NGC 1114 - Galaxy

<!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 1114 - 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" }; 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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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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. 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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 1114</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="Eridanus Constellation" href='./?img_source=IMG_448:all&ra=2.818694&de=-16.99278&zoom=3&show_box=1&box_ra=2.818694&box_de=-16.99278&box_width=8&box_height=8&box_var_size=1' rel='nofollow'> <img title="Eridanus Constellation" src='http://images.sky-map.org/star_img_thumb/000/000448.jpeg' border=0 width="150" height="100" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:129px;top:60px;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:5069, rerun:301, field:143, camcol:2" href='./?img_source=SDSS&img_id=1002655100:all&img_borders=1002655100&ra=2.818694&de=-16.99278&zoom=10&show_box=1&box_ra=2.818694&box_de=-16.99278&box_width=8&box_height=8&box_var_size=1' rel='nofollow'> <img title="SDSS3 frame. Run:5069, rerun:301, field:143, camcol:2" src='http://data.sdss3.org/sas/dr8/groups/boss/photoObj/frames/301/5069/2/frame-thumb-irg-005069-2-0143.jpg' border=0 width="150" height="109" style='position:absolute;left:0px;top:0px;border:0px solid #aaa;'><div style='position:absolute;left:9px;top:32px;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_278_sg96-xd-int_2color. RA=2.8399620056152335, Dec=-17.7353000640869" href='./?img_source=GALEX&img_id=1010020288:all&img_borders=1010020288&ra=2.818694&de=-16.99278&zoom=9&show_box=1&box_ra=2.818694&box_de=-16.99278&box_width=8&box_height=8&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_278_sg96-xd-int_2color. RA=2.8399620056152335, Dec=-17.7353000640869" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50278-AIS_278/d/01-main/0001-img/06-try/qa/AIS_278_sg96-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:96px;top:-2px;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_283_sg79-xd-int_2color. RA=2.8313219706217465, Dec=-16.2405109405518" href='./?img_source=GALEX&img_id=1010020690:all&img_borders=1010020690&ra=2.818694&de=-16.99278&zoom=9&show_box=1&box_ra=2.818694&box_de=-16.99278&box_width=8&box_height=8&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_283_sg79-xd-int_2color. RA=2.8313219706217465, Dec=-16.2405109405518" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50283-AIS_283/d/01-main/0001-img/06-try/qa/AIS_283_sg79-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:84px;top:129px;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_278_sg49-xd-int_2color. RA=2.79544474283854, Dec=-17.0268592834473" href='./?img_source=GALEX&img_id=1010020246:all&img_borders=1010020246&ra=2.818694&de=-16.99278&zoom=9&show_box=1&box_ra=2.818694&box_de=-16.99278&box_width=8&box_height=8&box_var_size=1' rel='nofollow'> <img title="GALEX frame AIS_278_sg49-xd-int_2color. RA=2.79544474283854, Dec=-17.0268592834473" src='http://galex.stsci.edu/GR4/data/GR4/pipe/02-vsn/50278-AIS_278/d/01-main/0001-img/06-try/qa/AIS_278_sg49-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:36px;top:64px;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=2.818694&de=-16.99278&action=edit' rel='nofollow'>Upload your image</a></font> <br><br><a href='star_dss_image.jsp?ra=2.818694&de=-16.99278&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=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=1999MNRAS.308..897L&link_type=ABSTRACT'><b>The QDOT all-sky IRAS galaxy redshift survey</b></a><br><font size=-1><i>We describe the construction of the QDOT survey, which is publiclyavailable from an anonymous FTP account. The catalogue consists ofinfrared properties and redshifts of an all-sky sample of 2387 IRASgalaxies brighter than the IRAS PSC 60-μm completeness limit(S_60>0.6Jy), sparsely sampled at a rate of one-in-six. At |b|>10deg, after removing a small number of Galactic sources, the redshiftcompleteness is better than 98per cent (2086/2127). New redshifts for1401 IRAS sources were obtained to complete the catalogue; themeasurement and reduction of these are described, and the new redshiftstabulated here. We also tabulate all sources at |b|>10 deg with noredshift so far, and sources with conflicting alternative redshiftseither from our own work, or from published velocities. A list