Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal
Identifieur interne : 001838 ( Istex/Corpus ); précédent : 001837; suivant : 001839Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal
Auteurs : G. F. Lewis ; R. A. Ibata ; S. C. Chapman ; A. Mcconnachie ; M. J. Irwin ; E. Tolstoy ; N. R. TanvirSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-03-11.
English descriptors
- KwdEn :
- Andromeda galaxy, Arcmin, Barycentric distance, Centre, Cetus, Cetus dwarf, Cetus dwarf galaxy, Dwarf, Dwarf galaxies, Dwarf population, Dwarf spheroidal galaxies, Dwarf systems, Dynamical properties, Extratidal stars, Galaxy, Gure, Heliocentric velocity, Ibata, Internal velocity dispersion, Irwin, Journal compilation, Keck telescope, Kinematic, Large galaxies, Linear model, Local group, Local group dwarf galaxies, Local group velocity, Local universe, Lower panel, Lter analysis, Major axis, Mass traces light, Mcconnachie, Mcconnachie irwin, Milky, Mnras, Open circles, Open squares, Other candidate, Other members, Poisson sampling, Previous interactions, Radial orbit, Rotational velocity, Sagittarius dirr, Separate ccds, Solid body rotation, Solid circles, Solid line, Solid lines, Spatial distribution, Spectroscopic observations, Spectroscopic survey, Stellar, Stellar density, Stellar distribution, Surface brightness, Synthetic spectra, Systemic velocity, Tidal, Tidal debris, Tidal disruption, Tidal radius, Tidal tails, Upper panel, Velocity determination, Velocity dispersion, Velocity error.
- Teeft :
- Andromeda galaxy, Arcmin, Barycentric distance, Centre, Cetus, Cetus dwarf, Cetus dwarf galaxy, Dwarf, Dwarf galaxies, Dwarf population, Dwarf spheroidal galaxies, Dwarf systems, Dynamical properties, Extratidal stars, Galaxy, Gure, Heliocentric velocity, Ibata, Internal velocity dispersion, Irwin, Journal compilation, Keck telescope, Kinematic, Large galaxies, Linear model, Local group, Local group dwarf galaxies, Local group velocity, Local universe, Lower panel, Lter analysis, Major axis, Mass traces light, Mcconnachie, Mcconnachie irwin, Milky, Mnras, Open circles, Open squares, Other candidate, Other members, Poisson sampling, Previous interactions, Radial orbit, Rotational velocity, Sagittarius dirr, Separate ccds, Solid body rotation, Solid circles, Solid line, Solid lines, Spatial distribution, Spectroscopic observations, Spectroscopic survey, Stellar, Stellar density, Stellar distribution, Surface brightness, Synthetic spectra, Systemic velocity, Tidal, Tidal debris, Tidal disruption, Tidal radius, Tidal tails, Upper panel, Velocity determination, Velocity dispersion, Velocity error.
Abstract
This paper presents a study of the Cetus dwarf, an isolated dwarf galaxy within the Local Group. A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s−1 and with a velocity dispersion of 17 ± 2 km s−1; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s−1. The population is confirmed to be relatively metal‐poor, consistent with [Fe/H]∼−1.9, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. An analysis of Cetus' orbit through the Local Group indicates that it is at apocentre; taken in conjunction with the general dwarf population, this shows the mass of the Local Group to be ≳2 × 1012 M⊙.
