Testing formation mechanisms of the Milky Way's thick disc with RAVE
Identifieur interne : 001395 ( Istex/Corpus ); précédent : 001394; suivant : 001396Testing formation mechanisms of the Milky Way's thick disc with RAVE
Auteurs : Michelle L. Wilson ; Amina Helmi ; Heather L. Morrison ; Maarten A. Breddels ; O. Bienaymé ; J. Binney ; J. Bland-Hawthorn ; R. Campbell ; K. C. Freeman ; J. P. Fulbright ; B. K. Gibson ; G. Gilmore ; E. K. Grebel ; U. Munari ; J. F. Navarro ; Q. A. Parker ; W. Reid ; G. Seabroke ; A. Siebert ; A. Siviero ; M. Steinmetz ; M. E. K. Williams ; R. F. G. Wyse ; T. ZwitterSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-05-21.
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, 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.
- 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
Links to Exploration step
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Wilson</name><affiliation><mods:affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mlw36@case.edu</mods:affiliation></affiliation></author><author><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><affiliation><mods:affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mlw36@case.edu</mods:affiliation></affiliation></author><author><name sortKey="Morrison, Heather L" sort="Morrison, Heather L" uniqKey="Morrison H" first="Heather L." last="Morrison">Heather L. 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Navarro</name><affiliation><mods:affiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC V8W 3P6, Canada</mods:affiliation></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Reid, W" sort="Reid, W" uniqKey="Reid W" first="W." last="Reid">W. Reid</name><affiliation><mods:affiliation>Macquary University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. 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Steinmetz</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></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><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></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. Wyse</name><affiliation><mods:affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><mods:affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Slovenia</mods:affiliation></affiliation><affiliation><mods:affiliation>Center of excellence SPACE‐SI, Ljubljana, Slovenia</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088</idno><date when="2011" year="2011">2011</date><idno type="doi">10.1111/j.1365-2966.2011.18298.x</idno><idno type="url">https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001395</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001395</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">Testing formation mechanisms of the Milky Way's thick disc with RAVE</title><author><name sortKey="Wilson, Michelle L" sort="Wilson, Michelle L" uniqKey="Wilson M" first="Michelle L." last="Wilson">Michelle L. Wilson</name><affiliation><mods:affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mlw36@case.edu</mods:affiliation></affiliation></author><author><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><affiliation><mods:affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: mlw36@case.edu</mods:affiliation></affiliation></author><author><name sortKey="Morrison, Heather L" sort="Morrison, Heather L" uniqKey="Morrison H" first="Heather L." last="Morrison">Heather L. Morrison</name><affiliation><mods:affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</mods:affiliation></affiliation></author><author><name sortKey="Breddels, Maarten A" sort="Breddels, Maarten A" uniqKey="Breddels M" first="Maarten A." last="Breddels">Maarten A. Breddels</name><affiliation><mods:affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienaymé">O. Bienaymé</name><affiliation><mods:affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</mods:affiliation></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><mods:affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford OX1 3NP</mods:affiliation></affiliation></author><author><name sortKey="Bland Awthorn, J" sort="Bland Awthorn, J" uniqKey="Bland Awthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name><affiliation><mods:affiliation>RSAA Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</mods:affiliation></affiliation></author><author><name sortKey="Fulbright, J P" sort="Fulbright, J P" uniqKey="Fulbright J" first="J. P." last="Fulbright">J. P. Fulbright</name><affiliation><mods:affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author><author><name sortKey="Gibson, B K" sort="Gibson, B K" uniqKey="Gibson B" first="B. K." last="Gibson">B. K. Gibson</name><affiliation><mods:affiliation>Jeremiah Horrocks Institute for Astrophysics & Supercomputing, University of Central Lancashire, Preston PR1 2HE</mods:affiliation></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name><affiliation><mods:affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, D‐69120 Heidelberg, Germany</mods:affiliation></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><mods:affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</mods:affiliation></affiliation></author><author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name><affiliation><mods:affiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC V8W 3P6, Canada</mods:affiliation></affiliation></author><author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Reid, W" sort="Reid, W" uniqKey="Reid W" first="W." last="Reid">W. Reid</name><affiliation><mods:affiliation>Macquary