The tidal trail of NGC 205?
Identifieur interne : 002297 ( Istex/Corpus ); précédent : 002296; suivant : 002298The tidal trail of NGC 205?
Auteurs : A. W. Mcconnachie ; M. J. Irwin ; G. F. Lewis ; R. A. Ibata ; S. C. Chapman ; A. M. N. Ferguson ; N. R. TanvirSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2004-07.
English descriptors
- KwdEn :
- California institute, Carbon stars, Carter sadler, Central regions, Colour, Deep imaging spectrograph, Different metallicities, Disc, Disc component, Disc population, Dispersion, Eld, Field camera, Galactic haloes, Galaxy, Giant branch, Globular cluster, Ibata, Initial results, Irwin, Isaac newton telescope, Local group, Mateo, Middle panel, Minor axis, Mnras, Outer disc, Peterson caldwell, Radial velocities, Radial velocity, Similar galactocentric radius, Solid curves, Stellar, Stellar stream, Stellar streams, Structure formation, Surface brightness, Systemic velocity, Tidal, Tidal disruption, Tidal trail, Velocity dispersion.
- Teeft :
- California institute, Carbon stars, Carter sadler, Central regions, Colour, Deep imaging spectrograph, Different metallicities, Disc, Disc component, Disc population, Dispersion, Eld, Field camera, Galactic haloes, Galaxy, Giant branch, Globular cluster, Ibata, Initial results, Irwin, Isaac newton telescope, Local group, Mateo, Middle panel, Minor axis, Mnras, Outer disc, Peterson caldwell, Radial velocities, Radial velocity, Similar galactocentric radius, Solid curves, Stellar, Stellar stream, Stellar streams, Structure formation, Surface brightness, Systemic velocity, Tidal, Tidal disruption, Tidal trail, Velocity dispersion.
Abstract
Using data taken as part of the Isaac Newton Telescope Wide Field Camera (INT WFC) survey of M31, we have identified an arc‐like overdensity of blue, presumably metal‐poor, red giant branch stars in the north‐west quadrant of M31. This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of ΣV′≃ 28.5 ± 0.5 mag arcsec−2. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s−1, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.
Url:
DOI: 10.1111/j.1365-2966.2004.08076.x
Links to Exploration step
ISTEX:BB88755DA2BFD20E41E852274BB7F5C4B48B2123Le document en format XML
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This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of ΣV′≃ 28.5 ± 0.5 mag arcsec−2. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s−1, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>velocity dispersion</json:string><json:string>ibata</json:string><json:string>mnras</json:string><json:string>stellar</json:string><json:string>eld</json:string><json:string>colour</json:string><json:string>irwin</json:string><json:string>surface brightness</json:string><json:string>outer disc</json:string><json:string>tidal</json:string><json:string>stellar stream</json:string><json:string>stellar streams</json:string><json:string>radial velocities</json:string><json:string>mateo</json:string><json:string>tidal disruption</json:string><json:string>isaac newton telescope</json:string><json:string>disc population</json:string><json:string>tidal trail</json:string><json:string>similar galactocentric radius</json:string><json:string>dispersion</json:string><json:string>galaxy</json:string><json:string>disc</json:string><json:string>california institute</json:string><json:string>carbon stars</json:string><json:string>initial results</json:string><json:string>deep imaging spectrograph</json:string><json:string>local group</json:string><json:string>galactic haloes</json:string><json:string>field camera</json:string><json:string>middle panel</json:string><json:string>globular cluster</json:string><json:string>giant branch</json:string><json:string>different metallicities</json:string><json:string>central regions</json:string><json:string>minor axis</json:string><json:string>radial velocity</json:string><json:string>systemic velocity</json:string><json:string>solid curves</json:string><json:string>disc component</json:string><json:string>carter sadler</json:string><json:string>peterson caldwell</json:string><json:string>structure formation</json:string></teeft></keywords><author><json:item><name>A. W. McConnachie</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</json:string><json:string>E-mail: alan@ast.cam.ac.uk</json:string></affiliations></json:item><json:item><name>M. J. Irwin</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</json:string></affiliations></json:item><json:item><name>G. F. Lewis</name><affiliations><json:string>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>R. A. Ibata</name><affiliations><json:string>Observatoire de Strasbourg, 11, rue de l'Universite, F‐67000, Strasbourg, France</json:string></affiliations></json:item><json:item><name>S. C. Chapman</name><affiliations><json:string>California Institute of Technology, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>A. M. N. 