The kinematic footprints of five stellar streams in Andromeda's halo
Identifieur interne : 002E34 ( PascalFrancis/Curation ); précédent : 002E33; suivant : 002E35The kinematic footprints of five stellar streams in Andromeda's halo
Auteurs : S. C. Chapman [Royaume-Uni, Canada] ; R. Ibata [France] ; M. Irwin [Royaume-Uni] ; A. Koch [États-Unis] ; B. Letarte [États-Unis] ; N. Martin [Allemagne] ; M. Collins [Royaume-Uni] ; G. F. Lewis [Australie] ; A. Mcconnachie [Canada] ; J. Penarrubia [Canada] ; R. M. Rich [États-Unis] ; D. Trethewey [Royaume-Uni] ; A. Ferguson [Royaume-Uni] ; A. Huxor [Royaume-Uni] ; N. Tanvir [Royaume-Uni]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Spectrométrie.
English descriptors
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Abstract
We present a spectroscopic analysis of five stellar streams ('A', 'B', 'Cr', 'Cp' and 'D') as well as the extended star cluster, EC4, which lies within Stream 'C', all discovered in the halo of M31 from our Canada-France-Hawaii Telescope/MegaCam survey. These spectroscopic results were initially serendipitous, making use of our existing observations from the DEep Imaging Multi-Object Spectrograph mounted on the Keck II telescope, and thereby emphasizing the ubiquity of tidal streams that account for ∼70 per cent of the M31 halo stars in the targeted fields. Subsequent spectroscopy was then procured in Stream 'C' and Stream 'D' to trace the velocity gradient along the streams. Nine metal-rich ([Fe/H] ∼ -0.7) stars at vhel = -349.5 km s-1,σv,corr ∼ 5.1 ± 2.5km s-1 are proposed as a serendipitous detection of Stream'Cr', with follow-up kinematic identification at a further point along the stream. Seven metal-poor ([Fe/H] ∼-1.3) stars confined to a narrow, 15 km s-1 velocity bin centred at uhel = -285.6, σv,corr = 4.3+1.7-1.4 km s-1 represent a kinematic detection of Stream 'Cp', again with follow-up kinematic identification further along the stream. For the cluster EC4, candidate member stars with average [Fe/H] ∼-1.4, are found at vhel = -282 suggesting it could be related to Stream 'Cp'. No similarly obvious cold kinematic candidate is found for Stream 'D', although candidates are proposed in both of two spectroscopic pointings along the stream (both at ∼ -400 km s-1). Spectroscopy near the edge of Stream 'B' suggests a likely kinematic detection at vhel ∼ -330, σv,corr ∼ 6.9 km s-1, while a candidate kinematic detection of Stream 'A' is found (plausibly associated to M33 rather than M31) with vhel ∼ -170, σv,corr = 12.5 km s-1. The low dispersion of the streams in kinematics, physical thickness and metallicity makes it hard to reconcile with a scenario whereby these stream structures as an ensemble are related to the giant southern stream. We conclude that the M31 stellar halo is largely made up of multiple kinematically cold streams.
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Penarrubia</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Canada</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="04"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angles, LA California</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Trethewey, D" sort="Trethewey, D" uniqKey="Trethewey D" first="D." last="Trethewey">D. Trethewey</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Ferguson, A" sort="Ferguson, A" uniqKey="Ferguson A" first="A." last="Ferguson">A. Ferguson</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Huxor, A" sort="Huxor, A" uniqKey="Huxor A" first="A." last="Huxor">A. Huxor</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</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="09"><s1>Department of Physics and Astronomy, University of Leicester</s1><s2>Leicester LEI 7RH</s2><s3>GBR</s3><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">08-0513603</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 08-0513603 INIST</idno><idno type="RBID">Pascal:08-0513603</idno><idno type="wicri:Area/PascalFrancis/Corpus">003219</idno><idno type="wicri:Area/PascalFrancis/Curation">002E34</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The kinematic footprints of five stellar streams in Andromeda's halo</title><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, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Ibata, R" sort="Ibata, R" uniqKey="Ibata R" first="R." last="Ibata">R. Ibata</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Irwin, M" sort="Irwin, M" uniqKey="Irwin M" first="M." last="Irwin">M. Irwin</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 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="04"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angles, LA California</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Letarte, B" sort="Letarte, B" uniqKey="Letarte B" first="B." last="Letarte">B. Letarte</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Martin, N" sort="Martin, N" uniqKey="Martin N" first="N." last="Martin">N. Martin</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Max-Planck-Institut für Astronomie, Königstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>6 