University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name><affiliation><mods:affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT</mods:affiliation></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><mods:affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</mods:affiliation></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</mods:affiliation></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></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><mods:affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</mods:affiliation></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. Wyse</name><affiliation><mods:affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><mods:affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Slovenia</mods:affiliation></affiliation><affiliation><mods:affiliation>Center of excellence SPACE‐SI, Ljubljana, Slovenia</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">413</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="2235">2235</biblScope><biblScope unit="page" to="2241">2241</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-05-21">2011-05-21</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" 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="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></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><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>eccentricity distribution</json:string><json:string>thick disc</json:string><json:string>isochrone</json:string><json:string>mnras</json:string><json:string>breddels</json:string><json:string>eccentricity distributions</json:string><json:string>eccentricity</json:string><json:string>clump stars</json:string><json:string>zwitter</json:string><json:string>high eccentricities</json:string><json:string>velocity distributions</json:string><json:string>monthly notices</json:string><json:string>thin disc</json:string><json:string>scenario</json:string><json:string>radial migration</json:string><json:string>simulation</json:string><json:string>clump sample</json:string><json:string>triangular shape</json:string><json:string>high eccentricity</json:string><json:string>galactic</json:string><json:string>disc</json:string><json:string>padova isochrones</json:string><json:string>giant branch</json:string><json:string>velocity dispersions</json:string><json:string>distance overestimation</json:string><json:string>accretion model</json:string><json:string>younger stars</json:string><json:string>villalobos helmi</json:string><json:string>higher eccentricities</json:string><json:string>galaxy</json:string><json:string>accretion</json:string><json:string>milky</json:string><json:string>larger distances</json:string><json:string>absolute magnitude</json:string><json:string>distance errors</json:string><json:string>proper motion errors</json:string><json:string>internal data release</json:string><json:string>outer regions</json:string><json:string>disc formation mechanisms figure</json:string><json:string>absolute magnitudes</json:string><json:string>accretion scenario</json:string><json:string>galactic disc</json:string><json:string>minor merger</json:string><json:string>thick discs</json:string><json:string>galactic centre</json:string><json:string>velocity values</json:string><json:string>velocity errors</json:string><json:string>rapo rperi</json:string><json:string>asymmetric peak</json:string><json:string>smooth falloff</json:string><json:string>disc galaxy</json:string><json:string>systematic errors</json:string><json:string>secondary peak</json:string><json:string>proper motions</json:string><json:string>higher eccentricity</json:string><json:string>other hand</json:string><json:string>original distances</json:string><json:string>original distribution</json:string><json:string>such stars</json:string><json:string>radial velocity experiment</json:string><json:string>circular orbits</json:string><json:string>simple model</json:string><json:string>johns hopkins university</json:string><json:string>solar metallicity</json:string><json:string>relative fraction</json:string><json:string>fewer stars</json:string><json:string>original sample</json:string><json:string>halo stars</json:string><json:string>model star</json:string><json:string>heating model</json:string><json:string>halo</json:string><json:string>contamination</json:string><json:string>clump</json:string><json:string>star</json:string></teeft></keywords><author><json:item><name>Michelle L. Wilson</name><affiliations><json:string>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</json:string><json:string>E-mail: mlw36@case.edu</json:string></affiliations></json:item><json:item><name>Amina Helmi</name><affiliations><json:string>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</json:string><json:string>E-mail: mlw36@case.edu</json:string></affiliations></json:item><json:item><name>Heather L. Morrison</name><affiliations><json:string>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</json:string></affiliations></json:item><json:item><name>Maarten A. Breddels</name><affiliations><json:string>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</json:string></affiliations></json:item><json:item><name>O. Bienaymé</name><affiliations><json:string>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>J. Binney</name><affiliations><json:string>Rudolf Peierls Centre for Theoretical Physics, Oxford OX1 3NP</json:string></affiliations></json:item><json:item><name>J. Bland‐Hawthorn</name><affiliations><json:string>Anglo‐Australian Observatory, Sydney, Australia</json:string></affiliations></json:item><json:item><name>R. Campbell</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</json:string><json:string>Macquary University, Sydney, NSW 2109, Australia</json:string></affiliations></json:item><json:item><name>K. C. Freeman</name><affiliations><json:string>RSAA Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</json:string></affiliations></json:item><json:item><name>J. P. Fulbright</name><affiliations><json:string>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</json:string></affiliations></json:item><json:item><name>B. K. Gibson</name><affiliations><json:string>Jeremiah