Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry
Identifieur interne : 001845 ( PascalFrancis/Corpus ); précédent : 001844; suivant : 001846Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry
Auteurs : B. Burnett ; J. Binney ; S. Sharma ; M. Williams ; T. Zwitter ; O. Bienayme ; J. Bland-Hawthorn ; K. C. Freeman ; J. Fulbright ; B. Gibson ; G. Gilmore ; E. K. Grebel ; A. Helmi ; U. Munari ; J. F. Navarro ; Q. A. Parker ; G. M. Seabroke ; A. Siebert ; A. Siviero ; M. Steinmetz ; F. G. Watson ; R. F. G. WyseSource :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2011.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
Abstract
We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than ∼ 6000 K appear to be unbiased, but those to hotter dwarfs tend to be too small by ∼10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing |z| it broadens out and its median moves to [M/H] ≃ -0.5. Mean age as a function of distance from the Galactic centre and distance |z| from the Galactic plane shows the anticipated increase in mean age with |z|.
Notice en format standard (ISO 2709)
Pour connaître la documentation sur le format Inist Standard.
| pA |
|
|---|
Format Inist (serveur)
| NO : | PASCAL 11-0486083 INIST |
|---|---|
| ET : | Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry |
| AU : | BURNETT (B.); BINNEY (J.); SHARMA (S.); WILLIAMS (M.); ZWITTER (T.); BIENAYME (O.); BLAND-HAWTHORN (J.); FREEMAN (K. C.); FULBRIGHT (J.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WYSE (R. F. G.) |
| AF : | Rudolf Peierls Centre for Theoretical Physics, Keble Road/Oxford, OX1 3NP/Royaume-Uni (1 aut., 2 aut.); Sydney Institute for Astronomy, School of Physics A28, University of Sydney/NSW 2006/Australie (3 aut., 7 aut.); Astrophysikalisches Institut Potsdam, An der Sternwarte 16/14482 Potsdam/Allemagne (4 aut., 19 aut., 20 aut.); University of Ljubljana, Faculty of Mathematics and Physics, Jadranska 19/1000 Ljubljana/Slovénie (5 aut.); Center of excellence SPACE-SI, Askerceva cesta 12/1000 Ljubljana/Slovénie (5 aut.); Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université/67000 Strasbourg/France (6 aut., 18 aut.); Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd/ACT, Canberra/Australie (8 aut.); Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St/Baltimore, MD 21218/Etats-Unis (9 aut., 22 aut.); Jeremiah Horrocks Institute, University of Central Lancashire/Preston, PR1 2HE/Royaume-Uni (10 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge, CB3 OHA/Royaume-Uni (11 aut.); Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr. 12-14/69120 Heidelberg/Allemagne (12 aut.); Kapteyn Astronomical Institut, University of Groningen, Landleven 12/9747 AD, Groningen/Pays-Bas (13 aut.); INAF Osservatorio Astronomico di Padova/36012 Asiago (VI/Italie (14 aut.); Department of Physics and Astronomy, University of Victoria, PO Box 3055/Victoria, BC V8W 3P6/Canada (15 aut.); Department of Physics and Astronomy, Faculty of Sciences, Macquarie University/NSW 2109, Sydney/Australie (16 aut.); Mullard Space Science Laboratory, University College London, Holmbury St Mary/Dorking, RH5 6NT/Royaume-Uni (17 aut.); Dipartimento di Astronomia, Universita di Padova, Vicolo dellŠOsservatorio 2/35122 Padova/Italie (19 aut.); Australian Astronomical Observatory, PO Box 296/Epping, NSW 1710/Australie (21 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2011; Vol. 532; No. p. 2; A113.1-A113.14; Bibl. 1/2 p. |
| LA : | Anglais |
| EA : | We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than ∼ 6000 K appear to be unbiased, but those to hotter dwarfs tend to be too small by ∼10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing |z| it broadens out and its median moves to [M/H] ≃ -0.5. Mean age as a function of distance from the Galactic centre and distance |z| from the Galactic plane shows the anticipated increase in mean age with |z|. |
| CC : | 001E03 |
| FD : | Mesure distance; Modèle stellaire; Voie lactée; Paramètre physique; Catalogue astronomique; Vitesse radiale; Centre galactique; Métallicité; Age; Plan galactique; Galaxies disques; Abondance; Contenu stellaire; Structure galaxies |
| ED : | Distance measurement; Star models; Milky Way; Physical parameter; Astronomical catalogues; Radial velocity; Galactic centers; Metallicity; Age; Galactic planes; Disk galaxies; Abundance; Stellar content; Galaxy structure |
| SD : | Parámetro físico; Metalicidad; Edad; Contenido estelar; Estructura galaxias |
| LO : | INIST-14176.354000507292850330 |
| ID : | 11-0486083 |
Links to Exploration step
Pascal:11-0486083Le document en format XML