Url:
DOI: 10.1111/j.1365-2966.2007.11395.x
Links to Exploration step
ISTEX:80D5653725A378192CDACCD1B420928421C86262Le document en format XML
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Lewis</name><affiliation><mods:affiliation>Institute of Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: gfl@physics.usyd.edu.au</mods:affiliation></affiliation></author><author><name sortKey="Ibata, R A" sort="Ibata, R A" uniqKey="Ibata R" first="R. A." last="Ibata">R. A. Ibata</name><affiliation><mods:affiliation>Observatoire de Strasbourg, 11, rue de l'Universit, Strasbourg F‐67000, France</mods:affiliation></affiliation></author><author><name sortKey="Chapman, S C" sort="Chapman, S C" uniqKey="Chapman S" first="S. C." last="Chapman">S. C. Chapman</name><affiliation><mods:affiliation>California Institute of Technology, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Mcconnachie, A" sort="Mcconnachie, A" uniqKey="Mcconnachie A" first="A." last="Mcconnachie">A. Mcconnachie</name><affiliation><mods:affiliation>Department of Physics & Astronomy, University of Victoria, Victoria, BC VP8 1A1, Canada</mods:affiliation></affiliation></author><author><name sortKey="Irwin, M J" sort="Irwin, M J" uniqKey="Irwin M" first="M. J." last="Irwin">M. J. Irwin</name><affiliation><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Tolstoy, E" sort="Tolstoy, E" uniqKey="Tolstoy E" first="E." last="Tolstoy">E. Tolstoy</name><affiliation><mods:affiliation>Kapteyn Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Tanvir, N R" sort="Tanvir, N R" uniqKey="Tanvir N" first="N. R." last="Tanvir">N. R. Tanvir</name><affiliation><mods:affiliation>Physical Science, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">375</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="1364">1364</biblScope><biblScope unit="page" to="1370">1370</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-03-11">2007-03-11</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Andromeda galaxy</term><term>Arcmin</term><term>Barycentric distance</term><term>Centre</term><term>Cetus</term><term>Cetus dwarf</term><term>Cetus dwarf galaxy</term><term>Dwarf</term><term>Dwarf galaxies</term><term>Dwarf population</term><term>Dwarf spheroidal galaxies</term><term>Dwarf systems</term><term>Dynamical properties</term><term>Extratidal stars</term><term>Galaxy</term><term>Gure</term><term>Heliocentric velocity</term><term>Ibata</term><term>Internal velocity dispersion</term><term>Irwin</term><term>Journal compilation</term><term>Keck telescope</term><term>Kinematic</term><term>Large galaxies</term><term>Linear model</term><term>Local group</term><term>Local group dwarf galaxies</term><term>Local group velocity</term><term>Local universe</term><term>Lower panel</term><term>Lter analysis</term><term>Major axis</term><term>Mass traces light</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Milky</term><term>Mnras</term><term>Open circles</term><term>Open squares</term><term>Other candidate</term><term>Other members</term><term>Poisson sampling</term><term>Previous interactions</term><term>Radial orbit</term><term>Rotational velocity</term><term>Sagittarius dirr</term><term>Separate ccds</term><term>Solid body rotation</term><term>Solid circles</term><term>Solid line</term><term>Solid lines</term><term>Spatial distribution</term><term>Spectroscopic observations</term><term>Spectroscopic survey</term><term>Stellar</term><term>Stellar density</term><term>Stellar distribution</term><term>Surface brightness</term><term>Synthetic spectra</term><term>Systemic velocity</term><term>Tidal</term><term>Tidal debris</term><term>Tidal disruption</term><term>Tidal radius</term><term>Tidal tails</term><term>Upper panel</term><term>Velocity determination</term><term>Velocity dispersion</term><term>Velocity error</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Andromeda galaxy</term><term>Arcmin</term><term>Barycentric distance</term><term>Centre</term><term>Cetus</term><term>Cetus dwarf</term><term>Cetus dwarf galaxy</term><term>Dwarf</term><term>Dwarf galaxies</term><term>Dwarf population</term><term>Dwarf spheroidal galaxies</term><term>Dwarf systems</term><term>Dynamical properties</term><term>Extratidal stars</term><term>Galaxy</term><term>Gure</term><term>Heliocentric velocity</term><term>Ibata</term><term>Internal velocity dispersion</term><term>Irwin</term><term>Journal compilation</term><term>Keck telescope</term><term>Kinematic</term><term>Large galaxies</term><term>Linear model</term><term>Local group</term><term>Local group dwarf galaxies</term><term>Local group velocity</term><term>Local universe</term><term>Lower panel</term><term>Lter analysis</term><term>Major axis</term><term>Mass traces light</term><term>Mcconnachie</term><term>Mcconnachie irwin</term><term>Milky</term><term>Mnras</term><term>Open circles</term><term>Open squares</term><term>Other candidate</term><term>Other members</term><term>Poisson sampling</term><term>Previous interactions</term><term>Radial orbit</term><term>Rotational velocity</term><term>Sagittarius dirr</term><term>Separate ccds</term><term>Solid body rotation</term><term>Solid circles</term><term>Solid line</term><term>Solid lines</term><term>Spatial distribution</term><term>Spectroscopic observations</term><term>Spectroscopic