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Tanvir</name><affiliations><json:string>Physical Sciences, University of Hertfordshire, Hatfield AL10 9AB</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>galaxies: dwarf</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: general</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: interactions</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Local Group</value></json:item></subject><articleId><json:string>MNR8076</json:string></articleId><arkIstex>ark:/67375/WNG-DV18T9Q1-X</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>Using data taken as part of the Isaac Newton Telescope Wide Field Camera (INT WFC) survey of M31, we have identified an arc‐like overdensity of blue, presumably metal‐poor, red giant branch stars in the north‐west quadrant of M31. This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of ΣV′≃ 28.5 ± 0.5 mag arcsec−2. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s−1, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.</abstract><qualityIndicators><score>8.01</score><pdfWordCount>3814</pdfWordCount><pdfCharCount>19549</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>5</pdfPageCount><pdfPageSize>595.276 x 782.362 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>183</abstractWordCount><abstractCharCount>1071</abstractCharCount><keywordCount>4</keywordCount></qualityIndicators><title>The tidal trail of NGC 205?</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>351</volume><issue>4</issue><pages><first>L94</first><last>L98</last><total>5</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>1970</json:string><json:string>2004</json:string></date><geogName></geogName><orgName><json:string>University of Sydney</json:string><json:string>California Institute of Technology, Pasadena, CA</json:string><json:string>University of Hertfordshire</json:string><json:string>California Institute of Technology, the University of California</json:string><json:string>Australian Research Council</json:string><json:string>Keck Foundation</json:string><json:string>Institute Accepted</json:string><json:string>National Aeronautics and Space</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>J. Irwin</json:string><json:string>F. Lewis</json:string><json:string>Newton Telescope</json:string><json:string>La Palma</json:string><json:string>S. C. Chapman</json:string><json:string>A. M. N. Ferguson</json:string><json:string>A. Ibata</json:string><json:string>A. W. McConnachie</json:string><json:string>N. R. Tanvir</json:string></persName><placeName><json:string>Canada</json:string><json:string>Strasbourg</json:string><json:string>France</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Majewski et al. 2003</json:string><json:string>Hodge 1973</json:string><json:string>Ibata et al. 2001a</json:string><json:string>Tonry & Davis 1979</json:string><json:string>Peterson & Caldwell 1993</json:string><json:string>Searle & Zinn 1978</json:string><json:string>Sagar et al. 1999</json:string><json:string>White & Rees 1978</json:string><json:string>Carter & Sadler 1990</json:string><json:string>Mateo, Olszewski & Morrison 1998</json:string><json:string>A. W. McConnachie et al.</json:string><json:string>Chapman et al. 2003</json:string><json:string>Ibata et al. (2004)</json:string><json:string>Irwin et al.</json:string><json:string>Ferguson et al. 2002</json:string><json:string>Choi et al. (2002)</json:string><json:string>Mateo et al. 1998</json:string><json:string>Irwin & Hatzidimitriou 1995</json:string><json:string>Kent 1987</json:string><json:string>Da Costa & Armandroff 1990</json:string><json:string>Demers et al. (2003)</json:string><json:string>Choi, Guhathakurta & Johnston 2002</json:string><json:string>Mateo 1998</json:string><json:string>Dehnen & Binney 1998</json:string><json:string>Ibata et al. 2004</json:string><json:string>Demers, Battinelli & Letarte 2003</json:string><json:string>Bender et al. 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(1994)</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-DV18T9Q1-X</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - astronomie</json:string></inist></categories><publicationDate>2004</publicationDate><copyrightDate>2004</copyrightDate><doi><json:string>10.1111/j.1365-2966.2004.08076.x</json:string></doi><id>BB88755DA2BFD20E41E852274BB7F5C4B48B2123</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/BB88755DA2BFD20E41E852274BB7F5C4B48B2123/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/BB88755DA2BFD20E41E852274BB7F5C4B48B2123/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/BB88755DA2BFD20E41E852274BB7F5C4B48B2123/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">The tidal trail of NGC 205?