name":"Hubble Space Telescope Images","url":"https://www.academia.edu/Documents/in/Hubble_Space_Telescope_Images?f_ri=4363"},{"id":1460347,"name":"Astronomical","url":"https://www.academia.edu/Documents/in/Astronomical?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_50063190" data-work_id="50063190" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/50063190/The_bulk_of_the_cosmic_infrared_background_resolved_by_ISOCAM">The bulk of the cosmic infrared background resolved by ISOCAM</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Deep extragalactic surveys with ISOCAM revealed the presence of a large density of faint mid-infrared (MIR) sources. We have computed the 15 µm integrated galaxy light produced by these galaxies above a sensitivity limit of 50 µJy. It... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_50063190" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Deep extragalactic surveys with ISOCAM revealed the presence of a large density of faint mid-infrared (MIR) sources. We have computed the 15 µm integrated galaxy light produced by these galaxies above a sensitivity limit of 50 µJy. It sets a lower limit to the 15 µm extragalactic background light of (2.4 ± 0.5) nW m −2 sr −1. The redshift distribution of the ISOCAM galaxies is inferred from the spectroscopically complete sample of galaxies in the Hubble Deep Field North (HDFN). It peaks around z ∼ 0.8 in agreement with studies in other fields. The rest-frame 15 µm and bolometric infrared (8-1000 µm) luminosities of ISOCAM galaxies are computed using the correlations that we establish between the 6.75, 12, 15 µm and infrared (IR) luminosities of local galaxies. The resulting IR luminosities were double-checked using radio (1.4 GHz) flux densities from the ultra-deep VLA and WSRT surveys of the HDFN on a sample of 24 galaxies as well as on a sample of 109 local galaxies in common between ISOCAM and the NRAO VLA Sky Survey (NVSS). This comparison shows for the first time that MIR and radio luminosities correlate up to z ∼ 1. This result validates the bolometric IR luminosities derived from MIR luminosities unless both the radio-far infrared (FIR) and the MIR-FIR correlations become invalid around z ∼ 1. The fraction of IR light produced by active nuclei was computed from the cross-correlation with the deepest X-ray surveys from the Chandra and XMM-Newton observatories in the HDFN and Lockman Hole respectively. We find that at most 20% of the 15 µm integrated galaxy light is due to active galactic nuclei (AGNs) unless a large population of AGNs was missed by Chandra and XMM-Newton. About 75% of the ISOCAM galaxies are found to belong to the class of luminous infrared galaxies (LIR ≥ 10 11 L). They exhibit star formation rates of the order of ∼100 M yr −1. The comoving density of infrared light due to these luminous IR galaxies was more than 40 times larger at z ∼ 1 than today. The contribution of ISOCAM galaxies to the peak of the cosmic infrared background (CIRB) at 140 µm was computed from the MIR-FIR correlations for star forming galaxies and from the spectral energy distribution of the Seyfert 2, NGC 1068, for AGNs. We find that the galaxies unveiled by ISOCAM surveys are responsible for the bulk of the CIRB, i.e. (16 ± 5) nW m −2 sr −1 as compared to the (25 ± 7) nW m −2 sr −1 measured with the COBE satellite, with less than 10% due to AGNs. Since the CIRB contains most of the light radiated over the history of star formation in the universe, this means that a large fraction of present-day stars must have formed during a dusty starburst event similar to those revealed by ISOCAM.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/50063190" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="5c0b37abda1301a55c03b7819565a938" rel="nofollow" data-download="{"attachment_id":68187016,"asset_id":50063190,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/68187016/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="3786838" href="https://independent.academia.edu/AlbertoFranceschini">Alberto Franceschini</a><script data-card-contents-for-user="3786838" type="text/json">{"id":3786838,"first_name":"Alberto","last_name":"Franceschini","domain_name":"independent","page_name":"AlbertoFranceschini","display_name":"Alberto Franceschini","profile_url":"https://independent.academia.edu/AlbertoFranceschini?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_50063190 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="50063190"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 50063190, container: ".js-paper-rank-work_50063190", }); 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$(".js-view-count[data-work-id=50063190]").text(description); $(".js-view-count-work_50063190").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_50063190").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="50063190"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">15</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4742" rel="nofollow" href="https://www.academia.edu/Documents/in/Active_Galactic_Nuclei">Active Galactic Nuclei</a>, <script data-card-contents-for-ri="4742" type="text/json">{"id":4742,"name":"Active Galactic Nuclei","url":"https://www.academia.edu/Documents/in/Active_Galactic_Nuclei?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="5554" rel="nofollow" href="https://www.academia.edu/Documents/in/Luminous_Infrared_Galaxies">Luminous Infrared Galaxies</a>, <script data-card-contents-for-ri="5554" type="text/json">{"id":5554,"name":"Luminous Infrared Galaxies","url":"https://www.academia.edu/Documents/in/Luminous_Infrared_Galaxies?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a><script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=50063190]'), work: {"id":50063190,"title":"The bulk of the cosmic infrared background resolved by ISOCAM","created_at":"2021-07-19T00:20:44.206-07:00","url":"https://www.academia.edu/50063190/The_bulk_of_the_cosmic_infrared_background_resolved_by_ISOCAM?f_ri=4363","dom_id":"work_50063190","summary":"Deep extragalactic surveys with ISOCAM revealed the presence of a large density of faint mid-infrared (MIR) sources. We have computed the 15 µm integrated galaxy light produced by these galaxies above a sensitivity limit of 50 µJy. It sets a lower limit to the 15 µm extragalactic background light of (2.4 ± 0.5) nW m −2 sr −1. The redshift distribution of the ISOCAM galaxies is inferred from the spectroscopically complete sample of galaxies in the Hubble Deep Field North (HDFN). It peaks around z ∼ 0.8 in agreement with studies in other fields. The rest-frame 15 µm and bolometric infrared (8-1000 µm) luminosities of ISOCAM galaxies are computed using the correlations that we establish between the 6.75, 12, 15 µm and infrared (IR) luminosities of local galaxies. The resulting IR luminosities were double-checked using radio (1.4 GHz) flux densities from the ultra-deep VLA and WSRT surveys of the HDFN on a sample of 24 galaxies as well as on a sample of 109 local galaxies in common between ISOCAM and the NRAO VLA Sky Survey (NVSS). This comparison shows for the first time that MIR and radio luminosities correlate up to z ∼ 1. This result validates the bolometric IR luminosities derived from MIR luminosities unless both the radio-far infrared (FIR) and the MIR-FIR correlations become invalid around z ∼ 1. The fraction of IR light produced by active nuclei was computed from the cross-correlation with the deepest X-ray surveys from the Chandra and XMM-Newton observatories in the HDFN and Lockman Hole respectively. We find that at most 20% of the 15 µm integrated galaxy light is due to active galactic nuclei (AGNs) unless a large population of AGNs was missed by Chandra and XMM-Newton. About 75% of the ISOCAM galaxies are found to belong to the class of luminous infrared galaxies (LIR ≥ 10 11 L). They exhibit star formation rates of the order of ∼100 M yr −1. The comoving density of infrared light due to these luminous IR galaxies was more than 40 times larger at z ∼ 1 than today. The contribution of ISOCAM galaxies to the peak of the cosmic infrared background (CIRB) at 140 µm was computed from the MIR-FIR correlations for star forming galaxies and from the spectral energy distribution of the Seyfert 2, NGC 1068, for AGNs. We find that the galaxies unveiled by ISOCAM surveys are responsible for the bulk of the CIRB, i.e. (16 ± 5) nW m −2 sr −1 as compared to the (25 ± 7) nW m −2 sr −1 measured with the COBE satellite, with less than 10% due to AGNs. Since the CIRB contains most of the light radiated over the history of star formation in the universe, this means that a large fraction of present-day stars must have formed during a dusty starburst event similar to those revealed by ISOCAM.","downloadable_attachments":[{"id":68187016,"asset_id":50063190,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":3786838,"first_name":"Alberto","last_name":"Franceschini","domain_name":"independent","page_name":"AlbertoFranceschini","display_name":"Alberto Franceschini","profile_url":"https://independent.academia.edu/AlbertoFranceschini?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4742,"name":"Active Galactic Nuclei","url":"https://www.academia.edu/Documents/in/Active_Galactic_Nuclei?f_ri=4363","nofollow":true},{"id":5554,"name":"Luminous Infrared Galaxies","url":"https://www.academia.edu/Documents/in/Luminous_Infrared_Galaxies?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=4363"},{"id":58703,"name":"Cross Correlation","url":"https://www.academia.edu/Documents/in/Cross_Correlation?f_ri=4363"},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":106861,"name":"Dwarf Galaxies","url":"https://www.academia.edu/Documents/in/Dwarf_Galaxies?f_ri=4363"},{"id":249893,"name":"Mid-Infrared","url":"https://www.academia.edu/Documents/in/Mid-Infrared?f_ri=4363"},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363"},{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363"},{"id":977447,"name":"Starburst Galaxies","url":"https://www.academia.edu/Documents/in/Starburst_Galaxies?f_ri=4363"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=4363"},{"id":2599525,"name":"present day","url":"https://www.academia.edu/Documents/in/present_day?f_ri=4363"},{"id":3660251,"name":"Extragalactic Background Light","url":"https://www.academia.edu/Documents/in/Extragalactic_Background_Light?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_18310626 coauthored" data-work_id="18310626" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/18310626/Cosmic_reionization_by_stellar_sources_Population_II_stars">Cosmic reionization by stellar sources: Population II stars</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We study the reionisation of the Universe by stellar sources using a numerical approach that combines fast 3D radiative transfer calculations with high resolution hydrodynamical simulations. By supplementing a one-step radiative transfer... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_18310626" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We study the reionisation of the Universe by stellar sources using a numerical approach that combines fast 3D radiative transfer calculations with high resolution hydrodynamical simulations. By supplementing a one-step radiative transfer code specifically designed for following ionisation processes with an adaptive ray-tracing algorithm, we are able to significantly speed up the calculations to the point where handling a vast number of sources becomes technically feasible. This allows us to study how dim low-mass sources, excluded in previous investigations owing to computational limitations, affect the morphological evolution of the reionisation process.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/18310626" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a7db3cbd36f3b379004af683b399a5e0" rel="nofollow" data-download="{"attachment_id":39987508,"asset_id":18310626,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/39987508/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="38297020" href="https://independent.academia.edu/YoshidaNaoki">Naoki Yoshida</a><script data-card-contents-for-user="38297020" type="text/json">{"id":38297020,"first_name":"Naoki","last_name":"Yoshida","domain_name":"independent","page_name":"YoshidaNaoki","display_name":"Naoki Yoshida","profile_url":"https://independent.academia.edu/YoshidaNaoki?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-18310626">+1</span><div class="hidden js-additional-users-18310626"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://harvard.academia.edu/AaronSokasian">Aaron Sokasian</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-18310626'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-18310626').html(); 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By supplementing a one-step radiative transfer code specifically designed for following ionisation processes with an adaptive ray-tracing algorithm, we are able to significantly speed up the calculations to the point where handling a vast number of sources becomes technically feasible. This allows us to study how dim low-mass sources, excluded in previous investigations owing to computational limitations, affect the morphological evolution of the reionisation process.","downloadable_attachments":[{"id":39987508,"asset_id":18310626,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":38297020,"first_name":"Naoki","last_name":"Yoshida","domain_name":"independent","page_name":"YoshidaNaoki","display_name":"Naoki Yoshida","profile_url":"https://independent.academia.edu/YoshidaNaoki?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":38580581,"first_name":"Aaron","last_name":"Sokasian","domain_name":"harvard","page_name":"AaronSokasian","display_name":"Aaron Sokasian","profile_url":"https://harvard.academia.edu/AaronSokasian?f_ri=4363","photo":"https://0.academia-photos.com/38580581/122910140/112254483/s65_aaron.sokasian.png"}],"research_interests":[{"id":3364,"name":"Morphological evolution","url":"https://www.academia.edu/Documents/in/Morphological_evolution?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4742,"name":"Active Galactic Nuclei","url":"https://www.academia.edu/Documents/in/Active_Galactic_Nuclei?f_ri=4363","nofollow":true},{"id":11057,"name":"Intergalactic Medium","url":"https://www.academia.edu/Documents/in/Intergalactic_Medium?f_ri=4363","nofollow":true},{"id":110294,"name":"Negative Feedback","url":"https://www.academia.edu/Documents/in/Negative_Feedback?f_ri=4363"},{"id":160667,"name":"Ray Tracing","url":"https://www.academia.edu/Documents/in/Ray_Tracing?f_ri=4363"},{"id":309086,"name":"High Resolution","url":"https://www.academia.edu/Documents/in/High_Resolution?f_ri=4363"},{"id":442314,"name":"Radiative Transfer","url":"https://www.academia.edu/Documents/in/Radiative_Transfer?f_ri=4363"},{"id":487134,"name":"Effective mass","url":"https://www.academia.edu/Documents/in/Effective_mass?f_ri=4363"},{"id":764258,"name":"Ionizing Radiation","url":"https://www.academia.edu/Documents/in/Ionizing_Radiation?f_ri=4363"},{"id":869493,"name":"Sloan Digital Sky Survey","url":"https://www.academia.edu/Documents/in/Sloan_Digital_Sky_Survey?f_ri=4363"},{"id":1019577,"name":"Absorption Spectra","url":"https://www.academia.edu/Documents/in/Absorption_Spectra?f_ri=4363"},{"id":1150702,"name":"Simulation Analysis","url":"https://www.academia.edu/Documents/in/Simulation_Analysis?f_ri=4363"},{"id":1912509,"name":"Production Rate","url":"https://www.academia.edu/Documents/in/Production_Rate?f_ri=4363"},{"id":2195968,"name":"Electron scattering","url":"https://www.academia.edu/Documents/in/Electron_scattering?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_49146338" data-work_id="49146338" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/49146338/The_formation_of_the_Milky_Way">The formation of the Milky Way</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest">Contents: 1. Introduction. 2. Dark matter. 3. Angular momentum. 4. The halo. 5. The thick disk. 6. The thin disk. 7. The bulge. 8. History. 9. Discussion.</div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/49146338" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="c3052c2270ebcec0e055850816b8a318" rel="nofollow" data-download="{"attachment_id":67536340,"asset_id":49146338,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/67536340/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="33758034" href="https://independent.academia.edu/JHesser">J. Hesser</a><script data-card-contents-for-user="33758034" type="text/json">{"id":33758034,"first_name":"J.","last_name":"Hesser","domain_name":"independent","page_name":"JHesser","display_name":"J. Hesser","profile_url":"https://independent.academia.edu/JHesser?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_49146338 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="49146338"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 49146338, container: ".js-paper-rank-work_49146338", }); });</script></li><li class="js-percentile-work_49146338 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 49146338; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_49146338"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_49146338 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="49146338"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 49146338; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=49146338]").text(description); $(".js-view-count-work_49146338").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_49146338").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="49146338"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a>, <script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="383911" rel="nofollow" href="https://www.academia.edu/Documents/in/Spiral_Galaxies">Spiral Galaxies</a>, <script data-card-contents-for-ri="383911" type="text/json">{"id":383911,"name":"Spiral Galaxies","url":"https://www.academia.edu/Documents/in/Spiral_Galaxies?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="758278" rel="nofollow" href="https://www.academia.edu/Documents/in/Large_Scale">Large Scale</a><script data-card-contents-for-ri="758278" type="text/json">{"id":758278,"name":"Large Scale","url":"https://www.academia.edu/Documents/in/Large_Scale?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=49146338]'), work: {"id":49146338,"title":"The formation of the Milky Way","created_at":"2021-06-06T13:29:18.692-07:00","url":"https://www.academia.edu/49146338/The_formation_of_the_Milky_Way?f_ri=4363","dom_id":"work_49146338","summary":"Contents: 1. Introduction. 2. Dark matter. 3. Angular momentum. 4. The halo. 5. The thick disk. 6. The thin disk. 7. The bulge. 8. History. 9. Discussion.","downloadable_attachments":[{"id":67536340,"asset_id":49146338,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":33758034,"first_name":"J.","last_name":"Hesser","domain_name":"independent","page_name":"JHesser","display_name":"J. Hesser","profile_url":"https://independent.academia.edu/JHesser?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":383911,"name":"Spiral Galaxies","url":"https://www.academia.edu/Documents/in/Spiral_Galaxies?f_ri=4363","nofollow":true},{"id":758278,"name":"Large Scale","url":"https://www.academia.edu/Documents/in/Large_Scale?f_ri=4363","nofollow":true},{"id":1119718,"name":"Initial Condition","url":"https://www.academia.edu/Documents/in/Initial_Condition?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_23525357" data-work_id="23525357" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/23525357/The_LkHa_101_Cluster">The LkHa 101 Cluster</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">In the infrared, the heavily reddened LkH$\alpha$ 101 is one of the brightest young stars in the sky. Situated just north of the Taurus-Auriga complex in the L1482 dark cloud, it appears to be an early B-type star that has been... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_23525357" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">In the infrared, the heavily reddened LkH$\alpha$ 101 is one of the brightest young stars in the sky. Situated just north of the Taurus-Auriga complex in the L1482 dark cloud, it appears to be an early B-type star that has been serendipitously exposed during a rarely observed stage of early evolution, revealing a remarkable spectrum and a directly-imaged circumstellar disk. While detailed studies of this star and its circumstellar environment have become increasingly sophisticated in the 50 years since Herbig (1956) first pointed it out, the true nature of the object still remains a mystery. Recent work has renewed focus on the young cluster of stars surrounding LkH$\alpha$ 101, and what it can tell us about the enigmatic source at its center (e.g., massive star formation timescales, clustered formation mechanisms). This latter effort certainly deserves more intensive study. We describe the current knowledge of this region and point out interesting work that could be done in the future.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/23525357" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="2dafcd323150c248eaad97866bab5fff" rel="nofollow" data-download="{"attachment_id":43960473,"asset_id":23525357,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/43960473/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="29670411" href="https://independent.academia.edu/ScottWolk">Scott Wolk</a><script data-card-contents-for-user="29670411" type="text/json">{"id":29670411,"first_name":"Scott","last_name":"Wolk","domain_name":"independent","page_name":"ScottWolk","display_name":"Scott Wolk","profile_url":"https://independent.academia.edu/ScottWolk?f_ri=4363","photo":"https://gravatar.com/avatar/74dbd8afbbc97330e68b37039ddfba6a?s=65"}</script></span></span></li><li class="js-paper-rank-work_23525357 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="23525357"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 23525357, container: ".js-paper-rank-work_23525357", }); 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Situated just north of the Taurus-Auriga complex in the L1482 dark cloud, it appears to be an early B-type star that has been serendipitously exposed during a rarely observed stage of early evolution, revealing a remarkable spectrum and a directly-imaged circumstellar disk. While detailed studies of this star and its circumstellar environment have become increasingly sophisticated in the 50 years since Herbig (1956) first pointed it out, the true nature of the object still remains a mystery. Recent work has renewed focus on the young cluster of stars surrounding LkH$\\alpha$ 101, and what it can tell us about the enigmatic source at its center (e.g., massive star formation timescales, clustered formation mechanisms). This latter effort certainly deserves more intensive study. We describe the current knowledge of this region and point out interesting work that could be done in the future.","downloadable_attachments":[{"id":43960473,"asset_id":23525357,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":29670411,"first_name":"Scott","last_name":"Wolk","domain_name":"independent","page_name":"ScottWolk","display_name":"Scott Wolk","profile_url":"https://independent.academia.edu/ScottWolk?f_ri=4363","photo":"https://gravatar.com/avatar/74dbd8afbbc97330e68b37039ddfba6a?s=65"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=4363","nofollow":true},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_52512748" data-work_id="52512748" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/52512748/_title_The_Galaxy_Evolution_Explorer_title_"><title>The Galaxy Evolution Explorer</title></a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer Mission planned for launch in Fall 2002, will perform the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (1350-1750Å and 1750-2800Å) will range... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_52512748" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer Mission planned for launch in Fall 2002, will perform the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (1350-1750Å and 1750-2800Å) will range from an all-sky survey (limit m AB~2 0-21) to an ultra-deep survey of 4 square degrees (limit m AB~2 6). Three spectroscopic grism surveys (R=100-300) will be performed with various depths (m AB~2 0-25) and sky coverage (100 to 2 square degrees) over the 1350-2800Å band. The instrument includes a 50 cm modified Ritchey-Chrétien telescope, a dichroic beam splitter and astigmatism corrector, two large sealed tube microchannel plate detectors to simultaneously cover the two bands and the 1.2 degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. We will use the measured UV properties of local galaxies, along with corollary observations, to calibrate the UV-global star formation rate relationship in galaxies. We will apply this calibration to distant galaxies discovered in the deep imaging and spectroscopic surveys to map the history of star formation in the universe over the red shift range zero to two. The GALEX mission will include an Associate Investigator program for additional observations and supporting data analysis. This will support a wide variety of investigations made possible by the first UV sky survey.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/52512748" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="392b996c7bd179e0288c1c8c154d2bbd" rel="nofollow" data-download="{"attachment_id":69745377,"asset_id":52512748,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/69745377/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5629030" href="https://independent.academia.edu/AmitSen2">Amit Sen</a><script data-card-contents-for-user="5629030" type="text/json">{"id":5629030,"first_name":"Amit","last_name":"Sen","domain_name":"independent","page_name":"AmitSen2","display_name":"Amit Sen","profile_url":"https://independent.academia.edu/AmitSen2?f_ri=4363","photo":"https://0.academia-photos.com/5629030/2452758/2851167/s65_amit.sen.jpg"}</script></span></span></li><li class="js-paper-rank-work_52512748 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="52512748"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 52512748, container: ".js-paper-rank-work_52512748", }); 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$(".js-view-count[data-work-id=52512748]").text(description); $(".js-view-count-work_52512748").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_52512748").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="52512748"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4205" rel="nofollow" href="https://www.academia.edu/Documents/in/Data_Analysis">Data Analysis</a>, <script data-card-contents-for-ri="4205" type="text/json">{"id":4205,"name":"Data Analysis","url":"https://www.academia.edu/Documents/in/Data_Analysis?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="40276" rel="nofollow" href="https://www.academia.edu/Documents/in/Proceedings">Proceedings</a>, <script data-card-contents-for-ri="40276" type="text/json">{"id":40276,"name":"Proceedings","url":"https://www.academia.edu/Documents/in/Proceedings?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="87546" rel="nofollow" href="https://www.academia.edu/Documents/in/Ultraviolet">Ultraviolet</a><script data-card-contents-for-ri="87546" type="text/json">{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=52512748]'), work: {"id":52512748,"title":"\u003ctitle\u003eThe Galaxy Evolution Explorer\u003c/title\u003e","created_at":"2021-09-16T07:15:33.159-07:00","url":"https://www.academia.edu/52512748/_title_The_Galaxy_Evolution_Explorer_title_?f_ri=4363","dom_id":"work_52512748","summary":"The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer Mission planned for launch in Fall 2002, will perform the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (1350-1750Å and 1750-2800Å) will range from an all-sky survey (limit m AB~2 0-21) to an ultra-deep survey of 4 square degrees (limit m AB~2 6). Three spectroscopic grism surveys (R=100-300) will be performed with various depths (m AB~2 0-25) and sky coverage (100 to 2 square degrees) over the 1350-2800Å band. The instrument includes a 50 cm modified Ritchey-Chrétien telescope, a dichroic beam splitter and astigmatism corrector, two large sealed tube microchannel plate detectors to simultaneously cover the two bands and the 1.2 degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. We will use the measured UV properties of local galaxies, along with corollary observations, to calibrate the UV-global star formation rate relationship in galaxies. We will apply this calibration to distant galaxies discovered in the deep imaging and spectroscopic surveys to map the history of star formation in the universe over the red shift range zero to two. The GALEX mission will include an Associate Investigator program for additional observations and supporting data analysis. This will support a wide variety of investigations made possible by the first UV sky survey.","downloadable_attachments":[{"id":69745377,"asset_id":52512748,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5629030,"first_name":"Amit","last_name":"Sen","domain_name":"independent","page_name":"AmitSen2","display_name":"Amit Sen","profile_url":"https://independent.academia.edu/AmitSen2?f_ri=4363","photo":"https://0.academia-photos.com/5629030/2452758/2851167/s65_amit.sen.jpg"}],"research_interests":[{"id":4205,"name":"Data Analysis","url":"https://www.academia.edu/Documents/in/Data_Analysis?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":40276,"name":"Proceedings","url":"https://www.academia.edu/Documents/in/Proceedings?f_ri=4363","nofollow":true},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=4363","nofollow":true},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":181628,"name":"Mission Planning","url":"https://www.academia.edu/Documents/in/Mission_Planning?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_1987819" data-work_id="1987819" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/1987819/The_x_ray_advanced_concepts_testbed_XACT_sounding_rocket_payload">The x-ray advanced concepts testbed (XACT) sounding rocket payload</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The scientific objective of the X-ray Advanced Concepts Testbed (XACT) is to measure the X-ray polarization properties of the Crab Nebula, the Crab pulsar, and the accreting binary Her X-1. Polarimetry is a powerful tool for astrophysical... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_1987819" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The scientific objective of the X-ray Advanced Concepts Testbed (XACT) is to measure the X-ray polarization properties of the Crab Nebula, the Crab pulsar, and the accreting binary Her X-1. Polarimetry is a powerful tool for astrophysical investigation that has yet to be exploited in the X-ray band, where it promises unique insights into neutron stars, black holes, and other extreme-physics environments. With powerful new enabling technologies, XACT will demonstrate X-ray polarimetry as a practical and flight-ready astronomical technique. Additional technologies that XACT will bring to flight readiness will also provide new X-ray optics and calibration capabilities for NASA missions that pursue space-based X-ray spectroscopy, timing, and photometry.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/1987819" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="97a5e3b9a673057c66af0bd458359e1a" rel="nofollow" data-download="{"attachment_id":29495189,"asset_id":1987819,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/29495189/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="1764186" href="https://umbc.academia.edu/ErinBalsamo">Erin R Balsamo</a><script data-card-contents-for-user="1764186" type="text/json">{"id":1764186,"first_name":"Erin","last_name":"Balsamo","domain_name":"umbc","page_name":"ErinBalsamo","display_name":"Erin R Balsamo","profile_url":"https://umbc.academia.edu/ErinBalsamo?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_1987819 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="1987819"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 1987819, container: ".js-paper-rank-work_1987819", }); 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$(".js-view-count[data-work-id=1987819]").text(description); $(".js-view-count-work_1987819").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_1987819").