survey</term><term>Stellar</term><term>Stellar density</term><term>Stellar distribution</term><term>Surface brightness</term><term>Synthetic spectra</term><term>Systemic velocity</term><term>Tidal</term><term>Tidal debris</term><term>Tidal disruption</term><term>Tidal radius</term><term>Tidal tails</term><term>Upper panel</term><term>Velocity determination</term><term>Velocity dispersion</term><term>Velocity error</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">This paper presents a study of the Cetus dwarf, an isolated dwarf galaxy within the Local Group. A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s−1 and with a velocity dispersion of 17 ± 2 km s−1; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s−1. The population is confirmed to be relatively metal‐poor, consistent with [Fe/H]∼−1.9, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. An analysis of Cetus' orbit through the Local Group indicates that it is at apocentre; taken in conjunction with the general dwarf population, this shows the mass of the Local Group to be ≳2 × 1012 M⊙.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>cetus</json:string><json:string>local group</json:string><json:string>mnras</json:string><json:string>mcconnachie</json:string><json:string>dwarf</json:string><json:string>cetus dwarf galaxy</json:string><json:string>kinematic</json:string><json:string>ibata</json:string><json:string>cetus dwarf</json:string><json:string>arcmin</json:string><json:string>galaxy</json:string><json:string>dwarf galaxies</json:string><json:string>systemic velocity</json:string><json:string>irwin</json:string><json:string>stellar</json:string><json:string>gure</json:string><json:string>stellar density</json:string><json:string>journal compilation</json:string><json:string>tidal</json:string><json:string>velocity dispersion</json:string><json:string>mcconnachie irwin</json:string><json:string>solid circles</json:string><json:string>other members</json:string><json:string>spatial distribution</json:string><json:string>local group dwarf galaxies</json:string><json:string>local group velocity</json:string><json:string>rotational velocity</json:string><json:string>tidal radius</json:string><json:string>lter analysis</json:string><json:string>lower panel</json:string><json:string>open circles</json:string><json:string>tidal tails</json:string><json:string>large galaxies</json:string><json:string>milky</json:string><json:string>centre</json:string><json:string>surface brightness</json:string><json:string>previous interactions</json:string><json:string>velocity error</json:string><json:string>poisson sampling</json:string><json:string>synthetic spectra</json:string><json:string>tidal disruption</json:string><json:string>separate ccds</json:string><json:string>stellar distribution</json:string><json:string>dynamical properties</json:string><json:string>dwarf systems</json:string><json:string>dwarf spheroidal galaxies</json:string><json:string>andromeda galaxy</json:string><json:string>dwarf population</json:string><json:string>upper panel</json:string><json:string>velocity determination</json:string><json:string>extratidal stars</json:string><json:string>spectroscopic survey</json:string><json:string>mass traces light</json:string><json:string>spectroscopic observations</json:string><json:string>major axis</json:string><json:string>keck telescope</json:string><json:string>solid line</json:string><json:string>linear model</json:string><json:string>solid body rotation</json:string><json:string>internal velocity dispersion</json:string><json:string>solid lines</json:string><json:string>sagittarius dirr</json:string><json:string>heliocentric velocity</json:string><json:string>tidal debris</json:string><json:string>radial orbit</json:string><json:string>barycentric distance</json:string><json:string>other candidate</json:string><json:string>open squares</json:string><json:string>local universe</json:string></teeft></keywords><author><json:item><name>G. F. Lewis</name><affiliations><json:string>Institute of Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia</json:string><json:string>E-mail: gfl@physics.usyd.edu.au</json:string></affiliations></json:item><json:item><name>R. A. Ibata</name><affiliations><json:string>Observatoire de Strasbourg, 11, rue de l'Universit, Strasbourg F‐67000, 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. McConnachie</name><affiliations><json:string>Department of Physics & Astronomy, University of Victoria, Victoria, BC VP8 1A1, Canada</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>E. Tolstoy</name><affiliations><json:string>Kapteyn Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands</json:string></affiliations></json:item><json:item><name>N. R. Tanvir</name><affiliations><json:string>Physical Science, 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: individual: Cetus</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Local Group</value></json:item></subject><articleId><json:string>MNR11395</json:string></articleId><arkIstex>ark:/67375/WNG-5WKSPBFG-L</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>This paper presents a study of the Cetus dwarf, an isolated dwarf galaxy within the Local Group. A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s−1 and with a velocity dispersion of 17 ± 2 km s−1; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s−1. The population is confirmed to be relatively metal‐poor, consistent with [Fe/H]∼−1.9, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. An analysis of Cetus' orbit through the Local Group indicates that it is at apocentre; taken in conjunction with the general dwarf population, this shows the mass of the Local Group to be ≳2 × 1012 M⊙.