of 95ultraluminous galaxies (i.e. with L_60μm>10^12 L_solar) is alsoprovided. Of these, ~20per cent are AGN of some kind; the broad-lineobjects typically show strong Feii emission. Since the publication ofthe first QDOT papers, there have been several hundred velocity changes:some velocities are new, some QDOT velocities have been replaced by moreaccurate values, and some errors have been corrected. We also present anew analysis of the accuracy and linearity of IRAS 60-μm fluxes. Wefind that the flux uncertainties are well described by a combination of0.05-Jy fixed size uncertainty and 8per cent fractional uncertainty.This is not enough to cause the large Malmquist-type errors in the rateof evolution postulated by Fisher et al. We do, however, find marginalevidence for non-linearity in the PSC 60-μm flux scale, in the sensethat faint sources may have fluxes overestimated by about 5per centcompared with bright sources. We update some of the previous scientificanalyses to assess the changes. The main new results are as follows. (1)The luminosity function is very well determined overall but is uncertainby a factor of several at the very highest luminosities(L_60μm>5x10^12L_solar), as this is where the remainingunidentified objects are almost certainly concentrated. (2) Thebest-fitting rate of evolution is somewhat lower than our previousestimate; expressed as pure density evolution with density varying as(1+z)^p, we find p=5.6+/-2.3. Making a rough correction for the possible(but very uncertain) non-linearity of fluxes, we find p=4.5+/-2.3. (3)The dipole amplitude decreases a little, and the implied value of thedensity parameter, assuming that IRAS galaxies trace the mass, isΩ=0.9(+0.45, -0.25). (4) Finally, the estimate of density varianceon large scales changes negligibly, still indicating a significantdiscrepancy from the predictions of simple cold dark matter cosmogonies.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999AJ....117.2039H&link_type=ABSTRACT'><b>The I-Band Tully-Fisher Relation for SC Galaxies: 21 Centimeter H I Line Data</b></a><br><font size=-1><i>A compilation of 21 cm line spectral parameters specifically designedfor application of the Tully-Fisher (TF) distance method is presentedfor 1201 spiral galaxies, primarily field Sc galaxies, for which opticalI-band photometric imaging is also available. New H I line spectra havebeen obtained for 881 galaxies. For an additional 320 galaxies, spectraavailable in a digital archive have been reexamined to allow applicationof a single algorithm for the derivation of the TF velocity widthparameter. A velocity width algorithm is used that provides a robustmeasurement of rotational velocity and permits an estimate of the erroron that width taking into account the effects of instrumental broadeningand signal-to-noise. The digital data are used to establish regressionrelations between measurements of velocity widths using other commonprescriptions so that comparable widths can be derived throughconversion of values published in the literature. The uniform H I linewidths presented here provide the rotational velocity measurement to beused in deriving peculiar velocities via the TF method.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999AJ....117.1668H&link_type=ABSTRACT'><b>The I-Band Tully-Fisher Relation for SC Galaxies: Optical Imaging Data</b></a><br><font size=-1><i>Properties derived from the analysis of photometric I-band imagingobservations are presented for 1727 inclined spiral galaxies, mostly oftypes Sbc and Sc. The reduction, parameter extraction, and errorestimation procedures are discussed in detail. The asymptotic behaviorof the magnitude curve of growth and the radial variation in ellipticityand position angle are used in combination with the linearity of thesurface brightness falloff to fit the disk portion of the profile. TotalI-band magnitudes are calculated by extrapolating the detected surfacebrightness profile to a radius of eight disk scale lengths. Errors inthe magnitudes, typically ~0.04 mag, are dominated by uncertainties inthe sky subtraction and disk-fitting procedures. Comparison is made withthe similar imaging database of Mathewson, Ford, & Buchhorn, both aspresented originally by those authors and after reanalyzing theirdigital reduction files using identical disk-fitting procedures. Directcomparison is made of profile details for 292 galaxies observed incommon. Although some differences occur, good agreement is found,proving that the two data sets can be used in combination with onlyminor accommodation of those differences. The compilation of opticalproperties presented here is optimized for use in applications of theTully-Fisher relation as a secondary distance indicator in studies ofthe local peculiar velocity field.