THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM
Identifieur interne : 004A88 ( PascalFrancis/Curation ); précédent : 004A87; suivant : 004A89THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM
Auteurs : Ryan Leaman [Canada] ; Kim A. Venn [Canada] ; Alyson M. Brooks [États-Unis] ; Giuseppina Battaglia [Allemagne] ; Andrew A. Cole [Australie] ; Rodrigo A. Ibata [France] ; Mike J. Irwin [Royaume-Uni] ; Alan W. Mcconnachie [Canada] ; J. Trevor Mendel [Canada] ; Eline Tolstoy [Pays-Bas]Source :
- The Astrophysical journal [ 0004-637X ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Dynamique, Galaxies naines, Géante rouge, Etoile géante, Galaxies irrégulières, Triplet, Deimos, Métallicité, Age, Population stellaire, Rotation stellaire, Alignement, Cinématique, Courbe rotation, Dispersion vitesse, Nuage moléculaire géant, Sous structure, Boucle réaction, Groupe local, Groupe galaxies, Formation stellaire, Evolution dynamique, Abondance, Evolution galaxies, Satellite Mars.
English descriptors
- KwdEn :
- Abundance, Age, Alignment, Deimos, Dwarf galaxies, Dynamical evolution, Dynamics, Feedback, Galaxy evolution, Galaxy groups, Giant molecular cloud, Giant stars, Irregular galaxies, Kinematics, Local group, Mars satellite, Metallicity, Red giant stars, Rotation curve, Star formation, Stellar population, Stellar rotation, Substructure, Triplets, Velocity dispersion.
Abstract
We present spectroscopic data for 180 red giant branch (RGB) stars in the isolated dwarf irregular galaxy Wolf-Lundmark-Mellote (WLM). Observations of the calcium II triplet lines in spectra of RGB stars covering the entire galaxy were obtained with FORS2 at the Very Large Telescope and DEIMOS on Keck II, allowing us to derive velocities, metallicities, and ages for the stars. With accompanying photometric and radio data we have measured the structural parameters of the stellar and gaseous populations over the full galaxy. The stellar populations show an intrinsically thick configuration with 0.39 ≤ q0 ≤ 0.57. The stellar rotation in WLM is measured to be 17±1 km s-1; however, the ratio of rotation to pressure support for the stars is V/σ ∼ 1, in contrast to the gas, whose ratio is seven times larger. This, along with the structural data and alignment of the kinematic and photometric axes, suggests we are viewing WLM as a highly inclined oblate spheroid. Stellar rotation curves, corrected for asymmetric drift, are used to compute a dynamical mass of (4.3 ± 0.3) x 108 M◦. at the half-light radius (rh = 1656 ± 49 pc). The stellar velocity dispersion increases with stellar age in a manner consistent with giant molecular cloud and substructure interactions producing the heating in WLM. Coupled with WLM's isolation, this suggests that the extended vertical structure of its stellar and gaseous components and increase in stellar velocity dispersion with age are due to internal feedback, rather than tidally driven evolution. These represent some of the first observational results from an isolated Local Group dwarf galaxy that can offer important constraints on how strongly internal feedback and secular processes modulate star formation and dynamical evolution in low-mass isolated objects.