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="1987819"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">16</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="708" rel="nofollow" href="https://www.academia.edu/Documents/in/X_Ray_Astronomy">X Ray Astronomy</a>, <script data-card-contents-for-ri="708" type="text/json">{"id":708,"name":"X Ray Astronomy","url":"https://www.academia.edu/Documents/in/X_Ray_Astronomy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="6649" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared_Optics">Infrared Optics</a>, <script data-card-contents-for-ri="6649" type="text/json">{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="9820" rel="nofollow" href="https://www.academia.edu/Documents/in/Polarization_Ideology_">Polarization (Ideology)</a><script data-card-contents-for-ri="9820" type="text/json">{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=1987819]'), work: {"id":1987819,"title":"The x-ray advanced concepts testbed (XACT) sounding rocket payload","created_at":"2012-10-02T00:37:08.088-07:00","url":"https://www.academia.edu/1987819/The_x_ray_advanced_concepts_testbed_XACT_sounding_rocket_payload?f_ri=4363","dom_id":"work_1987819","summary":"The scientific objective of the X-ray Advanced Concepts Testbed (XACT) is to measure the X-ray polarization properties of the Crab Nebula, the Crab pulsar, and the accreting binary Her X-1. Polarimetry is a powerful tool for astrophysical investigation that has yet to be exploited in the X-ray band, where it promises unique insights into neutron stars, black holes, and other extreme-physics environments. With powerful new enabling technologies, XACT will demonstrate X-ray polarimetry as a practical and flight-ready astronomical technique. Additional technologies that XACT will bring to flight readiness will also provide new X-ray optics and calibration capabilities for NASA missions that pursue space-based X-ray spectroscopy, timing, and photometry.","downloadable_attachments":[{"id":29495189,"asset_id":1987819,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":1764186,"first_name":"Erin","last_name":"Balsamo","domain_name":"umbc","page_name":"ErinBalsamo","display_name":"Erin R Balsamo","profile_url":"https://umbc.academia.edu/ErinBalsamo?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":708,"name":"X Ray Astronomy","url":"https://www.academia.edu/Documents/in/X_Ray_Astronomy?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=4363","nofollow":true},{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=4363","nofollow":true},{"id":11673,"name":"X-ray Physics","url":"https://www.academia.edu/Documents/in/X-ray_Physics?f_ri=4363"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363"},{"id":37884,"name":"Space Exploration","url":"https://www.academia.edu/Documents/in/Space_Exploration?f_ri=4363"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363"},{"id":61024,"name":"Nasa","url":"https://www.academia.edu/Documents/in/Nasa?f_ri=4363"},{"id":89919,"name":"Robots","url":"https://www.academia.edu/Documents/in/Robots?f_ri=4363"},{"id":177538,"name":"Moon","url":"https://www.academia.edu/Documents/in/Moon?f_ri=4363"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363"},{"id":553730,"name":"Sounding Rockets","url":"https://www.academia.edu/Documents/in/Sounding_Rockets?f_ri=4363"},{"id":610448,"name":"XACT","url":"https://www.academia.edu/Documents/in/XACT?f_ri=4363"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4174128" data-work_id="4174128" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4174128/An_Estimate_of_the_Prevalence_of_Biocompatible_and_Habitable_Planets">An Estimate of the Prevalence of Biocompatible and Habitable Planets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4174128" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical  carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to assess the possible abundance of both biocompatible and habitable planets. (Biocompatible planets are defined as worlds where the long-term presence of surface liquid water provides environmental conditions suitable for the origin and evolution of life. Habitable planets are those worlds with more specifically Earth-like conditions.) The model gives an estimate of 1 biocompatible planet per 39 stars, with the subset of habitable planets being much rarer at 1 such planet per 413 stars. The nearest biocompatible planet may thus lie ~ 14 LY distant and the nearest habitable planet ~ 31 LY away. If planets form in multiple star systems then the above planet/star ratios may be more than doubled. By applying these results to stars in the solar neighbourhood, it is possible to identify 28 stars at distances of < 22 LY with a non-zero probability of possessing a biocompatible planet.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4174128" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="bbd93d866d3110254b90f873c2b0829d" rel="nofollow" data-download="{"attachment_id":31676540,"asset_id":4174128,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676540/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=4363","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4174128 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4174128"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4174128, container: ".js-paper-rank-work_4174128", }); });</script></li><li class="js-percentile-work_4174128 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4174128; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4174128"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4174128 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4174128"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4174128; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4174128]").text(description); $(".js-view-count-work_4174128").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4174128").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4174128"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="5001" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrobiology">Astrobiology</a>, <script data-card-contents-for-ri="5001" type="text/json">{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" rel="nofollow" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="194384" rel="nofollow" href="https://www.academia.edu/Documents/in/Planet_Formation">Planet Formation</a><script data-card-contents-for-ri="194384" type="text/json">{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4174128]'), work: {"id":4174128,"title":"An Estimate of the Prevalence of Biocompatible and Habitable Planets","created_at":"2013-08-05T02:03:34.217-07:00","url":"https://www.academia.edu/4174128/An_Estimate_of_the_Prevalence_of_Biocompatible_and_Habitable_Planets?f_ri=4363","dom_id":"work_4174128","summary":"A Monte Carlo computer model of extra-solar planetary formation and evolution, which includes the planetary geochemical carbon cycle, is presented. The results of a run of one million galactic disc stars are shown where the aim was to assess the possible abundance of both biocompatible and habitable planets. (Biocompatible planets are defined as worlds where the long-term presence of surface liquid water provides environmental conditions suitable for the origin and evolution of life. Habitable planets are those worlds with more specifically Earth-like conditions.) The model gives an estimate of 1 biocompatible planet per 39 stars, with the subset of habitable planets being much rarer at 1 such planet per 413 stars. The nearest biocompatible planet may thus lie ~ 14 LY distant and the nearest habitable planet ~ 31 LY away. If planets form in multiple star systems then the above planet/star ratios may be more than doubled. By applying these results to stars in the solar neighbourhood, it is possible to identify 28 stars at distances of \u003c 22 LY with a non-zero probability of possessing a biocompatible planet.","downloadable_attachments":[{"id":31676540,"asset_id":4174128,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=4363","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=4363","nofollow":true},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363","nofollow":true},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363","nofollow":true},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=4363"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_42126579" data-work_id="42126579" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/42126579/Hier_ist_wahrhaftig_ein_Loch_im_Himmel">Hier ist wahrhaftig ein Loch im Himmel</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The NGC 1999 reflection nebula features a dark patch with a size of ∼10,000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_42126579" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The NGC 1999 reflection nebula features a dark patch with a size of ∼10,000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160 µm maps, which reveal a flux deficit at the location of the globule. We estimate the globule mass needed to produce such an absorption feature to be a few tenths to a few M ⊙ . Inspired by this Herschel observation, we obtained APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC near-infrared images of the region. We do not detect a submillimer source at the location of the Herschel flux decrement; furthermore our observations place an upper limit on the mass of the globule of ∼2.4·10 −2 M ⊙ . Indeed, the submillimeter maps appear to show a flux depression as well. Furthermore, the near-infrared images detect faint background stars that are less affected by extinction inside the dark patch than in its surroundings. We suggest that the dark patch is in fact a hole or cavity in the material producing the NGC 1999 reflection nebula, excavated by protostellar jets from the V 380 Ori multiple system.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/42126579" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a7b6f35a2b3c7992824400b9a5d4aca8" rel="nofollow" data-download="{"attachment_id":62261458,"asset_id":42126579,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/62261458/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="60415163" href="https://gcuf.academia.edu/BabarAli">Babar Ali</a><script data-card-contents-for-user="60415163" type="text/json">{"id":60415163,"first_name":"Babar","last_name":"Ali","domain_name":"gcuf","page_name":"BabarAli","display_name":"Babar Ali","profile_url":"https://gcuf.academia.edu/BabarAli?f_ri=4363","photo":"https://0.academia-photos.com/60415163/17194386/17331931/s65_babar.ali.jpg"}</script></span></span></li><li class="js-paper-rank-work_42126579 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="42126579"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 42126579, container: ".js-paper-rank-work_42126579", }); });</script></li><li class="js-percentile-work_42126579 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 42126579; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_42126579"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_42126579 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="42126579"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 42126579; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=42126579]").text(description); $(".js-view-count-work_42126579").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_42126579").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="42126579"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a>, <script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="335361" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared">Infrared</a>, <script data-card-contents-for-ri="335361" type="text/json">{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="335363" rel="nofollow" href="https://www.academia.edu/Documents/in/Far_Infrared">Far Infrared</a><script data-card-contents-for-ri="335363" type="text/json">{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=42126579]'), work: {"id":42126579,"title":"Hier ist wahrhaftig ein Loch im Himmel","created_at":"2020-03-03T05:23:34.938-08:00","url":"https://www.academia.edu/42126579/Hier_ist_wahrhaftig_ein_Loch_im_Himmel?f_ri=4363","dom_id":"work_42126579","summary":"The NGC 1999 reflection nebula features a dark patch with a size of ∼10,000 AU, which has been interpreted as a small, dense foreground globule and possible site of imminent star formation. We present Herschel PACS far-infrared 70 and 160 µm maps, which reveal a flux deficit at the location of the globule. We estimate the globule mass needed to produce such an absorption feature to be a few tenths to a few M ⊙ . Inspired by this Herschel observation, we obtained APEX LABOCA and SABOCA submillimeter continuum maps, and Magellan PANIC near-infrared images of the region. We do not detect a submillimer source at the location of the Herschel flux decrement; furthermore our observations place an upper limit on the mass of the globule of ∼2.4·10 −2 M ⊙ . Indeed, the submillimeter maps appear to show a flux depression as well. Furthermore, the near-infrared images detect faint background stars that are less affected by extinction inside the dark patch than in its surroundings. We suggest that the dark patch is in fact a hole or cavity in the material producing the NGC 1999 reflection nebula, excavated by protostellar jets from the V 380 Ori multiple system.","downloadable_attachments":[{"id":62261458,"asset_id":42126579,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":60415163,"first_name":"Babar","last_name":"Ali","domain_name":"gcuf","page_name":"BabarAli","display_name":"Babar Ali","profile_url":"https://gcuf.academia.edu/BabarAli?f_ri=4363","photo":"https://0.academia-photos.com/60415163/17194386/17331931/s65_babar.ali.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true},{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363","nofollow":true},{"id":967970,"name":"Near Infrared Imaging","url":"https://www.academia.edu/Documents/in/Near_Infrared_Imaging?f_ri=4363"},{"id":2108071,"name":"Data Gathering","url":"https://www.academia.edu/Documents/in/Data_Gathering?f_ri=4363"},{"id":2936636,"name":"individual object","url":"https://www.academia.edu/Documents/in/individual_object?f_ri=4363"},{"id":3243321,"name":"Principal Investigator","url":"https://www.academia.edu/Documents/in/Principal_Investigator?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_69058334" data-work_id="69058334" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/69058334/The_Spitzer_C2D_legacy_results_star_formation_rates_and_efficiencies_evolution_and_lifetimes">The Spitzer C2D legacy results: star-formation rates and efficiencies; evolution and lifetimes</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. Three of the clouds were also mapped in dust continuum emission at 1.1 mm, and optical spectroscopy... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_69058334" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. Three of the clouds were also mapped in dust continuum emission at 1.1 mm, and optical spectroscopy has been obtained for some clouds. This paper combines information drawn from studies of individual clouds into a combined and updated statistical analysis of star formation rates and efficiencies, numbers and lifetimes for SED classes, and clustering properties. Current star formation efficiencies range from 3% to 6%; if star formation continues at current rates for 10 Myr, efficiencies could reach 15% to 30%. Star formation rates and rates per unit area vary from cloud to cloud; taken together, the five clouds are producing about 260 M ⊙ of stars per Myr. The star formation surface density is more than an order of magnitude larger than would be predicted from the Kennicutt relation used in extragalactic studies, reflecting the fact that those relations apply to larger scales, where more diffuse matter is included in the gas surface density. Measured against the dense gas probed by the maps of dust continuum emission, the efficiencies are much higher, with stellar masses similar to masses of dense gas, and the current stock of dense cores would be exhausted in 1.8 Myr on average. Nonetheless, star formation is still slow compared to that expected in a free fall time, even in the dense cores. The derived lifetime for the Class I phase is 0.54 Myr, considerably longer than some estimates. Similarly, the lifetime for the Class 0 SED class, 0.16 Myr, with the notable exception of the Ophiuchus cloud, is longer than early estimates. If photometry is corrected for estimated extinction before calculating class indicators, the lifetimes drop to 0.44 Myr for Class I and to 0.10 for Class 0. These lifetimes assume a continuous flow through the Class II phase and should be considered median lifetimes or half-lives. Star formation is highly concentrated to regions of high extinction, and the youngest objects are very strongly associated with dense cores. The great majority (90%) of young stars lie within loose clusters with at least 35 members and a stellar density of 1 M ⊙ pc −3. Accretion at the sound speed from an isothermal sphere over the lifetime derived for the Class I phase could build a star of about 0.25 M ⊙ , given an efficiency of 0.3. Building larger mass stars by using higher mass accretion rates could be problematic, as our data confirm and aggravate the "luminosity problem" for protostars. At a given T bol , the values for L bol are mostly less than predicted by standard infall models and scatter over several orders of magnitude. These results strongly suggest that accretion is time variable, with prolonged periods of very low accretion. Based on a very simple model and this sample of sources, half the mass of a star would be accreted during only 7% of the Class I lifetime, as represented by the eight most luminous objects.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/69058334" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="fbf9b0102e6de2c9556d4c46f7b2851e" rel="nofollow" data-download="{"attachment_id":79302087,"asset_id":69058334,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/79302087/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="166902693" href="https://independent.academia.edu/DeborahPadgett2">Deborah Padgett</a><script data-card-contents-for-user="166902693" type="text/json">{"id":166902693,"first_name":"Deborah","last_name":"Padgett","domain_name":"independent","page_name":"DeborahPadgett2","display_name":"Deborah Padgett","profile_url":"https://independent.academia.edu/DeborahPadgett2?f_ri=4363","photo":"https://0.academia-photos.com/166902693/46751288/36030364/s65_deborah.padgett.jpg"}</script></span></span></li><li class="js-paper-rank-work_69058334 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="69058334"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 69058334, container: ".js-paper-rank-work_69058334", }); });</script></li><li class="js-percentile-work_69058334 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 69058334; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_69058334"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_69058334 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="69058334"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 69058334; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=69058334]").text(description); $(".js-view-count-work_69058334").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_69058334").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="69058334"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">11</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="498" rel="nofollow" href="https://www.academia.edu/Documents/in/Physics">Physics</a>, <script data-card-contents-for-ri="498" type="text/json">{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="5187" rel="nofollow" href="https://www.academia.edu/Documents/in/Statistical_Analysis">Statistical Analysis</a><script data-card-contents-for-ri="5187" type="text/json">{"id":5187,"name":"Statistical Analysis","url":"https://www.academia.edu/Documents/in/Statistical_Analysis?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=69058334]'), work: {"id":69058334,"title":"The Spitzer C2D legacy results: star-formation rates and efficiencies; evolution and lifetimes","created_at":"2022-01-21T14:38:37.515-08:00","url":"https://www.academia.edu/69058334/The_Spitzer_C2D_legacy_results_star_formation_rates_and_efficiencies_evolution_and_lifetimes?f_ri=4363","dom_id":"work_69058334","summary":"The c2d Spitzer Legacy project obtained images and photometry with both IRAC and MIPS instruments for five large, nearby molecular clouds. Three of the clouds were also mapped in dust continuum emission at 1.1 mm, and optical spectroscopy has been obtained for some clouds. This paper combines information drawn from studies of individual clouds into a combined and updated statistical analysis of star formation rates and efficiencies, numbers and lifetimes for SED classes, and clustering properties. Current star formation efficiencies range from 3% to 6%; if star formation continues at current rates for 10 Myr, efficiencies could reach 15% to 30%. Star formation rates and rates per unit area vary from cloud to cloud; taken together, the five clouds are producing about 260 M ⊙ of stars per Myr. The star formation surface density is more than an order of magnitude larger than would be predicted from the Kennicutt relation used in extragalactic studies, reflecting the fact that those relations apply to larger scales, where more diffuse matter is included in the gas surface density. Measured against the dense gas probed by the maps of dust continuum emission, the efficiencies are much higher, with stellar masses similar to masses of dense gas, and the current stock of dense cores would be exhausted in 1.8 Myr on average. Nonetheless, star formation is still slow compared to that expected in a free fall time, even in the dense cores. The derived lifetime for the Class I phase is 0.54 Myr, considerably longer than some estimates. Similarly, the lifetime for the Class 0 SED class, 0.16 Myr, with the notable exception of the Ophiuchus cloud, is longer than early estimates. If photometry is corrected for estimated extinction before calculating class indicators, the lifetimes drop to 0.44 Myr for Class I and to 0.10 for Class 0. These lifetimes assume a continuous flow through the Class II phase and should be considered median lifetimes or half-lives. Star formation is highly concentrated to regions of high extinction, and the youngest objects are very strongly associated with dense cores. The great majority (90%) of young stars lie within loose clusters with at least 35 members and a stellar density of 1 M ⊙ pc −3. Accretion at the sound speed from an isothermal sphere over the lifetime derived for the Class I phase could build a star of about 0.25 M ⊙ , given an efficiency of 0.3. Building larger mass stars by using higher mass accretion rates could be problematic, as our data confirm and aggravate the \"luminosity problem\" for protostars. At a given T bol , the values for L bol are mostly less than predicted by standard infall models and scatter over several orders of magnitude. These results strongly suggest that accretion is time variable, with prolonged periods of very low accretion. Based on a very simple model and this sample of sources, half the mass of a star would be accreted during only 7% of the Class I lifetime, as represented by the eight most luminous objects.","downloadable_attachments":[{"id":79302087,"asset_id":69058334,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":166902693,"first_name":"Deborah","last_name":"Padgett","domain_name":"independent","page_name":"DeborahPadgett2","display_name":"Deborah Padgett","profile_url":"https://independent.academia.edu/DeborahPadgett2?f_ri=4363","photo":"https://0.academia-photos.com/166902693/46751288/36030364/s65_deborah.padgett.jpg"}],"research_interests":[{"id":498,"name":"Physics","url":"https://www.academia.edu/Documents/in/Physics?f_ri=4363","nofollow":true},{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":5187,"name":"Statistical Analysis","url":"https://www.academia.edu/Documents/in/Statistical_Analysis?f_ri=4363","nofollow":true},{"id":13033,"name":"Optical Spectroscopy","url":"https://www.academia.edu/Documents/in/Optical_Spectroscopy?f_ri=4363"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363"},{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363"},{"id":164269,"name":"Extinction","url":"https://www.academia.edu/Documents/in/Extinction?f_ri=4363"},{"id":417933,"name":"Continuous Flow","url":"https://www.academia.edu/Documents/in/Continuous_Flow?f_ri=4363"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_24500624 coauthored" data-work_id="24500624" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/24500624/College_Students_Preinstructional_Ideas_About_Stars_and_Star_Formation">College Students’ Preinstructional Ideas About Stars and Star Formation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">This study ͑Note 1͒ investigated the beliefs about stars that students hold when they enter an undergraduate introductory astronomy course for nonscience majors. Students' preinstructional ideas were investigated through the use of... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_24500624" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">This study ͑Note 1͒ investigated the beliefs about stars that students hold when they enter an undergraduate introductory astronomy course for nonscience majors. Students' preinstructional ideas were investigated through the use of several student-supplied-response ͑SSR͒ surveys, which asked students to describe their ideas about topics such as what is a star, how is starlight created, how are stars formed, are all stars the same, and more. The results from more than 2,200 responses suggest that although students often have some initial knowledge about stars, their knowledge is often incomplete or incorrect in important ways that could negatively impact instructional objectives.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/24500624" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="cb3c410549ce8c022723cc14767268a3" rel="nofollow" data-download="{"attachment_id":44833080,"asset_id":24500624,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/44833080/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="33148565" href="https://independent.academia.edu/BruceJohnson17">Bruce Johnson</a><script data-card-contents-for-user="33148565" type="text/json">{"id":33148565,"first_name":"Bruce","last_name":"Johnson","domain_name":"independent","page_name":"BruceJohnson17","display_name":"Bruce Johnson","profile_url":"https://independent.academia.edu/BruceJohnson17?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-24500624">+2</span><div class="hidden js-additional-users-24500624"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://temple.academia.edu/JanelleBailey">Janelle Bailey</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/EdwardPrather">Edward Prather</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-24500624'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-24500624').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_24500624 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="24500624"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 24500624, container: ".js-paper-rank-work_24500624", }); });</script></li><li class="js-percentile-work_24500624 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 24500624; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_24500624"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_24500624 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="24500624"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 24500624; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=24500624]").text(description); $(".js-view-count-work_24500624").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_24500624").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="24500624"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="47599" rel="nofollow" href="https://www.academia.edu/Documents/in/Astronomy">Astronomy</a>, <script data-card-contents-for-ri="47599" type="text/json">{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="49107" rel="nofollow" href="https://www.academia.edu/Documents/in/Astronomy_Education">Astronomy Education</a>, <script data-card-contents-for-ri="49107" type="text/json">{"id":49107,"name":"Astronomy Education","url":"https://www.academia.edu/Documents/in/Astronomy_Education?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="80657" rel="nofollow" href="https://www.academia.edu/Documents/in/Surveys">Surveys</a><script data-card-contents-for-ri="80657" type="text/json">{"id":80657,"name":"Surveys","url":"https://www.academia.edu/Documents/in/Surveys?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=24500624]'), work: {"id":24500624,"title":"College Students’ Preinstructional Ideas About Stars and Star Formation","created_at":"2016-04-17T16:23:47.113-07:00","url":"https://www.academia.edu/24500624/College_Students_Preinstructional_Ideas_About_Stars_and_Star_Formation?f_ri=4363","dom_id":"work_24500624","summary":"This study ͑Note 1͒ investigated the beliefs about stars that students hold when they enter an undergraduate introductory astronomy course for nonscience majors. Students' preinstructional ideas were investigated through the use of several student-supplied-response ͑SSR͒ surveys, which asked students to describe their ideas about topics such as what is a star, how is starlight created, how are stars formed, are all stars the same, and more. The results from more than 2,200 responses suggest that although students often have some initial knowledge about stars, their knowledge is often incomplete or incorrect in important ways that could negatively impact instructional objectives.","downloadable_attachments":[{"id":44833080,"asset_id":24500624,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":33148565,"first_name":"Bruce","last_name":"Johnson","domain_name":"independent","page_name":"BruceJohnson17","display_name":"Bruce Johnson","profile_url":"https://independent.academia.edu/BruceJohnson17?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":47158511,"first_name":"Janelle","last_name":"Bailey","domain_name":"temple","page_name":"JanelleBailey","display_name":"Janelle Bailey","profile_url":"https://temple.academia.edu/JanelleBailey?f_ri=4363","photo":"https://0.academia-photos.com/47158511/30534684/28287199/s65_janelle.bailey.jpg"},{"id":47359504,"first_name":"Edward","last_name":"Prather","domain_name":"independent","page_name":"EdwardPrather","display_name":"Edward Prather","profile_url":"https://independent.academia.edu/EdwardPrather?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363","nofollow":true},{"id":49107,"name":"Astronomy Education","url":"https://www.academia.edu/Documents/in/Astronomy_Education?f_ri=4363","nofollow":true},{"id":80657,"name":"Surveys","url":"https://www.academia.edu/Documents/in/Surveys?f_ri=4363","nofollow":true},{"id":102674,"name":"College Students","url":"https://www.academia.edu/Documents/in/College_Students?f_ri=4363"},{"id":508371,"name":"Curriculum and Pedagogy","url":"https://www.academia.edu/Documents/in/Curriculum_and_Pedagogy?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_50065726" data-work_id="50065726" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/50065726/Bsoft_Image_and_Molecular_Processing_in_Electron_Microscopy">Bsoft: Image and Molecular Processing in Electron Microscopy</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Software for the processing of electron micrographs in structural biology suffers from incompatibility between different packages, poor definition and choice of conventions, and a lack of coherence in software development. The solution... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_50065726" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Software for the processing of electron micrographs in structural biology suffers from incompatibility between different packages, poor definition and choice of conventions, and a lack of coherence in software development. The solution lies in adopting a common philosophy of interaction and conventions between the packages. To understand the choices required to have such common interfaces, I am developing a package called "Bsoft." Its foundations lie in the variety of different image file formats used in electron microscopy-a continually frustrating experience to the user and programmer alike. In Bsoft, this problem is greatly diminished by support for many different formats (including MRC, SPIDER, IMAGIC, SUPRIM, and PIF) and by separating algorithmic issues from image formatspecific issues. In addition, I implemented a generalized functionality for reading the tag-base STAR (self-defining text archiving and retrieval) parameter file format as a mechanism to exchanging parameters between different packages. Bsoft is written in highly portable code (tested on several Unix systems and under VMS) and offers a continually growing range of image processing functionality, such as Fourier transformation, cross-correlation, and interpolation. Finally, prerequisites for software collaboration are explored, which include agreements on information exchange and conventions, and tests to evaluate compatibility between packages.