The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI
Identifieur interne : 001862 ( PascalFrancis/Corpus ); précédent : 001861; suivant : 001863The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI
Auteurs : M. L. M. Collins ; S. C. Chapman ; R. M. Rich ; M. J. Irwin ; J. Penarrubia ; R. A. Ibata ; N. Arimoto ; A. M. Brooks ; A. M. N. Ferguson ; G. F. Lewis ; A. W. Mcconnachie ; K. VennSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
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Abstract
While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (Mhalf) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of vr = -393.1 ± 4.2 and -344.8 ± 2.5 km s-1, and dispersions of σv = 11.5+5.3-4.4 and 9.4+3.2-2.4 km s-1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. MV < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.
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| NO : | PASCAL 11-0475743 INIST |
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| ET : | The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI |
| AU : | COLLINS (M. L. M.); CHAPMAN (S. C.); RICH (R. M.); IRWIN (M. J.); PENARRUBIA (J.); IBATA (R. A.); ARIMOTO (N.); BROOKS (A. M.); FERGUSON (A. M. N.); LEWIS (G. F.); MCCONNACHIE (A. W.); VENN (K.) |
| AF : | Institute of Astronomy, Madingley Rise/Cambridge CB3 0HA/Royaume-Uni (1 aut., 2 aut., 4 aut., 5 aut.); Department of Physics and Astronomy, University of California/Los Angeles, CA 90095-1547/Etats-Unis (3 aut.); Observatoire de Strasbourg, 11, rue de l'Université/67000, Strasbourg/France (6 aut.); National Astronomical Observatory of Japan, Osawa 2-21-1/Mitaka, Tokyo/Japon (7 aut.); California Institute of Technology, M/C 350-17/Pasadena, CA 91125/Etats-Unis (8 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (9 aut.); Sydney Institute for Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (10 aut.); NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria/British Columbia V9E 2E7/Canada (11 aut.); Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road/Victoria, BC V8P 1A1/Canada (12 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 417; No. 2; Pp. 1170-1182; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (Mhalf) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of vr = -393.1 ± 4.2 and -344.8 ± 2.5 km s-1, and dispersions of σv = 11.5+5.3-4.4 and 9.4+3.2-2.4 km s-1 for And V and And VI, respectively, meaning these two objects are consistent with the trends in σv and rhalf set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. MV < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host. |
| CC : | 001E03 |
| FD : | Cinématique; Voie lactée; Deimos; Dispersion vitesse; Etoile baryon; Masse viriel; Rapport masse; Galaxies naines; Dynamique; Groupe local; Photométrie; Matière sombre; Satellite Mars |
| ED : | Kinematics; Milky Way; Deimos; Velocity dispersion; Baryon star; Virial mass; Mass ratio; Dwarf galaxies; Dynamics; Local group; Photometry; Dark matter; Mars satellite |
| SD : | Dispersión velocidad; Estrella baritrón; Masa virial; Relación masa; Satélite Marte |
| LO : | INIST-2067.354000505511680250 |
| ID : | 11-0475743 |
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Venn</name><affiliation><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0475743</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0475743 INIST</idno><idno type="RBID">Pascal:11-0475743</idno><idno type="wicri:Area/PascalFrancis/Corpus">001862</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI</title><author><name sortKey="Collins, M L M" sort="Collins, M L M" uniqKey="Collins M" first="M. L. M." last="Collins">M. L. M. Collins</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Rise</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></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><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Rise</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Rich, R M" sort="Rich, R M" uniqKey="Rich R" first="R. M." last="Rich">R. M. Rich</name><affiliation><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14></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><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Rise</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Penarrubia, J" sort="Penarrubia, J" uniqKey="Penarrubia J" first="J." last="Penarrubia">J. Penarrubia</name><affiliation><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Rise</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14></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><inist:fA14 i1="03"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Arimoto, N" sort="Arimoto, N" uniqKey="Arimoto N" first="N." last="Arimoto">N. Arimoto</name><affiliation><inist:fA14 i1="04"><s1>National Astronomical Observatory of Japan, Osawa 2-21-1</s1><s2>Mitaka, Tokyo</s2><s3>JPN</s3><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Brooks, A M" sort="Brooks, A M" uniqKey="Brooks A" first="A. M." last="Brooks">A. M. Brooks</name><affiliation><inist:fA14 i1="05"><s1>California Institute of Technology, M/C 350-17</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Ferguson, A M N" sort="Ferguson, A M N" uniqKey="Ferguson