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<!DOCTYPE HTML PUBLIC "-//W3C//DTD HTML 4.01 Transitional//EN"> <html> <head> <meta http-equiv="Content-Type" content="text/html; charset=UTF-8"> <title>NGC 4173 - Galaxy - SKY-MAP</title> <LINK href="homepage1.css" type="text/css" rel="stylesheet"> <link type="text/css" CHARSET="UTF-8" rel="stylesheet" href="coolbar.css"/> <link rel="stylesheet" type="text/css" href="dhtml-menu.css" /> <style type="text/css"> hr { height: 1px; color: #aaa; background-color: #aaa; border: 0; margin: .2em 0 .2em 0; } h1, h2, h3, h4, h5, h6 { color: white; background: none; font-weight: normal; margin: 0; padding-top: .5em; padding-bottom: .17em; border-bottom: 1px solid #aaa; } h1 { font-size: 188%; } h1 .editsection { font-size: 53%; } .sTitle { margin-bottom: .1em; } </style> </head> <body bgcolor="BLACK" style="margin: 0"> <DIV id="d_top_line" style="BORDER-TOP-WIDTH: thin; CLEAR: right; PADDING-RIGHT: 0px; DISPLAY: inline; PADDING-LEFT: 0px; FONT-WEIGHT: bold; BORDER-LEFT-WIDTH: thin; FONT-SIZE: 11pt; BORDER-LEFT-COLOR: white; FLOAT: right; VISIBILITY: visible; BORDER-BOTTOM-WIDTH: thin; BORDER-BOTTOM-COLOR: white; PADDING-BOTTOM: 0px; MARGIN: 0px; OVERFLOW: visible; COLOR: white; BORDER-TOP-COLOR: white; PADDING-TOP: 0px; FONT-FAMILY: Sans-Serif; POSITION: absolute; LEFT: 0px; TOP: 0px; WIDTH: 940px; HEIGHT: 68px; BORDER-RIGHT-WIDTH: thin; TEXT-DECORATION: none; BORDER-RIGHT-COLOR: white; BACKGROUND-IMAGE: url(images/background_top.jpg)" align="left"> <script type='text/javascript' src='/jsc/dhtml-menu'></script> <script type="text/javascript"> function become_top_sponsor(){ ddrivetip('<table style="width:408px;border:1px solid gray;background-color:black;color:DodgerBlue;font-family:verdana;font-size:8pt;"><tr><td>The "Inhabited Sky" program awards you the status of "Supernova" if you "inhabit" a star and your donation related to this star is the largest of all those made to date (by anyone). Once you have acquired the status of "Supernova", the star that you are "inhabiting" will fall into a special category - "All Supernovas Sky". From that point on the "Supernova" status will be yours forever. Note: if you "inhabit" more than one star, the total amount of donations does not determine the "Supernova", the status of "Supernova" refers to the donation related to only one star. There is no limit to the number of times that you can become the "Supernova". <font color="#00ffff">Simply click here to become a Supernova!</font></td></tr></table>', 'BLACK', 150, 25); } function why_to_sponsor(){ ddrivetip('<table style="width:408px;border:1px solid gray;background-color:black;color:DodgerBlue;font-family:verdana;font-size:8pt;"><tr><td>By "inhabiting a star" you bond your name forever both with your chosen star and SKY-MAP.ORG. You will receive a web page linked to your star on "INHABITED SKY" which becomes from now on, your own personal page, where you can place any business or personal information. <br><font style="FONT-SIZE:3px;"> </font><br><img src="images/SuperNova.jpg" border=0 width=404 height=288></td></tr></table>', 'BLACK', 150, 25); } function why_to_sponsor1(){ ddrivetip('<table style="width:408px;border:1px solid gray;background-color:black;color:DodgerBlue;font-family:verdana;font-size:8pt;"><tr><td>By "inhabiting a star" you bond your name forever both with your chosen star and SKY-MAP.ORG. You will receive a web page linked to your star on "INHABITED SKY" which becomes from now on, your own personal page, where you can place any business or personal information. <br><font style="FONT-SIZE:3px;"> </font><br>The authors imagine SKY-MAP.ORG as a bridge linking the incredibly beautiful, and unimaginably complex world of modern science to the world of your everyday person as well as to the world of children. The authors hope that their site will make it possible to intrigue all layers of society to the grandeur of the outer space. The dream of the authors is to awaken the general public’s interest in the outer space – for us all to recognize the consequences behind Stephen Hawking’s opinion, that humanity does not have a future, if it would not feel at home in the Universe.<br>You may sponsor SKY-MAP.ORG through joining "Inhabit a Star" program.</td></tr></table>', 'BLACK', 150, 25); } function show_message(message){ ddrivetip('<table style="width:208px;border:1px solid gray;background-color:black;color:white;font-family:verdana;font-size:10pt;"><tr><td>'+message+'</td></tr></table>', 'BLACK', 150, 25); } function become_latest_sponsor(){ ddrivetip('<table style="width:408px;border:1px solid gray;background-color:black;color:DodgerBlue;font-family:verdana;font-size:8pt;"><tr><td>With the "Inhabited Sky" program you can acquire "Nova" status as soon as you "inhabit" a star and you will retain this status until somebody else "inhabits" another star. If you subsequently "inhabit" another star, you will obtain "Nova" status again, meaning that there is no limit to the number of times that you can become the "Nova".</td></tr></table>', 'BLACK', 150, 25); } var submenu_top20 = { "-" : "javascript:alert('Product 2');", "Chich" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 2431'+'</b></font><br><font color=DodgerBlue size=-2>'+'This star belongs to the Girls and Woohoo.</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=2431", "BRAD SCOTT" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 6306'+'</b></font><br><font color=DodgerBlue size=-2>'+'WOW..I&#39;m humbled by the glorious magnitude of this project and grate full to be a contributor...<br>to the many children of the world...<br>&quot;Wish high,Wish far ,Wish hard. Wish upon a STAR&quot;<br>ALOHA</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=6306", "Jaekyu Eo" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 689612'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=689612", "estrela" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 690409'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://astronote.org", "Anna Blake" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 813006981'+'</b></font><br><font color=DodgerBlue size=-2>'+'Happy birthday Matthew, I hope you’ll like it!</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=813006981" }; var submenu_products = { "   Open Supernova’s Website" : "event:target:_blank:event:class:snap_noshots:href:http://my.sky-map.org?zoom=12&show_box=1&star_id=2431", "   20 LATEST SUPERNOVAS >>" : submenu_top20, "   The Sky of All Supernovas" : "event:class:snap_noshots:href:http://my.sky-map.org/?", "   How to Become Supernova?" : "event:onmouseover:become_top_sponsor():event:onmouseout:hideddrivetip():href:http:/adopt_services.jsp?top_price=250.00", "   Supernovas on SKY-MAP" : "event:onmouseover:why_to_sponsor1():event:onmouseout:hideddrivetip():href:/adopt_services.jsp?top_price=250.00", "   Inhabit a Star!" : "event:target:_blank:href:http:/adopt_services.jsp?top_price=250.00" }; var submenu_top20latest = { "-" : "javascript:alert('Product 2');", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1984252'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1984252", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 77816'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=77816", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 279782'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=279782", "Carla Criner" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1109643'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1109643", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1003956'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1003956", "Timothy Carter" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 624028832'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=624028832", "Misty Bell" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 412735'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=412735", "AMOL PANCHAL" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1577647'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1577647", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 819833'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=819833", "ANQI BAO" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 2390241'+'</b></font><br><font color=DodgerBlue size=-2>'+'A start for Leo-- the American Scholar</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=2390241", "Aleksandr Karmanov" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 872581'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=872581", "Ayrton84" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 364778'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=364778", "Kim Huybrechts" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1972251'+'</b></font><br><font color=DodgerBlue size=-2>'+'Star light, Star bright...