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/50065726" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="3bac4693e6eb81460131c4837d9c5864" rel="nofollow" data-download="{"attachment_id":68188828,"asset_id":50065726,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/68188828/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="46961426" href="https://independent.academia.edu/HeymannBernard">Bernard Heymann</a><script data-card-contents-for-user="46961426" type="text/json">{"id":46961426,"first_name":"Bernard","last_name":"Heymann","domain_name":"independent","page_name":"HeymannBernard","display_name":"Bernard Heymann","profile_url":"https://independent.academia.edu/HeymannBernard?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_50065726 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="50065726"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 50065726, container: ".js-paper-rank-work_50065726", }); 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$(".js-view-count[data-work-id=50065726]").text(description); $(".js-view-count-work_50065726").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_50065726").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="50065726"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">20</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="1185" rel="nofollow" href="https://www.academia.edu/Documents/in/Image_Processing">Image Processing</a>, <script data-card-contents-for-ri="1185" type="text/json">{"id":1185,"name":"Image Processing","url":"https://www.academia.edu/Documents/in/Image_Processing?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2184" rel="nofollow" href="https://www.academia.edu/Documents/in/Electron_Microscopy">Electron Microscopy</a>, <script data-card-contents-for-ri="2184" type="text/json">{"id":2184,"name":"Electron Microscopy","url":"https://www.academia.edu/Documents/in/Electron_Microscopy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2541" rel="nofollow" href="https://www.academia.edu/Documents/in/Structural_Biology">Structural Biology</a>, <script data-card-contents-for-ri="2541" type="text/json">{"id":2541,"name":"Structural Biology","url":"https://www.academia.edu/Documents/in/Structural_Biology?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2725" rel="nofollow" href="https://www.academia.edu/Documents/in/Documentation">Documentation</a><script data-card-contents-for-ri="2725" type="text/json">{"id":2725,"name":"Documentation","url":"https://www.academia.edu/Documents/in/Documentation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=50065726]'), work: {"id":50065726,"title":"Bsoft: Image and Molecular Processing in Electron Microscopy","created_at":"2021-07-19T02:15:48.894-07:00","url":"https://www.academia.edu/50065726/Bsoft_Image_and_Molecular_Processing_in_Electron_Microscopy?f_ri=4363","dom_id":"work_50065726","summary":"Software for the processing of electron micrographs in structural biology suffers from incompatibility between different packages, poor definition and choice of conventions, and a lack of coherence in software development. The solution lies in adopting a common philosophy of interaction and conventions between the packages. To understand the choices required to have such common interfaces, I am developing a package called \"Bsoft.\" Its foundations lie in the variety of different image file formats used in electron microscopy-a continually frustrating experience to the user and programmer alike. In Bsoft, this problem is greatly diminished by support for many different formats (including MRC, SPIDER, IMAGIC, SUPRIM, and PIF) and by separating algorithmic issues from image formatspecific issues. In addition, I implemented a generalized functionality for reading the tag-base STAR (self-defining text archiving and retrieval) parameter file format as a mechanism to exchanging parameters between different packages. Bsoft is written in highly portable code (tested on several Unix systems and under VMS) and offers a continually growing range of image processing functionality, such as Fourier transformation, cross-correlation, and interpolation. 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Biology","url":"https://www.academia.edu/Documents/in/Structural_Biology?f_ri=4363","nofollow":true},{"id":2725,"name":"Documentation","url":"https://www.academia.edu/Documents/in/Documentation?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363"},{"id":8129,"name":"Software Development","url":"https://www.academia.edu/Documents/in/Software_Development?f_ri=4363"},{"id":8137,"name":"Unix","url":"https://www.academia.edu/Documents/in/Unix?f_ri=4363"},{"id":24373,"name":"Atomic Force Microscopy","url":"https://www.academia.edu/Documents/in/Atomic_Force_Microscopy?f_ri=4363"},{"id":53293,"name":"Software","url":"https://www.academia.edu/Documents/in/Software?f_ri=4363"},{"id":58703,"name":"Cross Correlation","url":"https://www.academia.edu/Documents/in/Cross_Correlation?f_ri=4363"},{"id":75498,"name":"AFM","url":"https://www.academia.edu/Documents/in/AFM?f_ri=4363"},{"id":88861,"name":"Computer 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Function","url":"https://www.academia.edu/Documents/in/Generating_Function?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_495473" data-work_id="495473" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/495473/Fitting_the_integrated_spectral_energy_distributions_of_galaxies">Fitting the integrated spectral energy distributions of galaxies</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/495473" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa 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itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="102807" href="https://aip.academia.edu/JakobWalcher">Jakob Walcher</a><script data-card-contents-for-user="102807" type="text/json">{"id":102807,"first_name":"Jakob","last_name":"Walcher","domain_name":"aip","page_name":"JakobWalcher","display_name":"Jakob Walcher","profile_url":"https://aip.academia.edu/JakobWalcher?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_495473 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="495473"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 495473, container: ".js-paper-rank-work_495473", }); });</script></li><li class="js-percentile-work_495473 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget 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$(".js-view-count[data-work-id=495473]").text(description); $(".js-view-count-work_495473").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_495473").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="495473"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">7</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4205" rel="nofollow" href="https://www.academia.edu/Documents/in/Data_Analysis">Data Analysis</a>, <script data-card-contents-for-ri="4205" type="text/json">{"id":4205,"name":"Data Analysis","url":"https://www.academia.edu/Documents/in/Data_Analysis?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="87546" rel="nofollow" href="https://www.academia.edu/Documents/in/Ultraviolet">Ultraviolet</a>, <script data-card-contents-for-ri="87546" type="text/json">{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="335361" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared">Infrared</a><script data-card-contents-for-ri="335361" type="text/json">{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=495473]'), work: {"id":495473,"title":"Fitting the integrated spectral energy distributions of galaxies","created_at":"2011-03-27T22:03:54.273-07:00","url":"https://www.academia.edu/495473/Fitting_the_integrated_spectral_energy_distributions_of_galaxies?f_ri=4363","dom_id":"work_495473","summary":null,"downloadable_attachments":[{"id":2297870,"asset_id":495473,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":102807,"first_name":"Jakob","last_name":"Walcher","domain_name":"aip","page_name":"JakobWalcher","display_name":"Jakob Walcher","profile_url":"https://aip.academia.edu/JakobWalcher?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4205,"name":"Data Analysis","url":"https://www.academia.edu/Documents/in/Data_Analysis?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=4363","nofollow":true},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true},{"id":481229,"name":"Web Pages","url":"https://www.academia.edu/Documents/in/Web_Pages?f_ri=4363"},{"id":1228946,"name":"Physical Properties","url":"https://www.academia.edu/Documents/in/Physical_Properties?f_ri=4363"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4173808" data-work_id="4173808" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4173808/Extra_Solar_Planetary_Systems_A_Microcomputer_Simulation">Extra-Solar Planetary Systems: A Microcomputer Simulation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">""Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4173808" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">""Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain a greater insight into the complexities of planetary formation, researchers have concentrated on 'realistic' simulations of clearly defined and limited aspects of the problem of the formation of the Solar System. Attempts to describe the nature of planetary systems of other stars have been left largely to popular speculation. <br />The microcomputer model presented here produces a wide range of data for possible planetary systems with primary stars in the mass range 0.6 - 1.3 M⊙. A synthesis of current theory, research and speculation, the purpose of this model is not to add to our understanding of the processes that form planets, but to give an integrated view of the possible nature of extra-solar planetary systems and to investigate the possibility of a systematic variation in planetary characteristics with primary mass. ""</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4173808" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="36d0b9febc2bffd205fcc8c8e4e2cdbc" rel="nofollow" data-download="{"attachment_id":31676329,"asset_id":4173808,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31676329/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="5021359" href="https://independent.academia.edu/MartynFogg">Martyn Fogg</a><script data-card-contents-for-user="5021359" type="text/json">{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=4363","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}</script></span></span></li><li class="js-paper-rank-work_4173808 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4173808"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4173808, container: ".js-paper-rank-work_4173808", }); });</script></li><li class="js-percentile-work_4173808 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 4173808; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_4173808"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_4173808 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="4173808"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 4173808; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=4173808]").text(description); $(".js-view-count-work_4173808").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4173808").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4173808"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="41236" rel="nofollow" href="https://www.academia.edu/Documents/in/Extrasolar_planets">Extrasolar planets</a>, <script data-card-contents-for-ri="41236" type="text/json">{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="194384" rel="nofollow" href="https://www.academia.edu/Documents/in/Planet_Formation">Planet Formation</a>, <script data-card-contents-for-ri="194384" type="text/json">{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="334552" rel="nofollow" href="https://www.academia.edu/Documents/in/Habitable_Exoplanets">Habitable Exoplanets</a><script data-card-contents-for-ri="334552" type="text/json">{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4173808]'), work: {"id":4173808,"title":"Extra-Solar Planetary Systems: A Microcomputer Simulation","created_at":"2013-08-05T01:10:05.409-07:00","url":"https://www.academia.edu/4173808/Extra_Solar_Planetary_Systems_A_Microcomputer_Simulation?f_ri=4363","dom_id":"work_4173808","summary":"\"\"Knowledge of the physical and chemical processes which occur within the circum-stellar nebula of a newly formed star is still uncertain and permits a number of distinct theories to account for the formation of planets. In order to gain a greater insight into the complexities of planetary formation, researchers have concentrated on 'realistic' simulations of clearly defined and limited aspects of the problem of the formation of the Solar System. Attempts to describe the nature of planetary systems of other stars have been left largely to popular speculation.\r\nThe microcomputer model presented here produces a wide range of data for possible planetary systems with primary stars in the mass range 0.6 - 1.3 M⊙. A synthesis of current theory, research and speculation, the purpose of this model is not to add to our understanding of the processes that form planets, but to give an integrated view of the possible nature of extra-solar planetary systems and to investigate the possibility of a systematic variation in planetary characteristics with primary mass. \"\"","downloadable_attachments":[{"id":31676329,"asset_id":4173808,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":5021359,"first_name":"Martyn","last_name":"Fogg","domain_name":"independent","page_name":"MartynFogg","display_name":"Martyn Fogg","profile_url":"https://independent.academia.edu/MartynFogg?f_ri=4363","photo":"https://0.academia-photos.com/5021359/2182240/2558362/s65_martyn.fogg.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363","nofollow":true},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363","nofollow":true},{"id":334552,"name":"Habitable Exoplanets","url":"https://www.academia.edu/Documents/in/Habitable_Exoplanets?f_ri=4363","nofollow":true},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_9487185" data-work_id="9487185" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/9487185/Lack_of_PAH_emission_toward_low_mass_embedded_young_stellar_objects">Lack of PAH emission toward low-mass embedded young stellar objects</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The 3.3 micron PAH feature is undetected for the majority of the sample (97%), with typical upper limits of 5E-16 W/m^2. Compact 11.2 micron PAH emission is seen directly towards 1 out of the 53 Spitzer Short-High spectra, for a source... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_9487185" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The 3.3 micron PAH feature is undetected for the majority of the sample (97%), with typical upper limits of 5E-16 W/m^2. Compact 11.2 micron PAH emission is seen directly towards 1 out of the 53 Spitzer Short-High spectra, for a source that is borderline embedded. For all 12 sources with both VLT and Spitzer spectra, no PAH features are detected in either. In total, PAH features are detected toward at most 1 out of 63 (candidate) embedded protostars (<~ 2%), even lower than observed for class II T Tauri stars with disks (11-14%). Assuming typical class I stellar and envelope parameters, the absence of PAHs emission is most likely explained by the absence of emitting carriers through a PAH abundance at least an order of magnitude lower than in molecular clouds but similar to that found in disks. Thus, most PAHs likely enter the protoplanetary disks frozen out in icy layers on dust grains and/or in coagulated form.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/9487185" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="9611df96be431d6cfd5b46e7370edb68" rel="nofollow" data-download="{"attachment_id":35719124,"asset_id":9487185,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/35719124/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="22213384" href="https://sron.academia.edu/FredLahuis">Fred Lahuis</a><script data-card-contents-for-user="22213384" type="text/json">{"id":22213384,"first_name":"Fred","last_name":"Lahuis","domain_name":"sron","page_name":"FredLahuis","display_name":"Fred Lahuis","profile_url":"https://sron.academia.edu/FredLahuis?f_ri=4363","photo":"https://0.academia-photos.com/22213384/11619596/12957274/s65_fred.lahuis.jpg"}</script></span></span></li><li class="js-paper-rank-work_9487185 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="9487185"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 9487185, container: ".js-paper-rank-work_9487185", }); });</script></li><li class="js-percentile-work_9487185 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 9487185; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_9487185"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_9487185 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="9487185"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 9487185; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=9487185]").text(description); $(".js-view-count-work_9487185").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_9487185").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="9487185"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11125" rel="nofollow" href="https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_">Dust (Astronomy & Astrophysics)</a>, <script data-card-contents-for-ri="11125" type="text/json">{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="35657" rel="nofollow" href="https://www.academia.edu/Documents/in/Molecular_Clouds">Molecular Clouds</a>, <script data-card-contents-for-ri="35657" type="text/json">{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="195544" rel="nofollow" href="https://www.academia.edu/Documents/in/Planetary_Systems">Planetary Systems</a><script data-card-contents-for-ri="195544" type="text/json">{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=9487185]'), work: {"id":9487185,"title":"Lack of PAH emission toward low-mass embedded young stellar objects","created_at":"2014-11-24T23:46:00.304-08:00","url":"https://www.academia.edu/9487185/Lack_of_PAH_emission_toward_low_mass_embedded_young_stellar_objects?f_ri=4363","dom_id":"work_9487185","summary":"The 3.3 micron PAH feature is undetected for the majority of the sample (97%), with typical upper limits of 5E-16 W/m^2. Compact 11.2 micron PAH emission is seen directly towards 1 out of the 53 Spitzer Short-High spectra, for a source that is borderline embedded. For all 12 sources with both VLT and Spitzer spectra, no PAH features are detected in either. In total, PAH features are detected toward at most 1 out of 63 (candidate) embedded protostars (\u003c~ 2%), even lower than observed for class II T Tauri stars with disks (11-14%). Assuming typical class I stellar and envelope parameters, the absence of PAHs emission is most likely explained by the absence of emitting carriers through a PAH abundance at least an order of magnitude lower than in molecular clouds but similar to that found in disks. Thus, most PAHs likely enter the protoplanetary disks frozen out in icy layers on dust grains and/or in coagulated form.","downloadable_attachments":[{"id":35719124,"asset_id":9487185,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":22213384,"first_name":"Fred","last_name":"Lahuis","domain_name":"sron","page_name":"FredLahuis","display_name":"Fred Lahuis","profile_url":"https://sron.academia.edu/FredLahuis?f_ri=4363","photo":"https://0.academia-photos.com/22213384/11619596/12957274/s65_fred.lahuis.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11125,"name":"Dust (Astronomy \u0026 Astrophysics)","url":"https://www.academia.edu/Documents/in/Dust_Astronomy_and_Astrophysics_?f_ri=4363","nofollow":true},{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363","nofollow":true},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=4363","nofollow":true},{"id":249893,"name":"Mid-Infrared","url":"https://www.academia.edu/Documents/in/Mid-Infrared?f_ri=4363"},{"id":294029,"name":"T Tauri stars","url":"https://www.academia.edu/Documents/in/T_Tauri_stars?f_ri=4363"},{"id":442314,"name":"Radiative Transfer","url":"https://www.academia.edu/Documents/in/Radiative_Transfer?f_ri=4363"},{"id":444563,"name":"Acoustic Radiative Transfer Model","url":"https://www.academia.edu/Documents/in/Acoustic_Radiative_Transfer_Model?f_ri=4363"},{"id":925140,"name":"Circumstellar Matter","url":"https://www.academia.edu/Documents/in/Circumstellar_Matter?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_5009126" data-work_id="5009126" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/5009126/The_Evolution_of_the_Universe">The Evolution of the Universe</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The following assumptions of the Big Bang theory are challenged and found to be false: the cosmological principle, the assumption that all matter formed at the same time and the assumption regarding the cause of the cosmic microwave... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_5009126" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The following assumptions of the Big Bang theory are challenged and found to be false: the cosmological principle, the assumption that all matter formed at the same time and the assumption regarding the cause of the cosmic microwave background radiation (CMBR). <br /><br />The evolution of the universe is described based on the conclusion that the universe is finite with a space boundary. The CMBR is coming from a source located within the event horizon of the universe. There is sufficient mass in the universe to create an event horizon at the Schwarzschild radius. <br /><br />Galaxies form over time due to the energy released by the expansion of space. When a galaxy forms the matter formation is in the form of neutrons. Pairs of neutrons bond to form dark matter (dineutrons) and single neutrons decay to form protons and electrons which combine to form hydrogen. <br /><br />Conservation of energy must consider total energy which is mass (+ve) plus energy (+ve) plus spacetime curvature (-ve) so that the total energy of the universe is always zero. The predominant position of galaxy formation moves over time from the centre of the universe towards the boundary so that today the majority of new galaxy formation is taking place beyond our horizon of observation at 14 billion light years. <br /><br />The distribution of galaxies in a finite universe is such that there is a variation in gravitational acceleration depending on the distance from the centre of the universe. This gravitational acceleration results in the difference in the recession velocity of galaxies previously attributed to dark energy.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/5009126" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="153606fc77677dfef2e40308fa2d5226" rel="nofollow" data-download="{"attachment_id":65348930,"asset_id":5009126,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/65348930/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="6563051" href="https://cantab.academia.edu/RichardLewis">Richard Lewis</a><script data-card-contents-for-user="6563051" type="text/json">{"id":6563051,"first_name":"Richard","last_name":"Lewis","domain_name":"cantab","page_name":"RichardLewis","display_name":"Richard Lewis","profile_url":"https://cantab.academia.edu/RichardLewis?f_ri=4363","photo":"https://0.academia-photos.com/6563051/43692488/34709498/s65_richard.lewis.png"}</script></span></span></li><li class="js-paper-rank-work_5009126 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="5009126"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 5009126, container: ".js-paper-rank-work_5009126", }); });</script></li><li class="js-percentile-work_5009126 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 5009126; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_5009126"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_5009126 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="5009126"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 5009126; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=5009126]").text(description); $(".js-view-count-work_5009126").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_5009126").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="5009126"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">19</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="888" rel="nofollow" href="https://www.academia.edu/Documents/in/Cosmology_Physics_">Cosmology (Physics)</a>, <script data-card-contents-for-ri="888" type="text/json">{"id":888,"name":"Cosmology (Physics)","url":"https://www.academia.edu/Documents/in/Cosmology_Physics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1246" rel="nofollow" href="https://www.academia.edu/Documents/in/Gravitation">Gravitation</a>, <script data-card-contents-for-ri="1246" type="text/json">{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="3504" rel="nofollow" href="https://www.academia.edu/Documents/in/General_Relativity">General Relativity</a>, <script data-card-contents-for-ri="3504" type="text/json">{"id":3504,"name":"General Relativity","url":"https://www.academia.edu/Documents/in/General_Relativity?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a><script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=5009126]'), work: {"id":5009126,"title":"The Evolution of the Universe","created_at":"2013-11-06T00:52:26.490-08:00","url":"https://www.academia.edu/5009126/The_Evolution_of_the_Universe?f_ri=4363","dom_id":"work_5009126","summary":"The following assumptions of the Big Bang theory are challenged and found to be false: the cosmological principle, the assumption that all matter formed at the same time and the assumption regarding the cause of the cosmic microwave background radiation (CMBR). \n\nThe evolution of the universe is described based on the conclusion that the universe is finite with a space boundary. The CMBR is coming from a source located within the event horizon of the universe. There is sufficient mass in the universe to create an event horizon at the Schwarzschild radius. \n\nGalaxies form over time due to the energy released by the expansion of space. When a galaxy forms the matter formation is in the form of neutrons. Pairs of neutrons bond to form dark matter (dineutrons) and single neutrons decay to form protons and electrons which combine to form hydrogen. \n\nConservation of energy must consider total energy which is mass (+ve) plus energy (+ve) plus spacetime curvature (-ve) so that the total energy of the universe is always zero. The predominant position of galaxy formation moves over time from the centre of the universe towards the boundary so that today the majority of new galaxy formation is taking place beyond our horizon of observation at 14 billion light years. \n\nThe distribution of galaxies in a finite universe is such that there is a variation in gravitational acceleration depending on the distance from the centre of the universe. This gravitational acceleration results in the difference in the recession velocity of galaxies previously attributed to dark energy.","downloadable_attachments":[{"id":65348930,"asset_id":5009126,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":6563051,"first_name":"Richard","last_name":"Lewis","domain_name":"cantab","page_name":"RichardLewis","display_name":"Richard Lewis","profile_url":"https://cantab.academia.edu/RichardLewis?f_ri=4363","photo":"https://0.academia-photos.com/6563051/43692488/34709498/s65_richard.lewis.png"}],"research_interests":[{"id":888,"name":"Cosmology (Physics)","url":"https://www.academia.edu/Documents/in/Cosmology_Physics_?f_ri=4363","nofollow":true},{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=4363","nofollow":true},{"id":3504,"name":"General Relativity","url":"https://www.academia.edu/Documents/in/General_Relativity?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4751,"name":"Black Holes","url":"https://www.academia.edu/Documents/in/Black_Holes?f_ri=4363"},{"id":4818,"name":"Dark Matter","url":"https://www.academia.edu/Documents/in/Dark_Matter?f_ri=4363"},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363"},{"id":11058,"name":"Galaxy Clusters","url":"https://www.academia.edu/Documents/in/Galaxy_Clusters?f_ri=4363"},{"id":16620,"name":"Dark Energy","url":"https://www.academia.edu/Documents/in/Dark_Energy?f_ri=4363"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363"},{"id":29125,"name":"Gravitational Waves","url":"https://www.academia.edu/Documents/in/Gravitational_Waves?f_ri=4363"},{"id":47599,"name":"Astronomy","url":"https://www.academia.edu/Documents/in/Astronomy?f_ri=4363"},{"id":61631,"name":"High Redshift Universe","url":"https://www.academia.edu/Documents/in/High_Redshift_Universe?f_ri=4363"},{"id":74747,"name":"Cosmology and Gravitation","url":"https://www.academia.edu/Documents/in/Cosmology_and_Gravitation?f_ri=4363"},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":309434,"name":"Solar System","url":"https://www.academia.edu/Documents/in/Solar_System?f_ri=4363"},{"id":313728,"name":"Cosmological Constant","url":"https://www.academia.edu/Documents/in/Cosmological_Constant?f_ri=4363"},{"id":398159,"name":"Cold Dark Matter","url":"https://www.academia.edu/Documents/in/Cold_Dark_Matter?f_ri=4363"},{"id":993799,"name":"Cosmic Microwave Background Radiation","url":"https://www.academia.edu/Documents/in/Cosmic_Microwave_Background_Radiation?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_4806476" data-work_id="4806476" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/4806476/UV_Capabilities_to_Probe_the_Formation_of_Planetary_Systems_From_the_ISM_to_Planets">UV Capabilities to Probe the Formation of Planetary Systems: From the ISM to Planets</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Planetary systems are angular momentum reservoirs generated during star formation. Solutions to three of the most important problems in contemporary astrophysics are needed to understand the entire process of planetary system formation:... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_4806476" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Planetary systems are angular momentum reservoirs generated during star formation. Solutions to three of the most important problems in contemporary astrophysics are needed to understand the entire process of planetary system formation: The physics of the ISM. Stars form from dense molecular clouds that contain ∼ 30% of the total interstellar medium (ISM) mass. The structure, properties and lifetimes of molecular clouds are determined by the overall dynamics and evolution of a very complex system – the ISM. Understanding the physics of the ISM is of prime importance not only for Galactic but also for extragalactic and cosmological studies. Most of the ISM volume (∼ 65%) is filled with diffuse gas at temperatures between 3000 and 300 000 K, representing about 50% of the ISM mass. The physics of accretion and outflow. Powerful outflows are known to regulate angular momentum transport during star formation, the so-called accretion–outflow engine. Elementary physical considerations show that, to be efficient, the acceleration region for the outflows must be located close to the star (within 1 AU) where the gravitational field is strong. According to recent numerical simulations, this is also the region where terrestrial planets could form after 1 Myr. One should keep in mind that today the only evidence for life in the Universe comes from a planet located in this inner disk region (at 1 AU) from its parent star. The temperature of the accretion–outflow engine is between 3000 and 10 7 K. After 1 Myr, during the classical T Tauri stage, extinction is small and the engine becomes naked and can be observed at ultraviolet wavelengths. The physics of planet formation. Observations of volatiles released by dust, planetesimals and comets provide an extremely powerful tool for determining the relative abundances of the vaporizing species and for studying the photochemical and physical processes acting in the inner parts of young planetary systems. This region is illuminated by the strong UV radiation field produced by the star and the accretion–outflow engine. Absorption spectroscopy provides the most sensitive tool for determining the properties of the circumstellar gas as well as the characteristics of the atmospheres of the inner planets transiting the stellar disk. UV radiation also pumps the electronic transitions of the most abundant molecules (H 2, CO, etc.) that are observed in the UV. Here we argue that access to the UV spectral range is essential for making progress in this field, since the resonance lines of the most abundant atoms and ions at temperatures between 3000 and 300 000 K, together with the electronic transitions of the most abundant molecules (H 2, CO, OH, CS, S 2, CO 2+, C 2, O 2, O3, etc.) are at UV wavelengths. A powerful UV-optical instrument would provide an efficient mean for measuring the abundance of ozone in the atmosphere of the thousands of transiting planets expected to be detected by the next space missions (GAIA, Corot, Kepler, etc.). Thus, a follow-up UV mission would be optimal for identifying Earth-like candidates.