Horrocks Institute for Astrophysics & Supercomputing, University of Central Lancashire, Preston PR1 2HE</json:string></affiliations></json:item><json:item><name>G. Gilmore</name><affiliations><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>E. K. Grebel</name><affiliations><json:string>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, D‐69120 Heidelberg, Germany</json:string></affiliations></json:item><json:item><name>U. Munari</name><affiliations><json:string>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</json:string></affiliations></json:item><json:item><name>J. F. Navarro</name><affiliations><json:string>University of Victoria, PO Box 3055, Station CSC, Victoria, BC V8W 3P6, Canada</json:string></affiliations></json:item><json:item><name>Q. A. Parker</name><affiliations><json:string>Anglo‐Australian Observatory, Sydney, Australia</json:string><json:string>Macquary University, Sydney, NSW 2109, Australia</json:string></affiliations></json:item><json:item><name>W. Reid</name><affiliations><json:string>Macquary University, Sydney, NSW 2109, Australia</json:string></affiliations></json:item><json:item><name>G. Seabroke</name><affiliations><json:string>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT</json:string></affiliations></json:item><json:item><name>A. Siebert</name><affiliations><json:string>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>A. Siviero</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</json:string><json:string>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</json:string></affiliations></json:item><json:item><name>M. Steinmetz</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>M. E. K. Williams</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>R. F. G. Wyse</name><affiliations><json:string>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</json:string></affiliations></json:item><json:item><name>T. Zwitter</name><affiliations><json:string>Faculty of Mathematics and Physics, University of Ljubljana, Slovenia</json:string><json:string>Center of excellence SPACE‐SI, Ljubljana, Slovenia</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: disc</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: formation</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>solar neighbourhood</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxy: structure</value></json:item></subject><articleId><json:string>MNR18298</json:string></articleId><arkIstex>ark:/67375/WNG-L8P9SDC9-6</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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.</abstract><qualityIndicators><score>8.932</score><pdfWordCount>5636</pdfWordCount><pdfCharCount>31531</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>7</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>161</abstractWordCount><abstractCharCount>1039</abstractCharCount><keywordCount>4</keywordCount></qualityIndicators><title>Testing formation mechanisms of the Milky Way's thick disc with RAVE</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>413</volume><issue>3</issue><pages><first>2235</first><last>2241</last><total>7</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2011</json:string><json:string>2008</json:string></date><geogName></geogName><orgName><json:string>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH</json:string><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB</json:string><json:string>Research, the Natural Sciences and Engineering</json:string><json:string>Johns Hopkins University</json:string><json:string>University of Ljubljana, Slovenia</json:string><json:string>Jeremiah Horrocks Institute for Astrophysics</json:string><json:string>Astronomical Institute, PO Box</json:string><json:string>Slovenian Research Agency</json:string><json:string>Macquary University</json:string><json:string>Macquarie University</json:string><json:string>University of Victoria</json:string><json:string>University of Central Lancashire</json:string><json:string>Netherlands Research School for Astronomy, the Netherlands Organization for Scienti</json:string><json:string>Astrophysical Institute Potsdam, the Australian National University, the Australian Research Council, the French National Research Agency, the German Research</json:string><json:string>Istituto Nazionale</json:string><json:string>UK Schmidt Telescope</json:string><json:string>UK, Opticon, Strasbourg Observatory</json:string><json:string>European Research Council</json:string><json:string>Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT</json:string><json:string>Starting Grant GALACTICA-240271</json:string></orgName><orgName_funder><json:string>Starting Grant GALACTICA-240271</json:string></orgName_funder><orgName_provider></orgName_provider><persName><json:string>U. 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(2007)</json:string><json:string>Yoshii 1982</json:string><json:string>Minchev & Famaey 2010</json:string><json:string>M. L. Wilson et al.</json:string><json:string>Yoachim & Dalcanton 2006</json:string><json:string>Burstein 1979</json:string><json:string>Casetti-Dinescu et al. (2011)</json:string><json:string>Abadi et al. 2003</json:string><json:string>Gilmore & Reid 1983</json:string><json:string>Veltz et al. (2008)</json:string><json:string>Zwitter et al.</json:string><json:string>Edvardsson et al. 1993</json:string><json:string>Sales et al. (2009)</json:string><json:string>Abadi et al. (2003)</json:string><json:string>Dotter et al. 2008</json:string><json:string>Sales et al.