<br>My love will shine on you, <br>every day &amp; every night!!<br>HAPPY BIRTHDAY MAMA</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1972251", "Andy Marcus" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1535755'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1535755", "Lisa Palandri" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1127042'+'</b></font><br><font color=DodgerBlue size=-2>'+'Because I love him so much. A star can&#39;t belongs to a human but he will be the star of my life forever.</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1127042", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 1437618'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=1437618", "Aleksandr Karmanov" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 72428'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=72428", "Aleksandr Karmanov" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 316599'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=316599", "Aleksandr Karmanov" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 314169'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=314169", "Anonymous" : "event:target:_blank:event:onmouseover:show_message('<font size=-2><b>Star ID: 757760636'+'</b></font><br><font color=DodgerBlue size=-2>'+'</font>'):event:onmouseout:hideddrivetip():href:http://my.sky-map.org?zoom=12&show_box=1&star_id=757760636" }; 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border-width:0px;"> <td nowrap style="border-style: solid; border-color:yellow; border-width:0px;" align="left" valign="top" rowspan="2"> <DIV id="d_top_logo" style="FONT-SIZE: 20px; Z-INDEX: 100; CURSOR: default">SKY-MAP.<FONT color=red>ORG</FONT></DIV> </td> <td rowspan="2" style="FONT-SIZE: 12px;border-style: solid; border-color:yellow; border-width:0px;padding-top:0px;padding-bottom:0px;">&nbsp&nbsp&nbsp&nbsp&nbsp&nbsp&nbsp</td> <td rowspan="2" style="FONT-SIZE: 12px;height:13px;padding-top:0px;padding-bottom:0px;" align="left" nowrap>  </td> <td colspan="3" style="FONT-SIZE: 12px;height:13px;padding-top:0px;padding-bottom:0px;" align="left" nowrap>  </td> </tr> <tr> <td align="right" valign="top" style="border-style: solid; border-color:yellow; border-width:0px;padding-top:0px;padding-bottom:0px;" nowrap>  </td> <td style="FONT-SIZE: 12px;padding-top:0px;padding-bottom:0px;" valign="top"></td> <td align="left" style="padding-top:0px;padding-bottom:0px;" valign="top">  </td> </tr> </table> <FORM METHOD='POST' ACTION='?object=NGC+4170'> <DIV id="d_top_language_links" style="FONT-SIZE: 7pt; Z-INDEX: 100; POSITION: absolute; LEFT: 0px; TOP: -15px; WIDTH: 100%; TEXT-ALIGN: right; CURSOR: default"> <a href='?object=NGC+4170&locale=DE'>DE</a> <a href='?object=NGC+4170&locale=RU'>RU</a> <a href='?object=NGC+4170&locale=SV'>SV</a> <a href='?object=NGC+4170&locale=KO'>KO</a> <a href='?object=NGC+4170&locale=PT'>PT</a> <a href='?object=NGC+4170&locale=EL'>EL</a> <a href='?object=NGC+4170&locale=EN'>EN</a> <a href='?object=NGC+4170&locale=IT'>IT</a> <a href='?object=NGC+4170&locale=FR'>FR</a> <a href='?object=NGC+4170&locale=HU'>HU</a> <a href='?object=NGC+4170&locale=ES'>ES</a> <a href='?object=NGC+4170&locale=ZH'>ZH</a> <a href='?object=NGC+4170&locale=JA'>JA</a> <a href='?object=NGC+4170&locale=PL'>PL</a> <a href='?object=NGC+4170&locale=HE'>HE</a> <a href='?object=NGC+4170&locale=CA'>CA</a> <a href='?object=NGC+4170&locale=NL'>NL</a> <a href='?object=NGC+4170&locale=TR'>TR</a> <a href='?object=NGC+4170&locale=SR'>SR</a> </DIV> <DIV id="d_top_language" style="FONT-SIZE: 12px; Z-INDEX: 100; POSITION: absolute; LEFT: 0px; TOP: 6px; WIDTH: 100%; TEXT-ALIGN: right; CURSOR: default"> <span style="position: relative; top:0px; right: 16px"> <a href="https://twitter.com/SkyMapLaunch" class="twitter-follow-button" data-show-screen-name="true" data-show-count="false" style="height:15px">Follow @SkyMapLaunch</a> <script async="" src="//platform.twitter.com/widgets.js" charset="utf-8"></script> </span> <span style="position: relative; top:-5px; right: 6px"> <SELECT name='select_locale' class='TextField' ONCHANGE='this.form.submit();' ><OPTION value='DE'>Deutsch<OPTION value='RU'>Русский<OPTION value='SV'>Svenska<OPTION value='KO'>Korean<OPTION value='PT'>Português<OPTION value='EL'>Ελληνικά<OPTION value='EN' SELECTED>English<OPTION value='IT'>Italiano<OPTION value='FR'>Français<OPTION value='HU'>Magyar<OPTION value='ES'>Español<OPTION value='ZH'>Chinese<OPTION value='JA'>日本語<OPTION value='PL'>Polski<OPTION value='HE'>עִבְרִית<OPTION value='CA'>Català<OPTION value='NL'>Nederlands<OPTION value='TR'>Turkish<OPTION value='SR'>Srpski</SELECT> </span> </DIV> </FORM> <script type="text/javascript"> var currentLogo="Default"; var topLogos={Default:"SKY-MAP.<FONT color=red>ORG</FONT>",INHABITED:"<img src='images/star_b1_sm.gif' border=0 width=35 height=35 style='float:left;position:relative;top:-7;left:-2;'><font color=red>INHABITED</font> SKY",BLOGS:"<img src='images/star_b1_sm.gif' border=0 width=35 height=35 style='float:left;position:relative;top:-7;left:-2;'>BLOGS<font color=red>@</font>SKY",NEWS:"<img src='images/star_b1_sm.gif' border=0 width=35 height=35 style='float:left;position:relative;top:-7;left:-2;'>NEWS<font color=red>@</font>SKY",ET:"<FONT color=red>ET</FONT>.SKY-MAP"}; function fundraiser_label(){ ddrivetip('<table style="width:500px;border:1px solid gray;background-color:black;color:white;font-family:verdana;font-size:10pt"><tr><td><p>When we just started SKY-MAP five years ago, we thought only about the fun it would create for our own kids and hoped to open a wide window to the Universe for them. During the first three weeks of January 2011, SKY-MAP received over 1.5 million visitors from 190 countries.</p><p>The constant increase in traffic has made our servers slow and unstable and our environment has become insufficient. With such servers, it is almost impossible to upgrade the system with the new sets of astronomical data and we don’t have enough power to process all the Internet requests.</p><p>We urgently need to replace our two 6-years old servers. According to our calculations, $14,000US would be sufficient for us to purchase two new dual 6-core CPU servers. This hardware would be able to serve you perfectly and would give us enough space and flexibility for at least the immediate future.</p><p>We need your support in order for SKY-MAP (WIKISKY) to remain stable, fast, and advertisement-free.</p><p>We need your support to continue and intensify the development, enriching SKY-MAP with new data and functions.</p><br/><p align=center><em>Server upgrade fundraiser progress meter</em><br/><div style="width:467px;height:14px;position:relative;top:0px;left:15px;font-size:1px;cursor:pointer;border:1px #404040 solid"><img src="/img/servers_bar.png" style="position:absolute;left:0;top:0;width:467px;height:14px"><div style="position:absolute;left:0;top:0;height:14px;font-size:1px;width:68px;background-color:green;opacity:0.75;filter:alpha(opacity=75)"></div><div style="position:absolute;top:-1;left:9px;color:yellow;font-size:10pt;font-weight:bold">14.71%</p></div></p></td></tr></table>', 'BLACK', 150, 25); } function survive_label(){ ddrivetip('<table style="width:300px;border:1px solid gray;background-color:black;color:white;font-family:verdana;"><tr><td><font size=-1><i>"I don\'t think the human race will survive the next thousand years, unless we spread into space. There are too many accidents that can befall life on a single planet."</i><br><p align="right">Stephen Hawking</p></font></td></tr></table>', 'BLACK', 150, 25); } function service_label(){ ddrivetip('<table style="width:208px;border:1px solid gray;background-color:black;color:white;font-family:verdana;"><tr><td><img src="images/gift.jpg" border=0 style="float:left;position:relative;top:-1;left:0;"></td></tr></table>', 'BLACK', 150, 25); } function news_label(){ ddrivetip('<table style="width:300px;border:1px solid gray;background-color:black;color:white;font-family:verdana;font-size:8pt"><tr><td>The NEWS<font color=red>@</font>SKY (Space&Science) is a unique opportunity to browse hundreds of scientific and popular science Internet sites without a single mouse click!