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data-broccoli-component="user-info.followees-count" data-click-track="profile-expand-user-info-following"><p class="label">Following</p><p class="data">71</p></div></a><a><div class="stat-container js-profile-coauthors" data-broccoli-component="user-info.coauthors-count" data-click-track="profile-expand-user-info-coauthors"><p class="label">Co-author</p><p class="data">1</p></div></a><a href="/ManojenduChoudhury/mentions"><div class="stat-container"><p class="label">Mentions</p><p class="data">142</p></div></a><span><div class="stat-container"><p class="label"><span class="js-profile-total-view-text">Public Views</span></p><p class="data"><span class="js-profile-view-count"></span></p></div></span></div><div class="user-bio-container"><div class="profile-bio fake-truncate js-profile-about" style="margin: 0px;">High energy astronomy, data analyses and phenomenological interpretation, teaching, education, content development and management.<br /><div class="js-profile-less-about u-linkUnstyled u-tcGrayDarker u-textDecorationUnderline u-displayNone">less</div></div></div><div class="ri-section"><div class="ri-section-header"><span>Interests</span></div><div class="ri-tags-container"><a data-click-track="profile-user-info-expand-research-interests" data-has-card-for-ri-list="523639" href="https://www.academia.edu/Documents/in/Astronomy_and_Astrophysics_Data_analysis_and_phenomenological_interpretation_in_all_kinds_of_divers"><div id="js-react-on-rails-context" style="display:none" data-rails-context="{"inMailer":false,"i18nLocale":"en","i18nDefaultLocale":"en","href":"https://independent.academia.edu/ManojenduChoudhury","location":"/ManojenduChoudhury","scheme":"https","host":"independent.academia.edu","port":null,"pathname":"/ManojenduChoudhury","search":null,"httpAcceptLanguage":null,"serverSide":false}"></div> <div class="js-react-on-rails-component" style="display:none" data-component-name="Pill" data-props="{"color":"gray","children":["Astronomy and 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js-UserInfo-social-cv" data-broccoli-component="user-info.cv-button" data-click-track="profile-user-info-cv" data-cv-filename="M_Choudhury-resume.pdf" data-placement="top" data-toggle="tooltip" href="/ManojenduChoudhury/CurriculumVitae"><button class="ds2-5-text-link ds2-5-text-link--small" style="font-size: 20px; letter-spacing: 0.8px"><span class="ds2-5-text-link__content">CV</span></button></li><li><a class="ds2-5-text-link ds2-5-text-link--small" href="https://manojenduchoudhury.academia.edu/"><span class="ds2-5-text-link__content"><i class="fa fa-laptop"></i></span></a></li><li class="profile-profiles js-social-profiles-container"><i class="fa fa-spin fa-spinner"></i></li></ul></div></div></div><div class="right-panel-container"><div class="user-content-wrapper"><div class="uploads-container" id="social-redesign-work-container"><div class="upload-header"><h2 class="ds2-5-heading-sans-serif-xs">Uploads</h2></div><div class="documents-container backbone-social-profile-documents" style="width: 100%;"><div class="u-taCenter"></div><div class="profile--tab_content_container js-tab-pane tab-pane active" id="all"><div class="profile--tab_heading_container js-section-heading" data-section="Papers" id="Papers"><h3 class="profile--tab_heading_container">Papers by Manojendu Choudhury</h3></div><div class="js-work-strip profile--work_container" data-work-id="114794282"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/114794282/Black_Holes_and_the_Scientific_Process"><img alt="Research paper thumbnail of Black Holes and the Scientific Process" class="work-thumbnail" src="https://attachments.academia-assets.com/111392257/thumbnails/1.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/114794282/Black_Holes_and_the_Scientific_Process">Black Holes and the Scientific Process</a></div><div class="wp-workCard_item"><span>arXiv (Cornell University)</span><span>, Feb 5, 2015</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="e678c8d01ebe8dece5611d614ce7b8f7" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":111392257,"asset_id":114794282,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/111392257/download_file?st=MTczMjQwNTg5OCw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="114794282"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="114794282"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 114794282; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=114794282]").text(description); $(".js-view-count[data-work-id=114794282]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 114794282; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = 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href="https://www.academia.edu/114794281/Importance_of_method_validation_Implications_of_non_correlated_observables_in_sweet_taste_receptor_studies">Importance of method validation: Implications of non-correlated observables in sweet taste receptor studies</a></div><div class="wp-workCard_item"><span>arXiv (Cornell University)</span><span>, Nov 25, 2015</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="52cac3b02db4a42497a469e965073a98" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":111392255,"asset_id":114794281,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/111392255/download_file?st=MTczMjQwNTg5OCw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: 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href="https://www.academia.edu/110656219/Accretion_Ejection_Mechanism_of_Cygnus_X_3_Poster_"><img alt="Research paper thumbnail of Accretion-Ejection Mechanism of Cygnus X-3(Poster)" class="work-thumbnail" src="https://a.academia-assets.com/images/blank-paper.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/110656219/Accretion_Ejection_Mechanism_of_Cygnus_X_3_Poster_">Accretion-Ejection Mechanism of Cygnus X-3(Poster)</a></div><div class="wp-workCard_item"><span>Progress of Theoretical Physics Supplement</span><span>, Nov 15, 2004</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">Abstract Cygnus X-3 is one of the brightest sources in radio band among the Galactic microquasars...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">Abstract Cygnus X-3 is one of the brightest sources in radio band among the Galactic microquasars, exhibiting outflows in the form of jets. The X-ray SED shows that the source exists in both low as well as high states, correspondingly related to the radio emission. The X-ray emission shows features unique to this source, independent of its X-ray state as well radio emission. We discuss these properties of this source, as observed, in the recent years, by RXTE.</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="110656219"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="110656219"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 110656219; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=110656219]").text(description); $(".js-view-count[data-work-id=110656219]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 110656219; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='110656219']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 110656219, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (false){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "-1" } } $('.js-work-strip[data-work-id=110656219]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":110656219,"title":"Accretion-Ejection Mechanism of Cygnus X-3(Poster)","translated_title":"","metadata":{"abstract":"Abstract Cygnus X-3 is one of the brightest sources in radio band among the Galactic microquasars, exhibiting outflows in the form of jets. 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$(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="91442523"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective"><img alt="Research paper thumbnail of Cygnus-3: a phenomenological perspective" class="work-thumbnail" src="https://a.academia-assets.com/images/blank-paper.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective">Cygnus-3: a phenomenological perspective</a></div><div class="wp-workCard_item"><span>Bulletin of the Astronomical Society of India</span><span>, Sep 1, 2005</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Mano...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="91442523"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="91442523"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 91442523; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=91442523]").text(description); $(".js-view-count[data-work-id=91442523]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 91442523; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='91442523']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 91442523, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (false){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "-1" } } $('.js-work-strip[data-work-id=91442523]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":91442523,"title":"Cygnus-3: a phenomenological perspective","translated_title":"","metadata":{"abstract":"342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...","publication_date":{"day":1,"month":9,"year":2005,"errors":{}},"publication_name":"Bulletin of the Astronomical Society of