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Collins, M" sort="Collins, M" uniqKey="Collins M" first="M." last="Collins">M. Collins</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</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="07"><s1>Institute of Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Mcconnachie, A" sort="Mcconnachie, A" uniqKey="Mcconnachie A" first="A." last="Mcconnachie">A. Mcconnachie</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Penarrubia, J" sort="Penarrubia, J" uniqKey="Penarrubia J" first="J." last="Penarrubia">J. Penarrubia</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Canada</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="04"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angles, LA California</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>11 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Trethewey, D" sort="Trethewey, D" uniqKey="Trethewey D" first="D." last="Trethewey">D. Trethewey</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Ferguson, A" sort="Ferguson, A" uniqKey="Ferguson A" first="A." last="Ferguson">A. Ferguson</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Huxor, A" sort="Huxor, A" uniqKey="Huxor A" first="A." last="Huxor">A. Huxor</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</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="09"><s1>Department of Physics and Astronomy, University of Leicester</s1><s2>Leicester LEI 7RH</s2><s3>GBR</s3><sZ>15 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="2008">2008</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>Galaxies</term><term>Galaxy halo</term><term>Member star</term><term>Metallicity</term><term>Spectroscopy</term><term>Star clusters</term><term>Stellar kinematics</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Cinématique stellaire</term><term>Amas stellaire</term><term>Spectrométrie</term><term>Etoile membre</term><term>Métallicité</term><term>Halo galaxies</term><term>Galaxies</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Spectrométrie</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present a spectroscopic analysis of five stellar streams ('A', 'B', 'Cr', 'Cp' and 'D') as well as the extended star cluster, EC4, which lies within Stream 'C', all discovered in the halo of M31 from our Canada-France-Hawaii Telescope/MegaCam survey. These spectroscopic results were initially serendipitous, making use of our existing observations from the DEep Imaging Multi-Object Spectrograph mounted on the Keck II telescope, and thereby emphasizing the ubiquity of tidal streams that account for ∼70 per cent of the M31 halo stars in the targeted fields. Subsequent spectroscopy was then procured in Stream 'C' and Stream 'D' to trace the velocity gradient along the streams. Nine metal-rich ([Fe/H] ∼ -0.7) stars at v<sub>hel</sub> = -349.5 km s<sup>-1</sup>,σ<sub>v,corr</sub> ∼ 5.1 ± 2.5km s<sup>-1</sup> are proposed as a serendipitous detection of Stream'Cr', with follow-up kinematic identification at a further point along the stream. Seven metal-poor ([Fe/H] ∼-1.3) stars confined to a narrow, 15 km s<sup>-1</sup> velocity bin centred at u<sub>hel</sub> = -285.6, σ<sub>v,corr</sub> = 4.3<sup>+1.7</sup><sub>-1.4</sub> km s<sup>-1</sup> represent a kinematic detection of Stream 'Cp', again with follow-up kinematic identification further along the stream. For the cluster EC4, candidate member stars with average [Fe/H] ∼-1.4, are found at v<sub>hel</sub> = -282 suggesting it could be related to Stream 'Cp'. No similarly obvious cold kinematic candidate is found for Stream 'D', although candidates are proposed in both of two spectroscopic pointings along the stream (both at ∼ -400 km s<sup>-1</sup>). Spectroscopy near the edge of Stream 'B' suggests a likely kinematic detection at v<sub>hel</sub> ∼ -330, σ<sub>v,corr</sub> ∼ 6.9 km s<sup>-1</sup>, while a candidate kinematic detection of Stream 'A' is found (plausibly associated to M33 rather than M31) with v<sub>hel</sub> ∼ -170, σ<sub>v,corr</sub> = 12.5 km s<sup>-1</sup>. The low dispersion of the streams in kinematics, physical thickness and metallicity makes it hard to reconcile with a scenario whereby these stream structures as an ensemble are related to the giant southern stream. We conclude that the M31 stellar halo is largely made up of multiple kinematically cold streams.</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>390</s2></fA05><fA06><s2>4</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The kinematic footprints of five stellar streams in Andromeda's halo</s1></fA08><fA11 i1="01" i2="1"><s1>CHAPMAN (S. C.)</s1></fA11><fA11 i1="02" i2="1"><s1>IBATA (R.)</s1></fA11><fA11 i1="03" i2="1"><s1>IRWIN (M.)</s1></fA11><fA11 i1="04" i2="1"><s1>KOCH (A.)</s1></fA11><fA11 i1="05" i2="1"><s1>LETARTE (B.)</s1></fA11><fA11 i1="06" i2="1"><s1>MARTIN (N.)</s1></fA11><fA11 i1="07" i2="1"><s1>COLLINS (M.)</s1></fA11><fA11 i1="08" i2="1"><s1>LEWIS (G. F.)</s1></fA11><fA11 i1="09" i2="1"><s1>MCCONNACHIE (A.)</s1></fA11><fA11 i1="10" i2="1"><s1>PENARRUBIA (J.)</s1></fA11><fA11 i1="11" i2="1"><s1>RICH (R. M.)</s1></fA11><fA11 i1="12" i2="1"><s1>TRETHEWEY (D.)