Thick disk kinematics from RAVE and the solar motion
Identifieur interne : 000C94 ( PascalFrancis/Corpus ); précédent : 000C93; suivant : 000C95Thick disk kinematics from RAVE and the solar motion
Auteurs : S. Pasetto ; E. K. Grebel ; T. Zwitter ; C. Chiosi ; G. Bertelli ; O. Bienayme ; G. Seabroke ; J. Bland-Hawthorn ; C. Boeche ; B. K. Gibson ; G. Gilmore ; U. Munari ; J. F. Navarro ; Q. Parker ; W. Reid ; A. Silviero ; M. SteinmetzSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Cinématique stellaire, Vitesse radiale, Etoile proche, Disque galactique, Espace phase, Abondance, Population stellaire, Voie lactée, Contenu stellaire, Paramètre physique, Gravité surface, Galaxies, Modèle, Critère sélection, Rotation différentielle, Dispersion vitesse, Dynamique stellaire, Méthode analytique, Méthode numérique, Structure galaxies.
English descriptors
- KwdEn :
- Abundance, Analytical method, Differential rotation, Galactic disks, Galaxies, Galaxy structure, Milky Way, Models, Nearby stars, Numerical method, Phase space, Physical parameter, Radial velocity, Selection criterion, Stellar content, Stellar dynamics, Stellar kinematics, Stellar population, Surface gravity, Velocity dispersion.
Abstract
Context. Radial velocity surveys such as the RAdial Velocity Experiment (RAVE) provide us with measurements of hundreds of thousands of nearby stars most of which belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic disks (both thin and thick) one should make use of the multi-dimensional phase-space and the whole pattern of chemical abundances of their stellar populations. Aims. In this paper, with the aid of the RAVE survey, we study the thin and thick disks of the Milky Way, focusing on the latter. We present a technique to disentangle the stellar content of the two disks based on the kinematics and other stellar parameters such as the surface gravity of the stars. Using the Padova Galaxy model, we checked the ability of our method to correctly isolate the thick disk component from the Galaxy mixture of stellar populations. Methods. We introduce selection criteria in order to clean the observed radial velocities from the Galactic differential rotation and to take into account the partial sky coverage of RAVE. We developed a numerical technique to statistically disentangle thin and thick disks from their mixture. Results. We deduce the components of the solar motion relative to the local standard of rest (LSR) in the radial and vertical direction, the rotational lag of the thick disk component relative to the LSR, and the square root of the absolute value of the velocity dispersion tensor for the thick disk alone. The analysis of the thin disk is presented in another paper. We find good agreement with previous independent parameter determinations. In our analysis we used photometrically determined distances. In the Appendix we show that similar values can be found for the thick disk alone as derived in the main sections of our paper even without the knowledge of photometric distances.
Notice en format standard (ISO 2709)
Pour connaître la documentation sur le format Inist Standard.