</td></tr></table>', 'BLACK', 150, 25); } function gift_label(){ ddrivetip('<table style="width:172px;border:1px solid gray;background-color:black;color:white;font-family:verdana;"><tr><td><img src="images/gift.jpg" border=0 style="float:left;position:relative;top:-1;left:0;"></td></tr></table>', 'BLACK', 100, 25); } function service_label15(){ ddrivetip('<table style="width:352px;border:1px solid gray;background-color:black;color:white;font-family:verdana;"><tr><td><font size=-2>NEWS@SKY is a unique system, which brings together a large number of the Internet based information portals.All presented on NEWS@SKY media are part of the NEWS@SKY community. Under certain circumstances, any Internet information portal can become a member of this community.</font><br><img src="images/astar.jpg" border=0 style="float:left;position:relative;top:-1;left:0;"></td></tr></table>', 'BLACK', 100, 25); } function service_label8(){ ddrivetip('<table style="width:208px;border:1px solid gray;background-color:black;color:white;font-family:verdana;"><tr><td><img src="images/simpson5.jpg" border=0 style="float:left;position:relative;top:-1;left:0;"></td></tr></table>', 'BLACK', 100, 25); } function updateLogo(logoId, subLogo){ currentLogo=logoId; var newLogo=topLogos[logoId]; if (subLogo) newLogo+=" <font style='font-size:16px'>("+subLogo+")</font>"; document.getElementById("d_top_logo").innerHTML=newLogo; } var menuPress=['<a href="http://sky-map.org/wiki/Press_Releases" target="_blank"><font color=white>Press Releases</font></a>', '<a href="http://sky-map.org/wiki/Publications" target="_blank"><font color=white><nobr>SKY-MAP in World Media</nobr></font></a>']; 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text-align: left; position: absolute; width: 400px; border: 0px solid #aaa; padding: 2px; visibility: hidden; z-index: 100;'></div> <DIV id="d_body"style="POSITION: absolute; LEFT: 10px; TOP: 70px; WIDTH:930px; border:0px solid white"> <h1 class='sTitle'>NGC 4173</h1> <table border=0 cellpadding=2 cellspacing=0 width=100%> <tr valign=top><td align=left style='border-right: 1px solid #aaa;'> <br><a name='Images'></a><b>Contents</b><ul> <li><a href='#Images'>Images</a></li> <li><a href='#Articles'>Related articles</a></li> <li><a href='#Links'>Related links</a></li> <li><a href='#Groups'>Groups</a></li> </ul> <br><a name='Images'></a><h3>Images</h3> <table> <tr> <td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:25px;width:150;height:100;cursor:pointer'>  <a title="Leo Constellation" href='./?img_source=IMG_92:all&ra=12.205778&de=29.2075&zoom=3&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="Leo Constellation" src='http://images.sky-map.org/star_img_thumb/000/000092.jpeg' border=0 width="150" height="100" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:-3px;top:-5px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:25px;top:0px;width:100;height:150;cursor:pointer'>  <a title="Canes Venatici, Coma Berenices Constellations by Till Credner and Sven Kohle" href='./?img_source=IMG_1320:all&ra=12.205778&de=29.2075&zoom=3&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="Canes Venatici, Coma Berenices Constellations by Till Credner and Sven Kohle" src='http://images.sky-map.org/star_img_thumb/001/001320.jpeg' border=0 width="100" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:80px;top:81px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:20px;width:150;height:109;cursor:pointer'>  <a title="SDSS3 frame. Run:4649, rerun:301, field:14, camcol:2" href='./?img_source=SDSS&img_id=1002559310:all&img_borders=1002559310&ra=12.205778&de=29.2075&zoom=10&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="SDSS3 frame. Run:4649, rerun:301, field:14, camcol:2" src='http://data.sdss3.org/sas/dr8/groups/boss/photoObj/frames/301/4649/2/frame-thumb-irg-004649-2-0014.jpg' border=0 width="150" height="109" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:20px;width:150;height:109;cursor:pointer'>  <a title="SDSS3 frame. Run:4649, rerun:301, field:15, camcol:2" href='./?img_source=SDSS&img_id=1002559316:all&img_borders=1002559316&ra=12.205778&de=29.2075&zoom=10&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="SDSS3 frame. Run:4649, rerun:301, field:15, camcol:2" src='http://data.sdss3.org/sas/dr8/groups/boss/photoObj/frames/301/4649/2/frame-thumb-irg-004649-2-0015.jpg' border=0 width="150" height="109" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'></a></div></td></tr><tr><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:20px;width:150;height:109;cursor:pointer'>  <a title="SDSS3 frame. Run:5061, rerun:301, field:438, camcol:2" href='./?img_source=SDSS&img_id=1002651098:all&img_borders=1002651098&ra=12.205778&de=29.2075&zoom=10&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="SDSS3 frame. Run:5061, rerun:301, field:438, camcol:2" src='http://data.sdss3.org/sas/dr8/groups/boss/photoObj/frames/301/5061/2/frame-thumb-irg-005061-2-0438.jpg' border=0 width="150" height="109" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:0px;width:150;height:150;cursor:pointer'>  <a title="GALEX frame GI3_041006_NGC4245-xd-int_2color. RA=12.2655, Dec=29.742778" href='./?img_source=GALEX&img_id=1010031606:all&img_borders=1010031606&ra=12.205778&de=29.2075&zoom=9&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="GALEX frame GI3_041006_NGC4245-xd-int_2color. RA=12.2655, Dec=29.742778" src='http://galex.stsci.edu/GR4/data/GR5/pipe/01-vsn/23005-GI3_041006_NGC4245/d/01-main/0005-img/06-try/qa/GI3_041006_NGC4245-xd-int_2color_thumb.jpg' border=0 width="150" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:129px;top:117px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:0px;width:150;height:150;cursor:pointer'>  <a title="GALEX frame GI4_008001_KISSR0001-xd-int_2color. RA=12.226638666666666, Dec=29.21" href='./?img_source=GALEX&img_id=1010031681:all&img_borders=1010031681&ra=12.205778&de=29.2075&zoom=9&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="GALEX frame GI4_008001_KISSR0001-xd-int_2color. RA=12.226638666666666, Dec=29.21" src='http://galex.stsci.edu/GR4/data/GR5/pipe/01-vsn/24004-GI4_008001_KISSR0001/d/01-main/0005-img/06-try/qa/GI4_008001_KISSR0001-xd-int_2color_thumb.jpg' border=0 width="150" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:93px;top:68px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:0px;width:150;height:150;cursor:pointer'>  <a title="GALEX frame AIS_112_sg68-xd-int_2color. RA=12.205480957031266, Dec=28.7513904571533" href='./?img_source=GALEX&img_id=1010009275:all&img_borders=1010009275&ra=12.205778&de=29.2075&zoom=9&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_112_sg68-xd-int_2color. RA=12.205480957031266, Dec=28.7513904571533" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50112-AIS_112/d/01-main/0001-img/06-try/qa/AIS_112_sg68-xd-int_2color_thumb.jpg' border=0 width="150" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:67px;top:25px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td></tr><tr><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:0px;width:150;height:150;cursor:pointer'>  <a title="GALEX frame AIS_112_sg61-xd-int_2color. RA=12.171122233072934, Dec=29.7284507751465" href='./?img_source=GALEX&img_id=1010009268:all&img_borders=1010009268&ra=12.205778&de=29.2075&zoom=9&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_112_sg61-xd-int_2color. RA=12.171122233072934, Dec=29.7284507751465" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50112-AIS_112/d/01-main/0001-img/06-try/qa/AIS_112_sg61-xd-int_2color_thumb.jpg' border=0 width="150" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:25px;top:116px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td><td valign=top style='width:150;height:150;background-color:#181820;'><div style='position:relative;left:0px;top:0px;width:150;height:150;cursor:pointer'>  <a title="GALEX frame