</json:string><json:string>Zwitter et al. (2008)</json:string><json:string>Kregel et al. 2005</json:string><json:string>Zwitter et al. 2008</json:string><json:string>Demarque et al. 2004</json:string><json:string>Brook et al. (2004)</json:string><json:string>Yanny et al. 2009</json:string><json:string>Sellwood & Binney 2002</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-L8P9SDC9-6</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - astronomie</json:string></inist></categories><publicationDate>2011</publicationDate><copyrightDate>2011</copyrightDate><doi><json:string>10.1111/j.1365-2966.2011.18298.x</json:string></doi><id>6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Testing formation mechanisms of the Milky Way's thick disc with RAVE</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</licence></availability><date type="published" when="2011-05-21"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">Testing formation mechanisms of the Milky Way's thick disc with RAVE</title><title level="a" type="short">Testing thick disc formation mechanisms</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Michelle L.</forename><surname>Wilson</surname></persName><affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA<address><country key="US"></country></address></affiliation><affiliation>E‐mail: mlw36@case.edu (MLW); ahelmi@astro.rug.nl (AH)</affiliation></author><author xml:id="author-0001" role="corresp"><persName><forename type="first">Amina</forename><surname>Helmi</surname></persName><affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands<address><country key="NL"></country></address></affiliation><affiliation>E‐mail: mlw36@case.edu (MLW); ahelmi@astro.rug.nl (AH)</affiliation></author><author xml:id="author-0002"><persName><forename type="first">Heather L.</forename><surname>Morrison</surname></persName><affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">Maarten A.</forename><surname>Breddels</surname></persName><affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands<address><country key="NL"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">O.</forename><surname>Bienaymé</surname></persName><affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">J.</forename><surname>Binney</surname></persName><affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford OX1 3NP</affiliation></author><author xml:id="author-0006"><persName><forename type="first">J.</forename><surname>Bland‐Hawthorn</surname></persName><affiliation>Anglo‐Australian Observatory, Sydney, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">R.</forename><surname>Campbell</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation><affiliation>Macquary University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">K. C.</forename><surname>Freeman</surname></persName><affiliation>RSAA Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">J. P.</forename><surname>Fulbright</surname></persName><affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">B. K.</forename><surname>Gibson</surname></persName><affiliation>Jeremiah Horrocks Institute for Astrophysics & Supercomputing, University of Central Lancashire, Preston PR1 2HE</affiliation></author><author xml:id="author-0011"><persName><forename type="first">G.</forename><surname>Gilmore</surname></persName><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-0012"><persName><forename type="first">E. K.</forename><surname>Grebel</surname></persName><affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, D‐69120 Heidelberg, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">U.</forename><surname>Munari</surname></persName><affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0014"><persName><forename type="first">J. F.</forename><surname>Navarro</surname></persName><affiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC V8W 3P6, Canada<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">Q. A.</forename><surname>Parker</surname></persName><affiliation>Anglo‐Australian Observatory, Sydney, Australia<address><country key="AU"></country></address></affiliation><affiliation>Macquary University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0016"><persName><forename type="first">W.</forename><surname>Reid</surname></persName><affiliation>Macquary University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">G.</forename><surname>Seabroke</surname></persName><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT</affiliation></author><author xml:id="author-0018"><persName><forename type="first">A.</forename><surname>Siebert</surname></persName><affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0019"><persName><forename type="first">A.</forename><surname>Siviero</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation><affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0020"><persName><forename type="first">M.</forename><surname>Steinmetz</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0021"><persName><forename type="first">M. E. K.</forename><surname>Williams</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0022"><persName><forename type="first">R. F. G.</forename><surname>Wyse</surname></persName><affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0023"><persName><forename type="first">T.</forename><surname>Zwitter</surname></persName><affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Slovenia<address><country key="SI"></country></address></affiliation><affiliation>Center of excellence SPACE‐SI, Ljubljana, Slovenia<address><country key="SI"></country></address></affiliation></author><idno type="istex">6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088</idno><idno type="ark">ark:/67375/WNG-L8P9SDC9-6</idno><idno type="DOI">10.1111/j.1365-2966.2011.18298.x</idno><idno type="unit">MNR18298</idno><idno type="toTypesetVersion">file:MNR.MNR18298.