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Format Inist (serveur)
| NO : | PASCAL 13-0057314 INIST |
|---|---|
| ET : | Thick disk kinematics from RAVE and the solar motion |
| AU : | PASETTO (S.); GREBEL (E. K.); ZWITTER (T.); CHIOSI (C.); BERTELLI (G.); BIENAYME (O.); SEABROKE (G.); BLAND-HAWTHORN (J.); BOECHE (C.); GIBSON (B. K.); GILMORE (G.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q.); REID (W.); SILVIERO (A.); STEINMETZ (M.) |
| AF : | University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary/Dorking Surrey RH5 6NT/Royaume-Uni (1 aut., 7 aut.); Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14/69120 Heidelberg/Allemagne (1 aut., 2 aut., 9 aut.); University of Ljubljana, Faculty of Mathematics and Physics/1000 Ljubljana/Slovénie (3 aut.); Center of Excellence SPACE-SI, Askerceva cesta 12/1000 Ljubljana/Slovénie (3 aut.); Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3/35122 Padova/Italie (4 aut., 16 aut.); INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5/35122 Padova/Italie (5 aut., 12 aut.); Observatoire astronomique de Strasbourg 11 rue de l'Université/67000 Strasbourg/France (6 aut.); Sydney Institute for Astronomy, University of Sydney/NSW 2006/Australie (8 aut.); Jeremiah Horrocks Institute, University of Central Lancashire/Preston, PR1 2HE/Royaume-Uni (10 aut.); Monash Centre for Astrophysics, Monash University/Clayton 3800/Australie (10 aut.); Institute of Astronomy, Cambridge University, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (11 aut.); University of Victoria, Department of Physics and Astronomy/Victoria, BC V8P 5C2/Canada (13 aut.); Department of Physics and Astronomy, Macquarie University/NSW 2109/Australie (14 aut., 15 aut.); Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109/Australie (14 aut., 15 aut.); Australian Astronomical Observatory, PO Box 296/Epping, NSW 2121/Australie (14 aut.); Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16/14482 Potsdam/Allemagne (16 aut., 17 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 547; No. p. 2; 547A70.1-547A70.17; Bibl. 1 p. |
| LA : | Anglais |
| EA : | Context. Radial velocity surveys such as the RAdial Velocity Experiment (RAVE) provide us with measurements of hundreds of thousands of nearby stars most of which belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic disks (both thin and thick) one should make use of the multi-dimensional phase-space and the whole pattern of chemical abundances of their stellar populations. Aims. In this paper, with the aid of the RAVE survey, we study the thin and thick disks of the Milky Way, focusing on the latter. We present a technique to disentangle the stellar content of the two disks based on the kinematics and other stellar parameters such as the surface gravity of the stars. Using the Padova Galaxy model, we checked the ability of our method to correctly isolate the thick disk component from the Galaxy mixture of stellar populations. Methods. We introduce selection criteria in order to clean the observed radial velocities from the Galactic differential rotation and to take into account the partial sky coverage of RAVE. We developed a numerical technique to statistically disentangle thin and thick disks from their mixture. Results. We deduce the components of the solar motion relative to the local standard of rest (LSR) in the radial and vertical direction, the rotational lag of the thick disk component relative to the LSR, and the square root of the absolute value of the velocity dispersion tensor for the thick disk alone. The analysis of the thin disk is presented in another paper. We find good agreement with previous independent parameter determinations. In our analysis we used photometrically determined distances. In the Appendix we show that similar values can be found for the thick disk alone as derived in the main sections of our paper even without the knowledge of photometric distances. |
| CC : | 001E03 |
| FD : | Cinématique stellaire; Vitesse radiale; Etoile proche; Disque galactique; Espace phase; Abondance; Population stellaire; Voie lactée; Contenu stellaire; Paramètre physique; Gravité surface; Galaxies; Modèle; Critère sélection; Rotation différentielle; Dispersion vitesse; Dynamique stellaire; Méthode analytique; Méthode numérique; Structure galaxies |
| ED : | Stellar kinematics; Radial velocity; Nearby stars; Galactic disks; Phase space; Abundance; Stellar population; Milky Way; Stellar content; Physical parameter; Surface gravity; Galaxies; Models; Selection criterion; Differential rotation; Velocity dispersion; Stellar dynamics; Analytical method; Numerical method; Galaxy structure |
| SD : | Cinematica estelar; Población estelar; Contenido estelar; Parámetro físico; Modelo; Criterio selección; Dispersión velocidad; Método analítico; Método numérico; Estructura galaxias |
| LO : | INIST-14176.354000506259130100 |
| ID : | 13-0057314 |