AIS_112_sg67-xd-int_2color. RA=12.239607747395867, Dec=29.7047004699707" href='./?img_source=GALEX&img_id=1010009274:all&img_borders=1010009274&ra=12.205778&de=29.2075&zoom=9&show_box=1&box_ra=12.205778&box_de=29.2075&box_width=19&box_height=19&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_112_sg67-xd-int_2color. RA=12.239607747395867, Dec=29.7047004699707" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50112-AIS_112/d/01-main/0001-img/06-try/qa/AIS_112_sg67-xd-int_2color_thumb.jpg' border=0 width="150" height="150" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:109px;top:114px;width:14px;height:14px;border:1px solid #aaa;font-size:1px'></div></a></div></td> </tr> </table> <font size=-1><a href='user?page=images&ra=12.205778&de=29.2075&action=edit' rel='nofollow'>Upload your image</a></font> <br><br><a href='star_dss_image.jsp?ra=12.205778&de=29.2075&angle=.25' rel='nofollow'>DSS Images</a>   <a href='star_images.jsp'>Other Images</a> <br><br><br><a name='Articles'></a><h3>Related articles</h3> <table> <tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004AJ....127.3235S&link_type=ABSTRACT'><b>An IRAS High Resolution Image Restoration (HIRES) Atlas of All Interacting Galaxies in the IRAS Revised Bright Galaxy Sample</b></a><br><font size=-1><i>The importance of far-infrared observations for our understanding ofextreme activity in interacting and merging galaxies has beenillustrated by many studies. Even though two decades have passed sinceits launch, the most complete all-sky survey to date from which far-IRselected galaxy samples can be chosen is still that of the InfraredAstronomical Satellite (IRAS). However, the spatial resolution of theIRAS all-sky survey is insufficient to resolve the emission fromindividual galaxies in most interacting galaxy pairs, and hence previousstudies of their far-IR properties have had to concentrate either onglobal system properties or on the properties of very widely separatedand weakly interacting pairs. Using the HIRES image reconstructiontechnique, it is possible to achieve a spatial resolution ranging from30" to 1.5m (depending on wavelength and detector coverage), whichis a fourfold improvement over the normal resolution of IRAS. This issufficient to resolve the far-IR emission from the individual galaxiesin many interacting systems detected by IRAS, which is very importantfor meaningful comparisons with single, isolated galaxies. We presenthigh-resolution 12, 25, 60, and 100 μm images of 106 interactinggalaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS,Sanders et al.), a complete sample of all galaxies having a 60 μmflux density greater than 5.24 Jy. These systems were selected to haveat least two distinguishable galaxies separated by less than threeaverage galactic diameters, and thus we have excluded very widelyseparated systems and very advanced mergers. Additionally, some systemshave been included that are more than three galactic diameters apart,yet have separations less than 4' and are thus likely to suffer fromconfusion in the RBGS. The new complete survey has the same propertiesas the prototype survey of Surace et al. We find no increased tendencyfor infrared-bright galaxies to be associated with other infrared-brightgalaxies among the widely separated pairs studied here. We find smallenhancements in far-IR activity in multiple galaxy systems relative toRBGS noninteracting galaxies with the same blue luminosity distribution.We also find no differences in infrared activity (as measured byinfrared color and luminosity) between late- and early-type spiralgalaxies.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003ApJS..146..249B&link_type=ABSTRACT'><b>A Survey for H2O Megamasers. III. Monitoring Water Vapor Masers in Active Galaxies</b></a><br><font size=-1><i>We present single-dish monitoring of the spectra of 13 extragalacticwater megamasers taken over a period of 9 years and a single epoch ofsensitive spectra for seven others. The primary motivation is a searchfor drifting line velocities analogous to those of the systemic featuresin NGC 4258, which are known to result from centripetal acceleration ofgas in an edge-on, subparsec molecular disk. We detect a velocity driftanalogous to that in NGC 4258 in only one source, NGC 2639. Another, themaser source in NGC 1052, exhibits erratic changes in its broad maserprofile over time. Narrow maser features in all of the other diskgalaxies discussed here either remain essentially constant in velocityover the monitoring period or are sufficiently weak or variable inintensity that individual features cannot be traced reliably from oneepoch to the next. In the context of a circumnuclear, molecular diskmodel, our results suggest that either (a) the maser lines seen aresystemic features subject to a much smaller acceleration than present inNGC 4258, presumably because the gas is farther from the nuclear blackhole, or (b) we are detecting ``satellite'' lines for which theacceleration is in the plane of the sky.Our data include the first K-band science observations taken with thenew 100 m Green Bank Telescope (GBT). The GBT data were taken duringtesting and commissioning of several new components and so are subjectto some limitations; nevertheless, they are in most cases the mostsensitive H2O spectra ever taken for each source and cover800 MHz (~=10,800 km s-1) of bandwidth. Many new maserfeatures are detected in these observations. Our data also include atentative and a clear detection of the megamaser in NGC 6240 at epochs ayear and a few months, respectively, prior to the detections reported byHagiwara et al. and Nakai et al.We also report a search for water vapor masers toward the nuclei of 58highly inclined (i>80deg), nearby galaxies. These sourceswere selected to investigate the tendency that H2O megamasersfavor inclined galaxies. None were detected, confirming that megamasersare associated exclusively with active galactic nuclei.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003A%26A...408..465M&link_type=ABSTRACT'><b>A search for Low Surface Brightness galaxies in the near-infrared. III. Nançay H I line observations</b></a><br><font size=-1><i>A total of 334 Low Surface Brightness galaxies detected in the 2MASSall-sky near-infrared survey have been observed in the 21 cm H I lineusing the Nançay telescope. All have a Ks-band meancentral surface brightness, measured within a 5'' radius, fainter than18 mag arcsec-2 and a Ks-band isophotal radius atthe 20 mag arcsec-2 level larger than 20''. We present globalH I line parameters for the 171 clearly detected objects and the 23marginal detections, as well as upper limits for the undetected objects.The 171 clear detections comprise 50 previously uncatalogued objects and41 objects with a PGC entry only.Tables 3-5 are only available in electronic form at the CDS viaanonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/408/465Figures 1 and 2 are only available in electronic form athttp://www.edpsciences.org</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003A%26A...405...99M&link_type=ABSTRACT'><b>A search for Low Surface Brightness galaxies in the near-infrared. I. Selection of the sample</b></a><br><font size=-1><i>A sample of about 3800 Low Surface Brightness (LSB) galaxies wasselected using the all-sky near-infrared (J, H and Ks-band)2MASS survey. The selected objects have a mean central surfacebrightness within a 5'' radius around their centre fainter than 18 magarcsec-2 in the Ks band, making them the lowestsurface brightness galaxies detected by 2MASS. A description is given ofthe relevant properties of the 2MASS survey and the LSB galaxy selectionprocedure, as well as of basic photometric properties of the selectedobjects. The latter properties are compared to those of other samples ofgalaxies, of both LSBs and ``classical'' high surface brightness (HSB)objects, which were selected in the optical. The 2MASS LSBs have aBT_c-KT colour which is on average 0.9 mag bluerthan that of HSBs from the NGC. The 2MASS sample does not appear tocontain a significant population of red objects.All tables and Figs. 2a-c are only available in electronic form athttp://www.edpsciences.org</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003A%26A...405....5B&link_type=ABSTRACT'><b>A new catalogue of ISM content of normal galaxies</b></a><br><font size=-1><i>We have compiled a catalogue of the gas content for a sample of 1916galaxies, considered to be a fair representation of ``normality''. Thedefinition of a ``normal'' galaxy adopted in this