Testing formation mechanisms of the Milky Way's thick disc with RAVE
Identifieur interne : 006318 ( Main/Exploration ); précédent : 006317; suivant : 006319Testing formation mechanisms of the Milky Way's thick disc with RAVE
Auteurs : Michelle L. Wilson [États-Unis] ; Amina Helmi [Pays-Bas, États-Unis] ; Heather L. Morrison [États-Unis] ; Maarten A. Breddels [Pays-Bas] ; O. Bienaymé [France] ; J. Binney ; J. Bland-Hawthorn [Australie] ; R. Campbell [Allemagne, Australie] ; K. C. Freeman [Australie] ; J. P. Fulbright [États-Unis] ; B. K. Gibson ; G. Gilmore [Royaume-Uni] ; E. K. Grebel [Allemagne] ; U. Munari [Italie] ; J. F. Navarro [Canada] ; Q. A. Parker [Australie] ; W. Reid [Australie] ; G. Seabroke [Royaume-Uni] ; A. Siebert [France] ; A. Siviero [Allemagne, Italie] ; M. Steinmetz [Allemagne] ; M. E. K. Williams [Allemagne] ; R. F. G. Wyse [États-Unis] ; T. Zwitter [Slovénie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-05-21.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Simulation.
English descriptors
- KwdEn :
- Absolute magnitude, Absolute magnitudes, Accretion, Accretion model, Accretion scenario, Asymmetric peak, Breddels, Circular orbits, Clump, Clump sample, Clump stars, Contamination, Disc, Disc formation mechanisms figure, Disc galaxy, Disk galaxies, Distance errors, Distance overestimation, Eccentricity, Eccentricity distribution, Eccentricity distributions, Fewer stars, Formation mechanism, Galactic, Galactic centre, Galactic disc, Galaxy, Galaxy formation, Galaxy structure, Giant branch, Halo, Halo stars, Heating model, High eccentricities, High eccentricity, Higher eccentricities, Higher eccentricity, Internal data release, Isochrone, Johns hopkins university, Larger distances, Milky, Milky Way, Minor merger, Mnras, Model star, Models, Monthly notices, Orbits, Original distances, Original distribution, Original sample, Other hand, Outer regions, Padova isochrones, Proper motion errors, Proper motions, Radial migration, Radial velocity, Radial velocity experiment, Rapo rperi, Relative fraction, Scenario, Secondary peak, Simple model, Simulation, Smooth falloff, Solar metallicity, Solar neighborhood, Star, Star accretion, Such stars, Systematic errors, Thick disc, Thick discs, Thin disc, Triangular shape, Velocity dispersions, Velocity distributions, Velocity errors, Velocity values, Villalobos helmi, Younger stars, Zwitter.
- Teeft :
- Absolute magnitude, Absolute magnitudes, Accretion, Accretion model, Accretion scenario, Asymmetric peak, Breddels, Circular orbits, Clump, Clump sample, Clump stars, Contamination, Disc, Disc formation mechanisms figure, Disc galaxy, Distance errors, Distance overestimation, Eccentricity, Eccentricity distribution, Eccentricity distributions, Fewer stars, Galactic, Galactic centre, Galactic disc, Galaxy, Giant branch, Halo, Halo stars, Heating model, High eccentricities, High eccentricity, Higher eccentricities, Higher eccentricity, Internal data release, Isochrone, Johns hopkins university, Larger distances, Milky, Minor merger, Mnras, Model star, Monthly notices, Original distances, Original distribution, Original sample, Other hand, Outer regions, Padova isochrones, Proper motion errors, Proper motions, Radial migration, Radial velocity experiment, Rapo rperi, Relative fraction, Scenario, Secondary peak, Simple model, Simulation, Smooth falloff, Solar metallicity, Star, Such stars, Systematic errors, Thick disc, Thick discs, Thin disc, Triangular shape, Velocity dispersions, Velocity distributions, Velocity errors, Velocity values, Villalobos helmi, Younger stars, Zwitter.
Abstract
We study the eccentricity distribution of a thick‐disc sample of stars (defined as those with Vy > 50 km s−1 and 1 < |z|/kpc < 3) observed in the Radial Velocity Experiment (RAVE). We compare this distribution with those obtained in four simulations of galaxy formation taken from the literature as compiled by Sales et al. Each simulation emphasizes different scenarios for the origin of such stars (satellite accretion, heating of a pre‐existing thin disc during a merger, radial migration, and gas‐rich mergers). We find that the observed distribution peaks at low eccentricities and falls off smoothly and rather steeply to high eccentricities. This finding is fairly robust to changes in distances and to plausible assumptions about thin‐disc contamination. Our results favour models where the majority of stars formed in the Galaxy itself on orbits of modest eccentricity and disfavour the pure satellite accretion case. A gas‐rich merger origin where most of the stars form ‘in situ’ appears to be the most consistent with our data.