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/4806476" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="3280a83de0b9dda0c85c44eaa0e1ceb6" rel="nofollow" data-download="{"attachment_id":49624907,"asset_id":4806476,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/49624907/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="6211677" href="https://ucm.academia.edu/AnaInesGomezdeCastro">Ana I Gomez de Castro</a><script data-card-contents-for-user="6211677" type="text/json">{"id":6211677,"first_name":"Ana","last_name":"Gomez de Castro","domain_name":"ucm","page_name":"AnaInesGomezdeCastro","display_name":"Ana I Gomez de Castro","profile_url":"https://ucm.academia.edu/AnaInesGomezdeCastro?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_4806476 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="4806476"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 4806476, container: ".js-paper-rank-work_4806476", }); 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$(".js-view-count[data-work-id=4806476]").text(description); $(".js-view-count-work_4806476").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_4806476").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="4806476"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">14</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="716" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium">Interstellar Medium</a>, <script data-card-contents-for-ri="716" type="text/json">{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="35657" rel="nofollow" href="https://www.academia.edu/Documents/in/Molecular_Clouds">Molecular Clouds</a>, <script data-card-contents-for-ri="35657" type="text/json">{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="54501" rel="nofollow" href="https://www.academia.edu/Documents/in/Complex_System">Complex System</a><script data-card-contents-for-ri="54501" type="text/json">{"id":54501,"name":"Complex System","url":"https://www.academia.edu/Documents/in/Complex_System?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=4806476]'), work: {"id":4806476,"title":"UV Capabilities to Probe the Formation of Planetary Systems: From the ISM to Planets","created_at":"2013-10-17T22:11:32.694-07:00","url":"https://www.academia.edu/4806476/UV_Capabilities_to_Probe_the_Formation_of_Planetary_Systems_From_the_ISM_to_Planets?f_ri=4363","dom_id":"work_4806476","summary":"Planetary systems are angular momentum reservoirs generated during star formation. Solutions to three of the most important problems in contemporary astrophysics are needed to understand the entire process of planetary system formation: The physics of the ISM. Stars form from dense molecular clouds that contain ∼ 30% of the total interstellar medium (ISM) mass. The structure, properties and lifetimes of molecular clouds are determined by the overall dynamics and evolution of a very complex system – the ISM. Understanding the physics of the ISM is of prime importance not only for Galactic but also for extragalactic and cosmological studies. Most of the ISM volume (∼ 65%) is filled with diffuse gas at temperatures between 3000 and 300 000 K, representing about 50% of the ISM mass. The physics of accretion and outflow. Powerful outflows are known to regulate angular momentum transport during star formation, the so-called accretion–outflow engine. Elementary physical considerations show that, to be efficient, the acceleration region for the outflows must be located close to the star (within 1 AU) where the gravitational field is strong. According to recent numerical simulations, this is also the region where terrestrial planets could form after 1 Myr. One should keep in mind that today the only evidence for life in the Universe comes from a planet located in this inner disk region (at 1 AU) from its parent star. The temperature of the accretion–outflow engine is between 3000 and 10 7 K. After 1 Myr, during the classical T Tauri stage, extinction is small and the engine becomes naked and can be observed at ultraviolet wavelengths. The physics of planet formation. Observations of volatiles released by dust, planetesimals and comets provide an extremely powerful tool for determining the relative abundances of the vaporizing species and for studying the photochemical and physical processes acting in the inner parts of young planetary systems. This region is illuminated by the strong UV radiation field produced by the star and the accretion–outflow engine. Absorption spectroscopy provides the most sensitive tool for determining the properties of the circumstellar gas as well as the characteristics of the atmospheres of the inner planets transiting the stellar disk. UV radiation also pumps the electronic transitions of the most abundant molecules (H 2, CO, etc.) that are observed in the UV. Here we argue that access to the UV spectral range is essential for making progress in this field, since the resonance lines of the most abundant atoms and ions at temperatures between 3000 and 300 000 K, together with the electronic transitions of the most abundant molecules (H 2, CO, OH, CS, S 2, CO 2+, C 2, O 2, O3, etc.) are at UV wavelengths. A powerful UV-optical instrument would provide an efficient mean for measuring the abundance of ozone in the atmosphere of the thousands of transiting planets expected to be detected by the next space missions (GAIA, Corot, Kepler, etc.). Thus, a follow-up UV mission would be optimal for identifying Earth-like candidates.","downloadable_attachments":[{"id":49624907,"asset_id":4806476,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":6211677,"first_name":"Ana","last_name":"Gomez de Castro","domain_name":"ucm","page_name":"AnaInesGomezdeCastro","display_name":"Ana I Gomez de Castro","profile_url":"https://ucm.academia.edu/AnaInesGomezdeCastro?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363","nofollow":true},{"id":54501,"name":"Complex System","url":"https://www.academia.edu/Documents/in/Complex_System?f_ri=4363","nofollow":true},{"id":60658,"name":"Numerical Simulation","url":"https://www.academia.edu/Documents/in/Numerical_Simulation?f_ri=4363"},{"id":87546,"name":"Ultraviolet","url":"https://www.academia.edu/Documents/in/Ultraviolet?f_ri=4363"},{"id":112063,"name":"Uv Radiation","url":"https://www.academia.edu/Documents/in/Uv_Radiation?f_ri=4363"},{"id":114377,"name":"Absorption spectroscopy","url":"https://www.academia.edu/Documents/in/Absorption_spectroscopy?f_ri=4363"},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=4363"},{"id":380824,"name":"Ozone","url":"https://www.academia.edu/Documents/in/Ozone?f_ri=4363"},{"id":494642,"name":"Structural Properties","url":"https://www.academia.edu/Documents/in/Structural_Properties?f_ri=4363"},{"id":745347,"name":"Relative Abundance","url":"https://www.academia.edu/Documents/in/Relative_Abundance?f_ri=4363"},{"id":911616,"name":"Space Missions","url":"https://www.academia.edu/Documents/in/Space_Missions?f_ri=4363"},{"id":1282080,"name":"Terrestrial Planets","url":"https://www.academia.edu/Documents/in/Terrestrial_Planets?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_34239884" data-work_id="34239884" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/34239884/Evolutionary_self_consistent_models_of_HII_galaxies">Evolutionary self-consistent models of HII galaxies</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We have studied the viability of new theoretical models which combine a chemical evolution code, an evolutionary synthesis code and a photoionization code, to understand the star formation and evolution of Hii galaxies. The emission lines... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_34239884" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We have studied the viability of new theoretical models which combine a chemical evolution code, an evolutionary synthesis code and a photoionization code, to understand the star formation and evolution of Hii galaxies. The emission lines observed in Hii galaxies are reproduced by meas of the photoionization code CLOUDY, using as ionizing spectrum the spectral energy distribution of the modeled Hii galaxy, which, in turn, is calculated according to a Star Formation History (SFH) and a metallicity evolution given by a chemical evolution model. Our technique reproduces the observed diagnostic diagrams and equivalent width-color correlations for local Hii galaxies.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/34239884" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="ad2edd630d6e6d411caa823700042c1c" rel="nofollow" data-download="{"attachment_id":54153730,"asset_id":34239884,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/54153730/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="37436472" href="https://uam.academia.edu/%C3%81ngelesD%C3%ADaz">Ángeles Díaz</a><script data-card-contents-for-user="37436472" type="text/json">{"id":37436472,"first_name":"Ángeles","last_name":"Díaz","domain_name":"uam","page_name":"ÁngelesDíaz","display_name":"Ángeles Díaz","profile_url":"https://uam.academia.edu/%C3%81ngelesD%C3%ADaz?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_34239884 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="34239884"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 34239884, container: ".js-paper-rank-work_34239884", }); 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$(".js-view-count[data-work-id=34239884]").text(description); $(".js-view-count-work_34239884").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_34239884").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="34239884"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">7</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="14920" rel="nofollow" href="https://www.academia.edu/Documents/in/Chemical_Evolution">Chemical Evolution</a>, <script data-card-contents-for-ri="14920" type="text/json">{"id":14920,"name":"Chemical Evolution","url":"https://www.academia.edu/Documents/in/Chemical_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="23179" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysics">Astrophysics</a>, <script data-card-contents-for-ri="23179" type="text/json">{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="321836" rel="nofollow" href="https://www.academia.edu/Documents/in/Spectrum">Spectrum</a><script data-card-contents-for-ri="321836" type="text/json">{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=34239884]'), work: {"id":34239884,"title":"Evolutionary self-consistent models of HII galaxies","created_at":"2017-08-16T03:33:37.476-07:00","url":"https://www.academia.edu/34239884/Evolutionary_self_consistent_models_of_HII_galaxies?f_ri=4363","dom_id":"work_34239884","summary":"We have studied the viability of new theoretical models which combine a chemical evolution code, an evolutionary synthesis code and a photoionization code, to understand the star formation and evolution of Hii galaxies. The emission lines observed in Hii galaxies are reproduced by meas of the photoionization code CLOUDY, using as ionizing spectrum the spectral energy distribution of the modeled Hii galaxy, which, in turn, is calculated according to a Star Formation History (SFH) and a metallicity evolution given by a chemical evolution model. Our technique reproduces the observed diagnostic diagrams and equivalent width-color correlations for local Hii galaxies.","downloadable_attachments":[{"id":54153730,"asset_id":34239884,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":37436472,"first_name":"Ángeles","last_name":"Díaz","domain_name":"uam","page_name":"ÁngelesDíaz","display_name":"Ángeles Díaz","profile_url":"https://uam.academia.edu/%C3%81ngelesD%C3%ADaz?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":14920,"name":"Chemical Evolution","url":"https://www.academia.edu/Documents/in/Chemical_Evolution?f_ri=4363","nofollow":true},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363","nofollow":true},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=4363","nofollow":true},{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363"},{"id":1154248,"name":"Theoretical Model","url":"https://www.academia.edu/Documents/in/Theoretical_Model?f_ri=4363"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_246654" data-work_id="246654" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" rel="nofollow" href="https://www.academia.edu/246654/The_GALEX_Mission_and_Detectors">The GALEX Mission and Detectors</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We describe the Galaxy Evolution Explorer (GALEX) satellite that was launched in April 2003 specifically to accomplish far ultraviolet (FUV) and near ultraviolet (NUV) imaging and spectroscopic sky-surveys. GALEX is currently providing... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_246654" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We describe the Galaxy Evolution Explorer (GALEX) satellite that was launched in April 2003 specifically to accomplish far ultraviolet (FUV) and near ultraviolet (NUV) imaging and spectroscopic sky-surveys. GALEX is currently providing new and significant information on how ...</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/246654" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="204825" href="https://utdallas.academia.edu/rmalina">roger malina</a><script data-card-contents-for-user="204825" type="text/json">{"id":204825,"first_name":"roger","last_name":"malina","domain_name":"utdallas","page_name":"rmalina","display_name":"roger malina","profile_url":"https://utdallas.academia.edu/rmalina?f_ri=4363","photo":"https://0.academia-photos.com/204825/4057673/4733674/s65_roger.malina.jpg_oh_20abb8f3fad6a664927ae3e0a5dceb81_oe_5462408f___gda___1415396291_1388b7baf1128efaa0c96e7f6850e97a"}</script></span></span></li><li class="js-paper-rank-work_246654 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="246654"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 246654, container: ".js-paper-rank-work_246654", }); 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$(".js-view-count[data-work-id=246654]").text(description); $(".js-view-count-work_246654").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_246654").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="246654"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11048" rel="nofollow" href="https://www.academia.edu/Documents/in/Galactic_Astronomy">Galactic Astronomy</a>, <script data-card-contents-for-ri="11048" type="text/json">{"id":11048,"name":"Galactic Astronomy","url":"https://www.academia.edu/Documents/in/Galactic_Astronomy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="40276" rel="nofollow" href="https://www.academia.edu/Documents/in/Proceedings">Proceedings</a>, <script data-card-contents-for-ri="40276" type="text/json">{"id":40276,"name":"Proceedings","url":"https://www.academia.edu/Documents/in/Proceedings?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="55405" rel="nofollow" href="https://www.academia.edu/Documents/in/Sensors">Sensors</a><script data-card-contents-for-ri="55405" type="text/json">{"id":55405,"name":"Sensors","url":"https://www.academia.edu/Documents/in/Sensors?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=246654]'), work: {"id":246654,"title":"The GALEX Mission and Detectors","created_at":"2010-06-19T19:04:10.721-07:00","url":"https://www.academia.edu/246654/The_GALEX_Mission_and_Detectors?f_ri=4363","dom_id":"work_246654","summary":"We describe the Galaxy Evolution Explorer (GALEX) satellite that was launched in April 2003 specifically to accomplish far ultraviolet (FUV) and near ultraviolet (NUV) imaging and spectroscopic sky-surveys. GALEX is currently providing new and significant information on how ...","downloadable_attachments":[],"ordered_authors":[{"id":204825,"first_name":"roger","last_name":"malina","domain_name":"utdallas","page_name":"rmalina","display_name":"roger malina","profile_url":"https://utdallas.academia.edu/rmalina?f_ri=4363","photo":"https://0.academia-photos.com/204825/4057673/4733674/s65_roger.malina.jpg_oh_20abb8f3fad6a664927ae3e0a5dceb81_oe_5462408f___gda___1415396291_1388b7baf1128efaa0c96e7f6850e97a"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11048,"name":"Galactic Astronomy","url":"https://www.academia.edu/Documents/in/Galactic_Astronomy?f_ri=4363","nofollow":true},{"id":40276,"name":"Proceedings","url":"https://www.academia.edu/Documents/in/Proceedings?f_ri=4363","nofollow":true},{"id":55405,"name":"Sensors","url":"https://www.academia.edu/Documents/in/Sensors?f_ri=4363","nofollow":true},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":1215509,"name":"Orbital Dynamics","url":"https://www.academia.edu/Documents/in/Orbital_Dynamics?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_19066228" data-work_id="19066228" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/19066228/Reconnection_Diffusion_in_Turbulent_Fluids_and_its_Implications_for_Star_Formation">Reconnection Diffusion in Turbulent Fluids and its Implications for Star Formation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Fast reconnection of magnetic field in turbulent fluids allows the field to change its topology and connec- tions. As a result, the traditional concept of magnetic fields being frozen into the plasma is no longer applicable. Plasma... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_19066228" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Fast reconnection of magnetic field in turbulent fluids allows the field to change its topology and connec- tions. As a result, the traditional concept of magnetic fields being frozen into the plasma is no longer applicable. Plasma associated with a given magnetic field line at one instant is distributed along a different set of magnetic field lines at the next instant. This diffusion of plasmas and magnetic field is enabled by reconnection and therefore is termed ”reconnec- tion diffusion”. The astrophysical implications of this con- cept include heat transfer in plasmas, advection of heavy el- ements in interstellar medium, magnetic field generation etc. However, the most dramatic implications of the concept are related to the star formation process. The reason is that mag- netic fields are dynamically important for most of the stages of star formation. The existing theory of star formation has been developed ignoring the possibility of reconnection dif- fusion. Instead, it appeals to the decoupling of mass and magnetic field arising from neutrals drifting in respect to ions entrained on magnetic field lines, i.e. through the pro- cess that is termed ”ambipolar diffusion”. The predictions of ambipolar diffusion and reconnection diffusion are very different. For instance, if the ionization of media is high, am- bipolar diffusion predicts that the coupling of mass and mag- netic field is nearly perfect. At the same time, reconnection diffusion is independent of the ionization but depends on the scale of the turbulent eddies and on the turbulent velocities. In the paper we explain the physics of reconnection diffusion both from macroscopic and microscopic points of view, i.e. appealing to the reconnection of flux tubes and to the dif-<br />the dynamics of many key processes, including magnetic re- connection. Fast reconnection of magnetic field in turbulent fluids allows the field to change its topology and connec- tions. As a result, the traditional concept of magnetic fields being frozen into the plasma is no longer applicable. Plasma associated with a given magnetic field line at one instant is distributed along a different set of magnetic field lines at the next instant. This diffusion of plasmas and magnetic field is enabled by reconnection and therefore is termed ”reconnec- tion diffusion”. The astrophysical implications of this con- cept include heat transfer in plasmas, advection of heavy el- ements in interstellar medium, magnetic field generation etc. However, the most dramatic implications of the concept are related to the star formation process. The reason is that mag- netic fields are dynamically important for most of the stages of star formation. The existing theory of star formation has been developed ignoring the possibility of reconnection dif- fusion. Instead, it appeals to the decoupling of mass and magnetic field arising from neutrals drifting in respect to ions entrained on magnetic field lines, i.e. through the pro- cess that is termed ”ambipolar diffusion”. The predictions of ambipolar diffusion and reconnection diffusion are very different. For instance, if the ionization of media is high, am- bipolar diffusion predicts that the coupling of mass and mag- netic field is nearly perfect. At the same time, reconnection diffusion is independent of the ionization but depends on the scale of the turbulent eddies and on the turbulent velocities. In the paper we explain the physics of reconnection diffusion both from macroscopic and microscopic points of view. We make use of the Lazarian & Vishniac 1999 theory of magnetic reconnection and show that this theory is applicable to the partially ionized gas. We quantify the reconnection diffusion rate both for weak and strong MHD turbulence and address the problem of recon- nection diffusion acting together with ambipolar diffusion. In addition, we provide a criterion for correctly representing the magnetic diffusivity in simulations of star formation. We discuss the intimate relation between the processes of recon- nection diffusion, field wandering and turbulent mixing of a magnetized media and show that the role of the plasma ef- fects is limited to ”breaking up lines” on small scales and does not affect the rate of reconnection diffusion. We ad- dress the existing observational results and demonstrate how reconnection diffusion can explain the puzzles presented by observations, in particular, the observed higher magnetiza- tion of cloud cores in comparison with the magnetization of envelopes. We also outline a possible set of observational tests of the reconnection diffusion concept and discuss how the application of the new concept changes our understand- ing of star formation and its numerical modeling. Finally, we outline the differences of the process of reconnection diffusion and the process of accumulation of matter along magnetic field lines that is frequently invoked to explain the results of numerical simulations</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/19066228" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="174716985491c2eab746368be63ef5e0" rel="nofollow" data-download="{"attachment_id":40411412,"asset_id":19066228,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/40411412/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="39237502" href="https://wisc.academia.edu/ALazarian">A. Lazarian</a><script data-card-contents-for-user="39237502" type="text/json">{"id":39237502,"first_name":"A.","last_name":"Lazarian","domain_name":"wisc","page_name":"ALazarian","display_name":"A. Lazarian","profile_url":"https://wisc.academia.edu/ALazarian?f_ri=4363","photo":"https://0.academia-photos.com/39237502/18762506/18723319/s65_a..lazarian.jpg"}</script></span></span></li><li class="js-paper-rank-work_19066228 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="19066228"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 19066228, container: ".js-paper-rank-work_19066228", }); });</script></li><li class="js-percentile-work_19066228 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 19066228; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_19066228"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_19066228 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="19066228"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 19066228; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=19066228]").text(description); $(".js-view-count-work_19066228").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_19066228").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="19066228"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="2802" rel="nofollow" href="https://www.academia.edu/Documents/in/Turbulence">Turbulence</a>, <script data-card-contents-for-ri="2802" type="text/json">{"id":2802,"name":"Turbulence","url":"https://www.academia.edu/Documents/in/Turbulence?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="22999" rel="nofollow" href="https://www.academia.edu/Documents/in/Cosmic_Rays">Cosmic Rays</a>, <script data-card-contents-for-ri="22999" type="text/json">{"id":22999,"name":"Cosmic Rays","url":"https://www.academia.edu/Documents/in/Cosmic_Rays?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="121397" rel="nofollow" href="https://www.academia.edu/Documents/in/Magnetic_Reconnection">Magnetic Reconnection</a><script data-card-contents-for-ri="121397" type="text/json">{"id":121397,"name":"Magnetic Reconnection","url":"https://www.academia.edu/Documents/in/Magnetic_Reconnection?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=19066228]'), work: {"id":19066228,"title":"Reconnection Diffusion in Turbulent Fluids and its Implications for Star Formation","created_at":"2015-11-26T14:59:59.118-08:00","url":"https://www.academia.edu/19066228/Reconnection_Diffusion_in_Turbulent_Fluids_and_its_Implications_for_Star_Formation?f_ri=4363","dom_id":"work_19066228","summary":"Fast reconnection of magnetic field in turbulent fluids allows the field to change its topology and connec- tions. As a result, the traditional concept of magnetic fields being frozen into the plasma is no longer applicable. Plasma associated with a given magnetic field line at one instant is distributed along a different set of magnetic field lines at the next instant. This diffusion of plasmas and magnetic field is enabled by reconnection and therefore is termed ”reconnec- tion diffusion”. The astrophysical implications of this con- cept include heat transfer in plasmas, advection of heavy el- ements in interstellar medium, magnetic field generation etc. However, the most dramatic implications of the concept are related to the star formation process. The reason is that mag- netic fields are dynamically important for most of the stages of star formation. The existing theory of star formation has been developed ignoring the possibility of reconnection dif- fusion. Instead, it appeals to the decoupling of mass and magnetic field arising from neutrals drifting in respect to ions entrained on magnetic field lines, i.e. through the pro- cess that is termed ”ambipolar diffusion”. The predictions of ambipolar diffusion and reconnection diffusion are very different. For instance, if the ionization of media is high, am- bipolar diffusion predicts that the coupling of mass and mag- netic field is nearly perfect. At the same time, reconnection diffusion is independent of the ionization but depends on the scale of the turbulent eddies and on the turbulent velocities. In the paper we explain the physics of reconnection diffusion both from macroscopic and microscopic points of view, i.e. appealing to the reconnection of flux tubes and to the dif-\nthe dynamics of many key processes, including magnetic re- connection. Fast reconnection of magnetic field in turbulent fluids allows the field to change its topology and connec- tions. As a result, the traditional concept of magnetic fields being frozen into the plasma is no longer applicable. Plasma associated with a given magnetic field line at one instant is distributed along a different set of magnetic field lines at the next instant. This diffusion of plasmas and magnetic field is enabled by reconnection and therefore is termed ”reconnec- tion diffusion”. The astrophysical implications of this con- cept include heat transfer in plasmas, advection of heavy el- ements in interstellar medium, magnetic field generation etc. However, the most dramatic implications of the concept are related to the star formation process. The reason is that mag- netic fields are dynamically important for most of the stages of star formation. The existing theory of star formation has been developed ignoring the possibility of reconnection dif- fusion. Instead, it appeals to the decoupling of mass and magnetic field arising from neutrals drifting in respect to ions entrained on magnetic field lines, i.e. through the pro- cess that is termed ”ambipolar diffusion”. The predictions of ambipolar diffusion and reconnection diffusion are very different. For instance, if the ionization of media is high, am- bipolar diffusion predicts that the coupling of mass and mag- netic field is nearly perfect. At the same time, reconnection diffusion is independent of the ionization but depends on the scale of the turbulent eddies and on the turbulent velocities. In the paper we explain the physics of reconnection diffusion both from macroscopic and microscopic points of view. We make use of the Lazarian \u0026 Vishniac 1999 theory of magnetic reconnection and show that this theory is applicable to the partially ionized gas. We quantify the reconnection diffusion rate both for weak and strong MHD turbulence and address the problem of recon- nection diffusion acting together with ambipolar diffusion. In addition, we provide a criterion for correctly representing the magnetic diffusivity in simulations of star formation. We discuss the intimate relation between the processes of recon- nection diffusion, field wandering and turbulent mixing of a magnetized media and show that the role of the plasma ef- fects is limited to ”breaking up lines” on small scales and does not affect the rate of reconnection diffusion. We ad- dress the existing observational results and demonstrate how reconnection diffusion can explain the puzzles presented by observations, in particular, the observed higher magnetiza- tion of cloud cores in comparison with the magnetization of envelopes. We also outline a possible set of observational tests of the reconnection diffusion concept and discuss how the application of the new concept changes our understand- ing of star formation and its numerical modeling. Finally, we outline the differences of the process of reconnection diffusion and the process of accumulation of matter along magnetic field lines that is frequently invoked to explain the results of numerical simulations","downloadable_attachments":[{"id":40411412,"asset_id":19066228,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":39237502,"first_name":"A.","last_name":"Lazarian","domain_name":"wisc","page_name":"ALazarian","display_name":"A. Lazarian","profile_url":"https://wisc.academia.edu/ALazarian?f_ri=4363","photo":"https://0.academia-photos.com/39237502/18762506/18723319/s65_a..lazarian.jpg"}],"research_interests":[{"id":2802,"name":"Turbulence","url":"https://www.academia.edu/Documents/in/Turbulence?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":22999,"name":"Cosmic Rays","url":"https://www.academia.edu/Documents/in/Cosmic_Rays?f_ri=4363","nofollow":true},{"id":121397,"name":"Magnetic Reconnection","url":"https://www.academia.edu/Documents/in/Magnetic_Reconnection?f_ri=4363","nofollow":true},{"id":977840,"name":"Particle Acceleration","url":"https://www.academia.edu/Documents/in/Particle_Acceleration?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_17599371" data-work_id="17599371" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/17599371/The_Stellar_Content_of_Giant_H_ii_Regions_in_NGC_7714">The Stellar Content of Giant H ii Regions in NGC 7714</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">In this work we investigate the stellar content of three circumnuclear giant H II regions in the starburst galaxy NGC 7714. We model the stellar population that best reproduces the observational constraints given by the Ha image and the... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_17599371" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">In this work we investigate the stellar content of three circumnuclear giant H II regions in the starburst galaxy NGC 7714. We model the stellar population that best reproduces the observational constraints given by the Ha image and the optical spectroscopy from 3710 to 9700 Ó.