work implies that wehave purposely excluded from the catalogue galaxies having distortedmorphology (such as interaction bridges, tails or lopsidedness) and/orany signature of peculiar kinematics (such as polar rings,counterrotating disks or other decoupled components). In contrast, wehave included systems hosting active galactic nuclei (AGN) in thecatalogue. This catalogue revises previous compendia on the ISM contentof galaxies published by \citet{bregman} and \citet{casoli}, andcompiles data available in the literature from several small samples ofgalaxies. Masses for warm dust, atomic and molecular gas, as well asX-ray luminosities have been converted to a uniform distance scale takenfrom the Catalogue of Principal Galaxies (PGC). We have used twodifferent normalization factors to explore the variation of the gascontent along the Hubble sequence: the blue luminosity (LB)and the square of linear diameter (D225). Ourcatalogue significantly improves the statistics of previous referencecatalogues and can be used in future studies to define a template ISMcontent for ``normal'' galaxies along the Hubble sequence. The cataloguecan be accessed on-line and is also available at the Centre desDonnées Stellaires (CDS).The catalogue is available in electronic form athttp://dipastro.pd.astro.it/galletta/ismcat and at the CDS via anonymousftp to\ cdsarc.u-strasbg.fr (130.79.128.5) or via\http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/405/5</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002A%26A...390..863S&link_type=ABSTRACT'><b>The Westerbork HI survey of spiral and irregular galaxies. II. R-band surface photometry of late-type dwarf galaxies</b></a><br><font size=-1><i>R-band surface photometry is presented for 171 late-type dwarf andirregular galaxies. For a subsample of 46 galaxies B-band photometry ispresented as well. We present surface brightness profiles as well asisophotal and photometric parameters including magnitudes, diameters andcentral surface brightnesses. Absolute photometry is accurate to 0.1 magor better for 77% of the sample. For over 85% of the galaxies the radialsurface brightness profiles are consistent with published data withinthe measured photometric uncertainty. For most of the galaxies in thesample H I data have been obtained with the Westerbork Synthesis RadioTelescope. The galaxies in our sample are part of the WHISP project(Westerbork H I Survey of Spiral and Irregular Galaxies), which aims atmapping about 500 nearby spiral and irregular galaxies in H I. Theavailability of H I data makes this data set useful for a wide range ofstudies of the structure, dark matter content and kinematics oflate-type dwarf galaxies. Based on observations made with INT operatedon the island of La Palma by the Isaac Newton Group in the SpanishObservatorio del Roque de los Muchachos of the Instituto de Astrofisicade Canarias. The tables in Appendix A are only available in electronicform at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/390/863. Thefigures in Appendix B are only available in electronic formhttp://www.edpsciences.org</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001AJ....122.2893W&link_type=ABSTRACT'><b>Redshifts for 2410 Galaxies in the Century Survey Region</b></a><br><font size=-1><i>The Century Survey strip covers 102 deg2 within the limits8h5<=α<=16h5, 29.0d<=δ<=30.0d, equinoxB1950.0. The strip passes through the Corona Borealis supercluster andthe outer region of the Coma cluster. Within the Century Survey region,we have measured 2410 redshifts that constitute four overlappingcomplete redshift surveys: (1) 1728 galaxies with Kron-CousinsRph<=16.13 covering the entire strip, (2) 507 galaxieswith Rph<=16.4 in right ascension range8h32m<=α<=10h45m, equinox B1950.0, (3) 1251 galaxies withabsorption- and K-corrected RCCDc<=16.2 (where ``c''indicates ``corrected'') covering the right ascension range8h5<=α<=13h5, equinox B1950.0, and (4) 1255 galaxieswith absorption- and K-corrected VCCDc<=16.7 also coveringthe right ascension range 8h5<=α<=13h5, equinoxB1950.0. All these redshift samples are more than 98% complete to thespecified magnitude limit. We derived samples 1 and 2 from scans of thePOSS1 red (E) plates calibrated with CCD photometry. We derived samples3 and 4 from deep V and R CCD images covering the entire region. Weinclude coarse morphological types for all the galaxies in sample 1. Thedistribution of (V-R)CCD for each type correspondsappropriately with the classification. Work reported here is basedpartly on observations obtained at the Michigan-Dartmouth-MITObservatory.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001AJ....122..714B&link_type=ABSTRACT'><b>V- and R-band Galaxy Luminosity Functions and Low Surface Brightness Galaxies in the Century Survey</b></a><br><font size=-1><i>We use 64 deg2 of deep V and R CCD images to measure thelocal V- and R-band luminosity functions of galaxies. TheV0<16.7 and R0<16.2 redshift samples contain1255 and 1251 galaxies and are 98.1% and 98.2% complete, respectively.We apply k-corrections before the magnitude selection so that thecompleteness is to the same depth for all spectral types. The V and Rfaint-end slopes are surprisingly identical: α=-1.07+/-0.09.Representative Schechter function parameters for H0=100 are:M*R=-20.88+/-0.09,φ*R=0.016+/-0.003 Mpc-3 andM*V=-20.23+/-0.09,φ*V=0.020+/-0.003 Mpc-3. The V andR local luminosity densities,jR=(1.9+/-0.6)×108 Lsolar andjV=(2.2+/-0.7)×108 Lsolar, are inessential agreement with the recent 2 Degree Field Galaxy RedshiftSurvey and Sloan Digital Sky Survey determinations. All low surfacebrightness (LSB) galaxies fall in the large-scale structure delineatedby high surface brightness galaxies. The properties and surface numberdensity of our LSB galaxies are consistent with the LSB galaxy catalogof O'Neil, Bothun & Cornell, suggesting that our samples arecomplete for LSB galaxies to the magnitude limits. We measure colors,surface brightnesses, and luminosities for our samples, and find strongcorrelations among these galaxy properties. The color-surface brightnessrelation is(V-R)0=(-0.11+/-0.05)μR,0+(2.6+/-0.9).</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000BSAO...50....5K&link_type=ABSTRACT'><b>A list of peculiar velocities of RFGC galaxies</b></a><br><font size=-1><i>A list of radial velocities, HI line widths and peculiar velocities of1327 galaxies from the RFGC catalogue has been compiled using actualobservations and literature data. The list can be used for studying bulkmotions of galaxies, construction of the field of peculiar velocitiesand other tasks.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000ApJ...543..178G&link_type=ABSTRACT'><b>Nearby Optical Galaxies: Selection of the Sample and Identification of Groups</b></a><br><font size=-1><i>In this paper we describe the Nearby Optical Galaxy (NOG) sample, whichis a complete, distance-limited (cz<=6000 km s-1) andmagnitude-limited (B<=14) sample of ~7000 optical galaxies. Thesample covers 2/3 (8.27 sr) of the sky (|b|>20deg) andappears to have a good completeness in redshift (97%). We select thesample on the basis of homogenized corrected total blue magnitudes inorder to minimize systematic effects in galaxy sampling. We identify thegroups in this sample by means of both the hierarchical and thepercolation ``friends-of-friends'' methods. The resulting catalogs ofloose groups appear to be similar and are among the largest catalogs ofgroups currently available. Most of the NOG galaxies (~60%) are found tobe members of galaxy pairs (~580 pairs for a total of ~15% of objects)or groups with at least three members (~500 groups for a total of ~45%of objects). About 40% of galaxies are left ungrouped (field galaxies).We illustrate the main features of the NOG galaxy distribution. Comparedto previous optical and IRAS galaxy samples, the NOG provides a densersampling of the galaxy distribution in the nearby universe. Given itslarge sky coverage, the identification of groups, and its high-densitysampling, the NOG is suited to the analysis of the galaxy density fieldof the nearby universe, especially on small scales.