Links to Exploration step
Pascal:13-0057314Le document en format XML
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Seabroke</name><affiliation><inist:fA14 i1="01"><s1>University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary</s1><s2>Dorking Surrey RH5 6NT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bland Hawthorn, J" sort="Bland Hawthorn, J" uniqKey="Bland Hawthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><inist:fA14 i1="08"><s1>Sydney Institute for Astronomy, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Boeche, C" sort="Boeche, C" uniqKey="Boeche C" first="C." last="Boeche">C. Boeche</name><affiliation><inist:fA14 i1="02"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></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><inist:fA14 i1="09"><s1>Jeremiah Horrocks Institute, University of Central Lancashire</s1><s2>Preston, PR1 2HE</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="10"><s1>Monash Centre for Astrophysics, Monash University</s1><s2>Clayton 3800</s2><s3>AUS</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="11"><s1>Institute of Astronomy, Cambridge University, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><inist:fA14 i1="06"><s1>INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>5 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></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><inist:fA14 i1="12"><s1>University of Victoria, Department of Physics and Astronomy</s1><s2>Victoria, BC V8P 5C2</s2><s3>CAN</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q" sort="Parker, Q" uniqKey="Parker Q" first="Q." last="Parker">Q. Parker</name><affiliation><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, Macquarie University</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="14"><s1>Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109</s1><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="15"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 2121</s2><s3>AUS</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Reid, W" sort="Reid, W" uniqKey="Reid W" first="W." last="Reid">W. Reid</name><affiliation><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, Macquarie University</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="14"><s1>Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109</s1><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Silviero, A" sort="Silviero, A" uniqKey="Silviero A" first="A." last="Silviero">A. Silviero</name><affiliation><inist:fA14 i1="05"><s1>Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>4 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="16"><s1>Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="16"><s1>Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">13-0057314</idno><date when="2012">2012</date><idno type="stanalyst">PASCAL 13-0057314 INIST</idno><idno type="RBID">Pascal:13-0057314</idno><idno type="wicri:Area/PascalFrancis/Corpus">000C94</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Thick disk kinematics from RAVE and the solar motion</title><author><name sortKey="Pasetto, S" sort="Pasetto, S" uniqKey="Pasetto S" first="S." last="Pasetto">S. Pasetto</name><affiliation><inist:fA14 i1="01"><s1>University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary</s1><s2>Dorking Surrey RH5 6NT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></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><inist:fA14 i1="02"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><inist:fA14 i1="03"><s1>University of Ljubljana, Faculty of Mathematics and Physics</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>3 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="04"><s1>Center of Excellence SPACE-SI, Askerceva cesta 12</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>3 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Chiosi, C" sort="Chiosi, C" uniqKey="Chiosi C" first="C." last="Chiosi">C. Chiosi</name><affiliation><inist:fA14 i1="05"><s1>Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>4 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bertelli, G" sort="Bertelli, G" uniqKey="Bertelli G" first="G." last="Bertelli">G. Bertelli</name><affiliation><inist:fA14 i1="06"><s1>INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>5 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name><affiliation><inist:fA14 i1="07"><s1>Observatoire astronomique de Strasbourg 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name><affiliation><inist:fA14 i1="01"><s1>University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary</s1><s2>Dorking Surrey RH5 6NT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Bland Hawthorn, J" sort="Bland Hawthorn, J" uniqKey="Bland Hawthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><inist:fA14 i1="08"><s1>Sydney Institute for Astronomy, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Boeche, C" sort="Boeche, C" uniqKey="Boeche