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2011.413.issue-3</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">413</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="2235">2235</biblScope><biblScope unit="page" to="2241">2241</biblScope><biblScope unit="page-count">7</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2011-05-21"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>We study the eccentricity distribution of a thick‐disc sample of stars (defined as those with <emph><span><hi rend="italic">V<hi rend="subscript">y</hi></hi> > 50 km s<hi rend="superscript">−1</hi></span></emph> and <emph><span>1 < |<hi rend="italic">z</hi>|/kpc < 3</span></emph>) 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 ‘<hi rend="italic">in situ</hi>’ appears to be the most consistent with our data.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">Galaxy: disc</term><term xml:id="k2">Galaxy: formation</term><term xml:id="k3">solar neighbourhood</term><term xml:id="k4">Galaxy: structure</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="05103"><doi origin="wiley">10.1111/mnr.2011.413.issue-3</doi><numberingGroup><numbering type="journalVolume" number="413">413</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2011-05-21">May 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="61" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2011.18298.x</doi><idGroup><id type="unit" value="MNR18298"></id></idGroup><countGroup><count type="pageTotal" number="7"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.4.9 mode:FullText" date="2011-05-11"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-03-02"></event><event type="firstOnline" date="2011-03-02"></event><event type="publishedOnlineFinalForm" date="2011-05-11"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="2235">2235</numbering><numbering type="pageLast" number="2241">2241</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>mlw36@case.edu</email> (MLW); <email>ahelmi@astro.rug.nl</email> (AH)</correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR18298.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2011 January 5. Received 2010 December 12; in original form 2010 September 10</unparsedEditorialHistory><countGroup><count type="figureTotal" number="7"></count><count type="tableTotal" number="0"></count><count type="formulaTotal" number="57"></count><count type="referenceTotal" number="33"></count><count type="linksCrossRef" number="104"></count></countGroup><titleGroup><title type="main">Testing formation mechanisms of the Milky Way's thick disc with RAVE</title><title type="shortAuthors"><i>M. L. Wilson et al.</i></title><title type="short"><i>Testing thick disc formation mechanisms</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Michelle L.</givenNames><familyName>Wilson</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2" corresponding="yes"><personName><givenNames>Amina</givenNames><familyName>Helmi</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a1"><personName><givenNames>Heather L.</givenNames><familyName>Morrison</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a2"><personName><givenNames>Maarten A.</givenNames><familyName>Breddels</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a3"><personName><givenNames>O.</givenNames><familyName>Bienaymé</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a4"><personName><givenNames>J.</givenNames><familyName>Binney</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a5"><personName><givenNames>J.</givenNames><familyName>Bland‐Hawthorn</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a6 #a7"><personName><givenNames>R.</givenNames><familyName>Campbell</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a8"><personName><givenNames>K. C.</givenNames><familyName>Freeman</familyName></personName></creator><creator creatorRole="author" xml:id="cr10" affiliationRef="#a9"><personName><givenNames>J. P.</givenNames><familyName>Fulbright</familyName></personName></creator><creator creatorRole="author" xml:id="cr11" affiliationRef="#a10"><personName><givenNames>B. K.</givenNames><familyName>Gibson</familyName></personName></creator><creator creatorRole="author" xml:id="cr12" affiliationRef="#a11"><personName><givenNames>G.</givenNames><familyName>Gilmore</familyName></personName></creator><creator creatorRole="author" xml:id="cr13" affiliationRef="#a12"><personName><givenNames>E. K.</givenNames><familyName>Grebel</familyName></personName></creator><creator creatorRole="author" xml:id="cr14" affiliationRef="#a13"><personName><givenNames>U.</givenNames><familyName>Munari</familyName></personName></creator><creator creatorRole="author" xml:id="cr15" affiliationRef="#a14"><personName><givenNames>J. 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A.</givenNames><familyName>Parker</familyName></personName></creator><creator creatorRole="author" xml:id="cr17" affiliationRef="#a7"><personName><givenNames>W.</givenNames><familyName>Reid</familyName></personName></creator><creator creatorRole="author" xml:id="cr18" affiliationRef="#a15"><personName><givenNames>G.</givenNames><familyName>Seabroke</familyName></personName></creator><creator creatorRole="author" xml:id="cr19" affiliationRef="#a3"><personName><givenNames>A.</givenNames><familyName>Siebert</familyName></personName></creator><creator creatorRole="author" xml:id="cr20" affiliationRef="#a6 #a13"><personName><givenNames>A.</givenNames><familyName>Siviero</familyName></personName></creator><creator creatorRole="author" xml:id="cr21" affiliationRef="#a6"><personName><givenNames>M.</givenNames><familyName>Steinmetz</familyName></personName></creator><creator creatorRole="author" xml:id="cr22" affiliationRef="#a6"><personName><givenNames>M. E. 