<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry</title><author><name sortKey="Burnett, B" sort="Burnett, B" uniqKey="Burnett B" first="B." last="Burnett">B. Burnett</name><affiliation><inist:fA14 i1="01"><s1>Rudolf Peierls Centre for Theoretical Physics, Keble Road</s1><s2>Oxford, OX1 3NP</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><inist:fA14 i1="01"><s1>Rudolf Peierls Centre for Theoretical Physics, Keble Road</s1><s2>Oxford, OX1 3NP</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sharma, S" sort="Sharma, S" uniqKey="Sharma S" first="S." last="Sharma">S. Sharma</name><affiliation><inist:fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics A28, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 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="04"><s1>University of Ljubljana, Faculty of Mathematics and Physics, Jadranska 19</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Center of excellence SPACE-SI, Askerceva cesta 12</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 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="06"><s1>Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>18 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="02"><s1>Sydney Institute for Astronomy, School of Physics A28, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></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><inist:fA14 i1="07"><s1>Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd</s1><s2>ACT, Canberra</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Fulbright, J" sort="Fulbright, J" uniqKey="Fulbright J" first="J." last="Fulbright">J. Fulbright</name><affiliation><inist:fA14 i1="08"><s1>Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B" sort="Gibson, B" uniqKey="Gibson B" first="B." last="Gibson">B. 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></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="10"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge, CB3 OHA</s2><s3>GBR</s3><sZ>11 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="11"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="12"><s1>Kapteyn Astronomical Institut, University of Groningen, Landleven 12</s1><s2>9747 AD, Groningen</s2><s3>NLD</s3><sZ>13 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="13"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>36012 Asiago (VI</s2><s3>ITA</s3><sZ>14 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="14"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>15 aut.</sZ></inist:fA14></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><inist:fA14 i1="15"><s1>Department of Physics and Astronomy, Faculty of Sciences, Macquarie University</s1><s2>NSW 2109, Sydney</s2><s3>AUS</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation><inist:fA14 i1="16"><s1>Mullard Space Science Laboratory, University College London, Holmbury St Mary</s1><s2>Dorking, RH5 6NT</s2><s3>GBR</s3><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="06"><s1>Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="17"><s1>Dipartimento di Astronomia, Universita di Padova, Vicolo dellŠOsservatorio 2</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>19 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="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="18"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></inist:fA14></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><inist:fA14 i1="08"><s1>Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">11-0486083</idno><date when="2011">2011</date><idno type="stanalyst">PASCAL 11-0486083 INIST</idno><idno type="RBID">Pascal:11-0486083</idno><idno type="wicri:Area/PascalFrancis/Corpus">001845</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry</title><author><name sortKey="Burnett, B" sort="Burnett, B" uniqKey="Burnett B" first="B." last="Burnett">B. Burnett</name><affiliation><inist:fA14 i1="01"><s1>Rudolf Peierls Centre for Theoretical Physics, Keble Road</s1><s2>Oxford, OX1 3NP</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><inist:fA14 i1="01"><s1>Rudolf Peierls Centre for Theoretical Physics, Keble Road</s1><s2>Oxford, OX1 3NP</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Sharma, S" sort="Sharma, S" uniqKey="Sharma S" first="S." last="Sharma">S. Sharma</name><affiliation><inist:fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics A28, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 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="04"><s1>University of Ljubljana, Faculty of Mathematics and Physics, Jadranska 19</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Center of excellence SPACE-SI, Askerceva cesta 12</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 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="06"><s1>Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>18 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="02"><s1>Sydney Institute for Astronomy, School of Physics A28, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></inist:fA14></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><inist:fA14 i1="07"><s1>Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd</s1><s2>ACT, Canberra</s2><s3>AUS</s3><sZ>8 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Fulbright, J" sort="Fulbright, J" uniqKey="Fulbright J" first="J." last="Fulbright">J. Fulbright</name><affiliation><inist:fA14 i1="08"><s1>Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>22 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B" sort="Gibson, B" uniqKey="Gibson B" first="B." last="Gibson">B. 