C" first="C." last="Boeche">C. Boeche</name><affiliation><inist:fA14 i1="02"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></inist:fA14></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><inist:fA14 i1="09"><s1>Jeremiah Horrocks Institute, University of Central Lancashire</s1><s2>Preston, PR1 2HE</s2><s3>GBR</s3><sZ>10 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="10"><s1>Monash Centre for Astrophysics, Monash University</s1><s2>Clayton 3800</s2><s3>AUS</s3><sZ>10 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="11"><s1>Institute of Astronomy, Cambridge University, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>11 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><inist:fA14 i1="06"><s1>INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>5 aut.</sZ><sZ>12 aut.</sZ></inist:fA14></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><inist:fA14 i1="12"><s1>University of Victoria, Department of Physics and Astronomy</s1><s2>Victoria, BC V8P 5C2</s2><s3>CAN</s3><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Parker, Q" sort="Parker, Q" uniqKey="Parker Q" first="Q." last="Parker">Q. Parker</name><affiliation><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, Macquarie University</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="14"><s1>Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109</s1><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="15"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 2121</s2><s3>AUS</s3><sZ>14 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Reid, W" sort="Reid, W" uniqKey="Reid W" first="W." last="Reid">W. Reid</name><affiliation><inist:fA14 i1="13"><s1>Department of Physics and Astronomy, Macquarie University</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="14"><s1>Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109</s1><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Silviero, A" sort="Silviero, A" uniqKey="Silviero A" first="A." last="Silviero">A. Silviero</name><affiliation><inist:fA14 i1="05"><s1>Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>4 aut.</sZ><sZ>16 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="16"><s1>Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><inist:fA14 i1="16"><s1>Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno><imprint><date when="2012">2012</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title><title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title><idno type="ISSN">0004-6361</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Abundance</term><term>Analytical method</term><term>Differential rotation</term><term>Galactic disks</term><term>Galaxies</term><term>Galaxy structure</term><term>Milky Way</term><term>Models</term><term>Nearby stars</term><term>Numerical method</term><term>Phase space</term><term>Physical parameter</term><term>Radial velocity</term><term>Selection criterion</term><term>Stellar content</term><term>Stellar dynamics</term><term>Stellar kinematics</term><term>Stellar population</term><term>Surface gravity</term><term>Velocity dispersion</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Cinématique stellaire</term><term>Vitesse radiale</term><term>Etoile proche</term><term>Disque galactique</term><term>Espace phase</term><term>Abondance</term><term>Population stellaire</term><term>Voie lactée</term><term>Contenu stellaire</term><term>Paramètre physique</term><term>Gravité surface</term><term>Galaxies</term><term>Modèle</term><term>Critère sélection</term><term>Rotation différentielle</term><term>Dispersion vitesse</term><term>Dynamique stellaire</term><term>Méthode analytique</term><term>Méthode numérique</term><term>Structure galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. Radial velocity surveys such as the RAdial Velocity Experiment (RAVE) provide us with measurements of hundreds of thousands of nearby stars most of which belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic disks (both thin and thick) one should make use of the multi-dimensional phase-space and the whole pattern of chemical abundances of their stellar populations. Aims. In this paper, with the aid of the RAVE survey, we study the thin and thick disks of the Milky Way, focusing on the latter. We present a technique to disentangle the stellar content of the two disks based on the kinematics and other stellar parameters such as the surface gravity of the stars. Using the Padova Galaxy model, we checked the ability of our method to correctly isolate the thick disk component from the Galaxy mixture of stellar populations. Methods. We introduce selection criteria in order to clean the observed radial velocities from the Galactic differential rotation and to take into account the partial sky coverage of RAVE. We developed a numerical technique to statistically disentangle thin and thick disks from their mixture. Results. We deduce the components of the solar motion relative to the local standard of rest (LSR) in the radial and vertical direction, the rotational lag of the thick disk component relative to the LSR, and the square root of the absolute value of the velocity dispersion tensor for the thick disk alone. The analysis of the thin disk is presented in another paper. We find good agreement with previous independent parameter determinations. In our analysis we used photometrically determined distances. In the Appendix we show that similar values can be found for the thick disk alone as derived in the main sections of our paper even without the knowledge of photometric distances.