</abstract><qualityIndicators><score>9.295</score><pdfWordCount>4883</pdfWordCount><pdfCharCount>28541</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>7</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>201</abstractWordCount><abstractCharCount>1308</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal</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>375</volume><issue>4</issue><pages><first>1364</first><last>1370</last><total>7</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2005</json:string><json:string>2007</json:string><json:string>11s</json:string></date><geogName></geogName><orgName><json:string>Kapteyn Institute, University of Groningen, Postbus</json:string><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>Keck Foundation</json:string><json:string>Caltech</json:string><json:string>Department of Physics</json:string><json:string>University of Victoria</json:string><json:string>University of California</json:string><json:string>Institute of Astronomy, Madingley Road, Cambridge CB</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>E. Tolstoy</json:string><json:string>W. M. Keck</json:string><json:string>J. Irwin</json:string><json:string>G. 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. Ibata</json:string><json:string>Group</json:string><json:string>N. R. Tanvir</json:string><json:string>Stars</json:string><json:string>A. McConnachie</json:string></persName><placeName><json:string>Groningen</json:string><json:string>Canada</json:string><json:string>Strasbourg</json:string><json:string>Velocity</json:string><json:string>France</json:string><json:string>Netherlands</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Willman et al. 2005a,b</json:string><json:string>Zucker et al. 2006a,b</json:string><json:string>Faber et al. 2003</json:string><json:string>White & Rees 1978</json:string><json:string>McConnachie et al. 2006</json:string><json:string>Johnston, Choi & Guhathakurta 2002</json:string><json:string>Mayer et al. 2002</json:string><json:string>Ibata et al. 2001</json:string><json:string>Klypin et al. 1999</json:string><json:string>Venn et al. 2004</json:string><json:string>McConnachie et al. 2005</json:string><json:string>McConnachie & Irwin 2006</json:string><json:string>G. F. 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(2001a,b, 2006)</json:string><json:string>Rockosi et al. 2002</json:string><json:string>Kepner et al. 1999</json:string><json:string>Stoehr et al. 2002</json:string><json:string>Belokurov et al. 2006a,b</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-5WKSPBFG-L</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 biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string><json:string>4 - genetique des eucaryotes. evolution biologique et moleculaire</json:string></inist></categories><publicationDate>2007</publicationDate><copyrightDate>2007</copyrightDate><doi><json:string>10.1111/j.1365-2966.2007.11395.x</json:string></doi><id>80D5653725A378192CDACCD1B420928421C86262</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/80D5653725A378192CDACCD1B420928421C86262/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/80D5653725A378192CDACCD1B420928421C86262/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/80D5653725A378192CDACCD1B420928421C86262/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-03-11"></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">Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal</title><title level="a" type="short">The Cetus dwarf galaxy</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">G. F.</forename><surname>Lewis</surname></persName><affiliation>Institute of Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation><affiliation>E‐mail: gfl@physics.usyd.edu.au</affiliation></author><author xml:id="author-0001"><persName><forename type="first">R. A.</forename><surname>Ibata</surname></persName><affiliation>Observatoire de Strasbourg, 11, rue de l'Universit, Strasbourg F‐67000, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0002"><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-0003"><persName><forename type="first">A.</forename><surname>McConnachie</surname></persName><affiliation>Department of Physics & Astronomy, University of Victoria, Victoria, BC VP8 1A1, Canada<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0004"><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-0005"><persName><forename type="first">E.</forename><surname>Tolstoy</surname></persName><affiliation>Kapteyn Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands<address><country key="NL"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">N. R.</forename><surname>Tanvir</surname></persName><affiliation>Physical Science, University of Hertfordshire, Hatfield AL10 9AB</affiliation></author><idno type="istex">80D5653725A378192CDACCD1B420928421C86262</idno><idno type="ark">ark:/67375/WNG-5WKSPBFG-L</idno><idno type="DOI">10.1111/j.1365-2966.2007.11395.x</idno><idno type="unit">MNR11395</idno><idno type="toTypesetVersion">file:MNR.MNR11395.