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/17599371" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="c00ada7c661480938931802d9303a38e" rel="nofollow" data-download="{"attachment_id":39605039,"asset_id":17599371,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/39605039/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="37436472" href="https://uam.academia.edu/%C3%81ngelesD%C3%ADaz">Ángeles Díaz</a><script data-card-contents-for-user="37436472" type="text/json">{"id":37436472,"first_name":"Ángeles","last_name":"Díaz","domain_name":"uam","page_name":"ÁngelesDíaz","display_name":"Ángeles Díaz","profile_url":"https://uam.academia.edu/%C3%81ngelesD%C3%ADaz?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_17599371 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="17599371"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 17599371, container: ".js-paper-rank-work_17599371", }); 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$(".js-view-count[data-work-id=17599371]").text(description); $(".js-view-count-work_17599371").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_17599371").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="17599371"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">10</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="13033" rel="nofollow" href="https://www.academia.edu/Documents/in/Optical_Spectroscopy">Optical Spectroscopy</a><script data-card-contents-for-ri="13033" type="text/json">{"id":13033,"name":"Optical Spectroscopy","url":"https://www.academia.edu/Documents/in/Optical_Spectroscopy?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=17599371]'), work: {"id":17599371,"title":"The Stellar Content of Giant H ii Regions in NGC 7714","created_at":"2015-11-02T01:08:43.391-08:00","url":"https://www.academia.edu/17599371/The_Stellar_Content_of_Giant_H_ii_Regions_in_NGC_7714?f_ri=4363","dom_id":"work_17599371","summary":"In this work we investigate the stellar content of three circumnuclear giant H II regions in the starburst galaxy NGC 7714. We model the stellar population that best reproduces the observational constraints given by the Ha image and the optical spectroscopy from 3710 to 9700 Ó.","downloadable_attachments":[{"id":39605039,"asset_id":17599371,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":37436472,"first_name":"Ángeles","last_name":"Díaz","domain_name":"uam","page_name":"ÁngelesDíaz","display_name":"Ángeles Díaz","profile_url":"https://uam.academia.edu/%C3%81ngelesD%C3%ADaz?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":13033,"name":"Optical Spectroscopy","url":"https://www.academia.edu/Documents/in/Optical_Spectroscopy?f_ri=4363","nofollow":true},{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363"},{"id":97563,"name":"Galaxy evolution","url":"https://www.academia.edu/Documents/in/Galaxy_evolution?f_ri=4363"},{"id":321836,"name":"Spectrum","url":"https://www.academia.edu/Documents/in/Spectrum?f_ri=4363"},{"id":962097,"name":"Star Clusters","url":"https://www.academia.edu/Documents/in/Star_Clusters?f_ri=4363"},{"id":977447,"name":"Starburst Galaxies","url":"https://www.academia.edu/Documents/in/Starburst_Galaxies?f_ri=4363"},{"id":1228946,"name":"Physical Properties","url":"https://www.academia.edu/Documents/in/Physical_Properties?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_53050499" data-work_id="53050499" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/53050499/Discovery_of_large_scale_gravitational_infall_in_a_massive_protostellar_cluster">Discovery of large-scale gravitational infall in a massive protostellar cluster</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We report Mopra Australia Telescope National Facility (ATNF), Anglo-Australian Telescope and Atacama Submillimeter Telescope Experiment observations of a molecular clump in Carina, BYF73 = G286.21+0.17, which give evidence of large-scale... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_53050499" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We report Mopra Australia Telescope National Facility (ATNF), Anglo-Australian Telescope and Atacama Submillimeter Telescope Experiment observations of a molecular clump in Carina, BYF73 = G286.21+0.17, which give evidence of large-scale gravitational infall in the dense gas. From the millimetre and far-infrared data, the clump has a mass of ~2 × 104Msolar, luminosity of ~2-3 × 104Lsolar and diameter of ~0.9 pc. From radiative transfer modelling, we derive a mass infall rate of ~3.4 × 10-2Msolaryr-1. If confirmed, this rate for gravitational infall in a molecular core or clump may be the highest yet seen. The near-infrared K-band imaging shows an adjacent compact HII region and IR cluster surrounded by a shell-like photodissociation region showing H2 emission. At the molecular infall peak, the K imaging also reveals a deeply embedded group of stars with associated H2 emission. The combination of these features is very unusual, and we suggest that they indicate the ongoing formation ...</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/53050499" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="210250ff0951d5f2418191ec0c1cb6f6" rel="nofollow" data-download="{"attachment_id":70016901,"asset_id":53050499,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/70016901/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="57155228" href="https://independent.academia.edu/YoshinoriYonekura">Yoshinori Yonekura</a><script data-card-contents-for-user="57155228" type="text/json">{"id":57155228,"first_name":"Yoshinori","last_name":"Yonekura","domain_name":"independent","page_name":"YoshinoriYonekura","display_name":"Yoshinori Yonekura","profile_url":"https://independent.academia.edu/YoshinoriYonekura?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_53050499 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="53050499"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 53050499, container: ".js-paper-rank-work_53050499", }); 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$(".js-view-count[data-work-id=53050499]").text(description); $(".js-view-count-work_53050499").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_53050499").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="53050499"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">18</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11124" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrochemistry">Astrochemistry</a>, <script data-card-contents-for-ri="11124" type="text/json">{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="14919" rel="nofollow" href="https://www.academia.edu/Documents/in/HII_Regions">HII Regions</a>, <script data-card-contents-for-ri="14919" type="text/json">{"id":14919,"name":"HII Regions","url":"https://www.academia.edu/Documents/in/HII_Regions?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="23940" rel="nofollow" href="https://www.academia.edu/Documents/in/Near_Infrared">Near Infrared</a><script data-card-contents-for-ri="23940" type="text/json">{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=53050499]'), work: {"id":53050499,"title":"Discovery of large-scale gravitational infall in a massive protostellar cluster","created_at":"2021-09-20T17:21:45.318-07:00","url":"https://www.academia.edu/53050499/Discovery_of_large_scale_gravitational_infall_in_a_massive_protostellar_cluster?f_ri=4363","dom_id":"work_53050499","summary":"We report Mopra Australia Telescope National Facility (ATNF), Anglo-Australian Telescope and Atacama Submillimeter Telescope Experiment observations of a molecular clump in Carina, BYF73 = G286.21+0.17, which give evidence of large-scale gravitational infall in the dense gas. From the millimetre and far-infrared data, the clump has a mass of ~2 × 104Msolar, luminosity of ~2-3 × 104Lsolar and diameter of ~0.9 pc. From radiative transfer modelling, we derive a mass infall rate of ~3.4 × 10-2Msolaryr-1. If confirmed, this rate for gravitational infall in a molecular core or clump may be the highest yet seen. The near-infrared K-band imaging shows an adjacent compact HII region and IR cluster surrounded by a shell-like photodissociation region showing H2 emission. At the molecular infall peak, the K imaging also reveals a deeply embedded group of stars with associated H2 emission. The combination of these features is very unusual, and we suggest that they indicate the ongoing formation ...","downloadable_attachments":[{"id":70016901,"asset_id":53050499,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":57155228,"first_name":"Yoshinori","last_name":"Yonekura","domain_name":"independent","page_name":"YoshinoriYonekura","display_name":"Yoshinori Yonekura","profile_url":"https://independent.academia.edu/YoshinoriYonekura?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=4363","nofollow":true},{"id":14919,"name":"HII Regions","url":"https://www.academia.edu/Documents/in/HII_Regions?f_ri=4363","nofollow":true},{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true},{"id":62320,"name":"Dynamics","url":"https://www.academia.edu/Documents/in/Dynamics?f_ri=4363"},{"id":90162,"name":"Kinematics","url":"https://www.academia.edu/Documents/in/Kinematics?f_ri=4363"},{"id":174322,"name":"Kinematics and Dynamics","url":"https://www.academia.edu/Documents/in/Kinematics_and_Dynamics?f_ri=4363"},{"id":176853,"name":"Luminosity","url":"https://www.academia.edu/Documents/in/Luminosity?f_ri=4363"},{"id":220059,"name":"Subject headings","url":"https://www.academia.edu/Documents/in/Subject_headings?f_ri=4363"},{"id":290733,"name":"Stars","url":"https://www.academia.edu/Documents/in/Stars?f_ri=4363"},{"id":328449,"name":"Molecules","url":"https://www.academia.edu/Documents/in/Molecules?f_ri=4363"},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363"},{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363"},{"id":442314,"name":"Radiative Transfer","url":"https://www.academia.edu/Documents/in/Radiative_Transfer?f_ri=4363"},{"id":758278,"name":"Large Scale","url":"https://www.academia.edu/Documents/in/Large_Scale?f_ri=4363"},{"id":962097,"name":"Star Clusters","url":"https://www.academia.edu/Documents/in/Star_Clusters?f_ri=4363"},{"id":1029319,"name":"Diameter","url":"https://www.academia.edu/Documents/in/Diameter?f_ri=4363"},{"id":1121984,"name":"Photodissociation","url":"https://www.academia.edu/Documents/in/Photodissociation?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_16086528" data-work_id="16086528" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/16086528/Protostars_and_Outflows_in_the_NGC_7538_IRS_9_Cloud_Core">Protostars and Outflows in the NGC 7538 IRS 9 Cloud Core</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">New high resolution observations of HCO + J = 1 → 0, H 13 CN J = 1 → 0, SO 2 2 → 1 1 , and continuum with BIMA at 3.4 mm show that the NGC 7538 -IRS 9 cloud core is a site of active ongoing star formation. Our observations reveal at least... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_16086528" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">New high resolution observations of HCO + J = 1 → 0, H 13 CN J = 1 → 0, SO 2 2 → 1 1 , and continuum with BIMA at 3.4 mm show that the NGC 7538 -IRS 9 cloud core is a site of active ongoing star formation. Our observations reveal at least three young bipolar molecular outflows, all ∼ 10,000 -20,000 years old. IRS 9 drives a bipolar, extreme high velocity outflow observed nearly pole on. South of IRS 9 we find a cold, protostellar condensation with a size of ∼ 14 ′′ × 6 ′′ with a mass > 250 M ⊙ . This is the center of one of the outflows and shows deep, red-shifted self absorption in HCO + , suggesting that there is a protostar embedded in the core, still in a phase of active accretion. This source is not detected in the far infrared, suggesting that the luminosity < 10 4 L ⊙ ; yet the mass of the outflow is ∼ 60 M ⊙ . The red-shifted HCO + self-absorption profiles observed toward the southern protostar and IRS 9 predict accretion rates of a few times 10 −4 to 10 −3 M ⊙ yr −1 . Deep VLA continuum observations at 3.6 cm show that IRS 9 coincides with a faint thermal VLA source, but no other young star in the IRS 9 region has any detectable free-free emission at a level of ∼ 60 µJy at 3.6 cm. The HCO + abundance is significantly enhanced in the hot IRS 9 outflow. A direct comparison of mass estimates from HCO + and CO for the well-characterized red-shifted IRS 9 outflow predicts an HCO + enhancement of more than a factor of 30, or [HCO + /H 2 ] ≥ 6 10 −8 .</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/16086528" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="7f1b8fb3eb9ae3c9bb7b3f70282dedc1" rel="nofollow" data-download="{"attachment_id":42753394,"asset_id":16086528,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/42753394/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="35210285" href="https://independent.academia.edu/MelvynWright">Melvyn Wright</a><script data-card-contents-for-user="35210285" type="text/json">{"id":35210285,"first_name":"Melvyn","last_name":"Wright","domain_name":"independent","page_name":"MelvynWright","display_name":"Melvyn Wright","profile_url":"https://independent.academia.edu/MelvynWright?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_16086528 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="16086528"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 16086528, container: ".js-paper-rank-work_16086528", }); 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$(".js-view-count[data-work-id=16086528]").text(description); $(".js-view-count-work_16086528").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_16086528").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="16086528"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="309086" rel="nofollow" href="https://www.academia.edu/Documents/in/High_Resolution">High Resolution</a><script data-card-contents-for-ri="309086" type="text/json">{"id":309086,"name":"High Resolution","url":"https://www.academia.edu/Documents/in/High_Resolution?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=16086528]'), work: {"id":16086528,"title":"Protostars and Outflows in the NGC 7538 IRS 9 Cloud Core","created_at":"2015-09-23T08:44:22.507-07:00","url":"https://www.academia.edu/16086528/Protostars_and_Outflows_in_the_NGC_7538_IRS_9_Cloud_Core?f_ri=4363","dom_id":"work_16086528","summary":"New high resolution observations of HCO + J = 1 → 0, H 13 CN J = 1 → 0, SO 2 2 → 1 1 , and continuum with BIMA at 3.4 mm show that the NGC 7538 -IRS 9 cloud core is a site of active ongoing star formation. Our observations reveal at least three young bipolar molecular outflows, all ∼ 10,000 -20,000 years old. IRS 9 drives a bipolar, extreme high velocity outflow observed nearly pole on. South of IRS 9 we find a cold, protostellar condensation with a size of ∼ 14 ′′ × 6 ′′ with a mass \u003e 250 M ⊙ . This is the center of one of the outflows and shows deep, red-shifted self absorption in HCO + , suggesting that there is a protostar embedded in the core, still in a phase of active accretion. This source is not detected in the far infrared, suggesting that the luminosity \u003c 10 4 L ⊙ ; yet the mass of the outflow is ∼ 60 M ⊙ . The red-shifted HCO + self-absorption profiles observed toward the southern protostar and IRS 9 predict accretion rates of a few times 10 −4 to 10 −3 M ⊙ yr −1 . Deep VLA continuum observations at 3.6 cm show that IRS 9 coincides with a faint thermal VLA source, but no other young star in the IRS 9 region has any detectable free-free emission at a level of ∼ 60 µJy at 3.6 cm. The HCO + abundance is significantly enhanced in the hot IRS 9 outflow. A direct comparison of mass estimates from HCO + and CO for the well-characterized red-shifted IRS 9 outflow predicts an HCO + enhancement of more than a factor of 30, or [HCO + /H 2 ] ≥ 6 10 −8 .","downloadable_attachments":[{"id":42753394,"asset_id":16086528,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":35210285,"first_name":"Melvyn","last_name":"Wright","domain_name":"independent","page_name":"MelvynWright","display_name":"Melvyn Wright","profile_url":"https://independent.academia.edu/MelvynWright?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":309086,"name":"High Resolution","url":"https://www.academia.edu/Documents/in/High_Resolution?f_ri=4363","nofollow":true},{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_3814793" data-work_id="3814793" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/3814793/The_Galactic_Habitable_Zone_Galactic_Chemical_Evolution">The Galactic Habitable Zone: Galactic Chemical Evolution</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We propose the concept of a "Galactic Habitable Zone" (GHZ). Analogous to the Circumstellar Habitable Zone (CHZ), the GHZ is that region in the Milky Way where an Earth-like planet can retain liquid water on its surface and provide a... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_3814793" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We propose the concept of a "Galactic Habitable Zone" (GHZ). Analogous to the Circumstellar Habitable Zone (CHZ), the GHZ is that region in the Milky Way where an Earth-like planet can retain liquid water on its surface and provide a long-term habitat for animal-like aerobic life. In this paper we examine the dependence of the GHZ on Galactic chemical evolution. The single most important factor is likely the dependence of terrestrial planet mass on the metallicity of its birth cloud. We estimate, very approximately, that a metallicity at least half that of the Sun is required to build a habitable terrestrial planet. The mass of a terrestrial planet has important consequences for interior heat loss, volatile inventory, and loss of atmosphere. A key issue is the production of planets that sustain plate tectonics, a critical recycling process that provides feedback to stabilize atmospheric temperatures on planets with oceans and atmospheres. Due to the more recent decline from the early intense star formation activity in the Milky Way, the concentration in the interstellar medium of the geophysically important radioisotopes 40 K, 235,238 U, and 232 Th has been declining relative to Fe, an abundant element in the Earth. Also likely important are the relative abundances of Si and Mg to Fe, which affects the mass of the core relative to the mantle in a terrestrial planet. All these elements and isotopes vary with time and location in the Milky Way; thus, planetary systems forming in other locations and times in the Milky Way with the same metallicity as the Sun will not necessarily form habitable Earth-like planets. As a result of the radial Galactic metallicity gradient, the outer limit of the GHZ is set primarily by the minimum required metallicity to build large terrestrial planets. Regions of the Milky Way least likely to contain Earth-mass planets are the halo (including globular clusters), the thick disk, and the outer thin disk. The bulge should contain Earth-mass planets, but stars in it have a mix of elements different from the Sun's. The existence of a luminosity-metallicity correlation among galaxies of all types means that many galaxies are too metal-poor to contain Earth-mass planets. Based on the observed luminosity function of nearby galaxies in the visual passband, we estimate that (1) the Milky Way is among the 1.3% most luminous (and hence most metal-rich) galaxies and (2) about 23% of stars in a typical ensemble of galaxies are more metal-rich than the average star in the Milky Way. The GHZ zone concept can be easily extrapolated to the universe as a whole, especially with regard to the changing star formation rate and its effect on metallicity and abundances of the long-lived radioisotopes.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/3814793" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="678f8fa02a18dd4fa10fb051dfba378d" rel="nofollow" data-download="{"attachment_id":31468566,"asset_id":3814793,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/31468566/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="4692397" href="https://unah.academia.edu/GuillermoGonzalez">Guillermo Gonzalez</a><script data-card-contents-for-user="4692397" type="text/json">{"id":4692397,"first_name":"Guillermo","last_name":"Gonzalez","domain_name":"unah","page_name":"GuillermoGonzalez","display_name":"Guillermo Gonzalez","profile_url":"https://unah.academia.edu/GuillermoGonzalez?f_ri=4363","photo":"https://0.academia-photos.com/4692397/1976750/2335036/s65_guillermo.gonzalez.jpg"}</script></span></span></li><li class="js-paper-rank-work_3814793 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="3814793"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 3814793, container: ".js-paper-rank-work_3814793", }); 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$(".js-view-count[data-work-id=3814793]").text(description); $(".js-view-count-work_3814793").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_3814793").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="3814793"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">15</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="407" rel="nofollow" href="https://www.academia.edu/Documents/in/Geochemistry">Geochemistry</a>, <script data-card-contents-for-ri="407" type="text/json">{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="409" rel="nofollow" href="https://www.academia.edu/Documents/in/Geophysics">Geophysics</a>, <script data-card-contents-for-ri="409" type="text/json">{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="716" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium">Interstellar Medium</a>, <script data-card-contents-for-ri="716" type="text/json">{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2449" rel="nofollow" href="https://www.academia.edu/Documents/in/Cosmochemistry">Cosmochemistry</a><script data-card-contents-for-ri="2449" type="text/json">{"id":2449,"name":"Cosmochemistry","url":"https://www.academia.edu/Documents/in/Cosmochemistry?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=3814793]'), work: {"id":3814793,"title":"The Galactic Habitable Zone: Galactic Chemical Evolution","created_at":"2013-06-29T00:41:18.912-07:00","url":"https://www.academia.edu/3814793/The_Galactic_Habitable_Zone_Galactic_Chemical_Evolution?f_ri=4363","dom_id":"work_3814793","summary":"We propose the concept of a \"Galactic Habitable Zone\" (GHZ). Analogous to the Circumstellar Habitable Zone (CHZ), the GHZ is that region in the Milky Way where an Earth-like planet can retain liquid water on its surface and provide a long-term habitat for animal-like aerobic life. In this paper we examine the dependence of the GHZ on Galactic chemical evolution. The single most important factor is likely the dependence of terrestrial planet mass on the metallicity of its birth cloud. We estimate, very approximately, that a metallicity at least half that of the Sun is required to build a habitable terrestrial planet. The mass of a terrestrial planet has important consequences for interior heat loss, volatile inventory, and loss of atmosphere. A key issue is the production of planets that sustain plate tectonics, a critical recycling process that provides feedback to stabilize atmospheric temperatures on planets with oceans and atmospheres. Due to the more recent decline from the early intense star formation activity in the Milky Way, the concentration in the interstellar medium of the geophysically important radioisotopes 40 K, 235,238 U, and 232 Th has been declining relative to Fe, an abundant element in the Earth. Also likely important are the relative abundances of Si and Mg to Fe, which affects the mass of the core relative to the mantle in a terrestrial planet. All these elements and isotopes vary with time and location in the Milky Way; thus, planetary systems forming in other locations and times in the Milky Way with the same metallicity as the Sun will not necessarily form habitable Earth-like planets. As a result of the radial Galactic metallicity gradient, the outer limit of the GHZ is set primarily by the minimum required metallicity to build large terrestrial planets. Regions of the Milky Way least likely to contain Earth-mass planets are the halo (including globular clusters), the thick disk, and the outer thin disk. The bulge should contain Earth-mass planets, but stars in it have a mix of elements different from the Sun's. The existence of a luminosity-metallicity correlation among galaxies of all types means that many galaxies are too metal-poor to contain Earth-mass planets. Based on the observed luminosity function of nearby galaxies in the visual passband, we estimate that (1) the Milky Way is among the 1.3% most luminous (and hence most metal-rich) galaxies and (2) about 23% of stars in a typical ensemble of galaxies are more metal-rich than the average star in the Milky Way. The GHZ zone concept can be easily extrapolated to the universe as a whole, especially with regard to the changing star formation rate and its effect on metallicity and abundances of the long-lived radioisotopes.","downloadable_attachments":[{"id":31468566,"asset_id":3814793,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":4692397,"first_name":"Guillermo","last_name":"Gonzalez","domain_name":"unah","page_name":"GuillermoGonzalez","display_name":"Guillermo Gonzalez","profile_url":"https://unah.academia.edu/GuillermoGonzalez?f_ri=4363","photo":"https://0.academia-photos.com/4692397/1976750/2335036/s65_guillermo.gonzalez.jpg"}],"research_interests":[{"id":407,"name":"Geochemistry","url":"https://www.academia.edu/Documents/in/Geochemistry?f_ri=4363","nofollow":true},{"id":409,"name":"Geophysics","url":"https://www.academia.edu/Documents/in/Geophysics?f_ri=4363","nofollow":true},{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true},{"id":2449,"name":"Cosmochemistry","url":"https://www.academia.edu/Documents/in/Cosmochemistry?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363"},{"id":40075,"name":"Planetary Formation","url":"https://www.academia.edu/Documents/in/Planetary_Formation?f_ri=4363"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363"},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363"},{"id":195544,"name":"Planetary Systems","url":"https://www.academia.edu/Documents/in/Planetary_Systems?f_ri=4363"},{"id":415653,"name":"Luminosity function","url":"https://www.academia.edu/Documents/in/Luminosity_function?f_ri=4363"},{"id":517654,"name":"Icarus","url":"https://www.academia.edu/Documents/in/Icarus?f_ri=4363"},{"id":745347,"name":"Relative Abundance","url":"https://www.academia.edu/Documents/in/Relative_Abundance?f_ri=4363"},{"id":814934,"name":"Plate tectonic","url":"https://www.academia.edu/Documents/in/Plate_tectonic?f_ri=4363"},{"id":1282080,"name":"Terrestrial Planets","url":"https://www.academia.edu/Documents/in/Terrestrial_Planets?f_ri=4363"},{"id":2263907,"name":"Heat Loss","url":"https://www.academia.edu/Documents/in/Heat_Loss?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_2615056" data-work_id="2615056" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/2615056/Chemical_and_physical_characterization_of_the_first_stages_of_protoplanetary_disk_formation">Chemical and physical characterization of the first stages of protoplanetary disk formation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Low mass stars, like our Sun, are born from the collapse of a molecular cloud. The matter falls in the center of the cloud, creating a protoplanetary disk surrounding a protostar. Planets and other solar system bodies will be formed in... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_2615056" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Low mass stars, like our Sun, are born from the collapse of a molecular cloud. The matter falls in the center of the cloud, creating a protoplanetary disk surrounding a protostar. Planets and other solar system bodies will be formed in the disk.The chemical composition of the interstellar matter and its evolution during the formation of the disk are important to better understand the formation process of these objects.I studied the chemical and physical evolution of this matter, from the cloud to the disk, using the chemical gas-grain code Nautilus.A sensitivity study to some parameters of the code (such as elemental abundances and parameters of grain surface chemistry) has been done. More particularly, the updates of rate coefficients and branching ratios of the reactions of our chemical network showed their importance, such as on the abundances of some chemical species, and on the code sensitivity to others parameters.Several physical models of collapsing dense core have also been considered. The more complex and solid approach has been to interface our chemical code with the radiation-magneto-hydrodynamic model of stellar formation RAMSES, in order to model in three dimensions the physical and chemical evolution of a young disk formation. Our study showed that the disk keeps imprints of the past history of the matter, and so its chemical composition is sensitive to the initial conditions.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/2615056" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="cd44b2f832f71d9e7fad0e3cd806764f" rel="nofollow" data-download="{"attachment_id":30622112,"asset_id":2615056,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/30622112/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="130522" href="https://virginia.academia.edu/UgoHincelin">Ugo Hincelin</a><script data-card-contents-for-user="130522" type="text/json">{"id":130522,"first_name":"Ugo","last_name":"Hincelin","domain_name":"virginia","page_name":"UgoHincelin","display_name":"Ugo Hincelin","profile_url":"https://virginia.academia.edu/UgoHincelin?f_ri=4363","photo":"https://0.academia-photos.com/130522/487960/614228/s65_ugo.hincelin.jpg"}</script></span></span></li><li class="js-paper-rank-work_2615056 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="2615056"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 2615056, container: ".js-paper-rank-work_2615056", }); });</script></li><li class="js-percentile-work_2615056 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 2615056; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_2615056"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_2615056 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="2615056"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 2615056; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=2615056]").text(description); $(".js-view-count-work_2615056").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_2615056").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="2615056"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">6</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="716" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium">Interstellar Medium</a>, <script data-card-contents-for-ri="716" type="text/json">{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="721" rel="nofollow" href="https://www.academia.edu/Documents/in/Magnetohydrodynamics">Magnetohydrodynamics</a>, <script data-card-contents-for-ri="721" type="text/json">{"id":721,"name":"Magnetohydrodynamics","url":"https://www.academia.edu/Documents/in/Magnetohydrodynamics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11124" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrochemistry">Astrochemistry</a><script data-card-contents-for-ri="11124" type="text/json">{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=2615056]'), work: {"id":2615056,"title":"Chemical and physical characterization of the first stages of protoplanetary disk formation","created_at":"2013-02-20T04:32:53.038-08:00","url":"https://www.academia.edu/2615056/Chemical_and_physical_characterization_of_the_first_stages_of_protoplanetary_disk_formation?f_ri=4363","dom_id":"work_2615056","summary":"Low mass stars, like our Sun, are born from the collapse of a molecular cloud. The matter falls in the center of the cloud, creating a protoplanetary disk surrounding a protostar. Planets and other solar system bodies will be formed in the disk.The chemical composition of the interstellar matter and its evolution during the formation of the disk are important to better understand the formation process of these objects.I studied the chemical and physical evolution of this matter, from the cloud to the disk, using the chemical gas-grain code Nautilus.A sensitivity study to some parameters of the code (such as elemental abundances and parameters of grain surface chemistry) has been done. More particularly, the updates of rate coefficients and branching ratios of the reactions of our chemical network showed their importance, such as on the abundances of some chemical species, and on the code sensitivity to others parameters.Several physical models of collapsing dense core have also been considered. The more complex and solid approach has been to interface our chemical code with the radiation-magneto-hydrodynamic model of stellar formation RAMSES, in order to model in three dimensions the physical and chemical evolution of a young disk formation. Our study showed that the disk keeps imprints of the past history of the matter, and so its chemical composition is sensitive to the initial conditions.","downloadable_attachments":[{"id":30622112,"asset_id":2615056,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":130522,"first_name":"Ugo","last_name":"Hincelin","domain_name":"virginia","page_name":"UgoHincelin","display_name":"Ugo Hincelin","profile_url":"https://virginia.academia.edu/UgoHincelin?f_ri=4363","photo":"https://0.academia-photos.com/130522/487960/614228/s65_ugo.hincelin.jpg"}],"research_interests":[{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true},{"id":721,"name":"Magnetohydrodynamics","url":"https://www.academia.edu/Documents/in/Magnetohydrodynamics?