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-6361</s0></fA01><fA02 i1="01"><s0>AAEJAF</s0></fA02><fA03 i2="1"><s0>Astron. astrophys. : (Berl., Print)</s0></fA03><fA05><s2>547</s2></fA05><fA06><s3>p. 2</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Thick disk kinematics from RAVE and the solar motion</s1></fA08><fA11 i1="01" i2="1"><s1>PASETTO (S.)</s1></fA11><fA11 i1="02" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="03" i2="1"><s1>ZWITTER (T.)</s1></fA11><fA11 i1="04" i2="1"><s1>CHIOSI (C.)</s1></fA11><fA11 i1="05" i2="1"><s1>BERTELLI (G.)</s1></fA11><fA11 i1="06" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="07" i2="1"><s1>SEABROKE (G.)</s1></fA11><fA11 i1="08" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="09" i2="1"><s1>BOECHE (C.)</s1></fA11><fA11 i1="10" i2="1"><s1>GIBSON (B. K.)</s1></fA11><fA11 i1="11" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="12" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="13" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="14" i2="1"><s1>PARKER (Q.)</s1></fA11><fA11 i1="15" i2="1"><s1>REID (W.)</s1></fA11><fA11 i1="16" i2="1"><s1>SILVIERO (A.)</s1></fA11><fA11 i1="17" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA14 i1="01"><s1>University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary</s1><s2>Dorking Surrey RH5 6NT</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="02"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ><sZ>9 aut.</sZ></fA14><fA14 i1="03"><s1>University of Ljubljana, Faculty of Mathematics and Physics</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Center of Excellence SPACE-SI, Askerceva cesta 12</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>3 aut.</sZ></fA14><fA14 i1="05"><s1>Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>4 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="06"><s1>INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>5 aut.</sZ><sZ>12 aut.</sZ></fA14><fA14 i1="07"><s1>Observatoire astronomique de Strasbourg 11 rue de l'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ></fA14><fA14 i1="08"><s1>Sydney Institute for Astronomy, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>8 aut.</sZ></fA14><fA14 i1="09"><s1>Jeremiah Horrocks Institute, University of Central Lancashire</s1><s2>Preston, PR1 2HE</s2><s3>GBR</s3><sZ>10 aut.</sZ></fA14><fA14 i1="10"><s1>Monash Centre for Astrophysics, Monash University</s1><s2>Clayton 3800</s2><s3>AUS</s3><sZ>10 aut.</sZ></fA14><fA14 i1="11"><s1>Institute of Astronomy, Cambridge University, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>11 aut.</sZ></fA14><fA14 i1="12"><s1>University of Victoria, Department of Physics and Astronomy</s1><s2>Victoria, BC V8P 5C2</s2><s3>CAN</s3><sZ>13 aut.</sZ></fA14><fA14 i1="13"><s1>Department of Physics and Astronomy, Macquarie University</s1><s2>NSW 2109</s2><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="14"><s1>Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109</s1><s3>AUS</s3><sZ>14 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="15"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 2121</s2><s3>AUS</s3><sZ>14 aut.</sZ></fA14><fA14 i1="16"><s1>Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>16 aut.</sZ><sZ>17 aut.</sZ></fA14><fA20><s2>547A70.1-547A70.17</s2></fA20><fA21><s1>2012</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000506259130100</s5></fA43><fA44><s0>0000</s0><s1>© 2013 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1 p.