A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI
Identifieur interne : 001D19 ( Istex/Corpus ); précédent : 001D18; suivant : 001D20A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI
Auteurs : B. Letarte ; S. C. Chapman ; M. Collins ; R. A. Ibata ; M. J. Irwin ; A. M. N. Ferguson ; G. F. Lewis ; N. Martin ; A. Mcconnachie ; N. TanvirSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2009-12-11.
English descriptors
- KwdEn :
- Bottom panel, Bottom panels, California institute, Candidate member stars, Candidate members, Dark matter halo mass, Deep imaging spectrograph, Deimos spectroscopy, Dispersion, Distance estimate, Dsph, Dsphs, Dwarf, Dwarf galaxies, Galactic, Galactic foreground, Galaxy, Giant branch, Giant branches, Gilmore, Halo, Halo stars, Horizontal branch, Ibata, Inverse variance, Irwin, Journal compilation, Kinematic data, Lled squares, Lled triangles, Local group, Mcconnachie, Median, Median interquartile range, Median metallicity, Member stars, Metallicities, Minor axis, Mnras, Orbital properties, Padova isochrones, Radial velocities, Radial velocity, Recent years, Richstone tremaine, Robust, Robust members, Satellite galaxies, Satellite populations, Spectroscopic, Spectroscopic survey, Stellar, Stellar halo, Target stars, Tight range, Total mass, Total masses, Trgb, Trgb distance, Velocity dispersion.
- Teeft :
- Bottom panel, Bottom panels, California institute, Candidate member stars, Candidate members, Dark matter halo mass, Deep imaging spectrograph, Deimos spectroscopy, Dispersion, Distance estimate, Dsph, Dsphs, Dwarf, Dwarf galaxies, Galactic, Galactic foreground, Galaxy, Giant branch, Giant branches, Gilmore, Halo, Halo stars, Horizontal branch, Ibata, Inverse variance, Irwin, Journal compilation, Kinematic data, Lled squares, Lled triangles, Local group, Mcconnachie, Median, Median interquartile range, Median metallicity, Member stars, Metallicities, Minor axis, Mnras, Orbital properties, Padova isochrones, Radial velocities, Radial velocity, Recent years, Richstone tremaine, Robust, Robust members, Satellite galaxies, Satellite populations, Spectroscopic, Spectroscopic survey, Stellar, Stellar halo, Target stars, Tight range, Total mass, Total masses, Trgb, Trgb distance, Velocity dispersion.
Abstract
We present the results of a spectroscopic survey of the recently discovered M31 satellites And XV and And XVI, lying at projected distances from the centre of M31 of 93 and 130 kpc, respectively. These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative voids (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as ∼6 km s−1 down to i∼ 21.5. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from MV≈−9.4 to −9.8. The And XV velocity dispersion is resolved with vr=−339+7−6 km s−1 and σv= 11+7−5 km s−1. The And XVI dispersion is not quite resolved at 1σ with vr=−385+5−6 km s−1 and σ= 0+10−indef km s−1. Using the photometry of the confirmed member stars, we find metallicities of And XV (median [Fe/H]=−1.58, interquartile range ±0.08) and And XVI (median [Fe/H]=−2.23, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic [Fe/H]=−1.8 (−2.1) for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass (∼108 M⊙) and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.