India"},"translated_abstract":"342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...","internal_url":"https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective","translated_internal_url":"","created_at":"2022-11-23T06:05:41.030-08:00","preview_url":null,"current_user_can_edit":null,"current_user_is_owner":null,"owner_id":523639,"coauthors_can_edit":true,"document_type":"paper","co_author_tags":[],"downloadable_attachments":[],"slug":"Cygnus_3_a_phenomenological_perspective","translated_slug":"","page_count":null,"language":"en","content_type":"Work","owner":{"id":523639,"first_name":"Manojendu","middle_initials":null,"last_name":"Choudhury","page_name":"ManojenduChoudhury","domain_name":"independent","created_at":"2011-06-30T22:16:37.707-07:00","display_name":"Manojendu Choudhury","url":"https://independent.academia.edu/ManojenduChoudhury"},"attachments":[],"research_interests":[{"id":3421497,"name":"Basi","url":"https://www.academia.edu/Documents/in/Basi"}],"urls":[]}, dispatcherData: dispatcherData }); $(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="91378554"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/91378554/Detection_of_nearly_periodic_spin_period_reversals_in_Vela_X_1_on_long_time_scales_inkling_of_solar_like_cycle_in_the_donor_star"><img alt="Research paper thumbnail of Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?" class="work-thumbnail" src="https://attachments.academia-assets.com/94682930/thumbnails/1.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/91378554/Detection_of_nearly_periodic_spin_period_reversals_in_Vela_X_1_on_long_time_scales_inkling_of_solar_like_cycle_in_the_donor_star">Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?</a></div><div class="wp-workCard_item"><span>Monthly Notices of the Royal Astronomical Society</span><span>, 2021</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X-1 over a period of 46 yr. Our analysis indicates nearly periodic variations in the spin period of the pulsar on time-scales of about 5.9 yr. There is suggestion of an overall spin-down behaviour of the pulsar though it is noticed that the source appears to stay near its equilibrium period 283.4 s since MJD 51000, with rather erratic spin-up/spin-down episodes around this value. Our study suggests nearly cyclic turnover in the spin behaviour of the pulsar from spin-up to spin-down regimes on time-scales of about 17–19 yr. To our knowledge, this is the first report of periodic variation in the spin behaviour of a wind-fed accreting pulsar. We also observe erratic episodes of spin-up and spin-down behaviour on relatively shorter time-scales that is a well-known archetype of this wind-fed X-ray pulsar. We investigate whether nearly periodic long-term spin period changes in the pulsar can be...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="ae3c3b8840b70dbd6b5ab3c541f2c836" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":94682930,"asset_id":91378554,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/94682930/download_file?st=MTczMjQwNTg5OSw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="91378554"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="91378554"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 91378554; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=91378554]").text(description); $(".js-view-count[data-work-id=91378554]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 91378554; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='91378554']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 91378554, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (true){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "ae3c3b8840b70dbd6b5ab3c541f2c836" } } $('.js-work-strip[data-work-id=91378554]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":91378554,"title":"Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?","translated_title":"","metadata":{"abstract":"We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X-1 over a period of 46 yr. 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To our knowledge, this is the first report of periodic variation in the spin behaviour of a wind-fed accreting pulsar. We also observe erratic episodes of spin-up and spin-down behaviour on relatively shorter time-scales that is a well-known archetype of this wind-fed X-ray pulsar. 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$(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="82382201"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/82382201/Preprint_typeset_using_L_ATEX_style_emulateapj_v_6_22_04_XMM_Newton_VIEW_OF_THE_ULTRA_LUMINOUS_X_RAY_SOURCES_IN_M_51"><img alt="Research paper thumbnail of Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51" class="work-thumbnail" src="https://attachments.academia-assets.com/88109640/thumbnails/1.