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11124,"name":"Astrochemistry","url":"https://www.academia.edu/Documents/in/Astrochemistry?f_ri=4363","nofollow":true},{"id":22930,"name":"Numerical Modelling","url":"https://www.academia.edu/Documents/in/Numerical_Modelling?f_ri=4363"},{"id":35657,"name":"Molecular Clouds","url":"https://www.academia.edu/Documents/in/Molecular_Clouds?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_38265683" data-work_id="38265683" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" rel="nofollow" href="https://www.academia.edu/38265683/Biological_Phenomena_Mimic_Astrophysical_Principles_of_Gravitation_Opening_Perspective_2018_">Biological Phenomena Mimic Astrophysical Principles of Gravitation – Opening Perspective (2018)</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">It is conjectured that phenomena in biological microworld could be equated with astrophysical principles of gravitation. Fluids, gases that constitute 50-90 % of the total accredited biomass causes seclusion from stronger external... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_38265683" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">It is conjectured that phenomena in biological microworld could be equated with astrophysical principles of gravitation. Fluids, gases that constitute 50-90 % of the total accredited biomass causes seclusion from stronger external gravitational fields. Seclusion due to buoyant condition is reflected in apparent ‘weight’ reduced. The g-value (self) to the tune of nanometer per second square in a massive body of a planet may be negligible, but in an isolated living mass at picometer distance, such acceleration is quite a significant force. Homogeneous and heterogeneous accretion; heating and cooling phenomena as well as the rhythmic pattern of growth due to elastic collisions in massive star; heat transfer mechanisms viz. radiation, (perspiration), conduction and convection; site of human core body temperature at liver, kidney, heart and parts of brain at central region under initial circular fetus situation; or coldest part of the periphery at toe, foot, hand demonstrates similarity between biological and astrophysical words. Mechanical movement of macromolecules under neutral buoyant condition of the principle ‘heavier molar mass plus higher the density- faster the central travel from periphery’ for nucleic acid and protein; fats & lipids in addition to molar mass and density- variation in temperature; distribution carbohydrates in protoplasm under miscible condition due to solubility under granular soil and gel properties were equated with movement phenomena under astrophysical principle. Centrifugation as standard protocol for separating organelles is considered as inversion or reversing the natural setting on losing its compression memory.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/38265683" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="7d62ad8d54f7735c1de79adc61d2fae3" rel="nofollow" data-download="{"attachment_id":58309458,"asset_id":38265683,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/58309458/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="2910896" rel="nofollow" href="https://independent.academia.edu/DrIreshRanjanBhattacharjee">Iresh Ranjan Bhattacharjee</a><script data-card-contents-for-user="2910896" type="text/json">{"id":2910896,"first_name":"Iresh Ranjan","last_name":"Bhattacharjee","domain_name":"independent","page_name":"DrIreshRanjanBhattacharjee","display_name":"Iresh Ranjan Bhattacharjee","profile_url":"https://independent.academia.edu/DrIreshRanjanBhattacharjee?f_ri=4363","photo":"https://0.academia-photos.com/2910896/18461822/18419673/s65_dr._iresh_ranjan.bhattacharjee.jpg"}</script></span></span></li><li class="js-paper-rank-work_38265683 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="38265683"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 38265683, container: ".js-paper-rank-work_38265683", }); });</script></li><li class="js-percentile-work_38265683 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 38265683; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_38265683"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_38265683 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="38265683"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 38265683; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=38265683]").text(description); $(".js-view-count-work_38265683").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_38265683").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="38265683"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">19</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="1246" rel="nofollow" href="https://www.academia.edu/Documents/in/Gravitation">Gravitation</a>, <script data-card-contents-for-ri="1246" type="text/json">{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1247" rel="nofollow" href="https://www.academia.edu/Documents/in/Quantum_Gravity">Quantum Gravity</a>, <script data-card-contents-for-ri="1247" type="text/json">{"id":1247,"name":"Quantum Gravity","url":"https://www.academia.edu/Documents/in/Quantum_Gravity?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2513" rel="nofollow" href="https://www.academia.edu/Documents/in/Molecular_Biology">Molecular Biology</a>, <script data-card-contents-for-ri="2513" type="text/json">{"id":2513,"name":"Molecular Biology","url":"https://www.academia.edu/Documents/in/Molecular_Biology?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a><script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=38265683]'), work: {"id":38265683,"title":"Biological Phenomena Mimic Astrophysical Principles of Gravitation – Opening Perspective (2018)","created_at":"2019-01-31T23:24:52.841-08:00","url":"https://www.academia.edu/38265683/Biological_Phenomena_Mimic_Astrophysical_Principles_of_Gravitation_Opening_Perspective_2018_?f_ri=4363","dom_id":"work_38265683","summary":"It is conjectured that phenomena in biological microworld could be equated with astrophysical principles of gravitation. Fluids, gases that constitute 50-90 % of the total accredited biomass causes seclusion from stronger external gravitational fields. Seclusion due to buoyant condition is reflected in apparent ‘weight’ reduced. The g-value (self) to the tune of nanometer per second square in a massive body of a planet may be negligible, but in an isolated living mass at picometer distance, such acceleration is quite a significant force. Homogeneous and heterogeneous accretion; heating and cooling phenomena as well as the rhythmic pattern of growth due to elastic collisions in massive star; heat transfer mechanisms viz. radiation, (perspiration), conduction and convection; site of human core body temperature at liver, kidney, heart and parts of brain at central region under initial circular fetus situation; or coldest part of the periphery at toe, foot, hand demonstrates similarity between biological and astrophysical words. Mechanical movement of macromolecules under neutral buoyant condition of the principle ‘heavier molar mass plus higher the density- faster the central travel from periphery’ for nucleic acid and protein; fats \u0026 lipids in addition to molar mass and density- variation in temperature; distribution carbohydrates in protoplasm under miscible condition due to solubility under granular soil and gel properties were equated with movement phenomena under astrophysical principle. Centrifugation as standard protocol for separating organelles is considered as inversion or reversing the natural setting on losing its compression memory.","downloadable_attachments":[{"id":58309458,"asset_id":38265683,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":2910896,"first_name":"Iresh Ranjan","last_name":"Bhattacharjee","domain_name":"independent","page_name":"DrIreshRanjanBhattacharjee","display_name":"Iresh Ranjan Bhattacharjee","profile_url":"https://independent.academia.edu/DrIreshRanjanBhattacharjee?f_ri=4363","photo":"https://0.academia-photos.com/2910896/18461822/18419673/s65_dr._iresh_ranjan.bhattacharjee.jpg"}],"research_interests":[{"id":1246,"name":"Gravitation","url":"https://www.academia.edu/Documents/in/Gravitation?f_ri=4363","nofollow":true},{"id":1247,"name":"Quantum Gravity","url":"https://www.academia.edu/Documents/in/Quantum_Gravity?f_ri=4363","nofollow":true},{"id":2513,"name":"Molecular Biology","url":"https://www.academia.edu/Documents/in/Molecular_Biology?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":5001,"name":"Astrobiology","url":"https://www.academia.edu/Documents/in/Astrobiology?f_ri=4363"},{"id":5398,"name":"Biotechnology","url":"https://www.academia.edu/Documents/in/Biotechnology?f_ri=4363"},{"id":11332,"name":"Gravitational Biology","url":"https://www.academia.edu/Documents/in/Gravitational_Biology?f_ri=4363"},{"id":13827,"name":"Cell Biology","url":"https://www.academia.edu/Documents/in/Cell_Biology?f_ri=4363"},{"id":16496,"name":"Fluid Dynamics","url":"https://www.academia.edu/Documents/in/Fluid_Dynamics?f_ri=4363"},{"id":22835,"name":"Gauge-Gravity Correspondence","url":"https://www.academia.edu/Documents/in/Gauge-Gravity_Correspondence?f_ri=4363"},{"id":23179,"name":"Astrophysics","url":"https://www.academia.edu/Documents/in/Astrophysics?f_ri=4363"},{"id":29125,"name":"Gravitational Waves","url":"https://www.academia.edu/Documents/in/Gravitational_Waves?f_ri=4363"},{"id":47884,"name":"Biological Sciences","url":"https://www.academia.edu/Documents/in/Biological_Sciences?f_ri=4363"},{"id":79394,"name":"Gravity","url":"https://www.academia.edu/Documents/in/Gravity?f_ri=4363"},{"id":178906,"name":"Nucleic Acids","url":"https://www.academia.edu/Documents/in/Nucleic_Acids?f_ri=4363"},{"id":457191,"name":"Analytical Ultracentrifugation","url":"https://www.academia.edu/Documents/in/Analytical_Ultracentrifugation?f_ri=4363"},{"id":931947,"name":"Self assembly of Macromolecules","url":"https://www.academia.edu/Documents/in/Self_assembly_of_Macromolecules?f_ri=4363"},{"id":1006724,"name":"Macromolecular (Proteins","url":"https://www.academia.edu/Documents/in/Macromolecular_Proteins?f_ri=4363"},{"id":2728978,"name":"Neutral Buoyancy","url":"https://www.academia.edu/Documents/in/Neutral_Buoyancy?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_35538530" data-work_id="35538530" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22">High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_35538530" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/35538530" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="4564ea6ab359b08eabc6743f53f54dc5" rel="nofollow" data-download="{"attachment_id":55404248,"asset_id":35538530,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/55404248/download_file?st=MTczOTc5OTU1MCw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="66695878" href="https://gucas.academia.edu/jhyuannaoc">Jinghua Yuan</a><script data-card-contents-for-user="66695878" type="text/json">{"id":66695878,"first_name":"Jinghua","last_name":"Yuan","domain_name":"gucas","page_name":"jhyuannaoc","display_name":"Jinghua Yuan","profile_url":"https://gucas.academia.edu/jhyuannaoc?f_ri=4363","photo":"https://0.academia-photos.com/66695878/17364443/17484885/s65_jinghua.yuan.jpg"}</script></span></span></li><li class="js-paper-rank-work_35538530 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="35538530"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 35538530, container: ".js-paper-rank-work_35538530", }); 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$(".js-view-count[data-work-id=35538530]").text(description); $(".js-view-count-work_35538530").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_35538530").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="35538530"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">4</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="24009" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_formation_Physics_">Star formation (Physics)</a>, <script data-card-contents-for-ri="24009" type="text/json">{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="70376" rel="nofollow" href="https://www.academia.edu/Documents/in/Massive_Star_Formation">Massive Star Formation</a>, <script data-card-contents-for-ri="70376" type="text/json">{"id":70376,"name":"Massive Star Formation","url":"https://www.academia.edu/Documents/in/Massive_Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="75789" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation">Interstellar Medium and Star formation</a><script data-card-contents-for-ri="75789" type="text/json">{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=35538530]'), work: {"id":35538530,"title":"High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22","created_at":"2017-12-29T17:29:23.908-08:00","url":"https://www.academia.edu/35538530/High_mass_Star_Formation_through_Filamentary_Collapse_and_Clump_fed_Accretion_in_G22?f_ri=4363","dom_id":"work_35538530","summary":"How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding high-mass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440 M e Myr −1 , suggesting the hub mass would be doubled in six free-fall times, adding up to ∼2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO + (3–2) and 13 CO(3–2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s −1 and 7.2×10 −4 M e yr −1 , respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11–15 M e and it is still growing with an accretion rate of 7×10 −5 M e yr −1. The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.","downloadable_attachments":[{"id":55404248,"asset_id":35538530,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":66695878,"first_name":"Jinghua","last_name":"Yuan","domain_name":"gucas","page_name":"jhyuannaoc","display_name":"Jinghua Yuan","profile_url":"https://gucas.academia.edu/jhyuannaoc?f_ri=4363","photo":"https://0.academia-photos.com/66695878/17364443/17484885/s65_jinghua.yuan.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":24009,"name":"Star formation (Physics)","url":"https://www.academia.edu/Documents/in/Star_formation_Physics_?f_ri=4363","nofollow":true},{"id":70376,"name":"Massive Star Formation","url":"https://www.academia.edu/Documents/in/Massive_Star_Formation?f_ri=4363","nofollow":true},{"id":75789,"name":"Interstellar Medium and Star formation","url":"https://www.academia.edu/Documents/in/Interstellar_Medium_and_Star_formation?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_12145087" data-work_id="12145087" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/12145087/Morphological_quenching_of_star_formation_making_early_type_galaxies_red">Morphological quenching of star formation: making early-type galaxies red</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We point out a natural mechanism for quenching of star formation in early-type galaxies. It automatically links the color of a galaxy with its morphology and does not require gas consumption, removal or termination of gas supply. Given... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_12145087" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We point out a natural mechanism for quenching of star formation in early-type galaxies. It automatically links the color of a galaxy with its morphology and does not require gas consumption, removal or termination of gas supply. Given that star formation takes place in gravitationally unstable gas disks, it can be quenched when a disk becomes stable against fragmentation to bound clumps. This can result from the growth of a stellar spheroid, for instance by mergers. We present the concept of morphological quenching (MQ) using standard disk instability analysis, and demonstrate its natural occurrence in a cosmological simulation using an efficient zoom-in technique. We show that the transition from a stellar disk to a spheroid can be sufficient to stabilize the gas disk, quench star formation, and turn an early-type galaxy red and dead while gas accretion continues. The turbulence necessary for disk stability can be stirred up by sheared perturbations within the disk in the absence of bound star-forming clumps. While other quenching mechanisms, such as gas stripping, AGN feedback, virial shock heating, and gravitational heating are limited to massive halos, the MQ can explain the appearance of red early-type galaxies also in halos less massive than ∼ 10 12 M ⊙ . The dense gas disks observed in some of today's red ellipticals may be the relics of this mechanism, whereas red galaxies with quenched gas disks could be more frequent at high redshift.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/12145087" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="70633fa8a7413240ae03610f2f3ae616" rel="nofollow" data-download="{"attachment_id":46333860,"asset_id":12145087,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/46333860/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="30479595" href="https://uzh.academia.edu/RomainTeyssier">Romain Teyssier</a><script data-card-contents-for-user="30479595" type="text/json">{"id":30479595,"first_name":"Romain","last_name":"Teyssier","domain_name":"uzh","page_name":"RomainTeyssier","display_name":"Romain Teyssier","profile_url":"https://uzh.academia.edu/RomainTeyssier?f_ri=4363","photo":"https://0.academia-photos.com/30479595/8851902/9881565/s65_romain.teyssier.jpg"}</script></span></span></li><li class="js-paper-rank-work_12145087 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="12145087"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 12145087, container: ".js-paper-rank-work_12145087", }); });</script></li><li class="js-percentile-work_12145087 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 12145087; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_12145087"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_12145087 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="12145087"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 12145087; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=12145087]").text(description); $(".js-view-count-work_12145087").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_12145087").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="12145087"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">5</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a><script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=12145087]'), work: {"id":12145087,"title":"Morphological quenching of star formation: making early-type galaxies red","created_at":"2015-04-28T22:31:41.722-07:00","url":"https://www.academia.edu/12145087/Morphological_quenching_of_star_formation_making_early_type_galaxies_red?f_ri=4363","dom_id":"work_12145087","summary":"We point out a natural mechanism for quenching of star formation in early-type galaxies. It automatically links the color of a galaxy with its morphology and does not require gas consumption, removal or termination of gas supply. Given that star formation takes place in gravitationally unstable gas disks, it can be quenched when a disk becomes stable against fragmentation to bound clumps. This can result from the growth of a stellar spheroid, for instance by mergers. We present the concept of morphological quenching (MQ) using standard disk instability analysis, and demonstrate its natural occurrence in a cosmological simulation using an efficient zoom-in technique. We show that the transition from a stellar disk to a spheroid can be sufficient to stabilize the gas disk, quench star formation, and turn an early-type galaxy red and dead while gas accretion continues. The turbulence necessary for disk stability can be stirred up by sheared perturbations within the disk in the absence of bound star-forming clumps. While other quenching mechanisms, such as gas stripping, AGN feedback, virial shock heating, and gravitational heating are limited to massive halos, the MQ can explain the appearance of red early-type galaxies also in halos less massive than ∼ 10 12 M ⊙ . The dense gas disks observed in some of today's red ellipticals may be the relics of this mechanism, whereas red galaxies with quenched gas disks could be more frequent at high redshift.","downloadable_attachments":[{"id":46333860,"asset_id":12145087,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":30479595,"first_name":"Romain","last_name":"Teyssier","domain_name":"uzh","page_name":"RomainTeyssier","display_name":"Romain Teyssier","profile_url":"https://uzh.academia.edu/RomainTeyssier?f_ri=4363","photo":"https://0.academia-photos.com/30479595/8851902/9881565/s65_romain.teyssier.jpg"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":61631,"name":"High Redshift Universe","url":"https://www.academia.edu/Documents/in/High_Redshift_Universe?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_6199770" data-work_id="6199770" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/6199770/A_Large_Massive_Rotating_Disk_Around_an_Isolated_Young_Stellar_Object">A Large, Massive, Rotating Disk Around an Isolated Young Stellar Object</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We present multi-wavelengths observations and a radiative transfer model of a newly discovered massive circumstellar disk of gas and dust which is one of the largest disks known today. Seen almost edge-on, the disk is resolved in... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_6199770" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present multi-wavelengths observations and a radiative transfer model of a newly discovered massive circumstellar disk of gas and dust which is one of the largest disks known today. Seen almost edge-on, the disk is resolved in high-resolution near-infrared (NIR) images and appears as a dark lane of high opacity intersecting a bipolar reflection nebula. Based on molecular line observations we estimate the distance to the object to be 3.5 kpc. This leads to a size for the dark lane of ~10500 AU but due to shadowing effects the true disk size could be smaller. In Spitzer/IRAC 3.6 micron images the elongated shape of the bipolar reflection nebula is still preserved and the bulk of the flux seems to come from disk regions that can be detected due to the slight inclination of the disk. At longer IRAC wavelengths, the flux is mainly coming from the central regions penetrating directly through the dust lane. Interferometric observations of the dust continuum emission at millimeter wavelengths with the SMA confirm this finding as the peak of the unresolved mm-emission coincides perfectly with the peak of the Spitzer/IRAC 5.8 micron flux and the center of the dark lane seen in the NIR images. Simultaneously acquired CO data reveal a molecular outflow along the northern part of the reflection nebula which seems to be the outflow cavity. An elongated gaseous disk component is also detected and shows signs of rotation. The emission is perpendicular to the molecular outflow and thus parallel to but even more extended than the dark lane in the NIR images. Based on the dust continuum and the CO observations we estimate a disk mass of up to a few solar masses depending on the underlying assumptions. Whether the disk-like structure is an actual accretion disk or rather a larger-scale flattened envelope or pseudodisk is difficult to discriminate with the current dataset (abridged).</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/6199770" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="95a408aa59043559cab9faac52b37df7" rel="nofollow" data-download="{"attachment_id":33076115,"asset_id":6199770,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/33076115/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="21835" href="https://esa.academia.edu/StephanBirkmann">Stephan Birkmann</a><script data-card-contents-for-user="21835" type="text/json">{"id":21835,"first_name":"Stephan","last_name":"Birkmann","domain_name":"esa","page_name":"StephanBirkmann","display_name":"Stephan Birkmann","profile_url":"https://esa.academia.edu/StephanBirkmann?f_ri=4363","photo":"https://0.academia-photos.com/21835/7279/3534467/s65_stephan.birkmann.jpeg"}</script></span></span></li><li class="js-paper-rank-work_6199770 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="6199770"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 6199770, container: ".js-paper-rank-work_6199770", }); });</script></li><li class="js-percentile-work_6199770 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 6199770; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_6199770"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_6199770 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="6199770"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 6199770; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=6199770]").text(description); $(".js-view-count-work_6199770").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_6199770").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="6199770"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="723" rel="nofollow" href="https://www.academia.edu/Documents/in/Astrophysical_Plasma">Astrophysical Plasma</a>, <script data-card-contents-for-ri="723" type="text/json">{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="23940" rel="nofollow" href="https://www.academia.edu/Documents/in/Near_Infrared">Near Infrared</a><script data-card-contents-for-ri="23940" type="text/json">{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=6199770]'), work: {"id":6199770,"title":"A Large, Massive, Rotating Disk Around an Isolated Young Stellar Object","created_at":"2014-02-24T23:51:58.095-08:00","url":"https://www.academia.edu/6199770/A_Large_Massive_Rotating_Disk_Around_an_Isolated_Young_Stellar_Object?f_ri=4363","dom_id":"work_6199770","summary":"We present multi-wavelengths observations and a radiative transfer model of a newly discovered massive circumstellar disk of gas and dust which is one of the largest disks known today. Seen almost edge-on, the disk is resolved in high-resolution near-infrared (NIR) images and appears as a dark lane of high opacity intersecting a bipolar reflection nebula. Based on molecular line observations we estimate the distance to the object to be 3.5 kpc. This leads to a size for the dark lane of ~10500 AU but due to shadowing effects the true disk size could be smaller. In Spitzer/IRAC 3.6 micron images the elongated shape of the bipolar reflection nebula is still preserved and the bulk of the flux seems to come from disk regions that can be detected due to the slight inclination of the disk. At longer IRAC wavelengths, the flux is mainly coming from the central regions penetrating directly through the dust lane. Interferometric observations of the dust continuum emission at millimeter wavelengths with the SMA confirm this finding as the peak of the unresolved mm-emission coincides perfectly with the peak of the Spitzer/IRAC 5.8 micron flux and the center of the dark lane seen in the NIR images. Simultaneously acquired CO data reveal a molecular outflow along the northern part of the reflection nebula which seems to be the outflow cavity. An elongated gaseous disk component is also detected and shows signs of rotation. The emission is perpendicular to the molecular outflow and thus parallel to but even more extended than the dark lane in the NIR images. Based on the dust continuum and the CO observations we estimate a disk mass of up to a few solar masses depending on the underlying assumptions. Whether the disk-like structure is an actual accretion disk or rather a larger-scale flattened envelope or pseudodisk is difficult to discriminate with the current dataset (abridged).","downloadable_attachments":[{"id":33076115,"asset_id":6199770,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":21835,"first_name":"Stephan","last_name":"Birkmann","domain_name":"esa","page_name":"StephanBirkmann","display_name":"Stephan Birkmann","profile_url":"https://esa.academia.edu/StephanBirkmann?f_ri=4363","photo":"https://0.academia-photos.com/21835/7279/3534467/s65_stephan.birkmann.jpeg"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true},{"id":153168,"name":"Data Collection","url":"https://www.academia.edu/Documents/in/Data_Collection?f_ri=4363"},{"id":309086,"name":"High Resolution","url":"https://www.academia.edu/Documents/in/High_Resolution?f_ri=4363"},{"id":444563,"name":"Acoustic Radiative Transfer Model","url":"https://www.academia.edu/Documents/in/Acoustic_Radiative_Transfer_Model?f_ri=4363"},{"id":2018143,"name":"Jet Propulsion Laboratory","url":"https://www.academia.edu/Documents/in/Jet_Propulsion_Laboratory?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_1155246" data-work_id="1155246" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/1155246/Evidence_for_Fragmentation_of_a_Large_Kuiper_Belt_Like_Object_and_an_LHB_like_Delivery_Event_in_the_1_Gyr_Eta_Corvi_System">Evidence for Fragmentation of a Large Kuiper Belt-Like Object and an LHB-like Delivery Event in the ~1 Gyr Eta Corvi System. </a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We have analyzed Spitzer and NASA/IRTF 2 - 35 \mum spectra of the warm, ~350 K circumstellar dust around the nearby MS star {\eta} Corvi (F2V, 1.4 \pm 0.3 Gyr). The spectra show clear evidence for warm, water- and carbon-rich dust at ~3... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_1155246" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We have analyzed Spitzer and NASA/IRTF 2 - 35 \mum spectra of the warm, ~350 K circumstellar dust around the nearby MS star {\eta} Corvi (F2V, 1.4 \pm 0.3 Gyr). The spectra show clear evidence for warm, water- and carbon-rich dust at ~3 AU from the central star, in the system's Terrestrial Habitability Zone. Spectral features due to ultra-primitive cometary material were found, in addition to features due to impact produced silica and high temperature carbonaceous phases. At least 9 x 10^18 kg of 0.1 - 100 \mum warm dust is present in a collisional equilibrium distribution with dn/da ~ a^-3.5, the equivalent of a 130 km radius KBO of 1.0 g/cm^3 density and similar to recent estimates of the mass delivered to the Earth at 0.6 - 0.8 Gyr during the Late Heavy Bombardment. We conclude that the parent body was a Kuiper-Belt body or bodies which captured a large amount of early primitive material in the first Myrs of the system's lifetime and preserved it in deep freeze at ~150 AU. At ~1.4 Gyr they were prompted by dynamical stirring of their parent Kuiper Belt into spiraling into the inner system, eventually colliding at 5-10 km/sec with a rocky planetary body of mass \leq MEarth at ~3 AU, delivering large amounts of water (>0.1% of MEarth's Oceans) and carbon-rich material. The Spitzer spectrum also closely matches spectra reported for the Ureilite meteorites of the Sudan Almahata Sitta fall in 2008, suggesting that one of the Ureilite parent bodies was a KBO.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/1155246" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="c2a6589a04d3d76d6e144ed777c851eb" rel="nofollow" data-download="{"attachment_id":32381970,"asset_id":1155246,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/32381970/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="208739" href="https://uni-muenster.academia.edu/AndreasMorlok">Andreas Morlok</a><script data-card-contents-for-user="208739" type="text/json">{"id":208739,"first_name":"Andreas","last_name":"Morlok","domain_name":"uni-muenster","page_name":"AndreasMorlok","display_name":"Andreas Morlok","profile_url":"https://uni-muenster.academia.edu/AndreasMorlok?f_ri=4363","photo":"https://0.academia-photos.com/208739/1148090/3205165/s65_andreas.morlok.jpg"}</script></span></span></li><li class="js-paper-rank-work_1155246 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="1155246"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 1155246, container: ".js-paper-rank-work_1155246", }); 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$(".js-view-count[data-work-id=1155246]").text(description); $(".js-view-count-work_1155246").