Url:
DOI: 10.1111/j.1365-2966.2009.15546.x
Links to Exploration step
ISTEX:996F6FA5D288CA5D1D86D862AC03DABA6725C549Le document en format XML
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Letarte</name><affiliation><mods:affiliation>California Institute of Technology, 1200 E. California Blvd, MC 105‐24, Pasadena, CA 91125, USA</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>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: schapman@ast.cam.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Collins, M" sort="Collins, M" uniqKey="Collins M" first="M." last="Collins">M. Collins</name><affiliation><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Ibata, R A" sort="Ibata, R A" uniqKey="Ibata R" first="R. A." last="Ibata">R. A. 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These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative voids (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as ∼6 km s−1 down to i∼ 21.5. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from MV≈−9.4 to −9.8. The And XV velocity dispersion is resolved with vr=−339+7−6 km s−1 and σv= 11+7−5 km s−1. The And XVI dispersion is not quite resolved at 1σ with vr=−385+5−6 km s−1 and σ= 0+10−indef km s−1. Using the photometry of the confirmed member stars, we find metallicities of And XV (median [Fe/H]=−1.58, interquartile range ±0.08) and And XVI (median [Fe/H]=−2.23, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic [Fe/H]=−1.8 (−2.1) for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass (∼108 M⊙) and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>mnras</json:string><json:string>member stars</json:string><json:string>spectroscopic</json:string><json:string>ibata</json:string><json:string>dsphs</json:string><json:string>mcconnachie</json:string><json:string>dsph</json:string><json:string>robust</json:string><json:string>metallicities</json:string><json:string>trgb</json:string><json:string>journal compilation</json:string><json:string>halo</json:string><json:string>local group</json:string><json:string>candidate member stars</json:string><json:string>satellite galaxies</json:string><json:string>irwin</json:string><json:string>median</json:string><json:string>velocity dispersion</json:string><json:string>giant branch</json:string><json:string>dwarf galaxies</json:string><json:string>radial velocity</json:string><json:string>spectroscopic survey</json:string><json:string>median interquartile range</json:string><json:string>radial velocities</json:string><json:string>galaxy</json:string><json:string>gilmore</json:string><json:string>galactic</json:string><json:string>stellar</json:string><json:string>halo stars</json:string><json:string>target stars</json:string><json:string>horizontal branch</json:string><json:string>padova isochrones</json:string><json:string>orbital properties</json:string><json:string>inverse variance</json:string><json:string>kinematic data</json:string><json:string>dwarf</json:string><json:string>dispersion</json:string><json:string>minor axis</json:string><json:string>giant branches</json:string><json:string>satellite populations</json:string><json:string>distance estimate</json:string><json:string>california institute</json:string><json:string>stellar halo</json:string><json:string>trgb distance</json:string><json:string>median metallicity</json:string><json:string>recent years</json:string><json:string>tight range</json:string><json:string>robust members</json:string><json:string>deep imaging spectrograph</json:string><json:string>total mass</json:string><json:string>deimos spectroscopy</json:string><json:string>bottom panel</json:string><json:string>lled squares</json:string><json:string>lled triangles</json:string><json:string>candidate members</json:string><json:string>dark matter halo mass</json:string><json:string>galactic foreground</json:string><json:string>bottom panels</json:string><json:string>richstone tremaine</json:string><json:string>total masses</json:string></teeft></keywords><author><json:item><name>B. Letarte</name><affiliations><json:string>California Institute of Technology, 1200 E. California Blvd, MC 105‐24, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>S. C. Chapman</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</json:string><json:string>E-mail: schapman@ast.cam.ac.uk</json:string></affiliations></json:item><json:item><name>M. Collins</name><affiliations><json:string>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>R. A. Ibata</name><affiliations><json:string>Observatoire de Strasbourg, 11, rue de l'Université, F‐67000 Strasbourg, France</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>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hil l, Edinburgh EH9 3HJ</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. Martin</name><affiliations><json:string>Max‐Planck‐Institut fur Astronomie, Konigstuhl 