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/82382201/Preprint_typeset_using_L_ATEX_style_emulateapj_v_6_22_04_XMM_Newton_VIEW_OF_THE_ULTRA_LUMINOUS_X_RAY_SOURCES_IN_M_51">Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51</a></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and NGC 5195). We confirm the presence of the seven known ULXs with luminosities exceeding the Eddington luminosity for a 10M ⊙ black hole, a low luminosity active galactic nucleus with 2−10 keV luminosity of 1.6 × 10 39 erg s −1, and soft thermal extended emission from NGC 5194 detected with Chandra. In addition, we also detected a new ULX with luminosity ∼ 10 39 erg s −1. We have studied the spectral and temporal properties of the LLAGN and 8 ULXs in NGC 5194, and an ULX in NGC 5195. Two ULXs in NGC 5194 show evidence for short-term variability, and all but two ULXs vary on long time scales (over a baseline of ∼ 2.5 years), providing strong evidence that these are accreting sources. One ULX in NGC 5194, source 69, shows possible periodic behavior in its X-ray flux. We derive a period of 5925 ± 200 s at a confidence level of 95%, based on three cycles. This period is lower than the period ...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="a42a1488736116d9ef97798302a9b128" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":88109640,"asset_id":82382201,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/88109640/download_file?st=MTczMjQwNTg5OSw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="82382201"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="82382201"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 82382201; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=82382201]").text(description); $(".js-view-count[data-work-id=82382201]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 82382201; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='82382201']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 82382201, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (true){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "a42a1488736116d9ef97798302a9b128" } } $('.js-work-strip[data-work-id=82382201]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":82382201,"title":"Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51","translated_title":"","metadata":{"abstract":"We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and NGC 5195). We confirm the presence of the seven known ULXs with luminosities exceeding the Eddington luminosity for a 10M ⊙ black hole, a low luminosity active galactic nucleus with 2−10 keV luminosity of 1.6 × 10 39 erg s −1, and soft thermal extended emission from NGC 5194 detected with Chandra. In addition, we also detected a new ULX with luminosity ∼ 10 39 erg s −1. We have studied the spectral and temporal properties of the LLAGN and 8 ULXs in NGC 5194, and an ULX in NGC 5195. Two ULXs in NGC 5194 show evidence for short-term variability, and all but two ULXs vary on long time scales (over a baseline of ∼ 2.5 years), providing strong evidence that these are accreting sources. One ULX in NGC 5194, source 69, shows possible periodic behavior in its X-ray flux. We derive a period of 5925 ± 200 s at a confidence level of 95%, based on three cycles. This period is lower than the period ...","publication_date":{"day":null,"month":null,"year":2008,"errors":{}}},"translated_abstract":"We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and NGC 5195). We confirm the presence of the seven known ULXs with luminosities exceeding the Eddington luminosity for a 10M ⊙ black hole, a low luminosity active galactic nucleus with 2−10 keV luminosity of 1.6 × 10 39 erg s −1, and soft thermal extended emission from NGC 5194 detected with Chandra. In addition, we also detected a new ULX with luminosity ∼ 10 39 erg s −1. We have studied the spectral and temporal properties of the LLAGN and 8 ULXs in NGC 5194, and an ULX in NGC 5195. Two ULXs in NGC 5194 show evidence for short-term variability, and all but two ULXs vary on long time scales (over a baseline of ∼ 2.5 years), providing strong evidence that these are accreting sources. One ULX in NGC 5194, source 69, shows possible periodic behavior in its X-ray flux. We derive a period of 5925 ± 200 s at a confidence level of 95%, based on three cycles. 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data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">The Spearman partial rank correlation test is used to determine the correlation between two or more variables. The partial rank coefficient is computed from the sampling distribution which may be derived by analogy with a parametric statistic (Macklin 1982). 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href="https://www.academia.edu/110656219/Accretion_Ejection_Mechanism_of_Cygnus_X_3_Poster_"><img alt="Research paper thumbnail of Accretion-Ejection Mechanism of Cygnus X-3(Poster)" class="work-thumbnail" src="https://a.academia-assets.com/images/blank-paper.