The remnants of galaxy formation from a panoramic survey of the region around M31
Identifieur interne : 003429 ( PascalFrancis/Curation ); précédent : 003428; suivant : 003430The remnants of galaxy formation from a panoramic survey of the region around M31
Auteurs : Alan W. Mcconnachie [Canada] ; Michael J. Irwin [Royaume-Uni] ; Rodrigo A. Ibata [France] ; John Dubinski [Canada] ; Lawrence M. Widrow [Canada] ; Nicolas F. Martin [Allemagne] ; Patrick Cote [Canada] ; Aaron L. Dotter [Canada] ; Julio F. Navarro [Canada] ; Annette M. N. Ferguson [Royaume-Uni] ; Thomas H. Puzia [Canada] ; Geraint F. Lewis [Australie] ; Arif Babu [Canada] ; Pauline Barmby [Canada] ; Olivier Bienayme [France] ; Scott C. Chapman [Royaume-Uni] ; Robert Cockcroft [Canada] ; Michellel M. Collins [Royaume-Uni] ; Mark A. Fardal [États-Unis] ; William E. Harris [Canada] ; Avon Huxor [Royaume-Uni] ; A. Dougal Mackey [Royaume-Uni] ; Jorge Penarrubia [Royaume-Uni] ; R. Michael Rich [États-Unis] ; Harvey B. Richer [Canada] ; Arnaud Siebert [France] ; Nial Tanvir [Royaume-Uni] ; David Valls-Gabaud [France] ; Kimberly A. Venn [Canada]Source :
- Nature : (London) [ 0028-0836 ] ; 2009.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Cosmologie.
English descriptors
- KwdEn :
Abstract
In hierarchical cosmological models', galaxies grow in mass through the continual accretion of smaller ones. The tidal disruption of these systems is expected to result in loosely bound stars surrounding the galaxy, at distances that reach 10-100 times the radius of the central disk2,3. The number, luminosity and morphology of the relics of this process provide significant clues to galaxy formation history4, but obtaining a comprehensive survey of these components is difficult because of their intrinsic faintness and vast extent. Here we report a panoramic survey of the Andromeda galaxy (M31). We detect stars and coherent structures that are almost certainly remnants of dwarf galaxies destroyed by the tidal field of M31. An improved census of their surviving counterparts implies that three-quarters of M31's satellites brighter than Mv = -6 await discovery. The brightest companion, Triangulum (M33), is surrounded by a stellar structure that provides persuasive evidence for a recent encounter with M31. This panorama of galaxy structure directly confirms the basic tenets of the hierarchical galaxy formation model and reveals the shared history of M31 and M33 in the unceasing build-up of galaxies.
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<author><name sortKey="Rich, R Michael" sort="Rich, R Michael" uniqKey="Rich R" first="R. Michael" last="Rich">R. Michael Rich</name>
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<series><title level="j" type="main">Nature : (London)</title>
<title level="j" type="abbreviated">Nature : (Lond.)</title>
<idno type="ISSN">0028-0836</idno>
<imprint><date when="2009">2009</date>
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<term>Cosmological models</term>
<term>Cosmology</term>
<term>Dwarf galaxies</term>
<term>Galaxy formation</term>
<term>Galaxy structure</term>
<term>Luminosity</term>
<term>Morphology</term>
<term>Stellar structure</term>
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<keywords scheme="Pascal" xml:lang="fr"><term>Formation galaxies</term>
<term>Modèle cosmologique</term>
<term>Galaxies naines</term>
<term>Accrétion</term>
<term>Luminosité</term>
<term>Morphologie</term>
<term>Structure stellaire</term>
<term>Structure galaxies</term>
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<front><div type="abstract" xml:lang="en">In hierarchical cosmological models', galaxies grow in mass through the continual accretion of smaller ones. The tidal disruption of these systems is expected to result in loosely bound stars surrounding the galaxy, at distances that reach 10-100 times the radius of the central disk<sup>2,3</sup>
. The number, luminosity and morphology of the relics of this process provide significant clues to galaxy formation history<sup>4</sup>
, but obtaining a comprehensive survey of these components is difficult because of their intrinsic faintness and vast extent. Here we report a panoramic survey of the Andromeda galaxy (M31). We detect stars and coherent structures that are almost certainly remnants of dwarf galaxies destroyed by the tidal field of M31. An improved census of their surviving counterparts implies that three-quarters of M31's satellites brighter than M<sub>v</sub>
= -6 await discovery. The brightest companion, Triangulum (M33), is surrounded by a stellar structure that provides persuasive evidence for a recent encounter with M31. This panorama of galaxy structure directly confirms the basic tenets of the hierarchical galaxy formation model and reveals the shared history of M31 and M33 in the unceasing build-up of galaxies.</div>
</front>
</TEI>
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<fA05><s2>461</s2>
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<fA06><s2>7260</s2>
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<fA08 i1="01" i2="1" l="ENG"><s1>The remnants of galaxy formation from a panoramic survey of the region around M31</s1>
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<fA11 i1="01" i2="1"><s1>MCCONNACHIE (Alan W.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>IRWIN (Michael J.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>IBATA (Rodrigo A.)</s1>
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<fA11 i1="04" i2="1"><s1>DUBINSKI (John)</s1>
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<fA11 i1="05" i2="1"><s1>WIDROW (Lawrence M.)</s1>
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<fA11 i1="06" i2="1"><s1>MARTIN (Nicolas F.)</s1>
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<fA11 i1="07" i2="1"><s1>COTE (Patrick)</s1>
</fA11>
<fA11 i1="08" i2="1"><s1>DOTTER (Aaron L.)</s1>
</fA11>
<fA11 i1="09" i2="1"><s1>NAVARRO (Julio F.)</s1>
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<fA11 i1="10" i2="1"><s1>FERGUSON (Annette M. N.)</s1>
</fA11>
<fA11 i1="11" i2="1"><s1>PUZIA (Thomas H.)</s1>
</fA11>
<fA11 i1="12" i2="1"><s1>LEWIS (Geraint F.)</s1>