17, D‐69117 Heidelberg, Germany</json:string></affiliations></json:item><json:item><name>A. McConnachie</name><affiliations><json:string>Department of Physics and Astronomy, University of Victoria, Victoria, B.C. V8P 1A1, Canada</json:string></affiliations></json:item><json:item><name>N. Tanvir</name><affiliations><json:string>Department of Physics and Astronomy, University of Leicester, Leicester LE17RH</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: And XV</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: individual: And XVI</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>MNR15546</json:string></articleId><arkIstex>ark:/67375/WNG-KXGTM9KQ-R</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present the results of a spectroscopic survey of the recently discovered M31 satellites And XV and And XVI, lying at projected distances from the centre of M31 of 93 and 130 kpc, respectively. These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative voids (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as ∼6 km s−1 down to i∼ 21.5. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from MV≈−9.4 to −9.8. The And XV velocity dispersion is resolved with vr=−339+7−6 km s−1 and σv= 11+7−5 km s−1. The And XVI dispersion is not quite resolved at 1σ with vr=−385+5−6 km s−1 and σ= 0+10−indef km s−1. Using the photometry of the confirmed member stars, we find metallicities of And XV (median [Fe/H]=−1.58, interquartile range ±0.08) and And XVI (median [Fe/H]=−2.23, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic [Fe/H]=−1.8 (−2.1) for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass (∼108 M⊙) and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.</abstract><qualityIndicators><score>10</score><pdfWordCount>5016</pdfWordCount><pdfCharCount>27422</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>7</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>271</abstractWordCount><abstractCharCount>1738</abstractCharCount><keywordCount>5</keywordCount></qualityIndicators><title>A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</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>400</volume><issue>3</issue><pages><first>1472</first><last>1478</last><total>7</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2009</json:string></date><geogName></geogName><orgName><json:string>University of Sydney</json:string><json:string>Department of Physics and Astronomy</json:string><json:string>Institute Accepted</json:string><json:string>Institute of Astronomy, School of Physics</json:string><json:string>University of Victoria</json:string><json:string>University of Leicester</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>S. C. Chapman</json:string><json:string>B. Letarte</json:string><json:string>A. M. N. Ferguson</json:string><json:string>A. Ibata</json:string><json:string>While</json:string><json:string>E. California</json:string><json:string>A. McConnachie</json:string><json:string>N. Tanvir</json:string></persName><placeName><json:string>Germany</json:string><json:string>Australia</json:string><json:string>Heidelberg</json:string><json:string>Edinburgh</json:string><json:string>Canada</json:string><json:string>Strasbourg</json:string><json:string>CA</json:string><json:string>France</json:string><json:string>Cambridge</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Koch et al. 2008</json:string><json:string>Martin et al.. 2007</json:string><json:string>Ibata et al. 2007</json:string><json:string>Schlegel, Finkbeiner & Davis 1998</json:string><json:string>Gottesman, Hunter & Boonyasait 2002</json:string><json:string>Bullock, Kravstov & Weinberg 2000</json:string><json:string>Faber et al. 2003</json:string><json:string>Tollerud et al. 2008</json:string><json:string>Majewski et al. 2007</json:string><json:string>Unavane, Wyse & Gilmore 1996</json:string><json:string>California Institute of Technology, 1200</json:string><json:string>Richstone & Tremaine 1986</json:string><json:string>Klypin et al. 1999</json:string><json:string>Martin et al. 2006</json:string><json:string>Chapman et al. 2008</json:string><json:string>Koch et al. 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(2007)</json:string><json:string>Schiavon et al. 1997</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-KXGTM9KQ-R</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>2009</publicationDate><copyrightDate>2009</copyrightDate><doi><json:string>10.1111/j.1365-2966.2009.15546.x</json:string></doi><id>996F6FA5D288CA5D1D86D862AC03DABA6725C549</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/996F6FA5D288CA5D1D86D862AC03DABA6725C549/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/996F6FA5D288CA5D1D86D862AC03DABA6725C549/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/996F6FA5D288CA5D1D86D862AC03DABA6725C549/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2009 The Authors. Journal compilation © 2009 RAS</licence></availability><date type="published" when="2009-12-11"></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">A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</title><title level="a" type="short">A Keck/DEIMOS spectroscopic survey</title><author xml:id="author-0000"><persName><forename type="first">B.