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998AJ....116....1D&link_type=ABSTRACT'><b>The Southern Sky Redshift Survey</b></a><br><font size=-1><i>We report redshifts, magnitudes, and morphological classifications for5369 galaxies with m_B <= 15.5 and for 57 galaxies fainter than thislimit, in two regions covering a total of 1.70 sr in the southerncelestial hemisphere. The galaxy catalog is drawn primarily from thelist of nonstellar objects identified in the Hubble Space TelescopeGuide Star Catalog (GSC). The galaxies have positions accurate to ~1"and magnitudes with an rms scatter of ~0.3 mag. We compute magnitudes(m_SSRS2) from the relation between instrumental GSC magnitudes and thephotometry by Lauberts & Valentijn. From a comparison with CCDphotometry, we find that our system is homogeneous across the sky andcorresponds to magnitudes measured at the isophotal level ~26 magarcsec^-2. The precision of the radial velocities is ~40 km s^-1, andthe redshift survey is more than 99% complete to the m_SSRS2 = 15.5 maglimit. This sample is in the direction opposite that of the CfA2; incombination the two surveys provide an important database for studies ofthe properties of galaxies and their large-scale distribution in thenearby universe. Based on observations obtained at Cerro TololoInter-American Observatory, National Optical Astronomy Observatories,operated by the Association of Universities for Research in Astronomy,Inc., under cooperative agreement with the National Science Foundation;Complejo Astronomico El Leoncito, operated under agreement between theConsejo Nacional de Investigaciones Científicas de laRepública Argentina and the National Universities of La Plata,Córdoba, and San Juan; the European Southern Observatory, LaSilla, Chile, partially under the bilateral ESO-ObservatórioNacional agreement; Fred Lawrence Whipple Observatory;Laboratório Nacional de Astrofísica, Brazil; and the SouthAfrican Astronomical Observatory.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998A%26AS..130..333T&link_type=ABSTRACT'><b>Kinematics of the local universe. VII. New 21-cm line measurements of 2112 galaxies</b></a><br><font size=-1><i>This paper presents 2112 new 21-cm neutral hydrogen line measurementscarried out with the meridian transit Nan\c cay radiotelescope. Amongthese data we give also 213 new radial velocities which complement thoselisted in three previous papers of this series. These new measurements,together with the HI data collected in LEDA, put to 6 700 the number ofgalaxies with 21-cm line width, radial velocity, and apparent diameterin the so-called KLUN sample. Figure 5 and Appendices A and B forcorresponding comments are available in electronic form at thehttp://www.edpsciences.com</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998A%26AS..128..299P&link_type=ABSTRACT'><b>Total magnitude, radius, colour indices, colour gradients and photometric type of galaxies</b></a><br><font size=-1><i>We present a catalogue of aperture photometry of galaxies, in UBVRI,assembled from three different origins: (i) an update of the catalogueof Buta et al. (1995) (ii) published photometric profiles and (iii)aperture photometry performed on CCD images. We explored different setsof growth curves to fit these data: (i) The Sersic law, (ii) The net ofgrowth curves used for the preparation of the RC3 and (iii) A linearinterpolation between the de Vaucouleurs (r(1/4) ) and exponential laws.Finally we adopted the latter solution. Fitting these growth curves, wederive (1) the total magnitude, (2) the effective radius, (3) the colourindices and (4) gradients and (5) the photometric type of 5169 galaxies.The photometric type is defined to statistically match the revisedmorphologic type and parametrizes the shape of the growth curve. It iscoded from -9, for very concentrated galaxies, to +10, for diffusegalaxies. Based in part on observations collected at the Haute-ProvenceObservatory.