Distances and metallicities for 17 Local Group galaxies
Identifieur interne : 001557 ( Istex/Corpus ); précédent : 001556; suivant : 001558Distances and metallicities for 17 Local Group galaxies
Auteurs : A. W. Mcconnachie ; M. J. Irwin ; A. M. N. Ferguson ; R. A. Ibata ; G. F. Lewis ; N. TanvirSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2005-01.
English descriptors
- KwdEn :
- Algorithm, Andromeda, Aparicio, Aquarius, Armandroff, Astron, Bellazzini, Bergh, Centre, Cetus, Colour, Costa, Distance determinations, Distance estimates, Distance modulus, Dwarf, Dwarf galaxies, Elliptical annulus, Error budget, Evolutionary track, Fainter, Foreground, Foreground contamination, Foreground stars, Freedman, Freedman madore, Galaxy, Gallagher, Giant branch, Globular clusters, Good agreement, Grebel guhathakurta, Guhathakurta, Heuristic, Heuristic signal, Hoessel, Irwin, Isaac newton telescope, Itrgb, Itrgb algorithm, Lgs3, Local foreground correction, Local group, Local group galaxies, Locus, Lower right panel, Luminosity, Luminosity function, Luminosity functions, Madore, Mcconnachie, Median, Median metallicity, Metallicities, Metallicity, Minniti zijlstra, Mnras, Modulus, Pegasus, Photometric, Photometric conditions, Photometry, Previous estimates, Reddening, Representative metallicity, Sarajedini, Semimajor axis, Spheroidal, Stellar, Stellar content, Stellar locus, Stellar objects, Stellar populations, Systematic uncertainties, Trgb, Trgb algorithm, Trgb location, Upper right panel, Zucker.
- Teeft :
- Algorithm, Andromeda, Aparicio, Aquarius, Armandroff, Astron, Bellazzini, Bergh, Centre, Cetus, Colour, Costa, Distance determinations, Distance estimates, Distance modulus, Dwarf, Dwarf galaxies, Elliptical annulus, Error budget, Evolutionary track, Fainter, Foreground, Foreground contamination, Foreground stars, Freedman, Freedman madore, Galaxy, Gallagher, Giant branch, Globular clusters, Good agreement, Grebel guhathakurta, Guhathakurta, Heuristic, Heuristic signal, Hoessel, Irwin, Isaac newton telescope, Itrgb, Itrgb algorithm, Lgs3, Local foreground correction, Local group, Local group galaxies, Locus, Lower right panel, Luminosity, Luminosity function, Luminosity functions, Madore, Mcconnachie, Median, Median metallicity, Metallicities, Metallicity, Minniti zijlstra, Mnras, Modulus, Pegasus, Photometric, Photometric conditions, Photometry, Previous estimates, Reddening, Representative metallicity, Sarajedini, Semimajor axis, Spheroidal, Stellar, Stellar content, Stellar locus, Stellar objects, Stellar populations, Systematic uncertainties, Trgb, Trgb algorithm, Trgb location, Upper right panel, Zucker.
Abstract
We have obtained Johnson V and Gunn i photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.