A" first="A. M. N." last="Ferguson">A. M. N. Ferguson</name><affiliation><inist:fA14 i1="06"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Lewis, G F" sort="Lewis, G F" uniqKey="Lewis G" first="G. F." last="Lewis">G. F. Lewis</name><affiliation><inist:fA14 i1="07"><s1>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Mcconnachie, A W" sort="Mcconnachie, A W" uniqKey="Mcconnachie A" first="A. W." last="Mcconnachie">A. W. Mcconnachie</name><affiliation><inist:fA14 i1="08"><s1>NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria</s1><s2>British Columbia V9E 2E7</s2><s3>CAN</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Venn, K" sort="Venn, K" uniqKey="Venn K" first="K." last="Venn">K. Venn</name><affiliation><inist:fA14 i1="09"><s1>Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2011">2011</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Baryon star</term><term>Dark matter</term><term>Deimos</term><term>Dwarf galaxies</term><term>Dynamics</term><term>Kinematics</term><term>Local group</term><term>Mars satellite</term><term>Mass ratio</term><term>Milky Way</term><term>Photometry</term><term>Velocity dispersion</term><term>Virial mass</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Cinématique</term><term>Voie lactée</term><term>Deimos</term><term>Dispersion vitesse</term><term>Etoile baryon</term><term>Masse viriel</term><term>Rapport masse</term><term>Galaxies naines</term><term>Dynamique</term><term>Groupe local</term><term>Photométrie</term><term>Matière sombre</term><term>Satellite Mars</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (M<sub>half</sub>) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of v<sub>r</sub> = -393.1 ± 4.2 and -344.8 ± 2.5 km s<sup>-1</sup>, and dispersions of σ<sub>v</sub> = 11.5<sup>+5.3</sup><sub>-4.4</sub> and 9.4<sup>+3.2</sup><sub>-2.4</sub> km s<sup>-1</sup> for And V and And VI, respectively, meaning these two objects are consistent with the trends in σ<sub>v</sub> and r<sub>half</sub> set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. M<sub>V</sub> < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>417</s2></fA05><fA06><s2>2</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI</s1></fA08><fA11 i1="01" i2="1"><s1>COLLINS (M. L. M.)</s1></fA11><fA11 i1="02" i2="1"><s1>CHAPMAN (S. C.)</s1></fA11><fA11 i1="03" i2="1"><s1>RICH (R. M.)</s1></fA11><fA11 i1="04" i2="1"><s1>IRWIN (M. J.)</s1></fA11><fA11 i1="05" i2="1"><s1>PENARRUBIA (J.)</s1></fA11><fA11 i1="06" i2="1"><s1>IBATA (R. A.)</s1></fA11><fA11 i1="07" i2="1"><s1>ARIMOTO (N.)</s1></fA11><fA11 i1="08" i2="1"><s1>BROOKS (A. M.)</s1></fA11><fA11 i1="09" i2="1"><s1>FERGUSON (A. M. N.)</s1></fA11><fA11 i1="10" i2="1"><s1>LEWIS (G. F.)</s1></fA11><fA11 i1="11" i2="1"><s1>MCCONNACHIE (A. W.)</s1></fA11><fA11 i1="12" i2="1"><s1>VENN (K.)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, Madingley Rise</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000, Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="04"><s1>National Astronomical Observatory of Japan, Osawa 2-21-1</s1><s2>Mitaka, Tokyo</s2><s3>JPN</s3><sZ>7 aut.</sZ></fA14><fA14 i1="05"><s1>California Institute of Technology, M/C 350-17</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>8 aut.</sZ></fA14><fA14 i1="06"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>9 aut.</sZ></fA14><fA14 i1="07"><s1>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>10 aut.</sZ></fA14><fA14 i1="08"><s1>NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria</s1><s2>British Columbia V9E 2E7</s2><s3>CAN</s3><sZ>11 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>12 aut.</sZ></fA14><fA20><s1>1170-1182</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000505511680250</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0475743</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>USA</s0></fA66><fC01 i1="01" l="ENG"><s0>While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (M<sub>half</sub>) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of v<sub>r</sub> = -393.1 ± 4.2 and -344.8 ± 2.5 km s<sup>-1</sup>, and dispersions of σ<sub>v</sub> = 11.5<sup>+5.3</sup><sub>-4.4</sub> and 9.4<sup>+3.2</sup><sub>-2.4</sub> km s<sup>-1</sup> for And V and And VI, respectively, meaning these two objects are consistent with the trends in σ<sub>v</sub> and r<sub>half</sub> set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. M<sub>V</sub> < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Cinématique</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Kinematics</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Voie lactée</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Milky Way</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Deimos</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Deimos</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Dispersion vitesse</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Velocity dispersion</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Dispersión velocidad</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Etoile baryon</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Baryon star</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Estrella