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998A%26AS..127..117P&link_type=ABSTRACT'><b>A catalogue of spatially resolved kinematics of galaxies: Bibliography</b></a><br><font size=-1><i>We present a catalogue of galaxies for which spatially resolved data ontheir internal kinematics have been published; there is no a priorirestriction regarding their morphological type. The catalogue lists thereferences to the articles where the data are published, as well as acoded description of these data: observed emission or absorption lines,velocity or velocity dispersion, radial profile or 2D field, positionangle. Tables 1, 2, and 3 are proposed in electronic form only, and areavailable from the CDS, via anonymous ftp to cdsarc.u-strasbg.fr (to130.79.128.5) or via http://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=1997AJ....114.2402C&link_type=ABSTRACT'><b>Optical Rotation Curves and Linewidths for Tully-Fisher Applications</b></a><br><font size=-1><i>Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....114.2402C&db_key=AST</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996MNRAS.281...27P&link_type=ABSTRACT'><b>The universal rotation curve of spiral galaxies - I. The dark matter connection</b></a><br><font size=-1><i>We use a homogeneous sample of about 1100 optical and radio rotationcurves (RCs) and relative surface photometry to investigate the mainmass structure properties of spirals, over a range of 6 mag and out to<~1.5 and 2 optical radii (for the optical and radio data,respectively). We confirm the strong dependence on luminosity for boththe profile and the amplitude of RCs claimed by Persic & Salucci.Spiral RCs show the striking feature that a single global parameter,e.g. luminosity, dictates the rotational velocity at any radius for anyobject, so revealing the existence of a universal RC. At highluminosities, there is a slight discrepancy between the profiles of RCsand those predicted from the luminous matter (LM) distributions: thisimplies a small, yet detectable, amount of dark matter (DM). At lowluminosities, the failure of the LM prediction is much more severe, andthe DM is the only relevant mass component. We show that the universalRC implies a number of scaling properties between dark and luminousgalactic structure parameters: (i) the DM/LM mass ratio scales inverselywith luminosity; (ii) the central halo density scales as L^-0.7 (iii)the halo core radius is comparable to the optical radius, but shrinksfor low luminosities; (iv) the total halo mass scales as L^0.5. Suchscaling properties can be represented as a curve in the(luminosity)-(DM/LM mass ratio)-(DM core radius)-(DM central density)space, which provides a geometrical description of the tight couplingbetween the dark and the luminous matter in spiral galaxies.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ApJS..107...97M&link_type=ABSTRACT'><b>Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation</b></a><br><font size=-1><i>I-band luminosities, rotational velocities, and redshifts of 1092 spiralgalaxies have been measured by CCD photometry and Hα spectroscopyusing the 1 m and 2.3 m telescopes at Siding Spring Observatory,respectively. The results are tabulated. Luminosity profiles andHα rotation curves are given for the galaxies. When these resultsare combined with similar data for 1355 spiral galaxies publishedpreviously (Mathewson, Ford, & Buchhorn, hereafter Paper I), itprovides a large, uniform, and unique data set with which to measure,via the Tully-Fisher relation, the peculiar velocities of galaxies inthe local universe to a distance of 11,000 km s^-1^ (Mathewson &Ford). Taking advantage of the opportunity for publishing this data inmachine-readable form, in the CD-ROM, we have also included similar datafor the 1355 galaxies in Paper I.</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..467G&link_type=ABSTRACT'><b>An image database. II. Catalogue between δ=-30deg and δ=70deg.</b></a><br><font size=-1><i>A preliminary list of 68.040 galaxies was built from extraction of35.841 digitized images of the Palomar Sky Survey (Paper I). For eachgalaxy, the basic parameters are obtained: coordinates, diameter, axisratio, total magnitude, position angle. On this preliminary list, weapply severe selection rules to get a catalog of 28.000 galaxies, wellidentified and well documented. For each parameter, a comparison is madewith standard measurements. The accuracy of the raw photometricparameters is quite good despite of the simplicity of the method.Without any local correction, the standard error on the total magnitudeis about 0.5 magnitude up to a total magnitude of B_T_=17. Significantsecondary effects are detected concerning the magnitudes: distance toplate center effect and air-mass effect.