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2007.375.issue-4</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">375</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="1364">1364</biblScope><biblScope unit="page" to="1370">1370</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-03-11"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>This paper presents a study of the Cetus dwarf, an isolated dwarf galaxy within the Local Group. A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s<hi rend="superscript">−1</hi> and with a velocity dispersion of 17 ± 2 km s<hi rend="superscript">−1</hi>; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s<hi rend="superscript">−1</hi>. The population is confirmed to be relatively metal‐poor, consistent with <emph><span>[Fe/H]∼−1.9</span></emph>, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. 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A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s<sup>−1</sup> and with a velocity dispersion of 17 ± 2 km s<sup>−1</sup>; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s<sup>−1</sup>. The population is confirmed to be relatively metal‐poor, consistent with <span type="mathematics">[Fe/H]∼−1.9</span>, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. An analysis of Cetus' orbit through the Local Group indicates that it is at apocentre; taken in conjunction with the general dwarf population, this shows the mass of the Local Group to be <span type="mathematics">≳2 × 10<sup>12</sup> M<sub>⊙</sub></span>.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>The Cetus dwarf galaxy</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Inside the whale: the structure and dynamics of the isolated Cetus dwarf spheroidal</title></titleInfo><name type="personal"><namePart type="given">G. F.</namePart><namePart type="family">Lewis</namePart><affiliation>Institute of Astronomy, School of Physics, A28, University of Sydney, NSW 2006, Australia</affiliation><affiliation>E-mail: gfl@physics.usyd.edu.au</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'Universit, Strasbourg F‐67000, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. 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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">E.</namePart><namePart type="family">Tolstoy</namePart><affiliation>Kapteyn Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands</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 Science, 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 Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2007-03-11</dateIssued><edition>Accepted 2006 December 11. Received 2006 December 6; in original form 2006 October 23</edition><copyrightDate encoding="w3cdtf">2007</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">7</extent><extent unit="tables">2</extent><extent unit="formulas">45</extent><extent unit="references">39</extent><extent unit="linksCrossRef">78</extent></physicalDescription><abstract lang="en">This paper presents a study of the Cetus dwarf, an isolated dwarf galaxy within the Local Group. A matched‐filter analysis of the INT/WFC imaging of this system reveals no evidence for significant tidal debris that could have been torn off the galaxy, bolstering the hypothesis that Cetus has never significantly interacted with either the Milky Way or M31. Additionally, Keck/Deimos spectroscopic observations identify this galaxy as a distinct kinematic population possessing a systematic velocity of −87 ± 2 km s−1 and with a velocity dispersion of 17 ± 2 km s−1; while tentative, these data also suggest that Cetus possesses a moderate rotational velocity of ∼8 km s−1. The population is confirmed to be relatively metal‐poor, consistent with [Fe/H]∼−1.9, and, assuming virial equilibrium, implies that the Cetus dwarf galaxy possesses a mass‐to‐light ratio of ∼70. It appears, therefore, that Cetus may represent a primordial dwarf galaxy, retaining the kinematic and structural properties lost by other members of the dwarf population of the Local Group in their interactions with the large galaxies. An analysis of Cetus' orbit through the Local Group indicates that it is at apocentre; taken in conjunction with the general dwarf population, this shows the mass of the Local Group to be ≳2 × 1012 M⊙.</abstract><subject lang="en"><genre>keywords</genre><topic>galaxies: dwarf</topic><topic>galaxies: individual: Cetus</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>2007</date><detail type="volume"><caption>vol.</caption><number>375</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>1364</start><end>1370</end><total>7</total></extent></part></relatedItem><identifier type="istex">80D5653725A378192CDACCD1B420928421C86262</identifier><identifier type="ark">ark:/67375/WNG-5WKSPBFG-L</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.11395.x</identifier><identifier type="ArticleID">MNR11395</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 Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/80D5653725A378192CDACCD1B420928421C86262/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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