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></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><inist:fA14 i1="10"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge, CB3 OHA</s2><s3>GBR</s3><sZ>11 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="11"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><inist:fA14 i1="12"><s1>Kapteyn Astronomical Institut, University of Groningen, Landleven 12</s1><s2>9747 AD, Groningen</s2><s3>NLD</s3><sZ>13 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="13"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>36012 Asiago (VI</s2><s3>ITA</s3><sZ>14 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="14"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>15 aut.</sZ></inist:fA14></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><inist:fA14 i1="15"><s1>Department of Physics and Astronomy, Faculty of Sciences, Macquarie University</s1><s2>NSW 2109, Sydney</s2><s3>AUS</s3><sZ>16 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation><inist:fA14 i1="16"><s1>Mullard Space Science Laboratory, University College London, Holmbury St Mary</s1><s2>Dorking, RH5 6NT</s2><s3>GBR</s3><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="06"><s1>Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="17"><s1>Dipartimento di Astronomia, Universita di Padova, Vicolo dellŠOsservatorio 2</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>19 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="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation><inist:fA14 i1="18"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></inist:fA14></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><inist:fA14 i1="08"><s1>Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>22 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="2011">2011</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>Age</term><term>Astronomical catalogues</term><term>Disk galaxies</term><term>Distance measurement</term><term>Galactic centers</term><term>Galactic planes</term><term>Galaxy structure</term><term>Metallicity</term><term>Milky Way</term><term>Physical parameter</term><term>Radial velocity</term><term>Star models</term><term>Stellar content</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Mesure distance</term><term>Modèle stellaire</term><term>Voie lactée</term><term>Paramètre physique</term><term>Catalogue astronomique</term><term>Vitesse radiale</term><term>Centre galactique</term><term>Métallicité</term><term>Age</term><term>Plan galactique</term><term>Galaxies disques</term><term>Abondance</term><term>Contenu stellaire</term><term>Structure galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than ∼ 6000 K appear to be unbiased, but those to hotter dwarfs tend to be too small by ∼10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing |z| it broadens out and its median moves to [M/H] ≃ -0.5. Mean age as a function of distance from the Galactic centre and distance |z| from the Galactic plane shows the anticipated increase in mean age with |z|.</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>532</s2></fA05><fA06><s3>p. 2</s3></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry</s1></fA08><fA11 i1="01" i2="1"><s1>BURNETT (B.)</s1></fA11><fA11 i1="02" i2="1"><s1>BINNEY (J.)</s1></fA11><fA11 i1="03" i2="1"><s1>SHARMA (S.)</s1></fA11><fA11 i1="04" i2="1"><s1>WILLIAMS (M.)</s1></fA11><fA11 i1="05" i2="1"><s1>ZWITTER (T.)</s1></fA11><fA11 i1="06" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="07" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="08" i2="1"><s1>FREEMAN (K. C.)</s1></fA11><fA11 i1="09" i2="1"><s1>FULBRIGHT (J.)</s1></fA11><fA11 i1="10" i2="1"><s1>GIBSON (B.)</s1></fA11><fA11 i1="11" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="12" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="13" i2="1"><s1>HELMI (A.)</s1></fA11><fA11 i1="14" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="15" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="16" i2="1"><s1>PARKER (Q. A.)</s1></fA11><fA11 i1="17" i2="1"><s1>SEABROKE (G. M.)</s1></fA11><fA11 i1="18" i2="1"><s1>SIEBERT (A.)</s1></fA11><fA11 i1="19" i2="1"><s1>SIVIERO (A.)</s1></fA11><fA11 i1="20" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA11 i1="21" i2="1"><s1>WATSON (F. G.)</s1></fA11><fA11 i1="22" i2="1"><s1>WYSE (R. F. G.)</s1></fA11><fA14 i1="01"><s1>Rudolf Peierls Centre for Theoretical Physics, Keble Road</s1><s2>Oxford, OX1 3NP</s2><s3>GBR</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></fA14><fA14 i1="02"><s1>Sydney Institute for Astronomy, School of Physics A28, University of Sydney</s1><s2>NSW 2006</s2><s3>AUS</s3><sZ>3 aut.