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<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM</title><author><name sortKey="Leaman, Ryan" sort="Leaman, Ryan" uniqKey="Leaman R" first="Ryan" last="Leaman">Ryan Leaman</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Venn, Kim A" sort="Venn, Kim A" uniqKey="Venn K" first="Kim A." last="Venn">Kim A. Venn</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. 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CA 91125</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Battaglia, Giuseppina" sort="Battaglia, Giuseppina" uniqKey="Battaglia G" first="Giuseppina" last="Battaglia">Giuseppina Battaglia</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>European Southern Observatory, Karl-Schwarzschild-Strasse 2</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>4 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Cole, Andrew A" sort="Cole, Andrew A" uniqKey="Cole A" first="Andrew A." last="Cole">Andrew A. Cole</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>School of Mathematics & Physics, University of Tasmania, Private Bag 37</s1><s2>Hobart, TAS</s2><s3>AUS</s3><sZ>5 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. 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BC V9E 2E7</s2><s3>CAN</s3><sZ>8 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Trevor Mendel, J" sort="Trevor Mendel, J" uniqKey="Trevor Mendel J" first="J." last="Trevor Mendel">J. Trevor Mendel</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Tolstoy, Eline" sort="Tolstoy, Eline" uniqKey="Tolstoy E" first="Eline" last="Tolstoy">Eline Tolstoy</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Kapteyn Institute, University of Groningen, Postbus 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>10 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">12-0195455</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 12-0195455 INIST</idno><idno type="RBID">Pascal:12-0195455</idno><idno type="wicri:Area/PascalFrancis/Corpus">001425</idno><idno type="wicri:Area/PascalFrancis/Curation">004A88</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM</title><author><name sortKey="Leaman, Ryan" sort="Leaman, Ryan" uniqKey="Leaman R" first="Ryan" last="Leaman">Ryan Leaman</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Venn, Kim A" sort="Venn, Kim A" uniqKey="Venn K" first="Kim A." last="Venn">Kim A. Venn</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Brooks, Alyson M" sort="Brooks, Alyson M" uniqKey="Brooks A" first="Alyson M." last="Brooks">Alyson M. Brooks</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>California Institute of Technology, M/C 350-17</s1><s2>Pasadena. CA 91125</s2><s3>USA</s3><sZ>3 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Battaglia, Giuseppina" sort="Battaglia, Giuseppina" uniqKey="Battaglia G" first="Giuseppina" last="Battaglia">Giuseppina Battaglia</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>European Southern Observatory, Karl-Schwarzschild-Strasse 2</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>4 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Cole, Andrew A" sort="Cole, Andrew A" uniqKey="Cole A" first="Andrew A." last="Cole">Andrew A. Cole</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>School of Mathematics & Physics, University of Tasmania, Private Bag 37</s1><s2>Hobart, TAS</s2><s3>AUS</s3><sZ>5 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. Ibata</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Observatoire Astronomique. Universite de Strasbourg. CNRS. 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Irwin, Mike J" sort="Irwin, Mike J" uniqKey="Irwin M" first="Mike J." last="Irwin">Mike J. Irwin</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>7 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Mcconnachie, Alan W" sort="Mcconnachie, Alan W" uniqKey="Mcconnachie A" first="Alan W." last="Mcconnachie">Alan W. Mcconnachie</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>NRC Herzberg Institute of Astrophysics. 5071 West Saanich Road</s1><s2>Victoria. BC V9E 2E7</s2><s3>CAN</s3><sZ>8 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Trevor Mendel, J" sort="Trevor Mendel, J" uniqKey="Trevor Mendel J" first="J." last="Trevor Mendel">J. Trevor Mendel</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Tolstoy, Eline" sort="Tolstoy, Eline" uniqKey="Tolstoy E" first="Eline" last="Tolstoy">Eline Tolstoy</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Kapteyn Institute, University of Groningen, Postbus 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>10 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author></analytic><series><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">The Astrophysical journal</title><title level="j" type="abbreviated">Astrophys. j.