Url:
DOI: 10.1111/j.1365-2966.2004.08514.x
Links to Exploration step
ISTEX:72AA634C0514A6DE50BDF8B40D403202489B61DCLe document en format XML
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The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>trgb</json:string><json:string>metallicity</json:string><json:string>itrgb</json:string><json:string>luminosity</json:string><json:string>luminosity function</json:string><json:string>reddening</json:string><json:string>luminosity functions</json:string><json:string>mnras</json:string><json:string>photometry</json:string><json:string>armandroff</json:string><json:string>costa</json:string><json:string>stellar</json:string><json:string>metallicities</json:string><json:string>mcconnachie</json:string><json:string>andromeda</json:string><json:string>aquarius</json:string><json:string>algorithm</json:string><json:string>pegasus</json:string><json:string>lgs3</json:string><json:string>heuristic</json:string><json:string>upper right panel</json:string><json:string>galaxy</json:string><json:string>lower right panel</json:string><json:string>local group</json:string><json:string>heuristic signal</json:string><json:string>error budget</json:string><json:string>bellazzini</json:string><json:string>itrgb algorithm</json:string><json:string>stellar populations</json:string><json:string>median metallicity</json:string><json:string>madore</json:string><json:string>cetus</json:string><json:string>stellar locus</json:string><json:string>photometric</json:string><json:string>bergh</json:string><json:string>freedman</json:string><json:string>local group galaxies</json:string><json:string>sarajedini</json:string><json:string>hoessel</json:string><json:string>spheroidal</json:string><json:string>colour</json:string><json:string>irwin</json:string><json:string>astron</json:string><json:string>gallagher</json:string><json:string>stellar content</json:string><json:string>guhathakurta</json:string><json:string>trgb algorithm</json:string><json:string>giant branch</json:string><json:string>modulus</json:string><json:string>zucker</json:string><json:string>fainter</json:string><json:string>median</json:string><json:string>distance estimates</json:string><json:string>representative metallicity</json:string><json:string>dwarf galaxies</json:string><json:string>distance modulus</json:string><json:string>dwarf</json:string><json:string>foreground</json:string><json:string>aparicio</json:string><json:string>freedman madore</json:string><json:string>previous estimates</json:string><json:string>stellar objects</json:string><json:string>trgb location</json:string><json:string>systematic uncertainties</json:string><json:string>grebel guhathakurta</json:string><json:string>centre</json:string><json:string>locus</json:string><json:string>semimajor axis</json:string><json:string>foreground stars</json:string><json:string>foreground contamination</json:string><json:string>minniti zijlstra</json:string><json:string>elliptical annulus</json:string><json:string>evolutionary track</json:string><json:string>local foreground correction</json:string><json:string>distance determinations</json:string><json:string>photometric conditions</json:string><json:string>isaac newton telescope</json:string><json:string>globular clusters</json:string><json:string>good agreement</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>A. M. N. Ferguson</name><affiliations><json:string>Max‐Planck‐Institut für Astrophysik, Karl‐Schwarzschild‐Str. 1, Postfach 1317, D‐85741 Garching, Germany</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>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>N. 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: general</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Local Group</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: stellar content</value></json:item></subject><articleId><json:string>MNR8514</json:string></articleId><arkIstex>ark:/67375/WNG-PQZLXX0K-8</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We have obtained Johnson V and Gunn i photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically >0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</abstract><qualityIndicators><score>9.976</score><pdfWordCount>11415</pdfWordCount><pdfCharCount>60706</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>19</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>248</abstractWordCount><abstractCharCount>1489</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Distances and metallicities for 17 Local Group galaxies</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>356</volume><issue>3</issue><pages><first>979</first><last>997</last></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2005</json:string><json:string>2003</json:string></date><geogName></geogName><orgName><json:string>University of Sydney</json:string><json:string>University of Hertfordshire</json:string><json:string>Institute of Astronomy, School of Physics</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>A. M. N. Ferguson</json:string><json:string>A. Ibata</json:string><json:string>A. W. McConnachie</json:string><json:string>N. Tanvir</json:string></persName><placeName><json:string>Australia</json:string><json:string>Canada</json:string><json:string>Strasbourg</json:string><json:string>France</json:string><json:string>Cambridge</json:string></placeName><ref_url><json:string>http://www.ast.cam.ac.uk/</json:string></ref_url><ref_bibl><json:string>Walton et al. 2001</json:string><json:string>Irwin & Lewis 2001</json:string><json:string>McConnachie et al. 2004a</json:string><json:string>Bellazzini et al. (2004)</json:string><json:string>Schlegel et al. (1998)</json:string><json:string>Bellazzini et al. 2001, 2004</json:string><json:string>Ibata et al. 2001</json:string><json:string>A. W. McConnachie et al.</json:string><json:string>Armandroff, Jacoby & Davies 1999</json:string><json:string>Irwin et al.</json:string><json:string>Ferguson et al. 2002</json:string><json:string>Bellazzini et al. 2003</json:string><json:string>Bellazzini et al. (2001)</json:string><json:string>Zucker et al. 2004</json:string><json:string>Thompson et al. (2001)</json:string><json:string>Landolt 1992</json:string><json:string>Da Costa & Armandroff 1990</json:string><json:string>VandenBerg et al. (2000)</json:string><json:string>Irwin et al. 2004</json:string><json:string>Karachentsev & Karachentseva 1999</json:string><json:string>Armandroff, Davies & Jacoby 1998</json:string><json:string>Ferguson et al.