</s0></fA45><fA47 i1="01" i2="1"><s0>13-0057314</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Astronomy and astrophysics : (Berlin. Print)</s0></fA64><fA66 i1="01"><s0>FRA</s0></fA66><fC01 i1="01" l="ENG"><s0>Context. Radial velocity surveys such as the RAdial Velocity Experiment (RAVE) provide us with measurements of hundreds of thousands of nearby stars most of which belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic disks (both thin and thick) one should make use of the multi-dimensional phase-space and the whole pattern of chemical abundances of their stellar populations. Aims. In this paper, with the aid of the RAVE survey, we study the thin and thick disks of the Milky Way, focusing on the latter. We present a technique to disentangle the stellar content of the two disks based on the kinematics and other stellar parameters such as the surface gravity of the stars. Using the Padova Galaxy model, we checked the ability of our method to correctly isolate the thick disk component from the Galaxy mixture of stellar populations. Methods. We introduce selection criteria in order to clean the observed radial velocities from the Galactic differential rotation and to take into account the partial sky coverage of RAVE. We developed a numerical technique to statistically disentangle thin and thick disks from their mixture. Results. We deduce the components of the solar motion relative to the local standard of rest (LSR) in the radial and vertical direction, the rotational lag of the thick disk component relative to the LSR, and the square root of the absolute value of the velocity dispersion tensor for the thick disk alone. The analysis of the thin disk is presented in another paper. We find good agreement with previous independent parameter determinations. In our analysis we used photometrically determined distances. In the Appendix we show that similar values can be found for the thick disk alone as derived in the main sections of our paper even without the knowledge of photometric distances.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Cinématique stellaire</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Stellar kinematics</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Cinematica estelar</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Radial velocity</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Etoile proche</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Nearby stars</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Disque galactique</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Galactic disks</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Espace phase</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Phase space</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Abondance</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Abundance</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Population stellaire</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Stellar population</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Población estelar</s0><s5>32</s5></fC03><fC03 i1="08" i2="3" l="FRE"><s0>Voie lactée</s0><s5>33</s5></fC03><fC03 i1="08" i2="3" l="ENG"><s0>Milky Way</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Contenu stellaire</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Stellar content</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Contenido estelar</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Paramètre physique</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Physical parameter</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Parámetro físico</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Gravité surface</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Surface gravity</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Galaxies</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Galaxies</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Modèle</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Models</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Modelo</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Critère sélection</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Selection criterion</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Criterio selección</s0><s5>39</s5></fC03><fC03 i1="15" i2="3" l="FRE"><s0>Rotation différentielle</s0><s5>40</s5></fC03><fC03 i1="15" i2="3" l="ENG"><s0>Differential rotation</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Dispersion vitesse</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Velocity dispersion</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Dispersión velocidad</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Dynamique stellaire</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>Stellar dynamics</s0><s5>42</s5></fC03><fC03 i1="18" i2="X" l="FRE"><s0>Méthode analytique</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="ENG"><s0>Analytical method</s0><s5>43</s5></fC03><fC03 i1="18" i2="X" l="SPA"><s0>Método analítico</s0><s5>43</s5></fC03><fC03 i1="19" i2="X" l="FRE"><s0>Méthode numérique</s0><s5>44</s5></fC03><fC03 i1="19" i2="X" l="ENG"><s0>Numerical method</s0><s5>44</s5></fC03><fC03 i1="19" i2="X" l="SPA"><s0>Método numérico</s0><s5>44</s5></fC03><fC03 i1="20" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>45</s5></fC03><fN21><s1>035</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 13-0057314 INIST</NO><ET>Thick disk kinematics from RAVE and the solar motion</ET><AU>PASETTO (S.); GREBEL (E. K.); ZWITTER (T.); CHIOSI (C.); BERTELLI (G.); BIENAYME (O.); SEABROKE (G.); BLAND-HAWTHORN (J.); BOECHE (C.); GIBSON (B. K.); GILMORE (G.