</forename><surname>Letarte</surname></persName><affiliation>California Institute of Technology, 1200 E. California Blvd, MC 105‐24, Pasadena, CA 91125, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0001" role="corresp"><persName><forename type="first">S. C.</forename><surname>Chapman</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>E‐mail: schapman@ast.cam.ac.uk</affiliation></author><author xml:id="author-0002"><persName><forename type="first">M.</forename><surname>Collins</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</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'Université, F‐67000 Strasbourg, France<address><country key="FR"></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">A. M. N.</forename><surname>Ferguson</surname></persName><affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hil l, Edinburgh EH9 3HJ</affiliation></author><author xml:id="author-0006"><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-0007"><persName><forename type="first">N.</forename><surname>Martin</surname></persName><affiliation>Max‐Planck‐Institut fur Astronomie, Konigstuhl 17, D‐69117 Heidelberg, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">A.</forename><surname>McConnachie</surname></persName><affiliation>Department of Physics and Astronomy, University of Victoria, Victoria, B.C. V8P 1A1, Canada<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">N.</forename><surname>Tanvir</surname></persName><affiliation>Department of Physics and Astronomy, University of Leicester, Leicester LE17RH</affiliation></author><idno type="istex">996F6FA5D288CA5D1D86D862AC03DABA6725C549</idno><idno type="ark">ark:/67375/WNG-KXGTM9KQ-R</idno><idno type="DOI">10.1111/j.1365-2966.2009.15546.x</idno><idno type="unit">MNR15546</idno><idno type="toTypesetVersion">file:MNR.MNR15546.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.2009.400.issue-3</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">400</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1472">1472</biblScope><biblScope unit="page" to="1478">1478</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2009-12-11"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We present the results of a spectroscopic survey of the recently discovered M31 satellites And XV and And XVI, lying at projected distances from the centre of M31 of 93 and 130 kpc, respectively. These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative <hi rend="italic">voids</hi> (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as <emph><span>∼6 km s<hi rend="superscript">−1</hi></span></emph> down to <emph><span><hi rend="italic">i</hi>∼ 21.5</span></emph>. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from <emph><span><hi rend="italic">M</hi><hi rend="subscript">V</hi>≈−9.4</span></emph> to −9.8. The And XV velocity dispersion is resolved with <emph><span><hi rend="italic">v</hi><hi rend="subscript"><hi rend="italic">r</hi></hi>=−339<hi rend="superscript">+7</hi><hi rend="subscript">−6</hi> km s<hi rend="superscript">−1</hi></span></emph> and <emph><span>σ<hi rend="subscript"><hi rend="italic">v</hi></hi>= 11<hi rend="superscript">+7</hi><hi rend="subscript">−5</hi> km s<hi rend="superscript">−1</hi></span></emph>. The And XVI dispersion is not quite resolved at 1σ with <emph><span><hi rend="italic">v</hi><hi rend="subscript"><hi rend="italic">r</hi></hi>=−385<hi rend="superscript">+5</hi><hi rend="subscript">−6</hi> km s<hi rend="superscript">−1</hi></span></emph> and <emph><span>σ= 0<hi rend="superscript">+10</hi><hi rend="subscript">−indef</hi> km s<hi rend="superscript">−1</hi></span></emph>. Using the photometry of the confirmed member stars, we find metallicities of And XV (median <emph><span>[Fe/H]=−1.58</span></emph>, interquartile range ±0.08) and And XVI (median <emph><span>[Fe/H]=−2.23</span></emph>, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic <emph><span>[Fe/H]=−1.8 (−2.1)</span></emph> for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass <emph><span>(∼10<hi rend="superscript">8</hi> M<hi rend="subscript">⊙</hi>)</span></emph> and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">galaxies: dwarf</term><term xml:id="k2">galaxies: individual: And XV</term><term xml:id="k3">galaxies: individual: And XVI</term><term xml:id="k4">Local Group</term><term xml:id="k5">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/996F6FA5D288CA5D1D86D862AC03DABA6725C549/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 Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="12003"><doi origin="wiley">10.1111/mnr.2009.400.issue-3</doi><numberingGroup><numbering type="journalVolume" number="400">400</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2009-12-11">December 2009</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="27" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.15546.x</doi><idGroup><id type="unit" value="MNR15546"></id></idGroup><countGroup><count type="pageTotal" number="7"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2009 The Authors. 