The kinematic identification of a thick stellar disc in M31
Identifieur interne : 004232 ( PascalFrancis/Curation ); précédent : 004231; suivant : 004233The kinematic identification of a thick stellar disc in M31
Auteurs : M. L. M. Collins [États-Unis] ; S. C. Chapman [États-Unis] ; R. A. Ibata [France] ; M. J. Irwin [États-Unis] ; R. M. Rich [États-Unis] ; A. M. N. Ferguson [États-Unis] ; G. F. Lewis [Australie] ; N. Tanvir [Royaume-Uni] ; A. Koch [Royaume-Uni]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.
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Abstract
We present the first characterization of a thick-disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south-west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of ?Δù? = 46.0 ± 3.9 km s-1. The velocity dispersion of the thick disc is σthick= 50.8±1.9 km s-1, greater than the value of dispersion we determine for the thin disc, σthin= 35.7 ± 1.0 km s-1. The thick disc is more metal poor than the thin disc, with [Fe/H]spec=-1.0±0.1 compared with [Fe/H]spec=-0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of hr = 7.3±1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1±0.2 and 2.8± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick-disc component of 2.4 x1010 < M*,thick < 4.1× 1010 M◦.. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.
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Ferguson</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>USA</s3><sZ>6 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="05"><s1>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>7 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Tanvir, N" sort="Tanvir, N" uniqKey="Tanvir N" first="N." last="Tanvir">N. Tanvir</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Koch, A" sort="Koch, A" uniqKey="Koch A" first="A." last="Koch">A. Koch</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0260679</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0260679 INIST</idno><idno type="RBID">Pascal:11-0260679</idno><idno type="wicri:Area/PascalFrancis/Corpus">001D11</idno><idno type="wicri:Area/PascalFrancis/Curation">004232</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The kinematic identification of a thick stellar disc in M31</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 wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="02"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ></inist:fA14><country>France</country></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 wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="03"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="04"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>USA</s3><sZ>6 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="05"><s1>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>7 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Tanvir, N" sort="Tanvir, N" uniqKey="Tanvir N" first="N." last="Tanvir">N. Tanvir</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Koch, A" sort="Koch, A" uniqKey="Koch A" first="A." last="Koch">A. Koch</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Department of Physics & Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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>Abundance</term><term>Deimos</term><term>Formation mechanism</term><term>Galaxy evolution</term><term>Galaxy structure</term><term>Local group</term><term>Mars satellite</term><term>Metallicity</term><term>Milky Way</term><term>Spiral galaxies</term><term>Stellar dynamics</term><term>Stellar kinematics</term><term>Velocity dispersion</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Cinématique stellaire</term><term>Galaxies spirales</term><term>Deimos</term><term>Métallicité</term><term>Dispersion vitesse</term><term>Voie lactée</term><term>Mécanisme formation</term><term>Dynamique stellaire</term><term>Abondance</term><term>Evolution galaxies</term><term>Groupe local</term><term>Structure galaxies</term><term>Satellite Mars</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present the first characterization of a thick-disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south-west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of ?Δù? = 46.0 ± 3.9 km s<sup>-1</sup>. The velocity dispersion of the thick disc is σ<sub>thick</sub>= 50.8±1.9 km s<sup>-1</sup>, greater than the value of dispersion we determine for the thin disc, σ<sub>thin</sub>= 35.7 ± 1.0 km s<sup>-1</sup>. The thick disc is more metal poor than the thin disc, with [Fe/H]<sub>spec</sub>=-1.0±0.1 compared with [Fe/H]<sub>spec</sub>=-0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of h<sub>r</sub> = 7.3±1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1±0.2 and 2.8± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick-disc component of 2.4 x10<sup>10</sup> < M<sub>*,thick</sub> < 4.1× 10<sup>10</sup> M<sub>◦.</sub>. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.</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>413</s2></fA05><fA06><s2>3</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The kinematic identification of a thick stellar disc in M31</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>IBATA (R. A.)</s1></fA11><fA11 i1="04" i2="1"><s1>IRWIN (M. J.)</s1></fA11><fA11 i1="05" i2="1"><s1>RICH (R. M.)</s1></fA11><fA11 i1="06" i2="1"><s1>FERGUSON (A. M. N.)</s1></fA11><fA11 i1="07" i2="1"><s1>LEWIS (G. F.)</s1></fA11><fA11 i1="08" i2="1"><s1>TANVIR (N.)</s1></fA11><fA11 i1="09" i2="1"><s1>KOCH (A.)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>USA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>4 aut.</sZ></fA14><fA14 i1="02"><s1>Observatoire de Strasbourg, 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angeles, CA 90095-1547</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="04"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>USA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="05"><s1>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>7 aut.</sZ></fA14><fA14 i1="06"><s1>Department of Physics & Astronomy, University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>9 aut.</sZ></fA14><fA20><s1>1548-1568</s1></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000192127200050</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.1/2</s0></fA45><fA47 i1="01" i2="1"><s0>11-0260679</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>We present the first characterization of a thick-disc component in the Andromeda galaxy (M31) using kinematic data from the DEIMOS instrument on Keck II. Using 21 fields in the south-west of the galaxy, we measure the lag of this component with respect to the thin disc, as well as the dispersion, metallicity and scalelength of the component. We find an average lag between the two components of ?Δù? = 46.0 ± 3.9 km s<sup>-1</sup>. The velocity dispersion of the thick disc is σ<sub>thick</sub>= 50.8±1.9 km s<sup>-1</sup>, greater than the value of dispersion we determine for the thin disc, σ<sub>thin</sub>= 35.7 ± 1.0 km s<sup>-1</sup>. The thick disc is more metal poor than the thin disc, with [Fe/H]<sub>spec</sub>=-1.0±0.1 compared with [Fe/H]<sub>spec</sub>=-0.7 ± 0.05 for the thin disc. We measure a radial scalelength of the thin and thick discs of h<sub>r</sub> = 7.3±1.0 and 8.0 ± 1.2 kpc, respectively. From this, we infer scaleheights for both discs of 1.1±0.2 and 2.8± 0.6 kpc, both of which are approximately two to three times larger than those observed in the Milky Way. We estimate a mass range for the thick-disc component of 2.4 x10<sup>10</sup> < M<sub>*,thick</sub> < 4.1× 10<sup>10</sup> M<sub>◦.</sub>. This value provides a useful constraint on possible formation mechanisms, as any proposed method for forming a thick disc must be able to heat (or deposit) at least this amount of material.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Cinématique stellaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Stellar kinematics</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Cinematica estelar</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Galaxies spirales</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Spiral galaxies</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>Métallicité</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Metallicity</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Metalicidad</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Dispersion vitesse</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Velocity dispersion</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Dispersión velocidad</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Voie lactée</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Milky Way</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Mécanisme formation</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Formation mechanism</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Mecanismo formacion</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Dynamique stellaire</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Stellar dynamics</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Abondance</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Abundance</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Groupe local</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Local group</s0><s5>36</s5></fC03><fC03 i1="12" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>37</s5></fC03><fC03 i1="12" i2="X" l="SPA"><s0>Estructura galaxias</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>178</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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