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/110656219/Accretion_Ejection_Mechanism_of_Cygnus_X_3_Poster_">Accretion-Ejection Mechanism of Cygnus X-3(Poster)</a></div><div class="wp-workCard_item"><span>Progress of Theoretical Physics Supplement</span><span>, Nov 15, 2004</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">Abstract Cygnus X-3 is one of the brightest sources in radio band among the Galactic microquasars...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">Abstract Cygnus X-3 is one of the brightest sources in radio band among the Galactic microquasars, exhibiting outflows in the form of jets. The X-ray SED shows that the source exists in both low as well as high states, correspondingly related to the radio emission. The X-ray emission shows features unique to this source, independent of its X-ray state as well radio emission. 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$(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="91442523"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective"><img alt="Research paper thumbnail of Cygnus-3: a phenomenological perspective" class="work-thumbnail" src="https://a.academia-assets.com/images/blank-paper.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective">Cygnus-3: a phenomenological perspective</a></div><div class="wp-workCard_item"><span>Bulletin of the Astronomical Society of India</span><span>, Sep 1, 2005</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Mano...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="91442523"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="91442523"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 91442523; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=91442523]").text(description); $(".js-view-count[data-work-id=91442523]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 91442523; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='91442523']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 91442523, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (false){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "-1" } } $('.js-work-strip[data-work-id=91442523]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":91442523,"title":"Cygnus-3: a phenomenological perspective","translated_title":"","metadata":{"abstract":"342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...","publication_date":{"day":1,"month":9,"year":2005,"errors":{}},"publication_name":"Bulletin of the Astronomical Society of India"},"translated_abstract":"342 Bulletin of the Astronomical Society of India Cygnus X-3: a phenomenological perspective Manojendu Choudhury National Centre for Radio Astrophysics, TIFR, Pune Abstract. Cygnus X-3 is one of the most enigmatic X-ray binary systems with an undetermined compact object and a Woif-Rayet companion, persistent in the X-ray, infra-red and radio regimes of the electromagnetic spectrum. In the hard X-ray state of this source, the recent results of the radio X-ray correlations, in analogy with similar features from the confirmed black hole sources, ...","internal_url":"https://www.academia.edu/91442523/Cygnus_3_a_phenomenological_perspective","translated_internal_url":"","created_at":"2022-11-23T06:05:41.030-08:00","preview_url":null,"current_user_can_edit":null,"current_user_is_owner":null,"owner_id":523639,"coauthors_can_edit":true,"document_type":"paper","co_author_tags":[],"downloadable_attachments":[],"slug":"Cygnus_3_a_phenomenological_perspective","translated_slug":"","page_count":null,"language":"en","content_type":"Work","owner":{"id":523639,"first_name":"Manojendu","middle_initials":null,"last_name":"Choudhury","page_name":"ManojenduChoudhury","domain_name":"independent","created_at":"2011-06-30T22:16:37.707-07:00","display_name":"Manojendu Choudhury","url":"https://independent.academia.edu/ManojenduChoudhury"},"attachments":[],"research_interests":[{"id":3421497,"name":"Basi","url":"https://www.academia.edu/Documents/in/Basi"}],"urls":[]}, dispatcherData: dispatcherData }); $(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="91378554"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/91378554/Detection_of_nearly_periodic_spin_period_reversals_in_Vela_X_1_on_long_time_scales_inkling_of_solar_like_cycle_in_the_donor_star"><img alt="Research paper thumbnail of Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?" class="work-thumbnail" src="https://attachments.academia-assets.com/94682930/thumbnails/1.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/91378554/Detection_of_nearly_periodic_spin_period_reversals_in_Vela_X_1_on_long_time_scales_inkling_of_solar_like_cycle_in_the_donor_star">Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?