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q.); REID (W.); SILVIERO (A.); STEINMETZ (M.)</AU><AF>University College London, Department of Space & Climate Physics, Mullard Space Science Laboratory, Holmbury St. Mary/Dorking Surrey RH5 6NT/Royaume-Uni (1 aut., 7 aut.); Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Monchhofstr. 12-14/69120 Heidelberg/Allemagne (1 aut., 2 aut., 9 aut.); University of Ljubljana, Faculty of Mathematics and Physics/1000 Ljubljana/Slovénie (3 aut.); Center of Excellence SPACE-SI, Askerceva cesta 12/1000 Ljubljana/Slovénie (3 aut.); Department of Physics and Astronomy "G. Galilei", Padova University, Vicolo dell'Osservatorio 3/35122 Padova/Italie (4 aut., 16 aut.); INAF - Padova Astronomical Observatory, Vicolo dell'Osservatorio 5/35122 Padova/Italie (5 aut., 12 aut.); Observatoire astronomique de Strasbourg 11 rue de l'Université/67000 Strasbourg/France (6 aut.); Sydney Institute for Astronomy, University of Sydney/NSW 2006/Australie (8 aut.); Jeremiah Horrocks Institute, University of Central Lancashire/Preston, PR1 2HE/Royaume-Uni (10 aut.); Monash Centre for Astrophysics, Monash University/Clayton 3800/Australie (10 aut.); Institute of Astronomy, Cambridge University, Madingley Road/Cambridge CB3 0HA/Royaume-Uni (11 aut.); University of Victoria, Department of Physics and Astronomy/Victoria, BC V8P 5C2/Canada (13 aut.); Department of Physics and Astronomy, Macquarie University/NSW 2109/Australie (14 aut., 15 aut.); Macquarie research centre in Astronomy, Astrophysics and Astrophotonics, Macquarie University NSW 2109/Australie (14 aut., 15 aut.); Australian Astronomical Observatory, PO Box 296/Epping, NSW 2121/Australie (14 aut.); Leibniz-Institut fur Astrophysik Potsdam (AIP), An der Sternwarte 16/14482 Potsdam/Allemagne (16 aut., 17 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2012; Vol. 547; No. p. 2; 547A70.1-547A70.17; Bibl. 1 p.</SO><LA>Anglais</LA><EA>Context. Radial velocity surveys such as the RAdial Velocity Experiment (RAVE) provide us with measurements of hundreds of thousands of nearby stars most of which belong to the Galactic thin, thick disk or halo. Ideally, to study the Galactic disks (both thin and thick) one should make use of the multi-dimensional phase-space and the whole pattern of chemical abundances of their stellar populations. Aims. In this paper, with the aid of the RAVE survey, we study the thin and thick disks of the Milky Way, focusing on the latter. We present a technique to disentangle the stellar content of the two disks based on the kinematics and other stellar parameters such as the surface gravity of the stars. Using the Padova Galaxy model, we checked the ability of our method to correctly isolate the thick disk component from the Galaxy mixture of stellar populations. Methods. We introduce selection criteria in order to clean the observed radial velocities from the Galactic differential rotation and to take into account the partial sky coverage of RAVE. We developed a numerical technique to statistically disentangle thin and thick disks from their mixture. Results. We deduce the components of the solar motion relative to the local standard of rest (LSR) in the radial and vertical direction, the rotational lag of the thick disk component relative to the LSR, and the square root of the absolute value of the velocity dispersion tensor for the thick disk alone. The analysis of the thin disk is presented in another paper. We find good agreement with previous independent parameter determinations. In our analysis we used photometrically determined distances. In the Appendix we show that similar values can be found for the thick disk alone as derived in the main sections of our paper even without the knowledge of photometric distances.</EA><CC>001E03</CC><FD>Cinématique stellaire; Vitesse radiale; Etoile proche; Disque galactique; Espace phase; Abondance; Population stellaire; Voie lactée; Contenu stellaire; Paramètre physique; Gravité surface; Galaxies; Modèle; Critère sélection; Rotation différentielle; Dispersion vitesse; Dynamique stellaire; Méthode analytique; Méthode numérique; Structure galaxies</FD><ED>Stellar kinematics; Radial velocity; Nearby stars; Galactic disks; Phase space; Abundance; Stellar population; Milky Way; Stellar content; Physical parameter; Surface gravity; Galaxies; Models; Selection criterion; Differential rotation; Velocity dispersion; Stellar dynamics; Analytical method; Numerical method; Galaxy structure</ED><SD>Cinematica estelar; Población estelar; Contenido estelar; Parámetro físico; Modelo; Criterio selección; Dispersión velocidad; Método analítico; Método numérico; Estructura galaxias</SD><LO>INIST-14176.354000506259130100</LO><ID>13-0057314</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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