</sZ><sZ>7 aut.</sZ></fA14><fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam, An der Sternwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>4 aut.</sZ><sZ>19 aut.</sZ><sZ>20 aut.</sZ></fA14><fA14 i1="04"><s1>University of Ljubljana, Faculty of Mathematics and Physics, Jadranska 19</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 aut.</sZ></fA14><fA14 i1="05"><s1>Center of excellence SPACE-SI, Askerceva cesta 12</s1><s2>1000 Ljubljana</s2><s3>SVN</s3><sZ>5 aut.</sZ></fA14><fA14 i1="06"><s1>Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>6 aut.</sZ><sZ>18 aut.</sZ></fA14><fA14 i1="07"><s1>Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd</s1><s2>ACT, Canberra</s2><s3>AUS</s3><sZ>8 aut.</sZ></fA14><fA14 i1="08"><s1>Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>9 aut.</sZ><sZ>22 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>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge, CB3 OHA</s2><s3>GBR</s3><sZ>11 aut.</sZ></fA14><fA14 i1="11"><s1>Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr. 12-14</s1><s2>69120 Heidelberg</s2><s3>DEU</s3><sZ>12 aut.</sZ></fA14><fA14 i1="12"><s1>Kapteyn Astronomical Institut, University of Groningen, Landleven 12</s1><s2>9747 AD, Groningen</s2><s3>NLD</s3><sZ>13 aut.</sZ></fA14><fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova</s1><s2>36012 Asiago (VI</s2><s3>ITA</s3><sZ>14 aut.</sZ></fA14><fA14 i1="14"><s1>Department of Physics and Astronomy, University of Victoria, PO Box 3055</s1><s2>Victoria, BC V8W 3P6</s2><s3>CAN</s3><sZ>15 aut.</sZ></fA14><fA14 i1="15"><s1>Department of Physics and Astronomy, Faculty of Sciences, Macquarie University</s1><s2>NSW 2109, Sydney</s2><s3>AUS</s3><sZ>16 aut.</sZ></fA14><fA14 i1="16"><s1>Mullard Space Science Laboratory, University College London, Holmbury St Mary</s1><s2>Dorking, RH5 6NT</s2><s3>GBR</s3><sZ>17 aut.</sZ></fA14><fA14 i1="17"><s1>Dipartimento di Astronomia, Universita di Padova, Vicolo dellŠOsservatorio 2</s1><s2>35122 Padova</s2><s3>ITA</s3><sZ>19 aut.</sZ></fA14><fA14 i1="18"><s1>Australian Astronomical Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>21 aut.</sZ></fA14><fA20><s2>A113.1-A113.14</s2></fA20><fA21><s1>2011</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>14176</s2><s5>354000507292850330</s5></fA43><fA44><s0>0000</s0><s1>© 2011 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>11-0486083</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>We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than ∼ 6000 K appear to be unbiased, but those to hotter dwarfs tend to be too small by ∼10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing |z| it broadens out and its median moves to [M/H] ≃ -0.5. Mean age as a function of distance from the Galactic centre and distance |z| from the Galactic plane shows the anticipated increase in mean age with |z|.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Mesure distance</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Distance measurement</s0><s5>26</s5></fC03><fC03 i1="02" i2="3" l="FRE"><s0>Modèle stellaire</s0><s5>27</s5></fC03><fC03 i1="02" i2="3" l="ENG"><s0>Star models</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Voie lactée</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Milky Way</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Paramètre physique</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Physical parameter</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Parámetro físico</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Catalogue astronomique</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Astronomical catalogues</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Radial velocity</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Centre galactique</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Galactic centers</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Métallicité</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Metallicity</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Metalicidad</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Age</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Age</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Edad</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Plan galactique</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Galactic planes</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Abondance</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Abundance</s0><s5>37</s5></fC03><fC03 i1="13" i2="X" l="FRE"><s0>Contenu stellaire</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="ENG"><s0>Stellar content</s0><s5>38</s5></fC03><fC03 i1="13" i2="X" l="SPA"><s0>Contenido estelar</s0><s5>38</s5></fC03><fC03 i1="14" i2="X" l="FRE"><s0>Structure galaxies</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="ENG"><s0>Galaxy structure</s0><s5>39</s5></fC03><fC03 i1="14" i2="X" l="SPA"><s0>Estructura galaxias</s0><s5>39</s5></fC03><fN21><s1>339</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 11-0486083 INIST</NO><ET>Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry</ET><AU>BURNETT (B.); BINNEY (J.); SHARMA (S.); WILLIAMS (M.); ZWITTER (T.); BIENAYME (O.); BLAND-HAWTHORN (J.); FREEMAN (K. C.); FULBRIGHT (J.