Url:
DOI: 10.1111/j.1365-2966.2011.18298.x
Affiliations:
- Allemagne, Australie, Canada, France, Italie, Pays-Bas, Royaume-Uni, Slovénie, États-Unis
- Alsace (région administrative), Angleterre, Angleterre de l'Est, Bade-Wurtemberg, District de Karlsruhe, Grand Est, Grand Londres, Maryland, Nouvelle-Galles du Sud, Ohio
- Cambridge, Heidelberg, Londres, Strasbourg, Sydney
- University College de Londres, Université de Cambridge, Université de Strasbourg
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Le document en format XML
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Siebert</name><affiliation wicri:level="4"><country xml:lang="fr">France</country><wicri:regionArea>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg</wicri:regionArea><placeName><settlement type="city">Strasbourg</settlement><region type="region" nuts="2">Grand Est</region><region type="old region" nuts="2">Alsace (région administrative)</region><settlement type="city">Strasbourg</settlement></placeName><orgName type="university">Université de Strasbourg</orgName></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam</wicri:regionArea><wicri:noRegion>14482 Potsdam</wicri:noRegion><wicri:noRegion>14482 Potsdam</wicri:noRegion></affiliation><affiliation wicri:level="1"><country xml:lang="fr">Italie</country><wicri:regionArea>INAF Astronomical Observatory of Padova, 36012 Asiago</wicri:regionArea><wicri:noRegion>36012 Asiago</wicri:noRegion></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam</wicri:regionArea><wicri:noRegion>14482 Potsdam</wicri:noRegion><wicri:noRegion>14482 Potsdam</wicri:noRegion></affiliation></author><author><name sortKey="Williams, M E K" sort="Williams, M E K" uniqKey="Williams M" first="M. E. K." last="Williams">M. E. K. Williams</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam</wicri:regionArea><wicri:noRegion>14482 Potsdam</wicri:noRegion><wicri:noRegion>14482 Potsdam</wicri:noRegion></affiliation></author><author><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. 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centre</term><term>Galactic disc</term><term>Galaxy</term><term>Galaxy formation</term><term>Galaxy structure</term><term>Giant branch</term><term>Halo</term><term>Halo stars</term><term>Heating model</term><term>High eccentricities</term><term>High eccentricity</term><term>Higher eccentricities</term><term>Higher eccentricity</term><term>Internal data release</term><term>Isochrone</term><term>Johns hopkins university</term><term>Larger distances</term><term>Milky</term><term>Milky Way</term><term>Minor merger</term><term>Mnras</term><term>Model star</term><term>Models</term><term>Monthly notices</term><term>Orbits</term><term>Original distances</term><term>Original distribution</term><term>Original sample</term><term>Other hand</term><term>Outer regions</term><term>Padova isochrones</term><term>Proper motion errors</term><term>Proper motions</term><term>Radial migration</term><term>Radial velocity</term><term>Radial velocity experiment</term><term>Rapo rperi</term><term>Relative fraction</term><term>Scenario</term><term>Secondary peak</term><term>Simple model</term><term>Simulation</term><term>Smooth falloff</term><term>Solar metallicity</term><term>Solar neighborhood</term><term>Star</term><term>Star accretion</term><term>Such stars</term><term>Systematic errors</term><term>Thick disc</term><term>Thick discs</term><term>Thin disc</term><term>Triangular shape</term><term>Velocity dispersions</term><term>Velocity distributions</term><term>Velocity errors</term><term>Velocity values</term><term>Villalobos helmi</term><term>Younger stars</term><term>Zwitter</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Accrétion stellaire</term><term>Excentricité</term><term>Formation galaxies</term><term>Galaxies disques</term><term>Modèle</term><term>Mécanisme formation</term><term>Orbite</term><term>Structure galaxies</term><term>Vitesse radiale</term><term>Voie lactée</term><term>Voisinage solaire</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitude</term><term>Absolute magnitudes</term><term>Accretion</term><term>Accretion model</term><term>Accretion scenario</term><term>Asymmetric peak</term><term>Breddels</term><term>Circular orbits</term><term>Clump</term><term>Clump sample</term><term>Clump stars</term><term>Contamination</term><term>Disc</term><term>Disc formation mechanisms figure</term><term>Disc galaxy</term><term>Distance errors</term><term>Distance overestimation</term><term>Eccentricity</term><term>Eccentricity distribution</term><term>Eccentricity distributions</term><term>Fewer stars</term><term>Galactic</term><term>Galactic centre</term><term>Galactic disc</term><term>Galaxy</term><term>Giant branch</term><term>Halo</term><term>Halo stars</term><term>Heating model</term><term>High eccentricities</term><term>High eccentricity</term><term>Higher eccentricities</term><term>Higher eccentricity</term><term>Internal data release</term><term>Isochrone</term><term>Johns hopkins university</term><term>Larger distances</term><term>Milky</term><term>Minor merger</term><term>Mnras</term><term>Model star</term><term>Monthly notices</term><term>Original distances</term><term>Original distribution</term><term>Original sample</term><term>Other hand</term><term>Outer