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E‐mail: <email>schapman@ast.cam.ac.uk</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR15546.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2009 August 14. Received 2009 August 12; in original form 2009 January 7</unparsedEditorialHistory><countGroup><count type="figureTotal" number="6"></count><count type="tableTotal" number="2"></count><count type="formulaTotal" number="58"></count><count type="referenceTotal" number="52"></count><count type="linksCrossRef" number="95"></count></countGroup><titleGroup><title type="main">A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</title><title type="shortAuthors"><i>B. Letarte et al.</i></title><title type="short"><i>A Keck/DEIMOS spectroscopic survey</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1"><personName><givenNames>B.</givenNames><familyName>Letarte</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2" corresponding="yes"><personName><givenNames>S. C.</givenNames><familyName>Chapman</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a2"><personName><givenNames>M.</givenNames><familyName>Collins</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="#a2"><personName><givenNames>M. 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F.</givenNames><familyName>Lewis</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a6"><personName><givenNames>N.</givenNames><familyName>Martin</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a7"><personName><givenNames>A.</givenNames><familyName>McConnachie</familyName></personName></creator><creator creatorRole="author" xml:id="cr10" affiliationRef="#a8"><personName><givenNames>N.</givenNames><familyName>Tanvir</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="US"><unparsedAffiliation>California Institute of Technology, 1200 E. California Blvd, MC 105‐24, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a2"><unparsedAffiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11, rue de l'Université, F‐67000 Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a4"><unparsedAffiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hil l, Edinburgh EH9 3HJ</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="AU"><unparsedAffiliation>Institute of Astronomy, School of Physics, A29, University of Sydney, NSW 2006, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut fur Astronomie, Konigstuhl 17, D‐69117 Heidelberg, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="CA"><unparsedAffiliation>Department of Physics and Astronomy, University of Victoria, Victoria, B.C. V8P 1A1, Canada</unparsedAffiliation></affiliation><affiliation xml:id="a8"><unparsedAffiliation>Department of Physics and Astronomy, University of Leicester, Leicester LE17RH</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">galaxies: dwarf</keyword><keyword xml:id="k2">galaxies: individual: And XV</keyword><keyword xml:id="k3">galaxies: individual: And XVI</keyword><keyword xml:id="k4">Local Group</keyword><keyword xml:id="k5">galaxies: stellar content</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present the results of a spectroscopic survey of the recently discovered M31 satellites And XV and And XVI, lying at projected distances from the centre of M31 of 93 and 130 kpc, respectively. These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative <i>voids</i> (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as <span type="mathematics">∼6 km s<sup>−1</sup></span> down to <span type="mathematics"><i>i</i>∼ 21.5</span>. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from <span type="mathematics"><i>M</i><sub>V</sub>≈−9.4</span> to −9.8. The And XV velocity dispersion is resolved with <span type="mathematics"><i>v</i><sub><i>r</i></sub>=−339<sup>+7</sup><sub>−6</sub> km s<sup>−1</sup></span> and <span type="mathematics">σ<sub><i>v</i></sub>= 11<sup>+7</sup><sub>−5</sub> km s<sup>−1</sup></span>. The And XVI dispersion is not quite resolved at 1σ with <span type="mathematics"><i>v</i><sub><i>r</i></sub>=−385<sup>+5</sup><sub>−6</sub> km s<sup>−1</sup></span> and <span type="mathematics">σ= 0<sup>+10</sup><sub>−indef</sub> km s<sup>−1</sup></span>. Using the photometry of the confirmed member stars, we find metallicities of And XV (median <span type="mathematics">[Fe/H]=−1.58</span>, interquartile range ±0.08) and And XVI (median <span type="mathematics">[Fe/H]=−2.23</span>, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic <span type="mathematics">[Fe/H]=−1.8 (−2.1)</span> for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass <span type="mathematics">(∼10<sup>8</sup> M<sub>⊙</sub>)</span> and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>A Keck/DEIMOS spectroscopic survey</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>A Keck/DEIMOS spectroscopic survey of the faint M 31 satellites And XV and And XVI</title></titleInfo><name type="personal"><namePart type="given">B.