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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 ‘<i>in situ</i>’ appears to be the most consistent with our data.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Testing formation mechanisms of the Milky Way's thick disc with RAVE</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Testing thick disc formation mechanisms</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Testing formation mechanisms of the Milky Way's thick disc with RAVE</title></titleInfo><name type="personal"><namePart type="given">Michelle L.</namePart><namePart type="family">Wilson</namePart><affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</affiliation><affiliation>E-mail: mlw36@case.edu</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Amina</namePart><namePart type="family">Helmi</namePart><affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</affiliation><affiliation>E-mail: mlw36@case.edu</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Heather L.</namePart><namePart type="family">Morrison</namePart><affiliation>Department of Astronomy, Case Western University, Cleveland, OH 44106, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Maarten A.</namePart><namePart type="family">Breddels</namePart><affiliation>Kapteyn Astronomical Institute, PO Box 800 Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">O.</namePart><namePart type="family">Bienaymé</namePart><affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Binney</namePart><affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford OX1 3NP</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Bland‐Hawthorn</namePart><affiliation>Anglo‐Australian Observatory, Sydney, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Campbell</namePart><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</affiliation><affiliation>Macquary University, Sydney, NSW 2109, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K. C.</namePart><namePart type="family">Freeman</namePart><affiliation>RSAA Australian National University, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. P.</namePart><namePart type="family">Fulbright</namePart><affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B. K.</namePart><namePart type="family">Gibson</namePart><affiliation>Jeremiah Horrocks Institute for Astrophysics & Supercomputing, University of Central Lancashire, Preston PR1 2HE</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Gilmore</namePart><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E. K.</namePart><namePart type="family">Grebel</namePart><affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, D‐69120 Heidelberg, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">U.</namePart><namePart type="family">Munari</namePart><affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. F.</namePart><namePart type="family">Navarro</namePart><affiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC V8W 3P6, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Q. A.</namePart><namePart type="family">Parker</namePart><affiliation>Anglo‐Australian Observatory, Sydney, Australia</affiliation><affiliation>Macquary University, Sydney, NSW 2109, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">W.</namePart><namePart type="family">Reid</namePart><affiliation>Macquary University, Sydney, NSW 2109, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Seabroke</namePart><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking RH5 6NT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siebert</namePart><affiliation>Université de Strasbourg, Observatoire Astronomique, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siviero</namePart><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</affiliation><affiliation>INAF Astronomical Observatory of Padova, 36012 Asiago, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Steinmetz</namePart><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. E. K.</namePart><namePart type="family">Williams</namePart><affiliation>Astrophysikalishes Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. F. G.</namePart><namePart type="family">Wyse</namePart><affiliation>Johns Hopkins University, 3400 N Charles Street, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Zwitter</namePart><affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Slovenia</affiliation><affiliation>Center of excellence SPACE‐SI, Ljubljana, Slovenia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-05-21</dateIssued><edition>Accepted 2011 January 5. Received 2010 December 12; in original form 2010 September 10</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">7</extent><extent unit="tables">0</extent><extent unit="formulas">57</extent><extent unit="references">33</extent><extent unit="linksCrossRef">104</extent></physicalDescription><abstract 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.</abstract><subject lang="en"><genre>keywords</genre><topic>Galaxy: disc</topic><topic>Galaxy: formation</topic><topic>solar neighbourhood</topic><topic>Galaxy: structure</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>413</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>2235</start><end>2241</end><total>7</total></extent></part></relatedItem><identifier type="istex">6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088</identifier><identifier type="ark">ark:/67375/WNG-L8P9SDC9-6</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.18298.x</identifier><identifier type="ArticleID">MNR18298</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/6A8D4C23A7E99AC152CE26CF4C9E0AD1F8F03088/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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