</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Science Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2004-07"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">The tidal trail of NGC 205?</title><title level="a" type="short">The tidal trail of NGC 205?</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">A. W.</forename><surname>McConnachie</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</affiliation><affiliation>E‐mail: alan@ast.cam.ac.uk</affiliation></author><author xml:id="author-0001"><persName><forename type="first">M. J.</forename><surname>Irwin</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</affiliation></author><author xml:id="author-0002"><persName><forename type="first">G. F.</forename><surname>Lewis</surname></persName><affiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">R. A.</forename><surname>Ibata</surname></persName><affiliation>Observatoire de Strasbourg, 11, rue de l'Universite, F‐67000, Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">S. C.</forename><surname>Chapman</surname></persName><affiliation>California Institute of Technology, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">A. M. N.</forename><surname>Ferguson</surname></persName><affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Str. 1, Postfach 1317, D‐85741 Garching, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">N. 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Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2004-07"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>Using data taken as part of the Isaac Newton Telescope Wide Field Camera (INT WFC) survey of M31, we have identified an arc‐like overdensity of blue, presumably metal‐poor, red giant branch stars in the north‐west quadrant of M31. This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of <emph><span>Σ<hi rend="subscript"><hi rend="italic">V</hi>′</hi>≃ 28.5 ± 0.5 mag arcsec<hi rend="superscript">−2</hi></span></emph>. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s<hi rend="superscript">−1</hi>, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">galaxies: dwarf</term><term xml:id="k2">galaxies: general</term><term xml:id="k3">galaxies: interactions</term><term xml:id="k4">Local Group</term></keywords><keywords rend="tocHeading1"><term>Letters</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/BB88755DA2BFD20E41E852274BB7F5C4B48B2123/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Science Ltd</publisherName><publisherLoc> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . 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E‐mail: <email>alan@ast.cam.ac.uk</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR8076.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2004 May 27. Received 2004 May 19; in original form 2004 March 10</unparsedEditorialHistory><countGroup><count type="figureTotal" number="3"></count><count type="tableTotal" number="0"></count><count type="formulaTotal" number="25"></count><count type="referenceTotal" number="33"></count><count type="linksCrossRef" number="71"></count></countGroup><titleGroup><title type="main">The tidal trail of NGC 205?</title><title type="shortAuthors"><i>A. W. McConnachie et al.</i></title><title type="short"><i>The tidal trail of NGC 205?</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>A. W.</givenNames><familyName>McConnachie</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>M. J.</givenNames><familyName>Irwin</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2"><personName><givenNames>G. F.</givenNames><familyName>Lewis</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3"><personName><givenNames>R. A.</givenNames><familyName>Ibata</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a4"><personName><givenNames>S. C.</givenNames><familyName>Chapman</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a5"><personName><givenNames>A. M. N.</givenNames><familyName>Ferguson</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a6"><personName><givenNames>N. R.