</a></div><div class="wp-workCard_item"><span>Monthly Notices of the Royal Astronomical Society</span><span>, 2021</span></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X-1 over a period of 46 yr. Our analysis indicates nearly periodic variations in the spin period of the pulsar on time-scales of about 5.9 yr. There is suggestion of an overall spin-down behaviour of the pulsar though it is noticed that the source appears to stay near its equilibrium period 283.4 s since MJD 51000, with rather erratic spin-up/spin-down episodes around this value. Our study suggests nearly cyclic turnover in the spin behaviour of the pulsar from spin-up to spin-down regimes on time-scales of about 17–19 yr. To our knowledge, this is the first report of periodic variation in the spin behaviour of a wind-fed accreting pulsar. We also observe erratic episodes of spin-up and spin-down behaviour on relatively shorter time-scales that is a well-known archetype of this wind-fed X-ray pulsar. We investigate whether nearly periodic long-term spin period changes in the pulsar can be...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="ae3c3b8840b70dbd6b5ab3c541f2c836" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":94682930,"asset_id":91378554,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/94682930/download_file?st=MTczMjQwNTg5OSw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="91378554"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="91378554"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 91378554; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=91378554]").text(description); $(".js-view-count[data-work-id=91378554]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 91378554; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='91378554']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 91378554, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (true){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "ae3c3b8840b70dbd6b5ab3c541f2c836" } } $('.js-work-strip[data-work-id=91378554]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":91378554,"title":"Detection of nearly periodic spin period reversals in Vela X-1 on long time-scales: inkling of solar-like cycle in the donor star?","translated_title":"","metadata":{"abstract":"We explore the long-term evolution of the spin period of the high-mass X-ray binary pulsar Vela X-1 over a period of 46 yr. Our analysis indicates nearly periodic variations in the spin period of the pulsar on time-scales of about 5.9 yr. There is suggestion of an overall spin-down behaviour of the pulsar though it is noticed that the source appears to stay near its equilibrium period 283.4 s since MJD 51000, with rather erratic spin-up/spin-down episodes around this value. Our study suggests nearly cyclic turnover in the spin behaviour of the pulsar from spin-up to spin-down regimes on time-scales of about 17–19 yr. To our knowledge, this is the first report of periodic variation in the spin behaviour of a wind-fed accreting pulsar. We also observe erratic episodes of spin-up and spin-down behaviour on relatively shorter time-scales that is a well-known archetype of this wind-fed X-ray pulsar. 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To our knowledge, this is the first report of periodic variation in the spin behaviour of a wind-fed accreting pulsar. We also observe erratic episodes of spin-up and spin-down behaviour on relatively shorter time-scales that is a well-known archetype of this wind-fed X-ray pulsar. 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$(this).data('initialized', true); } }); $a.trackClickSource(".js-work-strip-work-link", "profile_work_strip") }); </script> <div class="js-work-strip profile--work_container" data-work-id="82382201"><div class="profile--work_thumbnail hidden-xs"><a class="js-work-strip-work-link" data-click-track="profile-work-strip-thumbnail" href="https://www.academia.edu/82382201/Preprint_typeset_using_L_ATEX_style_emulateapj_v_6_22_04_XMM_Newton_VIEW_OF_THE_ULTRA_LUMINOUS_X_RAY_SOURCES_IN_M_51"><img alt="Research paper thumbnail of Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51" class="work-thumbnail" src="https://attachments.academia-assets.com/88109640/thumbnails/1.jpg" /></a></div><div class="wp-workCard wp-workCard_itemContainer"><div class="wp-workCard_item wp-workCard--title"><a class="js-work-strip-work-link text-gray-darker" data-click-track="profile-work-strip-title" href="https://www.academia.edu/82382201/Preprint_typeset_using_L_ATEX_style_emulateapj_v_6_22_04_XMM_Newton_VIEW_OF_THE_ULTRA_LUMINOUS_X_RAY_SOURCES_IN_M_51">Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51</a></div><div class="wp-workCard_item"><span class="js-work-more-abstract-truncated">We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and...