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WYSE (R. F. G.)</AU><AF>Rudolf Peierls Centre for Theoretical Physics, Keble Road/Oxford, OX1 3NP/Royaume-Uni (1 aut., 2 aut.); Sydney Institute for Astronomy, School of Physics A28, University of Sydney/NSW 2006/Australie (3 aut., 7 aut.); Astrophysikalisches Institut Potsdam, An der Sternwarte 16/14482 Potsdam/Allemagne (4 aut., 19 aut., 20 aut.); University of Ljubljana, Faculty of Mathematics and Physics, Jadranska 19/1000 Ljubljana/Slovénie (5 aut.); Center of excellence SPACE-SI, Askerceva cesta 12/1000 Ljubljana/Slovénie (5 aut.); Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550, 11 rue de l'université/67000 Strasbourg/France (6 aut., 18 aut.); Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd/ACT, Canberra/Australie (8 aut.); Johns Hopkins University, Departement of Physics and Astronomy, 366 Bloomberg center, 3400 N. Charles St/Baltimore, MD 21218/Etats-Unis (9 aut., 22 aut.); Jeremiah Horrocks Institute, University of Central Lancashire/Preston, PR1 2HE/Royaume-Uni (10 aut.); Institute of Astronomy, University of Cambridge, Madingley Road/Cambridge, CB3 OHA/Royaume-Uni (11 aut.); Astronomisches Rechen-Institut, Zentrum fur Astronomie der Universität Heidelberg, Mönchhofstr. 12-14/69120 Heidelberg/Allemagne (12 aut.); Kapteyn Astronomical Institut, University of Groningen, Landleven 12/9747 AD, Groningen/Pays-Bas (13 aut.); INAF Osservatorio Astronomico di Padova/36012 Asiago (VI/Italie (14 aut.); Department of Physics and Astronomy, University of Victoria, PO Box 3055/Victoria, BC V8W 3P6/Canada (15 aut.); Department of Physics and Astronomy, Faculty of Sciences, Macquarie University/NSW 2109, Sydney/Australie (16 aut.); Mullard Space Science Laboratory, University College London, Holmbury St Mary/Dorking, RH5 6NT/Royaume-Uni (17 aut.); Dipartimento di Astronomia, Universita di Padova, Vicolo dellŠOsservatorio 2/35122 Padova/Italie (19 aut.); Australian Astronomical Observatory, PO Box 296/Epping, NSW 1710/Australie (21 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2011; Vol. 532; No. p. 2; A113.1-A113.14; Bibl. 1/2 p.</SO><LA>Anglais</LA><EA>We apply the method of Burnett & Binney (2010, MNRAS, 407, 339) for the determination of stellar distances and parameters to the internal catalogue of the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006, AJ, 132, 1645). Subsamples of stars that either have Hipparcos parallaxes or belong to well-studied clusters inspire confidence in the formal errors. Distances to dwarfs cooler than ∼ 6000 K appear to be unbiased, but those to hotter dwarfs tend to be too small by ∼10% of the formal errors. Distances to giants tend to be too large by about the same amount. The median distance error in the whole sample of 216000 stars is 28% and the error distribution is similar for both giants and dwarfs. Roughly half the stars in the RAVE survey are giants. The giant fraction is largest at low latitudes and in directions towards the Galactic Centre. Near the plane the metallicity distribution is remarkably narrow and centred on [M/H] = -0.04 dex; with increasing |z| it broadens out and its median moves to [M/H] ≃ -0.5. Mean age as a function of distance from the Galactic centre and distance |z| from the Galactic plane shows the anticipated increase in mean age with |z|.</EA><CC>001E03</CC><FD>Mesure distance; Modèle stellaire; Voie lactée; Paramètre physique; Catalogue astronomique; Vitesse radiale; Centre galactique; Métallicité; Age; Plan galactique; Galaxies disques; Abondance; Contenu stellaire; Structure galaxies</FD><ED>Distance measurement; Star models; Milky Way; Physical parameter; Astronomical catalogues; Radial velocity; Galactic centers; Metallicity; Age; Galactic planes; Disk galaxies; Abundance; Stellar content; Galaxy structure</ED><SD>Parámetro físico; Metalicidad; Edad; Contenido estelar; Estructura galaxias</SD><LO>INIST-14176.354000507292850330</LO><ID>11-0486083</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus
HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 001845 | SxmlIndent | more
Ou
HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 001845 | SxmlIndent | more
Pour mettre un lien sur cette page dans le réseau Wicri
{{Explor lien
|wiki= Wicri/Asie
|area= AustralieFrV1
|flux= PascalFrancis
|étape= Corpus
|type= RBID
|clé= Pascal:11-0486083
|texte= Distance determination for RAVE stars using stellar models: III. The nature of the RAVE survey and Milky Way chemistry
}}
| This area was generated with Dilib version V0.6.33. |  |