regions</term><term>Padova isochrones</term><term>Proper motion errors</term><term>Proper motions</term><term>Radial migration</term><term>Radial velocity experiment</term><term>Rapo rperi</term><term>Relative fraction</term><term>Scenario</term><term>Secondary peak</term><term>Simple model</term><term>Simulation</term><term>Smooth falloff</term><term>Solar metallicity</term><term>Star</term><term>Such stars</term><term>Systematic errors</term><term>Thick disc</term><term>Thick discs</term><term>Thin disc</term><term>Triangular shape</term><term>Velocity dispersions</term><term>Velocity distributions</term><term>Velocity errors</term><term>Velocity values</term><term>Villalobos helmi</term><term>Younger stars</term><term>Zwitter</term></keywords><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Simulation</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We study the eccentricity distribution of a thick‐disc sample of stars (defined as those with Vy > 50 km s−1 and 1 < |z|/kpc < 3) observed in the Radial Velocity Experiment (RAVE). We compare this distribution with those obtained in four simulations of galaxy formation taken from the literature as compiled by Sales et al. Each simulation emphasizes different scenarios for the origin of such stars (satellite accretion, heating of a pre‐existing thin disc during a merger, radial migration, and gas‐rich mergers). We find that the observed distribution peaks at low eccentricities and falls off smoothly and rather steeply to high eccentricities. This finding is fairly robust to changes in distances and to plausible assumptions about thin‐disc contamination. Our results favour models where the majority of stars formed in the Galaxy itself on orbits of modest eccentricity and disfavour the pure satellite accretion case. A gas‐rich merger origin where most of the stars form ‘in situ’ appears to be the most consistent with our data.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>Canada</li><li>France</li><li>Italie</li><li>Pays-Bas</li><li>Royaume-Uni</li><li>Slovénie</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Angleterre</li><li>Angleterre de l'Est</li><li>Bade-Wurtemberg</li><li>District de Karlsruhe</li><li>Grand Est</li><li>Grand Londres</li><li>Maryland</li><li>Nouvelle-Galles du Sud</li><li>Ohio</li></region><settlement><li>Cambridge</li><li>Heidelberg</li><li>Londres</li><li>Strasbourg</li><li>Sydney</li></settlement><orgName><li>University College de Londres</li><li>Université de Cambridge</li><li>Université de Strasbourg</li></orgName></list><tree><noCountry><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><name sortKey="Gibson, B K" sort="Gibson, B K" uniqKey="Gibson B" first="B. K." last="Gibson">B. K. Gibson</name></noCountry><country name="États-Unis"><region name="Ohio"><name sortKey="Wilson, Michelle L" sort="Wilson, Michelle L" uniqKey="Wilson M" first="Michelle L." last="Wilson">Michelle L. Wilson</name></region><name sortKey="Fulbright, J P" sort="Fulbright, J P" uniqKey="Fulbright J" first="J. P." last="Fulbright">J. P. Fulbright</name><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><name sortKey="Morrison, Heather L" sort="Morrison, Heather L" uniqKey="Morrison H" first="Heather L." last="Morrison">Heather L. Morrison</name><name sortKey="Wilson, Michelle L" sort="Wilson, Michelle L" uniqKey="Wilson M" first="Michelle L." last="Wilson">Michelle L. Wilson</name><name sortKey="Wyse, R F G" sort="Wyse, R F G" uniqKey="Wyse R" first="R. F. G." last="Wyse">R. F. G. Wyse</name></country><country name="Pays-Bas"><noRegion><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name></noRegion><name sortKey="Breddels, Maarten A" sort="Breddels, Maarten A" uniqKey="Breddels M" first="Maarten A." last="Breddels">Maarten A. Breddels</name></country><country name="France"><region name="Grand Est"><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienaymé">O. Bienaymé</name></region><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name></country><country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Bland Awthorn, J" sort="Bland Awthorn, J" uniqKey="Bland Awthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name></region><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><name sortKey="Reid, W" sort="Reid, W" uniqKey="Reid W" first="W." last="Reid">W. Reid</name></country><country name="Allemagne"><noRegion><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name></noRegion><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><name sortKey="Williams, M E K" sort="Williams, M E K" uniqKey="Williams M" first="M. E. K." last="Williams">M. E. K. Williams</name></country><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name></region><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name></country><country name="Italie"><noRegion><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name></noRegion><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name></country><country name="Canada"><noRegion><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name></noRegion></country><country name="Slovénie"><noRegion><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name></noRegion><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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