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<fA11 i1="13" i2="1"><s1>BABU (Arif)</s1>
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<fA11 i1="14" i2="1"><s1>BARMBY (Pauline)</s1>
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<fA11 i1="15" i2="1"><s1>BIENAYME (Olivier)</s1>
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<fA11 i1="16" i2="1"><s1>CHAPMAN (Scott C.)</s1>
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<fA11 i1="17" i2="1"><s1>COCKCROFT (Robert)</s1>
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<fA11 i1="18" i2="1"><s1>COLLINS (MichelleL M.)</s1>
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<fA11 i1="19" i2="1"><s1>FARDAL (Mark A.)</s1>
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<fA11 i1="22" i2="1"><s1>MACKEY (A. Dougal)</s1>
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<fA14 i1="05"><s1>Department of Physics, Engineering Physics, and Astronomy Queen's University</s1>
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<fA14 i1="06"><s1>MaxPlanck-Institut für Astronomie, Königstuhl 17</s1>
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<fA14 i1="07"><s1>Department of Physics and Astronomy, University of Victoria, 3800 Finnerty Road</s1>
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<sZ>8 aut.</sZ>
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<fA14 i1="08"><s1>Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill</s1>
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<fA14 i1="10"><s1>Department of Physics and Astronomy, University of Western Ontario, 1151 Richmond Street</s1>
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<sZ>14 aut.</sZ>
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<fA14 i1="11"><s1>Department of Physics and Astronomy, McMaster University</s1>
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<sZ>17 aut.</sZ>
<sZ>20 aut.</sZ>
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<fA14 i1="12"><s1>University of Massachusetts, Department of Astronomy, LGRT 619-E, 710 N. Pleasant Street</s1>
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<sZ>19 aut.</sZ>
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<fA14 i1="13"><s1>Department of Physics (Astrophysics Group), H. H. Wills Physics Laboratory, Tyndall Avenue</s1>
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<sZ>21 aut.</sZ>
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<fA14 i1="14"><s1>Department of Physics and Astronomy, University of California, Los Angeles, PAB, 430 Portola Plaza</s1>
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<sZ>24 aut.</sZ>
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<fA14 i1="15"><s1>Department of Physics and Astronomy, 6224 Agricultural Road, University of British Columbia</s1>
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<s3>CAN</s3>
<sZ>25 aut.</sZ>
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<fA14 i1="16"><s1>Department of Physics and Astronomy, University of Leicester</s1>
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<sZ>27 aut.</sZ>
</fA14>
<fA14 i1="17"><s1>Laboratoire Galaxies et Étoiles, Physique et Instrumentation, CNRS UMR 8111, Observatoire de Paris, 5 Place Jules Janssen</s1>
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<fA64 i1="01" i2="1"><s0>Nature : (London)</s0>
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<fA66 i1="01"><s0>GBR</s0>
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<fC01 i1="01" l="ENG"><s0>In hierarchical cosmological models', galaxies grow in mass through the continual accretion of smaller ones. The tidal disruption of these systems is expected to result in loosely bound stars surrounding the galaxy, at distances that reach 10-100 times the radius of the central disk<sup>2,3</sup>
. The number, luminosity and morphology of the relics of this process provide significant clues to galaxy formation history<sup>4</sup>
, but obtaining a comprehensive survey of these components is difficult because of their intrinsic faintness and vast extent. Here we report a panoramic survey of the Andromeda galaxy (M31). We detect stars and coherent structures that are almost certainly remnants of dwarf galaxies destroyed by the tidal field of M31. An improved census of their surviving counterparts implies that three-quarters of M31's satellites brighter than M<sub>v</sub>
= -6 await discovery. The brightest companion, Triangulum (M33), is surrounded by a stellar structure that provides persuasive evidence for a recent encounter with M31. This panorama of galaxy structure directly confirms the basic tenets of the hierarchical galaxy formation model and reveals the shared history of M31 and M33 in the unceasing build-up of galaxies.</s0>
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<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Galaxy formation</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="3" l="FRE"><s0>Modèle cosmologique</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Cosmological models</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Galaxies naines</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Dwarf galaxies</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Accrétion</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Accretion</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Luminosité</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Luminosity</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Morphologie</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Morphology</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Structure stellaire</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Stellar structure</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Structure galaxies</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Galaxy structure</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Estructura galaxias</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Cosmologie</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Cosmology</s0>
<s5>34</s5>
</fC03>
<fN21><s1>278</s1>
</fN21>
</pA>
</standard>
</inist>
</record>
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