</s1></fA11><fA11 i1="13" i2="1"><s1>FERGUSON (A.)</s1></fA11><fA11 i1="14" i2="1"><s1>HUXOR (A.)</s1></fA11><fA11 i1="15" i2="1"><s1>TANVIR (N.)</s1></fA11><fA14 i1="01"><s1>Institute of Astronomy, Madingley Road</s1><s2>Cambridge CB3 OHA</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ><sZ>7 aut.</sZ><sZ>12 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Physics and Astronomy, University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>9 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="03"><s1>Observatoire de Strasbourg, 11, rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>2 aut.</sZ></fA14><fA14 i1="04"><s1>Department of Physics and Astronomy, University of California</s1><s2>Los Angles, LA California</s2><s3>USA</s3><sZ>4 aut.</sZ><sZ>11 aut.</sZ></fA14><fA14 i1="05"><s1>California Institute of Technology</s1><s2>Pasadena, CA 91125</s2><s3>USA</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>Max-Planck-Institut für Astronomie, Königstuhl 17</s1><s2>69117 Heidelberg</s2><s3>DEU</s3><sZ>6 aut.</sZ></fA14><fA14 i1="07"><s1>Institute of Astronomy, School of Physics, A29, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1><s2>Edinburgh EH9 3HJ</s2><s3>GBR</s3><sZ>13 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="09"><s1>Department of Physics and Astronomy, University of Leicester</s1><s2>Leicester LEI 7RH</s2><s3>GBR</s3><sZ>15 aut.</sZ></fA14><fA20><s1>1437-1452</s1></fA20><fA21><s1>2008</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000185940450130</s5></fA43><fA44><s0>0000</s0><s1>© 2008 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>08-0513603</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>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present a spectroscopic analysis of five stellar streams ('A', 'B', 'Cr', 'Cp' and 'D') as well as the extended star cluster, EC4, which lies within Stream 'C', all discovered in the halo of M31 from our Canada-France-Hawaii Telescope/MegaCam survey. These spectroscopic results were initially serendipitous, making use of our existing observations from the DEep Imaging Multi-Object Spectrograph mounted on the Keck II telescope, and thereby emphasizing the ubiquity of tidal streams that account for ∼70 per cent of the M31 halo stars in the targeted fields. Subsequent spectroscopy was then procured in Stream 'C' and Stream 'D' to trace the velocity gradient along the streams. Nine metal-rich ([Fe/H] ∼ -0.7) stars at v<sub>hel</sub> = -349.5 km s<sup>-1</sup>,σ<sub>v,corr</sub> ∼ 5.1 ± 2.5km s<sup>-1</sup> are proposed as a serendipitous detection of Stream'Cr', with follow-up kinematic identification at a further point along the stream. Seven metal-poor ([Fe/H] ∼-1.3) stars confined to a narrow, 15 km s<sup>-1</sup> velocity bin centred at u<sub>hel</sub> = -285.6, σ<sub>v,corr</sub> = 4.3<sup>+1.7</sup><sub>-1.4</sub> km s<sup>-1</sup> represent a kinematic detection of Stream 'Cp', again with follow-up kinematic identification further along the stream. For the cluster EC4, candidate member stars with average [Fe/H] ∼-1.4, are found at v<sub>hel</sub> = -282 suggesting it could be related to Stream 'Cp'. No similarly obvious cold kinematic candidate is found for Stream 'D', although candidates are proposed in both of two spectroscopic pointings along the stream (both at ∼ -400 km s<sup>-1</sup>). Spectroscopy near the edge of Stream 'B' suggests a likely kinematic detection at v<sub>hel</sub> ∼ -330, σ<sub>v,corr</sub> ∼ 6.9 km s<sup>-1</sup>, while a candidate kinematic detection of Stream 'A' is found (plausibly associated to M33 rather than M31) with v<sub>hel</sub> ∼ -170, σ<sub>v,corr</sub> = 12.5 km s<sup>-1</sup>. The low dispersion of the streams in kinematics, physical thickness and metallicity makes it hard to reconcile with a scenario whereby these stream structures as an ensemble are related to the giant southern stream. We conclude that the M31 stellar halo is largely made up of multiple kinematically cold streams.</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>Amas stellaire</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Star clusters</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Spectrométrie</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Spectroscopy</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Etoile membre</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Member star</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Estrella miembro</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Métallicité</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="ENG"><s0>Metallicity</s0><s5>30</s5></fC03><fC03 i1="05" i2="X" l="SPA"><s0>Metalicidad</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Halo galaxies</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Galaxy halo</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Halo galaxia</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Galaxies</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Galaxies</s0><s5>32</s5></fC03><fN21><s1>336</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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