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000A%26AS..145..405L&link_type=ABSTRACT'><b>Box- and peanut-shaped bulges. I. Statistics</b></a><br><font size=-1><i>We present a classification for bulges of a complete sample of ~ 1350edge-on disk galaxies derived from the RC3 (Third Reference Catalogue ofBright Galaxies, de Vaucouleurs et al. \cite{rc3}). A visualclassification of the bulges using the Digitized Sky Survey (DSS) inthree types of b/p bulges or as an elliptical type is presented andsupported by CCD images. NIR observations reveal that dust extinctiondoes almost not influence the shape of bulges. There is no substantialdifference between the shape of bulges in the optical and in the NIR.Our analysis reveals that 45% of all bulges are box- and peanut-shaped(b/p). The frequency of b/p bulges for all morphological types from S0to Sd is > 40%. In particular, this is for the first time that such alarge frequency of b/p bulges is reported for galaxies as late as Sd.The fraction of the observed b/p bulges is large enough to explain theb/p bulges by bars. Partly based on observations collected at ESO/LaSilla (Chile), DSAZ/Calar Alto (Spain), and Lowell Observatory/Flagstaff(AZ/U.S.A.). Tables 6 and 7 are only available in electronic form at CDSvia anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or viahttp://cdsweb.u-strasbg.fr/Abstract.html</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000A%26AS..141..385V&link_type=ABSTRACT'><b>A neutral hydrogen survey of polar ring galaxies. III. Nançay observations and comparison with published data</b></a><br><font size=-1><i>A total of 50 optically selected polar ring galaxies, polar ring galaxycandidates and related objects were observed in the 21-cm H i line withthe Nançay decimetric radio telescope and 31 were detected. Theobjects, selected by their optical morphology, are all north ofdeclination -39o, and generally relatively nearby (V< 8000km s-1) and/or bright (mB< 15.5). The H i linedata are presented for all 74 galaxies observed for the survey with theEffelsberg, Green Bank or Nanç radio telescopes, as well as allother published H i line parameters of these objects. Three objects wereobserved and detected by us at Parkes. A total of 59 objects weredetected. For each object a brief description is given based on aliterature search.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999BSAO...47....5K&link_type=ABSTRACT'><b>The Revised Flat Galaxy Catalogue.</b></a><br><font size=-1><i>We present a new improved and completed version of the Flat GalaxyCatalogue (FGC) named the Revised Flat Galaxy Catalogue (RFGC)containing 4236 thin edge-on spiral galaxies and covering the whole sky.The Catalogue is intended to study large-scale cosmic streamings as wellas other problems of observational cosmology. The dipole moment ofdistribution of the RFGC galaxies (l = 273 degr; b =+19 degr) lieswithin statistical errors (+/-10 degr) in the direction of the LocalGroup motion towards the Microwave Background Radiation (MBR).</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999ApJS..125..409C&link_type=ABSTRACT'><b>Arcsecond Positions of UGC Galaxies</b></a><br><font size=-1><i>We present accurate B1950 and J2000 positions for all confirmed galaxiesin the Uppsala General Catalog (UGC). The positions were measuredvisually from Digitized Sky Survey images with rms uncertaintiesσ<=[(1.2")2+(θ/100)2]1/2,where θ is the major-axis diameter. We compared each galaxymeasured with the original UGC description to ensure high reliability.The full position list is available in the electronic version only.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999A%26AS..135..255K&link_type=ABSTRACT'><b>Nançay ``blind'' 21 CM line survey of the Canes Venatici group region</b></a><br><font size=-1><i>A radio spectroscopic driftscan survey in the 21 cm line with theNançay decimetric radio telescope of 0.08 steradians of sky inthe direction of the constellation Canes Venatici covering aheliocentric velocity range of -350 < V_hel < 2350 km s(-1)produced 53 spectral features, which was further reduced to a sample of33 reliably detected galaxies by extensive follow-up observations. Witha typical noise level of rms = 10 mJy after Hanning smoothing, thesurvey is - depending on where the detections are located with regard tothe centre of the beam - sensitive to M_HI = 1-2x10(8) {h}(-2) {M_sun}at 23 {h}(-1) Mpc and to M_HI = 4-8x10(7) {h}(-2) {M_sun} throughout theCVn groups. The survey region had been previously examined on deepoptical plates by \cite[Binggeli et al. (1990)]{bin90} and containsloose groups with many gas-rich galaxies as well as voids. No galaxiesthat had not been previously identified in these deep optical surveyswere uncovered in our H{sigma c i} survey, neither in the groups nor thevoids. The implication is that no substantial quantity of neutralhydrogen contained in gas-rich galaxies has been missed in thesewell-studied groups. All late-type members of our sample are listed inthe \cite[Fisher & Tully (1981b)]{fis81b} optically selected sampleof nearby late-type galaxies; the only system not contained in Fisherand Tully's Catalog is the S0 galaxy NGC 4203. Within the well-sampledCVn group volume with distances corrected for flow motions, the H {sigmac i} mass function is best fitted with the \cite[Zwaan et al.(1997)]{zwa97} H{sigma c i} mass function (alpha =-1.2) scaled by afactor of f=4.5 in account of the locally overdense region.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998ApJS..117....1V&link_type=ABSTRACT'><b>Atlas of H alpha Emission of a Sample of Nearby Hickson Compact Groups of Galaxies</b></a><br><font size=-1><i>H alpha and adjacent continuum images are presented for a sample ofnearby groups of galaxies extracted from the Atlas of Compact Groups ofGalaxies. Also, more detailed H alpha maps of the most remarkablegalaxies are shown in this paper. A short description of the H alphaemission for each of the galaxies with accordant redshift is presentedtogether with a morphological classification of the accordant galaxiesin the sample. A large fraction of ellipticals and lenticulars weredetected in H alpha . Also, clear signs of interactions were found inseven of the groups, but in only in three of them was H alpha emissiondetected along the tidal features. Candidates of dwarf galaxies werefound at the tips of the tidal tails developed during the interactionsin these three groups.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ApJ...466..795H&link_type=ABSTRACT'><b>The Absence of X-Ray Flashes from Nearby Galaxies and the Gamma-Ray Burst Distance Scale</b></a><br><font size=-1><i>If typical gamma-ray bursts (GRBs) have X-ray counterparts similar tothose detected by Ginga, then sensitive-focusing X-ray telescopes willbe able to detect GRBs 3 orders of magnitude fainter than the detectionlimit of the Burst and Transient Source Experiment (BATSE). If asubstantial portion of the burst population detected by BATSE originatesin a Galactic halo at distances greater than or equal to 150 kpc,existing X-ray telescopes will be able to detect GRBs in externalgalaxies out to a distance of at least 4.5 Mpc. As reported in Gotthelf,Hamilton, & Helfand, the imaging proportional counter (IPC) on boardthe Einstein Observatory detected 42 transient events with pointlikespatial characteristics and timescales of less than 10 s. These eventsare distributed isotropically on the sky; in particular, they are notconcentrated in the directions of nearby external galaxies. For halomodels of the BATSE bursts with radii of 150 kpc or greater, we wouldexpect to see several burst events in observations pointed toward nearbygalaxies. We see none. We therefore conclude that if the Gingadetections are representative of the population of GRBs sampled byBATSE, GRBs cannot originate in a Galactic halo population with limitingradii between 150 and 400 kpc. Inasmuch as halos with limiting radiioutside of this range have been excluded by the BATSE isotropymeasurements, our result indicates that all halo models are excluded.This result is independent of whether the flashes we do detect have anastronomical origin.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996A%26AS..117...39A&link_type=ABSTRACT'><b>Far infrared properties of Hickson compact groups of galaxies. I. High resolution IRAS maps and fluxes.