baritrón</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Masse viriel</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Virial mass</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Masa virial</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Rapport masse</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Mass ratio</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Relación masa</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Dynamique</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Dynamics</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Groupe local</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Local group</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Photométrie</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Photometry</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Matière sombre</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Dark matter</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Satellite Mars</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Mars satellite</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Satélite Marte</s0><s5>38</s5></fC03><fN21><s1>332</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0475743 INIST</NO><ET>The scatter about the 'Universal' dwarf spheroidal mass profile: a kinematic study of the M31 satellites And V and And VI</ET><AU>COLLINS (M. L. M.); CHAPMAN (S. C.); RICH (R. M.); IRWIN (M. J.); PENARRUBIA (J.); IBATA (R. A.); ARIMOTO (N.); BROOKS (A. M.); FERGUSON (A. M. N.); LEWIS (G. F.); MCCONNACHIE (A. W.); VENN (K.)</AU><AF>Institute of Astronomy, Madingley Rise/Cambridge CB3 0HA/Royaume-Uni (1 aut., 2 aut., 4 aut., 5 aut.); Department of Physics and Astronomy, University of California/Los Angeles, CA 90095-1547/Etats-Unis (3 aut.); Observatoire de Strasbourg, 11, rue de l'Université/67000, Strasbourg/France (6 aut.); National Astronomical Observatory of Japan, Osawa 2-21-1/Mitaka, Tokyo/Japon (7 aut.); California Institute of Technology, M/C 350-17/Pasadena, CA 91125/Etats-Unis (8 aut.); Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill/Edinburgh EH9 3HJ/Royaume-Uni (9 aut.); Sydney Institute for Astronomy, School of Physics, A29, University of Sydney/NSW 2006/Australie (10 aut.); NRC Herzberg Institute for Astrophysics, 5071 West Saanich Road, Victoria/British Columbia V9E 2E7/Canada (11 aut.); Department of Physics and Astronomy, University of Victoria, 3800 Finerty Road/Victoria, BC V8P 1A1/Canada (12 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 417; No. 2; Pp. 1170-1182; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>While the satellites of the Milky Way (MW) have been shown to be largely consistent in terms of their mass contained within one half-light radius (M<sub>half</sub>) with a 'universal' mass profile, a number of M31 satellites are found to be inconsistent with these relations, and seem kinematically colder in their central regions than their MW cousins. In this work, we present new kinematic and updated structural properties for two M31 dwarf spheroidals (dSph), And V and And VI, using data from the Keck Low Resolution Imaging Spectrograph (LRIS) and the DEep Imaging Multi-Object Spectrograph (DEIMOS) instruments and the Subaru Suprime-Cam imager. We measure systemic velocities of v<sub>r</sub> = -393.1 ± 4.2 and -344.8 ± 2.5 km s<sup>-1</sup>, and dispersions of σ<sub>v</sub> = 11.5<sup>+5.3</sup><sub>-4.4</sub> and 9.4<sup>+3.2</sup><sub>-2.4</sub> km s<sup>-1</sup> for And V and And VI, respectively, meaning these two objects are consistent with the trends in σ<sub>v</sub> and r<sub>half</sub> set by their MW counterparts. We also investigate the nature of this scatter about the MW dSph mass profiles for the 'classical' (i.e. M<sub>V</sub> < -8) MW and M31 dSph. When comparing both the 'classical' MW and M31 dSph to the best-fitting mass profiles in the size-velocity dispersion plane, we find general scatter in both the positive (i.e. hotter) and negative (i.e. colder) directions from these profiles. However, barring one exception (CVnI) only the M31 dSph are found to scatter towards a colder regime, and, excepting the And I dSph, only MW objects scatter to hotter dispersions. The scatter for the combined population is greater than expected from measurement errors alone. We assess this divide in the context of the differing disc-to-halo mass (i.e. stars and baryons to total virial mass) ratios of the two hosts and argue that the underlying mass profiles for dSph differ from galaxy to galaxy, and are modified by the baryonic component of the host.</EA><CC>001E03</CC><FD>Cinématique; Voie lactée; Deimos; Dispersion vitesse; Etoile baryon; Masse viriel; Rapport masse; Galaxies naines; Dynamique; Groupe local; Photométrie; Matière sombre; Satellite Mars</FD><ED>Kinematics; Milky Way; Deimos; Velocity dispersion; Baryon star; Virial mass; Mass ratio; Dwarf galaxies; Dynamics; Local group; Photometry; Dark matter; Mars satellite</ED><SD>Dispersión velocidad; Estrella baritrón; Masa virial; Relación masa; Satélite Marte</SD><LO>INIST-2067.354000505511680250</LO><ID>11-0475743</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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