</namePart><namePart type="family">Letarte</namePart><affiliation>California Institute of Technology, 1200 E. California Blvd, MC 105‐24, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. C.</namePart><namePart type="family">Chapman</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>E-mail: schapman@ast.cam.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Collins</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">R. A.</namePart><namePart type="family">Ibata</namePart><affiliation>Observatoire de Strasbourg, 11, rue de l'Université, F‐67000 Strasbourg, France</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">A. M. N.</namePart><namePart type="family">Ferguson</namePart><affiliation>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hil l, Edinburgh EH9 3HJ</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">N.</namePart><namePart type="family">Martin</namePart><affiliation>Max‐Planck‐Institut fur Astronomie, Konigstuhl 17, D‐69117 Heidelberg, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">McConnachie</namePart><affiliation>Department of Physics and Astronomy, University of Victoria, Victoria, B.C. V8P 1A1, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Tanvir</namePart><affiliation>Department of Physics and Astronomy, University of Leicester, Leicester LE17RH</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">2009-12-11</dateIssued><edition>Accepted 2009 August 14. Received 2009 August 12; in original form 2009 January 7</edition><copyrightDate encoding="w3cdtf">2009</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">6</extent><extent unit="tables">2</extent><extent unit="formulas">58</extent><extent unit="references">52</extent><extent unit="linksCrossRef">95</extent></physicalDescription><abstract lang="en">We present the results of a spectroscopic survey of the recently discovered M31 satellites And XV and And XVI, lying at projected distances from the centre of M31 of 93 and 130 kpc, respectively. These satellites lie to the south of M31, in regions of the stellar halo which wide‐field imaging has revealed as relative voids (compared to the ∼degree‐scale coherent stream‐like structures). Using the Deep Imaging Multi‐Object Spectrograph mounted on the Keck II telescope, we have defined probable members of these satellites, for which we derive radial velocities as precise as ∼6 km s−1 down to i∼ 21.5. While the distance to And XVI remains the same as previously reported (525 ± 50 kpc), we have demonstrated that the brightest three stars previously used to define the tip of the red giant branch in And XV are in fact Galactic, and And XV is actually likely to be much more distant at 770 ± 70 kpc (compared to the previous 630 kpc), increasing the luminosity from MV≈−9.4 to −9.8. The And XV velocity dispersion is resolved with vr=−339+7−6 km s−1 and σv= 11+7−5 km s−1. The And XVI dispersion is not quite resolved at 1σ with vr=−385+5−6 km s−1 and σ= 0+10−indef km s−1. Using the photometry of the confirmed member stars, we find metallicities of And XV (median [Fe/H]=−1.58, interquartile range ±0.08) and And XVI (median [Fe/H]=−2.23, interquartile range ±0.12). Stacking the spectra of the member stars, we find spectroscopic [Fe/H]=−1.8 (−2.1) for And XV (And XVI), with an uncertainty of ∼0.2 dex in both cases. Our measurements of And XV reasonably resolve its mass (∼108 M⊙) and suggest a polar orbit, while the velocity of And XVI suggests it is approaching the M31 escape velocity given its large M31 centric distance.</abstract><subject lang="en"><genre>keywords</genre><topic>galaxies: dwarf</topic><topic>galaxies: individual: And XV</topic><topic>galaxies: individual: And XVI</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>2009</date><detail type="volume"><caption>vol.</caption><number>400</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>1472</start><end>1478</end><total>7</total></extent></part></relatedItem><identifier type="istex">996F6FA5D288CA5D1D86D862AC03DABA6725C549</identifier><identifier type="ark">ark:/67375/WNG-KXGTM9KQ-R</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.15546.x</identifier><identifier type="ArticleID">MNR15546</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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