</b></a><br><font size=-1><i>The Far Infrared (FIR) properties of galaxies which are members ofcompact groups bear relevant information on the dynamical status and thephysical properties of these structures. All studies published so farhave been undermined by the poor sensitivity and spatial resolution ofthe IRAS-PSC and IRAS Sky Survey data. We used the HIRAS softwareavailable at the IRAS server at the Laboratory for Space Research inGroningen to fully exploit the redundancy of the IRAS data and toapproach the theoretical diffraction limit of IRAS. Among the 97 groupswhich were observed by IRAS, 62 were detected in at least one band,while reliable upper limits were derived for all the others. Among thedetected groups, 49 were fully or partially resolved, i.e. it waspossible to discriminate which member or members emit most of the FIRlight. At 60μm, for instance, 87 individual sources were detected in62 groups. In order to ease the comparison with data obtained at otherwavelengths - and in particular in the X and radio domains - we giveco-added and HIRAS maps for all the detected groups.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995MNRAS.273..139M&link_type=ABSTRACT'><b>The nature of discordant redshift galaxies in compact groups</b></a><br><font size=-1><i>We have analysed the sample of 92 compact groups in Hickson's revisedcatalogue to investigate whether the numbers and properties of thediscordant redshift galaxies in these groups are consistent with theprojection hypothesis. The main conclusion of our analysis is that thenumbers, sizes, magnitudes and morphological types of the discordantredshift galaxies in the Hickson compact groups are as expected if theseare due to chance projections of unrelated galaxies on the groups. Thedistribution of positions for the discordant galaxies in quintets,however, is more centrally concentrated than that predicted for auniform distribution of field interlopers. One of the possibleexplanations for this discrepancy is that compact groups can act asgravitational lenses, causing the brightening of background galaxiesthat would otherwise fall below the magnitude cut-off of the group.Distances to two galaxies in the Hickson compact group 61, one of them adiscordant redshift galaxy, have been determined using the Tully-Fisherrelation. Both objects were found to be at distances consistent withtheir redshifts and an expanding Universe. All these results support theview of a cosmological origin for galaxy redshifts.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995AZh....72..811K&link_type=ABSTRACT'><b>Statistical correlations between basic parameters of disk galaxies</b></a><br><font size=-1><i>Statistical relationships between principal galaxy parameters andsurface densities of these parameters are analyzed for a sample of 63disk galaxies. These parameters include the radius, the mass of theentire galaxy and its various components (H2, HI, total gas, dust,etc.), and blue and FIR luminosity. Of all possible two- andthree-parameter linear relations between the galaxy parameterlogarithms, we choose those that have high correlation coefficients andproceed to derive their coefficients. Some of these relations arecompared with the corresponding predictions of the single-zone model ofthe disk galaxy evolution. Other relations are considered from theviewpoint of interstellar medium properties in galaxies. We find thetheory to agree satisfactorily with observations and suggest ways ofimproving evolutionary models. The method of linear orthogonalregression used in the statistical analysis is described.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994A%26A...290...49G&link_type=ABSTRACT'><b>Galaxies with a low gas content in the Coma I cloud of galaxies.</b></a><br><font size=-1><i>We have observed the CO emission of six galaxies belonging to a smalldense group: NGC 4245, NGC 4251, NGC 4274, the elliptical NGC 4278, NGC4286 and NGC 4310. CO(1-0) and (2-1) lines have been detected and mappedin three galaxies. We present a comparison of the amount of molecularand atomic hydrogen in these galaxies with the expected amounts drawnfrom samples found in the literature. It is clear that most of the groupgalaxies have lower than average total gas masses, due to a largedeficiency of atomic hydrogen. Despite the large dispersion present inthe CO emission of galaxies, their content of molecular gas lies in theexpected range given their rather early types. This study shows thatgalaxies strongly deficient in HI do not exclusively belong to clusters,but can be found also in dense galaxy groups. The CO emission of thegalaxies, hence presumably their H_2_ content, is however not affectedby the environment; this conclusion holds for the group galaxies as wellas for the spirals previously studied in the Virgo and Coma clusters.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994A%26A...288..705G&link_type=ABSTRACT'><b>H I deficiency in the Coma I cloud of galaxies</b></a><br><font size=-1><i>We present new H I observations of galaxies in the Coma I group. Of the32 most probable members of the group, 16 are gas poor and 16 havenormal H I contents. The 16 gas poor galaxies include 4 ellipticals, 5S0s, and 7 spirals with a definite H I deficiency (more than a factor offour). Most of the 16 gas poor or H I deficient galaxies areconcentrated within a radius of 500 kpc of a centroid near the galaxyNGC 4274, suggesting that this region contains a compact core ofintergalactic matter that has stripped the gas from some of thegalaxies. Seven gas poor galaxies are even within a projected radius of130 kpc of this position. This possible existence of a dense core ofintragroup gas may explain the large H I deficiency in the barred spiralNGC 4314. which has 100 times less H I mass than would be expected fromits luminosity and stellar mass. In this galaxy the gas is 99%molecular, 1% atomic and nearly all in the central region. We suspectthe extreme H I deficiency in NGC 4314 is due to two distinct causes:ram pressure stripping of the gas in its outer parts, plus action of itsbar or an ancient tidal interaction with another galaxy that transferredgas from the inner parts of NGC 4314 to the center where H I wasconverted to H_2_.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ApJS...85....1N&link_type=ABSTRACT'><b>A revised catalog of CfA1 galaxy groups in the Virgo/Great Attractor flow field</b></a><br><font size=-1><i>A new identification of groups and clusters in the CfA1 Catalog ofHuchra et al. is presented, using a percolation algorithm to identifydensity enhancements. It is shown that in the resulting catalog,contamination by interlopers is significantly reduced. The Schechterluminosity function is redetermined, including the Malmquist bias.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993Ap%26SS.209..181A&link_type=ABSTRACT'><b>On actual presence of discordant-redshift galaxies in compact groups</b></a><br><font size=-1><i>Hickson's compact galaxy groups were classified using the statisticalcriterion which includes the radial velocities of galaxies as well astheir relative positions. These groups on the whole and their componentsare identified as the confident and probable non-chance ones as well asprobable and confident chance ones. All confident chance objects havethe discordant radial velocities with the differences of radialvelocities (DV) Epsilon between 1,000 km/s and 20,000 km/s. The specialclass of objects 'bright discordants' is selected. These galaxies havethe discordant radial velocities with DV Epsilon between 825 km/s and8440 km/s and have a strong tendency to be the brightest components oftheir groups. The lowest difference of radial velocities for the lastclass of objects mean value of DV = (1.0 +/- 0.2) x 103 km/sand we accept this value of DV as the lowest value of discordant radialvelocities. It is found that the biggest part of Hickson's compactgroups consist of non-chance aggregations of galaxies and some of thecases of discordant-redshifts require a special study in order toexplain their origin from a dynamic or some other point of view.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993AN....314...97K&link_type=ABSTRACT'><b>Flat galaxy catalogue</b></a><br><font size=-1><i>A systematic search for disklike edge-on-galaxies with a diameter largerthan a = 40 arcsec and a major-to-minor axis ratio a/b greater than 7was carried out by means of the Palomar Observatory Sky Survey and theESO/SERC survey. As a result, we present a new catalog of flat galaxies(FGC) containing 4455 objects and covering about 56 percent of the wholesky for the first time. The catalogue is assigned to study large-scalecosmic streamings and other problems of observational cosmology.