</json:string><json:string>McConnachie et al. 2003</json:string><json:string>Zucker et al. (2004)</json:string><json:string>Salaris & Cassisi 1997</json:string><json:string>Beers (2000)</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-PQZLXX0K-8</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>2005</publicationDate><copyrightDate>2005</copyrightDate><doi><json:string>10.1111/j.1365-2966.2004.08514.x</json:string></doi><id>72AA634C0514A6DE50BDF8B40D403202489B61DC</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/72AA634C0514A6DE50BDF8B40D403202489B61DC/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/72AA634C0514A6DE50BDF8B40D403202489B61DC/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/72AA634C0514A6DE50BDF8B40D403202489B61DC/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Distances and metallicities for 17 Local Group galaxies</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="2005-01"></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">Distances and metallicities for 17 Local Group galaxies</title><title level="a" type="short">Distances and metallicities in the Local Group</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">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-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">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-0005"><persName><forename type="first">N.</forename><surname>Tanvir</surname></persName><affiliation>Physical Sciences, University of Hertfordshire, Hatfield AL10 9AB</affiliation></author><idno type="istex">72AA634C0514A6DE50BDF8B40D403202489B61DC</idno><idno type="ark">ark:/67375/WNG-PQZLXX0K-8</idno><idno type="DOI">10.1111/j.1365-2966.2004.08514.x</idno><idno type="unit">MNR8514</idno><idno type="supplier">mnr8514</idno><idno type="toTypesetVersion">file:MNR.MNR8514.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.2005.356.issue-3</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">356</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="979">979</biblScope><biblScope unit="page" to="997">997</biblScope><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="2005-01"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We have obtained Johnson <hi rend="italic">V</hi> and Gunn <hi rend="italic">i</hi> photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute <hi rend="italic">I</hi> magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">galaxies: general</term><term xml:id="k2">Local Group</term><term xml:id="k3">galaxies: stellar content</term></keywords><keywords rend="tocHeading1"><term>Papers</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/72AA634C0514A6DE50BDF8B40D403202489B61DC/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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The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute <i>I</i> magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Distances and metallicities for 17 Local Group galaxies</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Distances and metallicities in the Local Group</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Distances and metallicities for 17 Local Group galaxies</title></titleInfo><name type="personal"><namePart type="given">A. 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Received 2004 August 16; in original form 2004 July 16</edition><copyrightDate encoding="w3cdtf">2005</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">15</extent><extent unit="tables">2</extent><extent unit="formulas">251</extent><extent unit="references">98</extent><extent unit="linksCrossRef">209</extent></physicalDescription><abstract lang="en">We have obtained Johnson V and Gunn i photometry for a large number of Local Group galaxies using the Isaac Newton Telescope Wide Field Camera (INT WFC). The majority of these galaxies are members of the M31 subgroup and the observations are deep enough to study the top few magnitudes of the red giant branch in each system. We previously measured the location of the tip of the red giant branch (TRGB) for Andromeda I, Andromeda II and M33 to within systematic uncertainties of typically <0.05 mag. As the TRGB acts as a standard candle in old, metal‐poor stellar populations, we were able to derive distances to each of these galaxies. Here we derive TRGB distances to the giant spiral galaxy M31 and 13 additional dwarf galaxies – NGC 205, 185, 147, Pegasus, WLM, LGS3, Cetus, Aquarius, And III, V, VI, VII and the newly discovered dwarf spheroidal And IX. The observations for each of the dwarf galaxies were intentionally taken in photometric conditions. In addition to the distances, we also self‐consistently derive the median metallicity of each system from the colour of their red giant branches. This allows us to take into account the small metallicity variation of the absolute I magnitude of the TRGB. The homogeneous nature of our data and the identical analysis applied to each of the 17 Local Group galaxies ensures that these estimates form a reliable set of distance and metallicity determinations that are ideal for comparative studies of Local Group galaxy properties.</abstract><subject lang="en"><genre>keywords</genre><topic>galaxies: general</topic><topic>Local Group</topic><topic>galaxies: stellar content</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>2005</date><detail type="volume"><caption>vol.</caption><number>356</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>979</start><end>997</end></extent></part></relatedItem><identifier type="istex">72AA634C0514A6DE50BDF8B40D403202489B61DC</identifier><identifier type="ark">ark:/67375/WNG-PQZLXX0K-8</identifier><identifier type="DOI">10.1111/j.1365-2966.2004.08514.x</identifier><identifier type="ArticleID">MNR8514</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/72AA634C0514A6DE50BDF8B40D403202489B61DC/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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