</title><idno type="ISSN">0004-637X</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance</term><term>Age</term><term>Alignment</term><term>Deimos</term><term>Dwarf galaxies</term><term>Dynamical evolution</term><term>Dynamics</term><term>Feedback</term><term>Galaxy evolution</term><term>Galaxy groups</term><term>Giant molecular cloud</term><term>Giant stars</term><term>Irregular galaxies</term><term>Kinematics</term><term>Local group</term><term>Mars satellite</term><term>Metallicity</term><term>Red giant stars</term><term>Rotation curve</term><term>Star formation</term><term>Stellar population</term><term>Stellar rotation</term><term>Substructure</term><term>Triplets</term><term>Velocity dispersion</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Dynamique</term><term>Galaxies naines</term><term>Géante rouge</term><term>Etoile géante</term><term>Galaxies irrégulières</term><term>Triplet</term><term>Deimos</term><term>Métallicité</term><term>Age</term><term>Population stellaire</term><term>Rotation stellaire</term><term>Alignement</term><term>Cinématique</term><term>Courbe rotation</term><term>Dispersion vitesse</term><term>Nuage moléculaire géant</term><term>Sous structure</term><term>Boucle réaction</term><term>Groupe local</term><term>Groupe galaxies</term><term>Formation stellaire</term><term>Evolution dynamique</term><term>Abondance</term><term>Evolution galaxies</term><term>Satellite Mars</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present spectroscopic data for 180 red giant branch (RGB) stars in the isolated dwarf irregular galaxy Wolf-Lundmark-Mellote (WLM). Observations of the calcium II triplet lines in spectra of RGB stars covering the entire galaxy were obtained with FORS2 at the Very Large Telescope and DEIMOS on Keck II, allowing us to derive velocities, metallicities, and ages for the stars. With accompanying photometric and radio data we have measured the structural parameters of the stellar and gaseous populations over the full galaxy. The stellar populations show an intrinsically thick configuration with 0.39 ≤ <sub>q0</sub> ≤ 0.57. The stellar rotation in WLM is measured to be 17±1 km s<sup>-1</sup>; however, the ratio of rotation to pressure support for the stars is V/σ ∼ 1, in contrast to the gas, whose ratio is seven times larger. This, along with the structural data and alignment of the kinematic and photometric axes, suggests we are viewing WLM as a highly inclined oblate spheroid. Stellar rotation curves, corrected for asymmetric drift, are used to compute a dynamical mass of (4.3 ± 0.3) x 10<sup>8</sup> M<sub>◦.</sub> at the half-light radius (r<sub>h</sub> = 1656 ± 49 pc). The stellar velocity dispersion increases with stellar age in a manner consistent with giant molecular cloud and substructure interactions producing the heating in WLM. Coupled with WLM's isolation, this suggests that the extended vertical structure of its stellar and gaseous components and increase in stellar velocity dispersion with age are due to internal feedback, rather than tidally driven evolution. These represent some of the first observational results from an isolated Local Group dwarf galaxy that can offer important constraints on how strongly internal feedback and secular processes modulate star formation and dynamical evolution in low-mass isolated objects.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0></fA01><fA02 i1="01"><s0>ASJOAB</s0></fA02><fA03 i2="1"><s0>Astrophys. j.</s0></fA03><fA05><s2>750</s2></fA05><fA06><s2>1</s2><s3>p. 1</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM</s1></fA08><fA11 i1="01" i2="1"><s1>LEAMAN (Ryan)</s1></fA11><fA11 i1="02" i2="1"><s1>VENN (Kim A.)</s1></fA11><fA11 i1="03" i2="1"><s1>BROOKS (Alyson M.)</s1></fA11><fA11 i1="04" i2="1"><s1>BATTAGLIA (Giuseppina)</s1></fA11><fA11 i1="05" i2="1"><s1>COLE (Andrew A.)</s1></fA11><fA11 i1="06" i2="1"><s1>IBATA (Rodrigo A.)</s1></fA11><fA11 i1="07" i2="1"><s1>IRWIN (Mike J.)</s1></fA11><fA11 i1="08" i2="1"><s1>MCCONNACHIE (Alan W.)</s1></fA11><fA11 i1="09" i2="1"><s1>TREVOR MENDEL (J.)</s1></fA11><fA11 i1="10" i2="1"><s1>TOLSTOY (Eline)</s1></fA11><fA14 i1="01"><s1>Department of Physics and Astronomy. University of Victoria</s1><s2>Victoria, BC V8P 1A1</s2><s3>CAN</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="02"><s1>California Institute of Technology, M/C 350-17</s1><s2>Pasadena. CA 91125</s2><s3>USA</s3><sZ>3 aut.</sZ></fA14><fA14 i1="03"><s1>European Southern Observatory, Karl-Schwarzschild-Strasse 2</s1><s2>85748 Garching</s2><s3>DEU</s3><sZ>4 aut.</sZ></fA14><fA14 i1="04"><s1>School of Mathematics & Physics, University of Tasmania, Private Bag 37</s1><s2>Hobart, TAS</s2><s3>AUS</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Observatoire Astronomique. Universite de Strasbourg. CNRS. 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="06"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>7 aut.</sZ></fA14><fA14 i1="07"><s1>NRC Herzberg Institute of Astrophysics. 5071 West Saanich Road</s1><s2>Victoria. BC V9E 2E7</s2><s3>CAN</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Kapteyn Institute, University of Groningen, Postbus 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>10 aut.</sZ></fA14><fA20><s2>33.1-33.20</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>512</s2><s5>354000509828920330</s5></fA43><fA44><s0>0000</s0><s1>© 2012 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>12-0195455</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present spectroscopic data for 180 red giant branch (RGB) stars in the isolated dwarf irregular galaxy Wolf-Lundmark-Mellote (WLM). Observations of the calcium II triplet lines in spectra of RGB stars covering the entire galaxy were obtained with FORS2 at the Very Large Telescope and DEIMOS on Keck II, allowing us to derive velocities, metallicities, and ages for the stars. With accompanying photometric and radio data we have measured the structural parameters of the stellar and gaseous populations over the full galaxy. The stellar populations show an intrinsically thick configuration with 0.39 ≤ <sub>q0</sub> ≤ 0.57. The stellar rotation in WLM is measured to be 17±1 km s<sup>-1</sup>; however, the ratio of rotation to pressure support for the stars is V/σ ∼ 1, in contrast to the gas, whose ratio is seven times larger. This, along with the structural data and alignment of the kinematic and photometric axes, suggests we are viewing WLM as a highly inclined oblate spheroid. Stellar rotation curves, corrected for asymmetric drift, are used to compute a dynamical mass of (4.3 ± 0.3) x 10<sup>8</sup> M<sub>◦.