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993A%26AS..100..537S&link_type=ABSTRACT'><b>Molecular gas in nearby galaxies. II - The data</b></a><br><font size=-1><i>The study reports observations of (C-12)O J = 1-0 emission from 50nearby spiral galaxies. This is part of a distance-limited survey ofnearby systems which are not strongly interacting with their neighbors.The observations were performed during December 1988 and March 1990using the NRAO 12-m telescope at Kitt Peak with the 3-mm SIS receiversand the 256-channel x 2-MHz spectrometers.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993A%26AS..100...47G&link_type=ABSTRACT'><b>General study of group membership. II - Determination of nearby groups</b></a><br><font size=-1><i>We present a whole sky catalog of nearby groups of galaxies taken fromthe Lyon-Meudon Extragalactic Database. From the 78,000 objects in thedatabase, we extracted a sample of 6392 galaxies, complete up to thelimiting apparent magnitude B0 = 14.0. Moreover, in order to considersolely the galaxies of the local universe, all the selected galaxieshave a known recession velocity smaller than 5500 km/s. Two methods wereused in group construction: a Huchra-Geller (1982) derived percolationmethod and a Tully (1980) derived hierarchical method. Each method gaveus one catalog. These were then compared and synthesized to obtain asingle catalog containing the most reliable groups. There are 485 groupsof a least three members in the final catalog.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993A%26A...272..123S&link_type=ABSTRACT'><b>Molecular Gas in Nearby Galaxies - Part One - Co/ Observations of a Distance-Limited Sample</b></a><br><font size=-1><i>This paper presents a discussion of ^12^CO J = 1 - 0 observations of adistance-limited sample of nearby spiral galaxies. The sample is biasedtowards high inclination galaxies at the lowest blue luminosities,suggesting a systematic effect. Two possible explanations are brieflydiscussed. The bias may be an artifact of the way Hubble types areassigned to galaxies or axis ratios measured, or it may indicate ameasurable effect of the local supercluster on lower mass galaxies. Themolecular mass is a relatively constant fraction (~2%) of the dynamicalmass within the region containing H_2_, but varies when the totaldynamical mass is considered (assuming a constant CO to H_2_ conversionfactor for all galaxies in the sample). The ratio of M(H_2_)/M_dyn_ isindependent of Hubble type. M(H_2_)/M(HI) is a strong function of Hubbletype, but this arises entirely because of the dependence of atomic masson type. The molecular masses and FIR luminosities are well correlated,but the average ratio of L_FIR_ to M(H_2_) is only ~1/2 that of previousstudies, which were based on (primarily) FIR selected samples. Thissuggests that the efficiency of star formation in a normal spiral galaxyis lower than that estimated by previous studies.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ApJS...79..197I&link_type=ABSTRACT'><b>Far-infrared luminosity functions of normal galaxies</b></a><br><font size=-1><i>A volume-limited sample is constructed from the Zwicky catalog and IRASdata base to examine the FIR luminosity functions of normal galaxies,and to investigate possible relationships between FIR emission andgalaxy morphology. Quantitative and unbiased treatment is provided by'survival analysis' statistical methods. It is found that the FIRdistributions of normal galaxies are better fit by lognormal thanSchechter functions. The total FIR emissivity (8 to 115 microns) ofnormal galaxies is approximately equal to half their emission in the Bplus V optical bands. Normal galaxy FIR emission is uncorrelated withthe basic S0-Sm Hubble sequence of spiral galaxy morphology, but appearsto be affected by de Vaucouleurs' (1959) revised morphologicalclassifications based on inner rings and S-shaped arms. Spirals withbars and inner rings are systematically fainter than unbarred spirals.It is suggested that bars and rings reduce the amount or spatiallyconfine the dust in spiral disks, resulting in lower efficiencyconversion of optical and UV photons into the IR.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992ApJ...399..353H&link_type=ABSTRACT'><b>Dynamical properties of compact groups of galaxies</b></a><br><font size=-1><i>Radial velocities are presented for 457 galaxies in the 100 Hicksoncompact groups. More than 84 percent of the galaxies measured havevelocities within 1000 km/s of the median velocity in the group.Ninety-two groups have at least three accordant members, and 69 groupshave at least four. The radial velocities of these groups range from1380 to 42,731 km/s with a median of 8889 km/s, corresponding to amedian distance of 89/h Mpc. The apparent space density of these systemsranges from 300 to as much as 10 exp 8 sq h/sq Mpc, which exceeds thedensities in the centers of rich clusters. The median projectedseparation between galaxies is 39/h kpc, comparable to the sizes of thegalaxies themselves. A significant correlation is found between crossingtime and the fraction of gas-rich galaxies in the groups, and a weakanticorrelation is found between crossing time and the luminositycontrast of the first-ranked galaxy.</i></font><br><br></td></tr> </table> <font size=-1><a href='article?action=new&obj1=2-370&lang=EN' rel='nofollow'>Submit a new article</a></font> <br><br><br><a name='Links'></a><h3>Related links</h3> <ul> <li>- No Links Found -</li> </ul> <font size=-1><a href='link.jsp?object_type=2&object_id=370&lang_id=EN&action=new' rel='nofollow'>Submit a new link</a></font> <br><br><br><a name='Groups'></a><h3>Member of following groups:</h3> <ul> <li><a href='group?id=17'>New General Catalogue (NGC)</a></li> <li><a href='groups'><font size=-1 style='white-space:nowrap'>[See all groups]</font></a></li> </ul> </td><td width=260 align=left> <div style='margin:0; border:1px solid #aaa; width:300px; height:300px;'> <script type="text/javascript" charset="UTF-8" src="skywindow.js?width=300&height=300&ra=12.2057777778&de=29.207499999999996&zoom=8&img_source=SDSS&img_id=all&locale=EN"></script> </div>  <br> <h4>Observation and Astrometry data</h4> <table> <tr><td nowrap>Constellation:</td><td><a href='?object_type=5&object_id=24&locale=EN'>Coma Berenices</a></td></tr> <tr><td nowrap>Right ascension:</td><td><a href='/?ra=12.2057777778&de=29.207499999999996&zoom=10&locale=EN' rel='nofollow'>12<sup>h</sup>12<sup>m</sup>20.80<sup>s</sup></a></td></tr> <tr><td nowrap>Declination:</td><td><a href='/?ra=12.2057777778&de=29.207499999999996&zoom=10&locale=EN' rel='nofollow'>+29Â°12'27.0"</a></td></tr> <tr><td nowrap>Aparent dimensions:</td><td>4.467′ × 0.891′</td></tr> </table> <br> Catalogs and designations: <hr width=100%> <table id="d_cat" style="font-size:11pt; width:100%"> <tr valign=top><td>Proper Names</td><td><b></b><small><i>   (<a href='names.jsp?object_type=2&object_id=370&lang_id=EN&action=list' rel='nofollow'>Edit</a>)</i></small> </td></tr><tr title='NGC 2000.0 (Sky Publishing, ed. Sinnott 1988)'><td nowrap><a href='http://vizier.u-strasbg.fr/viz-bin/VizieR-2?-source=VII/118'>NGC 2000.0</a></td><td nowrap><a href='http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=VII/118/ngc2000&Name=4173'>NGC 4173</a></td></tr> <tr title='HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)'><td nowrap><a href='http://vizier.u-strasbg.fr/viz-bin/VizieR-2?-source=VII/237'>HYPERLEDA-I</a></td><td nowrap><a href='http://vizier.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=VII/237&PGC=38897'>PGC 38897</a></td></tr> <tr><td colspan="2"><hr width=100%></td></tr> <tr id='d_load_cat'><td colspan="2"><a href='#' onclick='loadCatalogs(2,370);return false;' rel='nofollow'>→ Request more catalogs and designations from VizieR</a></td></tr> </table> <br> </td></tr> </table> <script type="text/javascript" charset="UTF-8"> </script> </div>  <script async src="https://www.googletagmanager.com/gtag/js?id=G-3PRTQ3JHKT"></script> <script> window.dataLayer = window.dataLayer || []; function gtag(){dataLayer.push(arguments);} gtag('js', new Date()); gtag('config', 'G-3PRTQ3JHKT'); </script> </body> </html>