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995ApJS...99..501P&link_type=ABSTRACT'><b>Rotation Curves of 967 Spiral Galaxies</b></a><br><font size=-1><i>We present the rotation curves of 967 southern spiral galaxies, obtainedby deprojecting and folding the raw Hα data originally publishedby Mathewson, Ford, & Buchhorn (1992). For 900 objects, we alsopresent, in figures and tables, the rotation curves smoothed on scalescorresponding to 5%-20% of the optical size; of these, 80 meet objectiveexcellence criteria and are suitable for individual detailed massmodeling, while 820, individually less compelling mainly because of themoderate statistics and/or limited extension, are suitable forstatistical studies. The remaining 67 curves suffer from severeasymmetries, small statistics, and large internal scatter that maylargely limit their use in galaxy structure studies. The deprojectedfolded curves, the smoothed curves, and various related quantities areavailable via anonymous ftp at galileo.sissa.it in the directory/users/ftp/pub/psrot.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993AJ....105.1637H&link_type=ABSTRACT'><b>The morphological catalogue of galaxies equatorial survey</b></a><br><font size=-1><i>We present 865 redshifts of galaxies located in the equatorial stripdelta between -17.5 deg and -2.5 deg in the right ascension rangebetween 20 h and 5 h. Redshifts have been obtained for the completesample of all 833 galaxies in the Morphological Catalog of Galaxies withmagnitudes brighter than m = 14.5 (corresponding approximately tom(Zwicky) = 15.0). This sample also includes three galaxies from othersources with more reliable magnitudes, satisfying this limit, and 29fainter galaxies, usually companions of the galaxies in the magnitudelimited sample. Our maps of a very large volume of nearby spacedemonstrate a variety of coherent large scale structures which includelarge voids, 20-50/h Mpc in diameter and large walls at least 70/h Mpcacross.</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=1992ApJS...81..413M&link_type=ABSTRACT'><b>A southern sky survey of the peculiar velocities of 1355 spiral galaxies</b></a><br><font size=-1><i>The paper presents data from photometric and spectroscopic observationsof 1355 southern spiral galaxies and uses them to determine theirdistances and peculiar velocities via the Tully-Fisher (TF) relation.I-band CCD surface photometry was carried out using the 1-m and 3.9-mtelescopes at Siding Spring Observatory. H-alpha rotation curves for 965galaxies and 551 H I profiles are presented. The physical parameters,photometric and velocity data, distances, and peculiar velocities of thegalaxies are presented in tabular form. The mean distance, systemicvelocity, and average peculiar velocity of 24 clusters in the sample aregiven. TF diagrams are presented for each cluster.</i></font><br><br></td></tr><tr><td colspan=2><a href='http://adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989PASP..101..360S&link_type=ABSTRACT'><b>Revised coordinates for 373 selected objects in the Southern Galaxy Catalogue</b></a><br><font size=-1><i>Improved positions have been determined for 373 galaxies listed in theSouthern Galaxy Catalogue of Corwin et al. (1985) as having poorcoordinates. The revised coordinates are expected to be good to 6 arcsec(rms) in each coordinate.</i></font><br><br></td></tr> </table> <font size=-1><a href='article?action=new&obj1=2-2845&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=2845&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=2.81869444446667&de=-16.992777778&zoom=9&img_source=DSS2&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=36&locale=EN'>Eridanus</a></td></tr> <tr><td nowrap>Right ascension:</td><td><a href='/?ra=2.81869444446667&de=-16.992777778&zoom=10&locale=EN' rel='nofollow'>02<sup>h</sup>49<sup>m</sup>07.30<sup>s</sup></a></td></tr> <tr><td nowrap>Declination:</td><td><a href='/?ra=2.81869444446667&de=-16.992777778&zoom=10&locale=EN' rel='nofollow'>-16Â°59'34.0"</a></td></tr> <tr><td nowrap>Aparent dimensions:</td><td>2.042′ × 0.813′</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=2845&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=1114'>NGC 1114</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=10669'>PGC 10669</a></td></tr> <tr><td colspan="2"><hr width=100%></td></tr> <tr id='d_load_cat'><td colspan="2"><a href='#' onclick='loadCatalogs(2,2845);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>

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NGC 1114 - Galaxy - SKY-MAP