</givenNames><familyName>Tanvir</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="AU"><unparsedAffiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11, rue de l'Universite, F‐67000, Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>California Institute of Technology, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Str. 1, Postfach 1317, D‐85741 Garching, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a6"><unparsedAffiliation>Physical Sciences, University of Hertfordshire, Hatfield AL10 9AB</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">galaxies: dwarf</keyword><keyword xml:id="k2">galaxies: general</keyword><keyword xml:id="k3">galaxies: interactions</keyword><keyword xml:id="k4">Local Group</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>Using data taken as part of the Isaac Newton Telescope Wide Field Camera (INT WFC) survey of M31, we have identified an arc‐like overdensity of blue, presumably metal‐poor, red giant branch stars in the north‐west quadrant of M31. This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of <span type="mathematics">Σ<sub><i>V</i>′</sub>≃ 28.5 ± 0.5 mag arcsec<sup>−2</sup></span>. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s<sup>−1</sup>, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The tidal trail of NGC 205?</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>The tidal trail of NGC 205?</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The tidal trail of NGC 205?</title></titleInfo><name type="personal"><namePart type="given">A. W.</namePart><namePart type="family">McConnachie</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</affiliation><affiliation>E-mail: alan@ast.cam.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. J.</namePart><namePart type="family">Irwin</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G. F.</namePart><namePart type="family">Lewis</namePart><affiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. A.</namePart><namePart type="family">Ibata</namePart><affiliation>Observatoire de Strasbourg, 11, rue de l'Universite, F‐67000, Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. C.</namePart><namePart type="family">Chapman</namePart><affiliation>California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. M. N.</namePart><namePart type="family">Ferguson</namePart><affiliation>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Str. 1, Postfach 1317, D‐85741 Garching, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N. R.</namePart><namePart type="family">Tanvir</namePart><affiliation>Physical Sciences, University of Hertfordshire, Hatfield AL10 9AB</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Science Ltd</publisher><place><placeTerm type="text">23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803</placeTerm></place><dateIssued encoding="w3cdtf">2004-07</dateIssued><edition>Accepted 2004 May 27. Received 2004 May 19; in original form 2004 March 10</edition><copyrightDate encoding="w3cdtf">2004</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">3</extent><extent unit="tables">0</extent><extent unit="formulas">25</extent><extent unit="references">33</extent><extent unit="linksCrossRef">71</extent></physicalDescription><abstract lang="en">Using data taken as part of the Isaac Newton Telescope Wide Field Camera (INT WFC) survey of M31, we have identified an arc‐like overdensity of blue, presumably metal‐poor, red giant branch stars in the north‐west quadrant of M31. This feature is ∼ 1° (15 kpc) in extent and has a surface brightness of ΣV′≃ 28.5 ± 0.5 mag arcsec−2. The arc appears to emanate from the dwarf elliptical galaxy NGC 205, and the colour of its red giant branch is significantly different from the M31 disc population but closely resembles that of NGC 205. Further, using data taken with the Deep Imaging Multi‐Object Spectrograph (DEIMOS) on Keck II, we identify the radial velocity signature of this arc. Its velocity dispersion is measured to be ≃ 10 km s−1, similar to that of the central regions of NGC 205 and typical of stellar streams. Based upon the spatial coincidence of these objects, the surface brightness, the velocity dispersions and the similarity in colour of the red giant branches, we postulate that the arc is part of a stellar stream, the progenitor of which is NGC 205.</abstract><subject lang="en"><genre>keywords</genre><topic>galaxies: dwarf</topic><topic>galaxies: general</topic><topic>galaxies: interactions</topic><topic>Local Group</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2004</date><detail type="volume"><caption>vol.</caption><number>351</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>L94</start><end>L98</end><total>5</total></extent></part></relatedItem><identifier type="istex">BB88755DA2BFD20E41E852274BB7F5C4B48B2123</identifier><identifier type="ark">ark:/67375/WNG-DV18T9Q1-X</identifier><identifier type="DOI">10.1111/j.1365-2966.2004.08076.x</identifier><identifier type="ArticleID">MNR8076</identifier><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Science Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/BB88755DA2BFD20E41E852274BB7F5C4B48B2123/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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