</span><a class="js-work-more-abstract" data-broccoli-component="work_strip.more_abstract" data-click-track="profile-work-strip-more-abstract" href="javascript:;"><span> more </span><span><i class="fa fa-caret-down"></i></span></a><span class="js-work-more-abstract-untruncated hidden">We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and NGC 5195). We confirm the presence of the seven known ULXs with luminosities exceeding the Eddington luminosity for a 10M ⊙ black hole, a low luminosity active galactic nucleus with 2−10 keV luminosity of 1.6 × 10 39 erg s −1, and soft thermal extended emission from NGC 5194 detected with Chandra. In addition, we also detected a new ULX with luminosity ∼ 10 39 erg s −1. We have studied the spectral and temporal properties of the LLAGN and 8 ULXs in NGC 5194, and an ULX in NGC 5195. Two ULXs in NGC 5194 show evidence for short-term variability, and all but two ULXs vary on long time scales (over a baseline of ∼ 2.5 years), providing strong evidence that these are accreting sources. One ULX in NGC 5194, source 69, shows possible periodic behavior in its X-ray flux. We derive a period of 5925 ± 200 s at a confidence level of 95%, based on three cycles. This period is lower than the period ...</span></div><div class="wp-workCard_item wp-workCard--actions"><span class="work-strip-bookmark-button-container"></span><a id="a42a1488736116d9ef97798302a9b128" class="wp-workCard--action" rel="nofollow" data-click-track="profile-work-strip-download" data-download="{"attachment_id":88109640,"asset_id":82382201,"asset_type":"Work","button_location":"profile"}" href="https://www.academia.edu/attachments/88109640/download_file?st=MTczMjQwNTg5OSw4LjIyMi4yMDguMTQ2&s=profile"><span><i class="fa fa-arrow-down"></i></span><span>Download</span></a><span class="wp-workCard--action visible-if-viewed-by-owner inline-block" style="display: none;"><span class="js-profile-work-strip-edit-button-wrapper profile-work-strip-edit-button-wrapper" data-work-id="82382201"><a class="js-profile-work-strip-edit-button" tabindex="0"><span><i class="fa fa-pencil"></i></span><span>Edit</span></a></span></span><span id="work-strip-rankings-button-container"></span></div><div class="wp-workCard_item wp-workCard--stats"><span><span><span class="js-view-count view-count u-mr2x" data-work-id="82382201"><i class="fa fa-spinner fa-spin"></i></span><script>$(function () { var workId = 82382201; window.Academia.workViewCountsFetcher.queue(workId, function (count) { var description = window.$h.commaizeInt(count) + " " + window.$h.pluralize(count, 'View'); $(".js-view-count[data-work-id=82382201]").text(description); $(".js-view-count[data-work-id=82382201]").attr('title', description).tooltip(); }); });</script></span></span><span><span class="percentile-widget hidden"><span class="u-mr2x work-percentile"></span></span><script>$(function () { var workId = 82382201; window.Academia.workPercentilesFetcher.queue(workId, function (percentileText) { var container = $(".js-work-strip[data-work-id='82382201']"); container.find('.work-percentile').text(percentileText.charAt(0).toUpperCase() + percentileText.slice(1)); container.find('.percentile-widget').show(); container.find('.percentile-widget').removeClass('hidden'); }); });</script></span><span><script>$(function() { new Works.PaperRankView({ workId: 82382201, container: "", }); });</script></span></div><div id="work-strip-premium-row-container"></div></div></div><script> require.config({ waitSeconds: 90 })(["https://a.academia-assets.com/assets/wow_profile-f77ea15d77ce96025a6048a514272ad8becbad23c641fc2b3bd6e24ca6ff1932.js","https://a.academia-assets.com/assets/work_edit-ad038b8c047c1a8d4fa01b402d530ff93c45fee2137a149a4a5398bc8ad67560.js"], function() { // from javascript_helper.rb var dispatcherData = {} if (true){ window.WowProfile.dispatcher = window.WowProfile.dispatcher || _.clone(Backbone.Events); dispatcherData = { dispatcher: window.WowProfile.dispatcher, downloadLinkId: "a42a1488736116d9ef97798302a9b128" } } $('.js-work-strip[data-work-id=82382201]').each(function() { if (!$(this).data('initialized')) { new WowProfile.WorkStripView({ el: this, workJSON: {"id":82382201,"title":"Preprint typeset using L ATEX style emulateapj v. 6/22/04 XMM-Newton VIEW OF THE ULTRA-LUMINOUS X-RAY SOURCES IN M 51","translated_title":"","metadata":{"abstract":"We present results based on XMM-Newton observation of the nearby spiral galaxy M 51 (NGC 5194 and NGC 5195). 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One ULX in NGC 5194, source 69, shows possible periodic behavior in its X-ray flux. We derive a period of 5925 ± 200 s at a confidence level of 95%, based on three cycles. 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