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_1155246").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="1155246"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">12</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="704" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared_Astronomy">Infrared Astronomy</a>, <script data-card-contents-for-ri="704" type="text/json">{"id":704,"name":"Infrared Astronomy","url":"https://www.academia.edu/Documents/in/Infrared_Astronomy?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="2417" rel="nofollow" href="https://www.academia.edu/Documents/in/Planetary_Science">Planetary Science</a>, <script data-card-contents-for-ri="2417" type="text/json">{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="6649" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared_Optics">Infrared Optics</a><script data-card-contents-for-ri="6649" type="text/json">{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=1155246]'), work: {"id":1155246,"title":"Evidence for Fragmentation of a Large Kuiper Belt-Like Object and an LHB-like Delivery Event in the ~1 Gyr Eta Corvi System. ","created_at":"2011-12-13T20:26:34.595-08:00","url":"https://www.academia.edu/1155246/Evidence_for_Fragmentation_of_a_Large_Kuiper_Belt_Like_Object_and_an_LHB_like_Delivery_Event_in_the_1_Gyr_Eta_Corvi_System?f_ri=4363","dom_id":"work_1155246","summary":"We have analyzed Spitzer and NASA/IRTF 2 - 35 \\mum spectra of the warm, ~350 K circumstellar dust around the nearby MS star {\\eta} Corvi (F2V, 1.4 \\pm 0.3 Gyr). The spectra show clear evidence for warm, water- and carbon-rich dust at ~3 AU from the central star, in the system's Terrestrial Habitability Zone. Spectral features due to ultra-primitive cometary material were found, in addition to features due to impact produced silica and high temperature carbonaceous phases. At least 9 x 10^18 kg of 0.1 - 100 \\mum warm dust is present in a collisional equilibrium distribution with dn/da ~ a^-3.5, the equivalent of a 130 km radius KBO of 1.0 g/cm^3 density and similar to recent estimates of the mass delivered to the Earth at 0.6 - 0.8 Gyr during the Late Heavy Bombardment. We conclude that the parent body was a Kuiper-Belt body or bodies which captured a large amount of early primitive material in the first Myrs of the system's lifetime and preserved it in deep freeze at ~150 AU. At ~1.4 Gyr they were prompted by dynamical stirring of their parent Kuiper Belt into spiraling into the inner system, eventually colliding at 5-10 km/sec with a rocky planetary body of mass \\leq MEarth at ~3 AU, delivering large amounts of water (\u003e0.1% of MEarth's Oceans) and carbon-rich material. The Spitzer spectrum also closely matches spectra reported for the Ureilite meteorites of the Sudan Almahata Sitta fall in 2008, suggesting that one of the Ureilite parent bodies was a KBO. ","downloadable_attachments":[{"id":32381970,"asset_id":1155246,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":208739,"first_name":"Andreas","last_name":"Morlok","domain_name":"uni-muenster","page_name":"AndreasMorlok","display_name":"Andreas Morlok","profile_url":"https://uni-muenster.academia.edu/AndreasMorlok?f_ri=4363","photo":"https://0.academia-photos.com/208739/1148090/3205165/s65_andreas.morlok.jpg"}],"research_interests":[{"id":704,"name":"Infrared Astronomy","url":"https://www.academia.edu/Documents/in/Infrared_Astronomy?f_ri=4363","nofollow":true},{"id":2417,"name":"Planetary Science","url":"https://www.academia.edu/Documents/in/Planetary_Science?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":6649,"name":"Infrared Optics","url":"https://www.academia.edu/Documents/in/Infrared_Optics?f_ri=4363","nofollow":true},{"id":9820,"name":"Polarization (Ideology)","url":"https://www.academia.edu/Documents/in/Polarization_Ideology_?f_ri=4363"},{"id":41236,"name":"Extrasolar planets","url":"https://www.academia.edu/Documents/in/Extrasolar_planets?f_ri=4363"},{"id":65899,"name":"Meteorites","url":"https://www.academia.edu/Documents/in/Meteorites?f_ri=4363"},{"id":78842,"name":"Infrared spectroscopy","url":"https://www.academia.edu/Documents/in/Infrared_spectroscopy?f_ri=4363"},{"id":194384,"name":"Planet Formation","url":"https://www.academia.edu/Documents/in/Planet_Formation?f_ri=4363"},{"id":619318,"name":"Debris disks","url":"https://www.academia.edu/Documents/in/Debris_disks?f_ri=4363"},{"id":721777,"name":"Achondrites","url":"https://www.academia.edu/Documents/in/Achondrites?f_ri=4363"},{"id":954495,"name":"Protostellar Disks","url":"https://www.academia.edu/Documents/in/Protostellar_Disks?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_542827" data-work_id="542827" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/542827/Globular_cluster_systems_in_nearby_dwarf_galaxies_I_HST_ACS_observations_and_dynamical_properties_of_globular_clusters_at_low_environmental_density">Globular cluster systems in nearby dwarf galaxiesI. HST/ACS observations and dynamical properties of globular clusters at low environmental density</a></div></div><div class="u-pb4x u-mt3x"></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/542827" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="ecf9e63ac40857c689d574dc8ef38ae5" rel="nofollow" data-download="{"attachment_id":2714407,"asset_id":542827,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/2714407/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="412798" href="https://uc-cl.academia.edu/ThomasHPuzia">Thomas H. Puzia</a><script data-card-contents-for-user="412798" type="text/json">{"id":412798,"first_name":"Thomas H.","last_name":"Puzia","domain_name":"uc-cl","page_name":"ThomasHPuzia","display_name":"Thomas H. Puzia","profile_url":"https://uc-cl.academia.edu/ThomasHPuzia?f_ri=4363","photo":"https://0.academia-photos.com/412798/354224/43283051/s65_thomas_h..puzia.jpg"}</script></span></span></li><li class="js-paper-rank-work_542827 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="542827"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 542827, container: ".js-paper-rank-work_542827", }); });</script></li><li class="js-percentile-work_542827 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 542827; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_542827"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_542827 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="542827"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 542827; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=542827]").text(description); $(".js-view-count-work_542827").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_542827").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="542827"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">25</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="10866" rel="nofollow" href="https://www.academia.edu/Documents/in/Morphology">Morphology</a>, <script data-card-contents-for-ri="10866" type="text/json">{"id":10866,"name":"Morphology","url":"https://www.academia.edu/Documents/in/Morphology?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11058" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Clusters">Galaxy Clusters</a>, <script data-card-contents-for-ri="11058" type="text/json">{"id":11058,"name":"Galaxy Clusters","url":"https://www.academia.edu/Documents/in/Galaxy_Clusters?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="65140" rel="nofollow" href="https://www.academia.edu/Documents/in/Models">Models</a><script data-card-contents-for-ri="65140" type="text/json">{"id":65140,"name":"Models","url":"https://www.academia.edu/Documents/in/Models?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=542827]'), work: {"id":542827,"title":"Globular cluster systems in nearby dwarf galaxiesI. HST/ACS observations and dynamical properties of globular clusters at low environmental density","created_at":"2011-04-24T10:30:22.335-07:00","url":"https://www.academia.edu/542827/Globular_cluster_systems_in_nearby_dwarf_galaxies_I_HST_ACS_observations_and_dynamical_properties_of_globular_clusters_at_low_environmental_density?f_ri=4363","dom_id":"work_542827","summary":null,"downloadable_attachments":[{"id":2714407,"asset_id":542827,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":412798,"first_name":"Thomas H.","last_name":"Puzia","domain_name":"uc-cl","page_name":"ThomasHPuzia","display_name":"Thomas H. Puzia","profile_url":"https://uc-cl.academia.edu/ThomasHPuzia?f_ri=4363","photo":"https://0.academia-photos.com/412798/354224/43283051/s65_thomas_h..puzia.jpg"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":10866,"name":"Morphology","url":"https://www.academia.edu/Documents/in/Morphology?f_ri=4363","nofollow":true},{"id":11058,"name":"Galaxy Clusters","url":"https://www.academia.edu/Documents/in/Galaxy_Clusters?f_ri=4363","nofollow":true},{"id":65140,"name":"Models","url":"https://www.academia.edu/Documents/in/Models?f_ri=4363","nofollow":true},{"id":76714,"name":"Color","url":"https://www.academia.edu/Documents/in/Color?f_ri=4363"},{"id":81504,"name":"Correlation","url":"https://www.academia.edu/Documents/in/Correlation?f_ri=4363"},{"id":106861,"name":"Dwarf Galaxies","url":"https://www.academia.edu/Documents/in/Dwarf_Galaxies?f_ri=4363"},{"id":137633,"name":"Feedback","url":"https://www.academia.edu/Documents/in/Feedback?f_ri=4363"},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363"},{"id":176853,"name":"Luminosity","url":"https://www.academia.edu/Documents/in/Luminosity?f_ri=4363"},{"id":209020,"name":"Accretion","url":"https://www.academia.edu/Documents/in/Accretion?f_ri=4363"},{"id":294030,"name":"Stellar winds","url":"https://www.academia.edu/Documents/in/Stellar_winds?f_ri=4363"},{"id":383911,"name":"Spiral Galaxies","url":"https://www.academia.edu/Documents/in/Spiral_Galaxies?f_ri=4363"},{"id":407349,"name":"Correlations","url":"https://www.academia.edu/Documents/in/Correlations?f_ri=4363"},{"id":413300,"name":"Analytical Model","url":"https://www.academia.edu/Documents/in/Analytical_Model?f_ri=4363"},{"id":415653,"name":"Luminosity function","url":"https://www.academia.edu/Documents/in/Luminosity_function?f_ri=4363"},{"id":494642,"name":"Structural Properties","url":"https://www.academia.edu/Documents/in/Structural_Properties?f_ri=4363"},{"id":962097,"name":"Star Clusters","url":"https://www.academia.edu/Documents/in/Star_Clusters?f_ri=4363"},{"id":963709,"name":"Mass Loss","url":"https://www.academia.edu/Documents/in/Mass_Loss?f_ri=4363"},{"id":966388,"name":"Wind Velocity","url":"https://www.academia.edu/Documents/in/Wind_Velocity?f_ri=4363"},{"id":1154248,"name":"Theoretical Model","url":"https://www.academia.edu/Documents/in/Theoretical_Model?f_ri=4363"},{"id":1181250,"name":"Hubble Space Telescope Images","url":"https://www.academia.edu/Documents/in/Hubble_Space_Telescope_Images?f_ri=4363"},{"id":1874422,"name":"Dynamic Properties","url":"https://www.academia.edu/Documents/in/Dynamic_Properties?f_ri=4363"},{"id":2495917,"name":"Escape Velocity","url":"https://www.academia.edu/Documents/in/Escape_Velocity?f_ri=4363"},{"id":2599525,"name":"present day","url":"https://www.academia.edu/Documents/in/present_day?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_21557335" data-work_id="21557335" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/21557335/From_pre_stellar_cores_to_protostars_The_initial_conditions_of_star_formation">From pre-stellar cores to protostars: The initial conditions of star formation</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest">To appear in Protostars and Planets IV, eds. V. Mannings, AP Boss, and SS Russell (Tucson: Univ. of Arizona Press) Accepted 1999 January ... FROM PRE-STELLAR CORES TO PROTOSTARS: THE INITIAL CONDITIONS OF STAR FORMATION</div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/21557335" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="23687b27c9dcd3efa637bd09542132b9" rel="nofollow" data-download="{"attachment_id":42059953,"asset_id":21557335,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/42059953/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="42672119" href="https://independent.academia.edu/DerekWardThompson">Derek Ward-Thompson</a><script data-card-contents-for-user="42672119" type="text/json">{"id":42672119,"first_name":"Derek","last_name":"Ward-Thompson","domain_name":"independent","page_name":"DerekWardThompson","display_name":"Derek Ward-Thompson","profile_url":"https://independent.academia.edu/DerekWardThompson?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_21557335 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="21557335"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 21557335, container: ".js-paper-rank-work_21557335", }); 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$(".js-view-count[data-work-id=21557335]").text(description); $(".js-view-count-work_21557335").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_21557335").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="21557335"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">4</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="535357" rel="nofollow" href="https://www.academia.edu/Documents/in/Low_Mass_Stars">Low Mass Stars</a>, <script data-card-contents-for-ri="535357" type="text/json">{"id":535357,"name":"Low Mass Stars","url":"https://www.academia.edu/Documents/in/Low_Mass_Stars?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="889723" rel="nofollow" href="https://www.academia.edu/Documents/in/Radio_Telescope">Radio Telescope</a>, <script data-card-contents-for-ri="889723" type="text/json">{"id":889723,"name":"Radio Telescope","url":"https://www.academia.edu/Documents/in/Radio_Telescope?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1119718" rel="nofollow" href="https://www.academia.edu/Documents/in/Initial_Condition">Initial Condition</a><script data-card-contents-for-ri="1119718" type="text/json">{"id":1119718,"name":"Initial Condition","url":"https://www.academia.edu/Documents/in/Initial_Condition?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=21557335]'), work: {"id":21557335,"title":"From pre-stellar cores to protostars: The initial conditions of star formation","created_at":"2016-02-04T08:46:41.982-08:00","url":"https://www.academia.edu/21557335/From_pre_stellar_cores_to_protostars_The_initial_conditions_of_star_formation?f_ri=4363","dom_id":"work_21557335","summary":"To appear in Protostars and Planets IV, eds. V. Mannings, AP Boss, and SS Russell (Tucson: Univ. of Arizona Press) Accepted 1999 January ... FROM PRE-STELLAR CORES TO PROTOSTARS: THE INITIAL CONDITIONS OF STAR FORMATION","downloadable_attachments":[{"id":42059953,"asset_id":21557335,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":42672119,"first_name":"Derek","last_name":"Ward-Thompson","domain_name":"independent","page_name":"DerekWardThompson","display_name":"Derek Ward-Thompson","profile_url":"https://independent.academia.edu/DerekWardThompson?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":535357,"name":"Low Mass Stars","url":"https://www.academia.edu/Documents/in/Low_Mass_Stars?f_ri=4363","nofollow":true},{"id":889723,"name":"Radio Telescope","url":"https://www.academia.edu/Documents/in/Radio_Telescope?f_ri=4363","nofollow":true},{"id":1119718,"name":"Initial Condition","url":"https://www.academia.edu/Documents/in/Initial_Condition?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_18664911 coauthored" data-work_id="18664911" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/18664911/Stellar_sources_of_the_interstellar_medium">Stellar sources of the interstellar medium</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">With the exception of the Big Bang, responsible for 1,2 H, 3,4 He, and 7 Li, stars act as sources for the composition of the interstellar medium. Cosmic rays are related to the latter and very probably due to acceleration of the mixed... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_18664911" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">With the exception of the Big Bang, responsible for 1,2 H, 3,4 He, and 7 Li, stars act as sources for the composition of the interstellar medium. Cosmic rays are related to the latter and very probably due to acceleration of the mixed interstellar medium by shock waves from supernova remnants. Thus, the understanding of the abundance evolution in the interstellar medium and especially the enrichment of heavy elements, as a function of space and time, is essential. It reflects the history of star formation and the lifetimes of the diverse contributing stellar objects. Therefore, the understanding of the endpoints of stellar evolution is essential as well. These are mainly planetary nebulae and type II/Ib/Ic supernovae as evolutionary endpoints of single stars, but also events in binary systems can contribute, like e.g. supernovae of type Ia, novae and possibly X-ray bursts and neutron star or neutron star -black hole mergers. Despite many efforts, a full and self-consistent understanding of supernovae (the main contributors to nucleosynthesis in galaxies) is not existing, yet. Their fingerprints, however, seen either in spectra, lightcurves, radioactivities/decay gammarays or in galactic evolution, can help to constrain the composition of their ejecta and related model uncertainties.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/18664911" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="dce5408de20908ec9102a54f10581d56" rel="nofollow" data-download="{"attachment_id":40189438,"asset_id":18664911,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/40189438/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="38739904" href="https://independent.academia.edu/PeterH%C3%B6flich">Peter Höflich</a><script data-card-contents-for-user="38739904" type="text/json">{"id":38739904,"first_name":"Peter","last_name":"Höflich","domain_name":"independent","page_name":"PeterHöflich","display_name":"Peter Höflich","profile_url":"https://independent.academia.edu/PeterH%C3%B6flich?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-18664911">+2</span><div class="hidden js-additional-users-18664911"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/WHix">W. Hix</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/HSchatz">H. Schatz</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-18664911'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-18664911').html(); } } new HoverPopover(popoverSettings); })();</script></li><li class="js-paper-rank-work_18664911 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="18664911"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 18664911, container: ".js-paper-rank-work_18664911", }); });</script></li><li class="js-percentile-work_18664911 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 18664911; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_18664911"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_18664911 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="18664911"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 18664911; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=18664911]").text(description); $(".js-view-count-work_18664911").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_18664911").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="18664911"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">9</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="712" rel="nofollow" href="https://www.academia.edu/Documents/in/Stellar_Evolution">Stellar Evolution</a>, <script data-card-contents-for-ri="712" type="text/json">{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="716" rel="nofollow" href="https://www.academia.edu/Documents/in/Interstellar_Medium">Interstellar Medium</a>, <script data-card-contents-for-ri="716" type="text/json">{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="40629" rel="nofollow" href="https://www.academia.edu/Documents/in/Big_Bang">Big Bang</a><script data-card-contents-for-ri="40629" type="text/json">{"id":40629,"name":"Big Bang","url":"https://www.academia.edu/Documents/in/Big_Bang?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=18664911]'), work: {"id":18664911,"title":"Stellar sources of the interstellar medium","created_at":"2015-11-19T19:04:17.376-08:00","url":"https://www.academia.edu/18664911/Stellar_sources_of_the_interstellar_medium?f_ri=4363","dom_id":"work_18664911","summary":"With the exception of the Big Bang, responsible for 1,2 H, 3,4 He, and 7 Li, stars act as sources for the composition of the interstellar medium. Cosmic rays are related to the latter and very probably due to acceleration of the mixed interstellar medium by shock waves from supernova remnants. Thus, the understanding of the abundance evolution in the interstellar medium and especially the enrichment of heavy elements, as a function of space and time, is essential. It reflects the history of star formation and the lifetimes of the diverse contributing stellar objects. Therefore, the understanding of the endpoints of stellar evolution is essential as well. These are mainly planetary nebulae and type II/Ib/Ic supernovae as evolutionary endpoints of single stars, but also events in binary systems can contribute, like e.g. supernovae of type Ia, novae and possibly X-ray bursts and neutron star or neutron star -black hole mergers. Despite many efforts, a full and self-consistent understanding of supernovae (the main contributors to nucleosynthesis in galaxies) is not existing, yet. Their fingerprints, however, seen either in spectra, lightcurves, radioactivities/decay gammarays or in galactic evolution, can help to constrain the composition of their ejecta and related model uncertainties.","downloadable_attachments":[{"id":40189438,"asset_id":18664911,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":38739904,"first_name":"Peter","last_name":"Höflich","domain_name":"independent","page_name":"PeterHöflich","display_name":"Peter Höflich","profile_url":"https://independent.academia.edu/PeterH%C3%B6flich?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":39057114,"first_name":"W.","last_name":"Hix","domain_name":"independent","page_name":"WHix","display_name":"W. Hix","profile_url":"https://independent.academia.edu/WHix?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":38843195,"first_name":"H.","last_name":"Schatz","domain_name":"independent","page_name":"HSchatz","display_name":"H. Schatz","profile_url":"https://independent.academia.edu/HSchatz?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":712,"name":"Stellar Evolution","url":"https://www.academia.edu/Documents/in/Stellar_Evolution?f_ri=4363","nofollow":true},{"id":716,"name":"Interstellar Medium","url":"https://www.academia.edu/Documents/in/Interstellar_Medium?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":40629,"name":"Big Bang","url":"https://www.academia.edu/Documents/in/Big_Bang?f_ri=4363","nofollow":true},{"id":56001,"name":"X Rays","url":"https://www.academia.edu/Documents/in/X_Rays?f_ri=4363"},{"id":173004,"name":"Relational Model","url":"https://www.academia.edu/Documents/in/Relational_Model?f_ri=4363"},{"id":235060,"name":"Black Hole","url":"https://www.academia.edu/Documents/in/Black_Hole?f_ri=4363"},{"id":837148,"name":"Shock Wave","url":"https://www.academia.edu/Documents/in/Shock_Wave?f_ri=4363"},{"id":912885,"name":"Gamma Ray","url":"https://www.academia.edu/Documents/in/Gamma_Ray?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_21557378" data-work_id="21557378" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/21557378/Looking_Into_the_Hearts_of_Bok_Globules_Millimeter_and_Submillimeter_Continuum_Images_of_Isolated_Star_Forming_Cores">Looking Into the Hearts of Bok Globules: Millimeter and Submillimeter Continuum Images of Isolated Star-Forming Cores</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We present the results of a comprehensive infrared, submillimetre, and millimetre continuum emission study of isolated low-mass star-forming cores in 32 Bok globules, with the aim to investigate the process of star formation in these... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_21557378" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present the results of a comprehensive infrared, submillimetre, and millimetre continuum emission study of isolated low-mass star-forming cores in 32 Bok globules, with the aim to investigate the process of star formation in these regions. The submillimetre and millimetre dust continuum emission maps together with the spectral energy distributions are used to model and derive the physical properties of the star-forming cores, such as luminosities, sizes, masses, densities, etc. Comparisons with ground-based near-infrared and space-based mid and far-infrared images from Spitzer are used to reveal the stellar content of the Bok globules, association of embedded young stellar objects with the submm dust cores, and the evolutionary stages of the individual sources. Submm dust continuum emission was detected in 26 out of the 32 globule cores observed. For 18 globules with detected (sub)mm cores we derive evolutionary stages and physical parameters of the embedded sources. We identify nine starless cores, most of which are presumably prestellar, nine Class 0 protostars, and twelve Class I YSOs. Specific source properties like bolometric temperature, core size, and central densities are discussed as function of evolutionary stage. We find that at least two thirds (16 out of 24) of the star-forming globules studied here show evidence of forming multiple stars on scales between 1,000 and 50,000 AU. However, we also find that most of these small prototstar and star groups are comprised of sources with different evolutionary stages, suggesting a picture of slow and sequential star formation in isolated globules.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/21557378" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="5a4f2f68ba73bb2f490bb6579ddc0736" rel="nofollow" data-download="{"attachment_id":42059983,"asset_id":21557378,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/42059983/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="42672119" href="https://independent.academia.edu/DerekWardThompson">Derek Ward-Thompson</a><script data-card-contents-for-user="42672119" type="text/json">{"id":42672119,"first_name":"Derek","last_name":"Ward-Thompson","domain_name":"independent","page_name":"DerekWardThompson","display_name":"Derek Ward-Thompson","profile_url":"https://independent.academia.edu/DerekWardThompson?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_21557378 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="21557378"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 21557378, container: ".js-paper-rank-work_21557378", }); });</script></li><li class="js-percentile-work_21557378 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 21557378; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_21557378"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_21557378 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="21557378"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 21557378; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=21557378]").text(description); $(".js-view-count-work_21557378").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_21557378").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="21557378"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="531" rel="nofollow" href="https://www.academia.edu/Documents/in/Organic_Chemistry">Organic Chemistry</a>, <script data-card-contents-for-ri="531" type="text/json">{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="23940" rel="nofollow" href="https://www.academia.edu/Documents/in/Near_Infrared">Near Infrared</a>, <script data-card-contents-for-ri="23940" type="text/json">{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="335361" rel="nofollow" href="https://www.academia.edu/Documents/in/Infrared">Infrared</a><script data-card-contents-for-ri="335361" type="text/json">{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=21557378]'), work: {"id":21557378,"title":"Looking Into the Hearts of Bok Globules: Millimeter and Submillimeter Continuum Images of Isolated Star-Forming Cores","created_at":"2016-02-04T08:46:48.951-08:00","url":"https://www.academia.edu/21557378/Looking_Into_the_Hearts_of_Bok_Globules_Millimeter_and_Submillimeter_Continuum_Images_of_Isolated_Star_Forming_Cores?f_ri=4363","dom_id":"work_21557378","summary":"We present the results of a comprehensive infrared, submillimetre, and millimetre continuum emission study of isolated low-mass star-forming cores in 32 Bok globules, with the aim to investigate the process of star formation in these regions. The submillimetre and millimetre dust continuum emission maps together with the spectral energy distributions are used to model and derive the physical properties of the star-forming cores, such as luminosities, sizes, masses, densities, etc. Comparisons with ground-based near-infrared and space-based mid and far-infrared images from Spitzer are used to reveal the stellar content of the Bok globules, association of embedded young stellar objects with the submm dust cores, and the evolutionary stages of the individual sources. Submm dust continuum emission was detected in 26 out of the 32 globule cores observed. For 18 globules with detected (sub)mm cores we derive evolutionary stages and physical parameters of the embedded sources. We identify nine starless cores, most of which are presumably prestellar, nine Class 0 protostars, and twelve Class I YSOs. Specific source properties like bolometric temperature, core size, and central densities are discussed as function of evolutionary stage. We find that at least two thirds (16 out of 24) of the star-forming globules studied here show evidence of forming multiple stars on scales between 1,000 and 50,000 AU. However, we also find that most of these small prototstar and star groups are comprised of sources with different evolutionary stages, suggesting a picture of slow and sequential star formation in isolated globules.","downloadable_attachments":[{"id":42059983,"asset_id":21557378,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":42672119,"first_name":"Derek","last_name":"Ward-Thompson","domain_name":"independent","page_name":"DerekWardThompson","display_name":"Derek Ward-Thompson","profile_url":"https://independent.academia.edu/DerekWardThompson?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":23940,"name":"Near Infrared","url":"https://www.academia.edu/Documents/in/Near_Infrared?f_ri=4363","nofollow":true},{"id":335361,"name":"Infrared","url":"https://www.academia.edu/Documents/in/Infrared?f_ri=4363","nofollow":true},{"id":335363,"name":"Far Infrared","url":"https://www.academia.edu/Documents/in/Far_Infrared?f_ri=4363"},{"id":535357,"name":"Low Mass Stars","url":"https://www.academia.edu/Documents/in/Low_Mass_Stars?f_ri=4363"},{"id":1228946,"name":"Physical Properties","url":"https://www.academia.edu/Documents/in/Physical_Properties?f_ri=4363"},{"id":2217031,"name":"Spectral Energy Distribution","url":"https://www.academia.edu/Documents/in/Spectral_Energy_Distribution?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_20538392" data-work_id="20538392" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/20538392/Water_in_Star_Forming_Regions_with_Herschel_WISH_overview">Water in Star-Forming Regions with Herschel (WISH): overview</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">Water is a key molecule for determining the physical and chemical structure of star-forming regions because of its large abundance variations, both in the gas and in the ice, between warm and cold regions. In this HIFI-led 429 hr Key... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_20538392" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">Water is a key molecule for determining the physical and chemical structure of star-forming regions because of its large abundance variations, both in the gas and in the ice, between warm and cold regions. In this HIFI-led 429 hr Key Program, we are obtaining a comprehensive set of water observations toward a large sample of well-characterized protostars, covering a wide range of masses and luminosities -from the lowest to the highest mass protostars-, as well as evolutionary stages -from the first stages represented by pre-stellar cores to the later stages represented by the pre-main sequence stars surrounded only by their protoplanetary disks. Lines of H2O and its isotopologues, as well as chemically related hydrides, are observed. In addition, selected high-frequency lines of CO isotopes, [O I] and [C II] are obtained with HIFI and PACS, and are complemented by ground-based HDO, CO and dust continuum maps to ensure a self-consistent data set for analysis. Limited mapping information on a few arcmin scale provides information on local variations due to outflows and clustered star formation. Together, the data elucidate the physical processes responsible for the warm gas (passive heating, UV or X-ray-heating, shocks, disks), probe dynamical processes associated with forming stars and planets (outflow, infall, turbulence), reveal the chemical evolution of water and the oxygen-reservoir, and test basic gas-grain chemical interactions. By the time of the COSPAR meeting, about half of our program should have been observed. This talk will present an overview of the main highlights.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/20538392" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="3f621fd7499bf23419123754c716441a" rel="nofollow" data-download="{"attachment_id":41948347,"asset_id":20538392,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/41948347/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="9126" href="https://ku-dk.academia.edu/LarsKristensen">Lars Kristensen</a><script data-card-contents-for-user="9126" type="text/json">{"id":9126,"first_name":"Lars","last_name":"Kristensen","domain_name":"ku-dk","page_name":"LarsKristensen","display_name":"Lars Kristensen","profile_url":"https://ku-dk.academia.edu/LarsKristensen?f_ri=4363","photo":"https://0.academia-photos.com/9126/9618811/10714185/s65_lars.kristensen.png"}</script></span></span></li><li class="js-paper-rank-work_20538392 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="20538392"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 20538392, container: ".js-paper-rank-work_20538392", }); 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$(".js-view-count[data-work-id=20538392]").text(description); $(".js-view-count-work_20538392").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_20538392").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="20538392"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">4</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="48458" rel="nofollow" href="https://www.academia.edu/Documents/in/High_Frequency">High Frequency</a>, <script data-card-contents-for-ri="48458" type="text/json">{"id":48458,"name":"High Frequency","url":"https://www.academia.edu/Documents/in/High_Frequency?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="575076" rel="nofollow" href="https://www.academia.edu/Documents/in/Heat_Shock">Heat Shock</a>, <script data-card-contents-for-ri="575076" type="text/json">{"id":575076,"name":"Heat Shock","url":"https://www.academia.edu/Documents/in/Heat_Shock?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1431633" rel="nofollow" href="https://www.academia.edu/Documents/in/Chemical_Structure">Chemical Structure</a><script data-card-contents-for-ri="1431633" type="text/json">{"id":1431633,"name":"Chemical Structure","url":"https://www.academia.edu/Documents/in/Chemical_Structure?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=20538392]'), work: {"id":20538392,"title":"Water in Star-Forming Regions with Herschel (WISH): overview","created_at":"2016-01-22T06:05:08.270-08:00","url":"https://www.academia.edu/20538392/Water_in_Star_Forming_Regions_with_Herschel_WISH_overview?f_ri=4363","dom_id":"work_20538392","summary":"Water is a key molecule for determining the physical and chemical structure of star-forming regions because of its large abundance variations, both in the gas and in the ice, between warm and cold regions. In this HIFI-led 429 hr Key Program, we are obtaining a comprehensive set of water observations toward a large sample of well-characterized protostars, covering a wide range of masses and luminosities -from the lowest to the highest mass protostars-, as well as evolutionary stages -from the first stages represented by pre-stellar cores to the later stages represented by the pre-main sequence stars surrounded only by their protoplanetary disks. Lines of H2O and its isotopologues, as well as chemically related hydrides, are observed. In addition, selected high-frequency lines of CO isotopes, [O I] and [C II] are obtained with HIFI and PACS, and are complemented by ground-based HDO, CO and dust continuum maps to ensure a self-consistent data set for analysis. Limited mapping information on a few arcmin scale provides information on local variations due to outflows and clustered star formation. Together, the data elucidate the physical processes responsible for the warm gas (passive heating, UV or X-ray-heating, shocks, disks), probe dynamical processes associated with forming stars and planets (outflow, infall, turbulence), reveal the chemical evolution of water and the oxygen-reservoir, and test basic gas-grain chemical interactions. By the time of the COSPAR meeting, about half of our program should have been observed. This talk will present an overview of the main highlights.","downloadable_attachments":[{"id":41948347,"asset_id":20538392,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":9126,"first_name":"Lars","last_name":"Kristensen","domain_name":"ku-dk","page_name":"LarsKristensen","display_name":"Lars Kristensen","profile_url":"https://ku-dk.academia.edu/LarsKristensen?f_ri=4363","photo":"https://0.academia-photos.com/9126/9618811/10714185/s65_lars.kristensen.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":48458,"name":"High Frequency","url":"https://www.academia.edu/Documents/in/High_Frequency?f_ri=4363","nofollow":true},{"id":575076,"name":"Heat Shock","url":"https://www.academia.edu/Documents/in/Heat_Shock?f_ri=4363","nofollow":true},{"id":1431633,"name":"Chemical Structure","url":"https://www.academia.edu/Documents/in/Chemical_Structure?f_ri=4363","nofollow":true}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_19320319 coauthored" data-work_id="19320319" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/19320319/THE_ACS_NEARBY_GALAXY_SURVEY_TREASURY_I_THE_STAR_FORMATION_HISTORY_OF_THE_M81_OUTER_DISK">THE ACS NEARBY GALAXY SURVEY TREASURY. I. THE STAR FORMATION HISTORY OF THE M81 OUTER DISK</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The ACS Nearby Galaxy Survey Treasury (ANGST) is a large Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) treasury program to obtain resolved stellar photometry for a volume-limited sample of galaxies out to 4 Mpc. As part... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_19320319" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The ACS Nearby Galaxy Survey Treasury (ANGST) is a large Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) treasury program to obtain resolved stellar photometry for a volume-limited sample of galaxies out to 4 Mpc. As part of this program, we have obtained deep ACS imaging of a field in the outer disk of the large spiral galaxy M81. The field contains the outskirts of a spiral arm as well as an area containing no current star formation. Our imaging results in a colormagnitude diagram (CMD) reaching to m F 814W = 28.8 and m F 606W = 29.5, one magnitude fainter than the red clump. Through detailed modeling of the full CMD, we quantify the age and metallicity distribution of the stellar populations contained in the field. The mean metallicity in the field is −1 < [M/H] < 0 and only a small fraction of stars have ages < ∼ 1 Gyr. The results show that most of the stars in this outer disk field were formed by z ∼ 1 and that the arm structure at this radius has a lifetime of > ∼ 100 Myr. We discuss the measured evolution of the M81 disk in the context of surveys of high-redshift disk galaxies and deep stellar photometry of other nearby galaxies. All of these indicate that massive spiral disks are mostly formed by z∼1 and that they have experienced rapid metal enrichment.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/19320319" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="dafb1015d38b1a1d979a640386ce56fa" rel="nofollow" data-download="{"attachment_id":42249550,"asset_id":19320319,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/42249550/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="39575728" href="https://independent.academia.edu/ADolphin">Andrew Dolphin</a><script data-card-contents-for-user="39575728" type="text/json">{"id":39575728,"first_name":"Andrew","last_name":"Dolphin","domain_name":"independent","page_name":"ADolphin","display_name":"Andrew Dolphin","profile_url":"https://independent.academia.edu/ADolphin?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span><span class="u-displayInlineBlock InlineList-item-text"> and <span class="u-textDecorationUnderline u-clickable InlineList-item-text js-work-more-authors-19320319">+2</span><div class="hidden js-additional-users-19320319"><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/EvanSkillman">Evan Skillman</a></span></div><div><span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a href="https://independent.academia.edu/PeterStetson">Peter Stetson</a></span></div></div></span><script>(function(){ var popoverSettings = { el: $('.js-work-more-authors-19320319'), placement: 'bottom', hide_delay: 200, html: true, content: function(){ return $('.js-additional-users-19320319').html(); 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I. THE STAR FORMATION HISTORY OF THE M81 OUTER DISK","created_at":"2015-12-01T14:03:15.686-08:00","url":"https://www.academia.edu/19320319/THE_ACS_NEARBY_GALAXY_SURVEY_TREASURY_I_THE_STAR_FORMATION_HISTORY_OF_THE_M81_OUTER_DISK?f_ri=4363","dom_id":"work_19320319","summary":"The ACS Nearby Galaxy Survey Treasury (ANGST) is a large Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) treasury program to obtain resolved stellar photometry for a volume-limited sample of galaxies out to 4 Mpc. As part of this program, we have obtained deep ACS imaging of a field in the outer disk of the large spiral galaxy M81. The field contains the outskirts of a spiral arm as well as an area containing no current star formation. Our imaging results in a colormagnitude diagram (CMD) reaching to m F 814W = 28.8 and m F 606W = 29.5, one magnitude fainter than the red clump. Through detailed modeling of the full CMD, we quantify the age and metallicity distribution of the stellar populations contained in the field. The mean metallicity in the field is −1 \u003c [M/H] \u003c 0 and only a small fraction of stars have ages \u003c ∼ 1 Gyr. The results show that most of the stars in this outer disk field were formed by z ∼ 1 and that the arm structure at this radius has a lifetime of \u003e ∼ 100 Myr. We discuss the measured evolution of the M81 disk in the context of surveys of high-redshift disk galaxies and deep stellar photometry of other nearby galaxies. All of these indicate that massive spiral disks are mostly formed by z∼1 and that they have experienced rapid metal enrichment.","downloadable_attachments":[{"id":42249550,"asset_id":19320319,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":39575728,"first_name":"Andrew","last_name":"Dolphin","domain_name":"independent","page_name":"ADolphin","display_name":"Andrew Dolphin","profile_url":"https://independent.academia.edu/ADolphin?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":65895241,"first_name":"Evan","last_name":"Skillman","domain_name":"independent","page_name":"EvanSkillman","display_name":"Evan Skillman","profile_url":"https://independent.academia.edu/EvanSkillman?f_ri=4363","photo":"/images/s65_no_pic.png"},{"id":56123645,"first_name":"Peter","last_name":"Stetson","domain_name":"independent","page_name":"PeterStetson","display_name":"Peter Stetson","profile_url":"https://independent.academia.edu/PeterStetson?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":61631,"name":"High Redshift Universe","url":"https://www.academia.edu/Documents/in/High_Redshift_Universe?f_ri=4363","nofollow":true},{"id":383911,"name":"Spiral Galaxies","url":"https://www.academia.edu/Documents/in/Spiral_Galaxies?f_ri=4363","nofollow":true},{"id":587957,"name":"Star formation History","url":"https://www.academia.edu/Documents/in/Star_formation_History?f_ri=4363","nofollow":true},{"id":1181250,"name":"Hubble Space Telescope Images","url":"https://www.academia.edu/Documents/in/Hubble_Space_Telescope_Images?f_ri=4363"},{"id":1460347,"name":"Astronomical","url":"https://www.academia.edu/Documents/in/Astronomical?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_61950730" data-work_id="61950730" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/61950730/Inflation_and_squeezed_quantum_states">Inflation and squeezed quantum states</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">The inflationary cosmology is analyzed from the point of view of squeezed quantum states. As noted by Grishchuk and Sidorov, the amplification of quantum fluctuations into macroscopic perturbations which occurs during cosmic inflation is... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_61950730" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">The inflationary cosmology is analyzed from the point of view of squeezed quantum states. As noted by Grishchuk and Sidorov, the amplification of quantum fluctuations into macroscopic perturbations which occurs during cosmic inflation is a process of quantum squeezing. We carefully develop the squeezed state formalism and derive the equations that govern the evolution of a gaussian initial state. We derive the power spectrum of density perturbations for a simple inflationary model and discuss its features. We conclude that the squeezed state formalism provides an interesting framework within which to study the amplification process, but,in disagreement with the claims of Grishchuk and Sidorov , that it does not provide us with any new physical results.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/61950730" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="9bfba8e66b57ec18df458dba79a3efb5" rel="nofollow" data-download="{"attachment_id":74850621,"asset_id":61950730,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/74850621/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="168938742" href="https://independent.academia.edu/TomislavProkopec">Tomislav Prokopec</a><script data-card-contents-for-user="168938742" type="text/json">{"id":168938742,"first_name":"Tomislav","last_name":"Prokopec","domain_name":"independent","page_name":"TomislavProkopec","display_name":"Tomislav Prokopec","profile_url":"https://independent.academia.edu/TomislavProkopec?f_ri=4363","photo":"https://0.academia-photos.com/168938742/57316513/45533182/s65_tomislav.prokopec.jpeg"}</script></span></span></li><li class="js-paper-rank-work_61950730 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="61950730"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 61950730, container: ".js-paper-rank-work_61950730", }); });</script></li><li class="js-percentile-work_61950730 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 61950730; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_61950730"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_61950730 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="61950730"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 61950730; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=61950730]").text(description); $(".js-view-count-work_61950730").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_61950730").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="61950730"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">15</a>  </div><span class="InlineList-item-text u-textTruncate u-pl10x"><a class="InlineList-item-text" data-has-card-for-ri="333" rel="nofollow" href="https://www.academia.edu/Documents/in/Field_Theory">Field Theory</a>, <script data-card-contents-for-ri="333" type="text/json">{"id":333,"name":"Field Theory","url":"https://www.academia.edu/Documents/in/Field_Theory?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="518" rel="nofollow" href="https://www.academia.edu/Documents/in/Quantum_Physics">Quantum Physics</a>, <script data-card-contents-for-ri="518" type="text/json">{"id":518,"name":"Quantum Physics","url":"https://www.academia.edu/Documents/in/Quantum_Physics?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="1247" rel="nofollow" href="https://www.academia.edu/Documents/in/Quantum_Gravity">Quantum Gravity</a>, <script data-card-contents-for-ri="1247" type="text/json">{"id":1247,"name":"Quantum Gravity","url":"https://www.academia.edu/Documents/in/Quantum_Gravity?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a><script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=61950730]'), work: {"id":61950730,"title":"Inflation and squeezed quantum states","created_at":"2021-11-18T09:38:09.078-08:00","url":"https://www.academia.edu/61950730/Inflation_and_squeezed_quantum_states?f_ri=4363","dom_id":"work_61950730","summary":"The inflationary cosmology is analyzed from the point of view of squeezed quantum states. As noted by Grishchuk and Sidorov, the amplification of quantum fluctuations into macroscopic perturbations which occurs during cosmic inflation is a process of quantum squeezing. We carefully develop the squeezed state formalism and derive the equations that govern the evolution of a gaussian initial state. We derive the power spectrum of density perturbations for a simple inflationary model and discuss its features. We conclude that the squeezed state formalism provides an interesting framework within which to study the amplification process, but,in disagreement with the claims of Grishchuk and Sidorov , that it does not provide us with any new physical results.","downloadable_attachments":[{"id":74850621,"asset_id":61950730,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":168938742,"first_name":"Tomislav","last_name":"Prokopec","domain_name":"independent","page_name":"TomislavProkopec","display_name":"Tomislav Prokopec","profile_url":"https://independent.academia.edu/TomislavProkopec?f_ri=4363","photo":"https://0.academia-photos.com/168938742/57316513/45533182/s65_tomislav.prokopec.jpeg"}],"research_interests":[{"id":333,"name":"Field Theory","url":"https://www.academia.edu/Documents/in/Field_Theory?f_ri=4363","nofollow":true},{"id":518,"name":"Quantum Physics","url":"https://www.academia.edu/Documents/in/Quantum_Physics?f_ri=4363","nofollow":true},{"id":1247,"name":"Quantum Gravity","url":"https://www.academia.edu/Documents/in/Quantum_Gravity?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":16619,"name":"Early Universe","url":"https://www.academia.edu/Documents/in/Early_Universe?f_ri=4363"},{"id":113317,"name":"Inflation","url":"https://www.academia.edu/Documents/in/Inflation?f_ri=4363"},{"id":211387,"name":"Electromagnetic Field","url":"https://www.academia.edu/Documents/in/Electromagnetic_Field?f_ri=4363"},{"id":290469,"name":"Phase Space","url":"https://www.academia.edu/Documents/in/Phase_Space?f_ri=4363"},{"id":386999,"name":"Power Spectrum","url":"https://www.academia.edu/Documents/in/Power_Spectrum?f_ri=4363"},{"id":584715,"name":"Quantum Fluctuation","url":"https://www.academia.edu/Documents/in/Quantum_Fluctuation?f_ri=4363"},{"id":612229,"name":"Background Radiation","url":"https://www.academia.edu/Documents/in/Background_Radiation?f_ri=4363"},{"id":701253,"name":"New Physics","url":"https://www.academia.edu/Documents/in/New_Physics?f_ri=4363"},{"id":892890,"name":"Point of View","url":"https://www.academia.edu/Documents/in/Point_of_View?f_ri=4363"},{"id":1253121,"name":"QUantum state engineering","url":"https://www.academia.edu/Documents/in/QUantum_state_engineering?f_ri=4363"},{"id":1600931,"name":"Perturbation Theory","url":"https://www.academia.edu/Documents/in/Perturbation_Theory?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_49146435" data-work_id="49146435" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/49146435/How_the_Milky_Way_Formed">How the Milky Way Formed</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest">LARGE MAGELLANIC CLOUD is one of the Milky WayÕs two largest satellite galaxies. Slowly spiraling into the Milky Way, the cloud will brießy rejuvenate our galaxy at some time in the distant future.</div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/49146435" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="779020952c15e6a72165717a5fdd20ce" rel="nofollow" data-download="{"attachment_id":67536246,"asset_id":49146435,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/67536246/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="33758034" href="https://independent.academia.edu/JHesser">J. Hesser</a><script data-card-contents-for-user="33758034" type="text/json">{"id":33758034,"first_name":"J.","last_name":"Hesser","domain_name":"independent","page_name":"JHesser","display_name":"J. Hesser","profile_url":"https://independent.academia.edu/JHesser?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_49146435 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="49146435"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 49146435, container: ".js-paper-rank-work_49146435", }); });</script></li><li class="js-percentile-work_49146435 InlineList-item InlineList-item--bordered hidden u-tcGrayDark"><span class="percentile-widget hidden"><span class="u-mr2x percentile-widget" style="display: none">•</span><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 49146435; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-percentile-work_49146435"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></li><li class="js-view-count-work_49146435 InlineList-item InlineList-item--bordered hidden"><div><span><span class="js-view-count view-count u-mr2x" data-work-id="49146435"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 49146435; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=49146435]").text(description); $(".js-view-count-work_49146435").attr('title', description).tooltip(); }); });</script></span><script>$(function() { $(".js-view-count-work_49146435").removeClass('hidden') })</script></div></li><li class="InlineList-item u-positionRelative" style="max-width: 250px"><div class="u-positionAbsolute" data-has-card-for-ri-list="49146435"><i class="fa fa-tag InlineList-item-icon u-positionRelative"></i>  <a class="InlineList-item-text u-positionRelative">8</a>  </div><span class="InlineList-item-text u-textTruncate u-pl9x"><a class="InlineList-item-text" data-has-card-for-ri="4363" rel="nofollow" href="https://www.academia.edu/Documents/in/Star_Formation">Star Formation</a>, <script data-card-contents-for-ri="4363" type="text/json">{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="4818" rel="nofollow" href="https://www.academia.edu/Documents/in/Dark_Matter">Dark Matter</a>, <script data-card-contents-for-ri="4818" type="text/json">{"id":4818,"name":"Dark Matter","url":"https://www.academia.edu/Documents/in/Dark_Matter?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="11050" rel="nofollow" href="https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution">Galaxy Formation and Evolution</a>, <script data-card-contents-for-ri="11050" type="text/json">{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true}</script><a class="InlineList-item-text" data-has-card-for-ri="40629" rel="nofollow" href="https://www.academia.edu/Documents/in/Big_Bang">Big Bang</a><script data-card-contents-for-ri="40629" type="text/json">{"id":40629,"name":"Big Bang","url":"https://www.academia.edu/Documents/in/Big_Bang?f_ri=4363","nofollow":true}</script></span></li><script>(function(){ if (true) { new Aedu.ResearchInterestListCard({ el: $('*[data-has-card-for-ri-list=49146435]'), work: {"id":49146435,"title":"How the Milky Way Formed","created_at":"2021-06-06T13:29:32.114-07:00","url":"https://www.academia.edu/49146435/How_the_Milky_Way_Formed?f_ri=4363","dom_id":"work_49146435","summary":"LARGE MAGELLANIC CLOUD is one of the Milky WayÕs two largest satellite galaxies. Slowly spiraling into the Milky Way, the cloud will brießy rejuvenate our galaxy at some time in the distant future.","downloadable_attachments":[{"id":67536246,"asset_id":49146435,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":33758034,"first_name":"J.","last_name":"Hesser","domain_name":"independent","page_name":"JHesser","display_name":"J. Hesser","profile_url":"https://independent.academia.edu/JHesser?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4818,"name":"Dark Matter","url":"https://www.academia.edu/Documents/in/Dark_Matter?f_ri=4363","nofollow":true},{"id":11050,"name":"Galaxy Formation and Evolution","url":"https://www.academia.edu/Documents/in/Galaxy_Formation_and_Evolution?f_ri=4363","nofollow":true},{"id":40629,"name":"Big Bang","url":"https://www.academia.edu/Documents/in/Big_Bang?f_ri=4363","nofollow":true},{"id":128599,"name":"Gravitational Collapse","url":"https://www.academia.edu/Documents/in/Gravitational_Collapse?f_ri=4363"},{"id":162319,"name":"Milky Way","url":"https://www.academia.edu/Documents/in/Milky_Way?f_ri=4363"},{"id":235060,"name":"Black Hole","url":"https://www.academia.edu/Documents/in/Black_Hole?f_ri=4363"},{"id":1409149,"name":"Scientific American","url":"https://www.academia.edu/Documents/in/Scientific_American?f_ri=4363"}]}, }) } })();</script></ul></li></ul></div></div><div class="u-borderBottom1 u-borderColorGrayLighter"><div class="clearfix u-pv7x u-mb0x js-work-card work_26971516" data-work_id="26971516" itemscope="itemscope" itemtype="https://schema.org/ScholarlyArticle"><div class="header"><div class="title u-fontSerif u-fs22 u-lineHeight1_3"><a class="u-tcGrayDarkest js-work-link" href="https://www.academia.edu/26971516/DETECTIONS_OF_WATER_ICE_HYDROCARBONS_AND_3_3_%CE%BCm_PAH_IN_z_2_ULIRGs">DETECTIONS OF WATER ICE, HYDROCARBONS, AND 3.3 μm PAH IN z ∼ 2 ULIRGs</a></div></div><div class="u-pb4x u-mt3x"><div class="summary u-fs14 u-fw300 u-lineHeight1_5 u-tcGrayDarkest"><div class="summarized">We present the first detections of the 3 µm water ice and 3.4 µm amorphous hydrocarbon (HAC) absorption features in z ∼ 2 ULIRGs. These are based on deep rest-frame 2 -8 µm Spitzer IRS spectra of 11 sources selected for their appreciable... <a class="more_link u-tcGrayDark u-linkUnstyled" data-container=".work_26971516" data-show=".complete" data-hide=".summarized" data-more-link-behavior="true" href="#">more</a></div><div class="complete hidden">We present the first detections of the 3 µm water ice and 3.4 µm amorphous hydrocarbon (HAC) absorption features in z ∼ 2 ULIRGs. These are based on deep rest-frame 2 -8 µm Spitzer IRS spectra of 11 sources selected for their appreciable silicate absorption. The HAC-to-silicate ratio for our z ∼ 2 sources is typically higher by a factor of 2 -5 than that observed in the Milky Way. This HAC 'excess' suggests compact nuclei with steep temperature gradients as opposed to predominantly host obscuration. Beside the above molecular absorption features, we detect the 3.3 µm PAH emission feature in one of our sources with three more individual spectra showing evidence for it. Stacking analysis suggests that water ice, hydrocarbons, and PAH are likely present in the bulk of this sample even when not individually detected. The most unexpected result of our study is the lack of clear detections of the 4.67 µm CO gas absorption feature. Only three of the sources show tentative signs of this feature and at significantly lower levels than has been observed in local ULIRGs. Overall, we find that the closest local analogs to our sources, in terms of 3 -4 µm color, HAC-to-silicate and ice-to-silicate ratios, as well as low PAH equivalent widths are sources dominated by deeply obscured nuclei. Such sources form only a small fraction of -2 -ULIRGs locally and are commonly believed to be dominated by buried AGN. Our sample suggests that, in absolute number, such buried AGN are at least an order of magnitude more common at z ∼ 2 than today. The presence of PAH suggests that significant levels of star-formation are present even if the obscured AGN typically dominate the power budget.</div></div></div><ul class="InlineList u-ph0x u-fs13"><li class="InlineList-item logged_in_only"><div class="share_on_academia_work_button"><a class="academia_share Button Button--inverseBlue Button--sm js-bookmark-button" data-academia-share="Work/26971516" data-share-source="work_strip" data-spinner="small_white_hide_contents"><i class="fa fa-plus"></i><span class="work-strip-link-text u-ml1x" data-content="button_text">Bookmark</span></a></div></li><li class="InlineList-item"><div class="download"><a id="a560722f146a1a7564cfddc849f17913" rel="nofollow" data-download="{"attachment_id":47234368,"asset_id":26971516,"asset_type":"Work","always_allow_download":false,"track":null,"button_location":"work_strip","source":null,"hide_modal":null}" class="Button Button--sm Button--inverseGreen js-download-button prompt_button doc_download" href="https://www.academia.edu/attachments/47234368/download_file?st=MTczOTc5OTU1MSw4LjIyMi4yMDguMTQ2&s=work_strip"><i class="fa fa-arrow-circle-o-down fa-lg"></i><span class="u-textUppercase u-ml1x" data-content="button_text">Download</span></a></div></li><li class="InlineList-item"><ul class="InlineList InlineList--bordered u-ph0x"><li class="InlineList-item InlineList-item--bordered"><span class="InlineList-item-text">by <span itemscope="itemscope" itemprop="author" itemtype="https://schema.org/Person"><a class="u-tcGrayDark u-fw700" data-has-card-for-user="50947836" href="https://independent.academia.edu/MasatoshiImanishi">Masatoshi Imanishi</a><script data-card-contents-for-user="50947836" type="text/json">{"id":50947836,"first_name":"Masatoshi","last_name":"Imanishi","domain_name":"independent","page_name":"MasatoshiImanishi","display_name":"Masatoshi Imanishi","profile_url":"https://independent.academia.edu/MasatoshiImanishi?f_ri=4363","photo":"/images/s65_no_pic.png"}</script></span></span></li><li class="js-paper-rank-work_26971516 InlineList-item InlineList-item--bordered hidden"><span class="js-paper-rank-view hidden u-tcGrayDark" data-paper-rank-work-id="26971516"><i class="u-m1x fa fa-bar-chart"></i><strong class="js-paper-rank"></strong></span><script>$(function() { new Works.PaperRankView({ workId: 26971516, container: ".js-paper-rank-work_26971516", }); 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These are based on deep rest-frame 2 -8 µm Spitzer IRS spectra of 11 sources selected for their appreciable silicate absorption. The HAC-to-silicate ratio for our z ∼ 2 sources is typically higher by a factor of 2 -5 than that observed in the Milky Way. This HAC 'excess' suggests compact nuclei with steep temperature gradients as opposed to predominantly host obscuration. Beside the above molecular absorption features, we detect the 3.3 µm PAH emission feature in one of our sources with three more individual spectra showing evidence for it. Stacking analysis suggests that water ice, hydrocarbons, and PAH are likely present in the bulk of this sample even when not individually detected. The most unexpected result of our study is the lack of clear detections of the 4.67 µm CO gas absorption feature. Only three of the sources show tentative signs of this feature and at significantly lower levels than has been observed in local ULIRGs. Overall, we find that the closest local analogs to our sources, in terms of 3 -4 µm color, HAC-to-silicate and ice-to-silicate ratios, as well as low PAH equivalent widths are sources dominated by deeply obscured nuclei. Such sources form only a small fraction of -2 -ULIRGs locally and are commonly believed to be dominated by buried AGN. Our sample suggests that, in absolute number, such buried AGN are at least an order of magnitude more common at z ∼ 2 than today. The presence of PAH suggests that significant levels of star-formation are present even if the obscured AGN typically dominate the power budget.","downloadable_attachments":[{"id":47234368,"asset_id":26971516,"asset_type":"Work","always_allow_download":false}],"ordered_authors":[{"id":50947836,"first_name":"Masatoshi","last_name":"Imanishi","domain_name":"independent","page_name":"MasatoshiImanishi","display_name":"Masatoshi Imanishi","profile_url":"https://independent.academia.edu/MasatoshiImanishi?f_ri=4363","photo":"/images/s65_no_pic.png"}],"research_interests":[{"id":531,"name":"Organic Chemistry","url":"https://www.academia.edu/Documents/in/Organic_Chemistry?f_ri=4363","nofollow":true},{"id":723,"name":"Astrophysical Plasma","url":"https://www.academia.edu/Documents/in/Astrophysical_Plasma?f_ri=4363","nofollow":true},{"id":4363,"name":"Star Formation","url":"https://www.academia.edu/Documents/in/Star_Formation?f_ri=4363","nofollow":true},{"id":4742,"name":"Active Galactic 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