</sub> at the half-light radius (r<sub>h</sub> = 1656 ± 49 pc). The stellar velocity dispersion increases with stellar age in a manner consistent with giant molecular cloud and substructure interactions producing the heating in WLM. Coupled with WLM's isolation, this suggests that the extended vertical structure of its stellar and gaseous components and increase in stellar velocity dispersion with age are due to internal feedback, rather than tidally driven evolution. These represent some of the first observational results from an isolated Local Group dwarf galaxy that can offer important constraints on how strongly internal feedback and secular processes modulate star formation and dynamical evolution in low-mass isolated objects.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Dynamique</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Dynamics</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Galaxies naines</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Dwarf galaxies</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Géante rouge</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Red giant stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Etoile géante</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Giant stars</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Galaxies irrégulières</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Irregular galaxies</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Triplet</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Triplets</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Deimos</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Deimos</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Métallicité</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Metallicity</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Metalicidad</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Age</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Age</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Edad</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Population stellaire</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Stellar population</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Población estelar</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Rotation stellaire</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Stellar rotation</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Alignement</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Alignment</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Cinématique</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Kinematics</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Courbe rotation</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Rotation curve</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Curva rotación</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Dispersion vitesse</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Velocity dispersion</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Dispersión velocidad</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Nuage moléculaire géant</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Giant molecular cloud</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Nube molecular gigante</s0><s5>41</s5></fC03><fC03 i1="17" i2="X" l="FRE"><s0>Sous structure</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="ENG"><s0>Substructure</s0><s5>42</s5></fC03><fC03 i1="17" i2="X" l="SPA"><s0>Subestructura</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Boucle réaction</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Feedback</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Groupe local</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Local group</s0><s5>44</s5></fC03><fC03 i1="20" i2="3" l="FRE"><s0>Groupe galaxies</s0><s5>45</s5></fC03><fC03 i1="20" i2="3" l="ENG"><s0>Galaxy groups</s0><s5>45</s5></fC03><fC03 i1="21" i2="3" l="FRE"><s0>Formation stellaire</s0><s5>46</s5></fC03><fC03 i1="21" i2="3" l="ENG"><s0>Star formation</s0><s5>46</s5></fC03><fC03 i1="22" i2="X" l="FRE"><s0>Evolution dynamique</s0><s5>47</s5></fC03><fC03 i1="22" i2="X" l="ENG"><s0>Dynamical evolution</s0><s5>47</s5></fC03><fC03 i1="22" i2="X" l="SPA"><s0>Evolución dinámica</s0><s5>47</s5></fC03><fC03 i1="23" i2="3" l="FRE"><s0>Abondance</s0><s5>48</s5></fC03><fC03 i1="23" i2="3" l="ENG"><s0>Abundance</s0><s5>48</s5></fC03><fC03 i1="24" i2="X" l="FRE"><s0>Evolution galaxies</s0><s5>49</s5></fC03><fC03 i1="24" i2="X" l="ENG"><s0>Galaxy evolution</s0><s5>49</s5></fC03><fC03 i1="24" i2="X" l="SPA"><s0>Evolución galaxias</s0><s5>49</s5></fC03><fC03 i1="25" i2="X" l="FRE"><s0>Satellite Mars</s0><s5>50</s5></fC03><fC03 i1="25" i2="X" l="ENG"><s0>Mars satellite</s0><s5>50</s5></fC03><fC03 i1="25" i2="X" l="SPA"><s0>Satélite Marte</s0><s5>50</s5></fC03><fN21><s1>149</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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|texte= THE RESOLVED STRUCTURE AND DYNAMICS OF AN ISOLATED DWARF GALAXY: A VLT AND KECK SPECTROSCOPIC SURVEY OF WLM
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