AustralieFrV1, PascalFrancis, Corpus, bibRecord, 002665

Distance determination for RAVE stars using stellar models

Identifieur interne : 002665 ( PascalFrancis/Corpus ); précédent : 002664; suivant : 002666

Distance determination for RAVE stars using stellar models

Auteurs : M. A. Breddels ; M. C. Smith ; A. Helmi ; O. Bienayme ; J. Binney ; J. Bland-Hawthorn ; C. Boeche ; B. C. M. Burnett ; R. Campbell ; K. C. Freeman ; B. Gibson ; G. Gilmore ; E. K. Grebel ; U. Munari ; J. F. Navarro ; Q. A. Parker ; G. M. Seabroke ; A. Siebert ; A. Siviero ; M. Steinmetz ; F. G. Watson ; M. Williams ; R. F. G. Wyse ; T. Zwitter

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2010.

RBID : Pascal:10-0258264

Descripteurs français

Pascal (Inist)
- Mesure distance, Modèle stellaire, Espace phase, Température effective, Gravité surface, Métallicité, Photométrie, Magnitude absolue, Mouvement propre, Vitesse radiale, Amas ouvert, Etoile séquence principale, Etoile géante, Incertitude, Plan galactique, Cinématique, Sous structure, Etoile proche, Etoile naine, Ellipsoïde, Catalogue astronomique, Méthode numérique, Méthode statistique, Galaxies, Dynamique, Structure galaxies, Amas stellaire.

English descriptors

KwdEn :
- Absolute magnitude, Astronomical catalogues, Distance measurement, Dwarf stars, Dynamics, Effective temperature, Ellipsoid, Galactic planes, Galaxies, Galaxy structure, Giant stars, Kinematics, Main sequence stars, Metallicity, Nearby stars, Numerical method, Open clusters, Phase space, Photometry, Proper motion, Radial velocity, Star clusters, Star models, Statistical method, Substructure, Surface gravity, Uncertainty.

Abstract

Aims. We develop a method for deriving distances from spectroscopic data and obtaining full 6D phase-space coordinates for the RAVE survey's second data release. Methods. We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J - K_s) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able to derive the full 6D phase-space coordinates for a large sample of RAVE stars. This method is tested with artificial data, Hipparcos trigonometric parallaxes and observations of the open cluster M 67. Results. When we applied our method to a set of 16 146 stars, we found that 25% (4037) of the stars have relative (statistical) distance errors of <35%, while 50% (8073) and 75% (12 110) have relative (statistical) errors smaller than 45% and 50%, respectively. Our various tests show that we can reliably estimate distances for main-sequence stars, but there is an indication of potential systematic problems with giant stars owing to uncertainties in the underlying stellar models. For the main-sequence star sample (defined as those with log(g) > 4), 25% (1744) have relative distance errors <31%, while 50% (3488) and 75% (5231) have relative errors smaller than 36% and 42%, respectively. Our full dataset shows the expected decrease in the metallicity of stars as a function of distance from the Galactic plane. The known kinematic substructures in the U and V velocity components of nearby dwarf stars are apparent in our dataset, confirming the accuracy of our data and the reliability of our technique. We provide independent measurements of the orientation of the UV velocity ellipsoid and of the solar motion, and they are in very good agreement with previous work. Conclusions. The distance catalogue for the RAVE second data release is available at http: //www. astro. rug. nl/∼rave, and will be updated in the future to include new data releases.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A14	`15`			`@1 Johns Hopkins University @2 Baltimore, MD @3 USA @Z 23 aut.`
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Format Inist (serveur)

NO :	PASCAL 10-0258264 INIST
ET :	Distance determination for RAVE stars using stellar models
AU :	BREDDELS (M. A.); SMITH (M. C.); HELMI (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); BOECHE (C.); BURNETT (B. C. M.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)
AF :	Kapteyn Astronomical Institute, University of Groningen, PO Box 800/9700 AV Groningen/Pays-Bas (1 aut., 2 aut., 3 aut.); Kavli Institute for Astronomy and Astrophysics, Peking University/Beijing 100871/Chine (2 aut.); Institute of Astronomy, University of Cambridge/Cambridge/Royaume-Uni (2 aut., 12 aut.); Université de Strasbourg, Observatoire Astronomique/Strasbourg/France (4 aut., 18 aut.); Rudolf Peierls Centre for Theoretical Physics/Oxford/Royaume-Uni (5 aut., 8 aut.); Anglo-Australian Observatory/Sydney/Australie (6 aut., 21 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (7 aut., 9 aut., 19 aut., 20 aut., 22 aut.); RSAA, Australian National University/Canberra/Australie (10 aut.); University of Central Lancashire/Preston/Royaume-Uni (11 aut.); Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg/Heidelberg/Allemagne (13 aut.); INAF, Astronomical Observatory of Padova/Asiago station/Italie (14 aut., 19 aut.); University of Victoria/Victoria/Canada (15 aut.); Macquarie University/Sydney/Australie (16 aut.); ECentre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University/Milton Keynes/Royaume-Uni (17 aut.); Johns Hopkins University/Baltimore, MD/Etats-Unis (23 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (24 aut.)
DT :	Publication en série; Niveau analytique
SO :	Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 511; 511A90.1-511A90.16; Bibl. 1/2 p.
LA :	Anglais
EA :	Aims. We develop a method for deriving distances from spectroscopic data and obtaining full 6D phase-space coordinates for the RAVE survey's second data release. Methods. We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J - K_s) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able to derive the full 6D phase-space coordinates for a large sample of RAVE stars. This method is tested with artificial data, Hipparcos trigonometric parallaxes and observations of the open cluster M 67. Results. When we applied our method to a set of 16 146 stars, we found that 25% (4037) of the stars have relative (statistical) distance errors of <35%, while 50% (8073) and 75% (12 110) have relative (statistical) errors smaller than 45% and 50%, respectively. Our various tests show that we can reliably estimate distances for main-sequence stars, but there is an indication of potential systematic problems with giant stars owing to uncertainties in the underlying stellar models. For the main-sequence star sample (defined as those with log(g) > 4), 25% (1744) have relative distance errors <31%, while 50% (3488) and 75% (5231) have relative errors smaller than 36% and 42%, respectively. Our full dataset shows the expected decrease in the metallicity of stars as a function of distance from the Galactic plane. The known kinematic substructures in the U and V velocity components of nearby dwarf stars are apparent in our dataset, confirming the accuracy of our data and the reliability of our technique. We provide independent measurements of the orientation of the UV velocity ellipsoid and of the solar motion, and they are in very good agreement with previous work. Conclusions. The distance catalogue for the RAVE second data release is available at http: //www. astro. rug. nl/∼rave, and will be updated in the future to include new data releases.
CC :	001E03
FD :	Mesure distance; Modèle stellaire; Espace phase; Température effective; Gravité surface; Métallicité; Photométrie; Magnitude absolue; Mouvement propre; Vitesse radiale; Amas ouvert; Etoile séquence principale; Etoile géante; Incertitude; Plan galactique; Cinématique; Sous structure; Etoile proche; Etoile naine; Ellipsoïde; Catalogue astronomique; Méthode numérique; Méthode statistique; Galaxies; Dynamique; Structure galaxies; Amas stellaire
ED :	Distance measurement; Star models; Phase space; Effective temperature; Surface gravity; Metallicity; Photometry; Absolute magnitude; Proper motion; Radial velocity; Open clusters; Main sequence stars; Giant stars; Uncertainty; Galactic planes; Kinematics; Substructure; Nearby stars; Dwarf stars; Ellipsoid; Astronomical catalogues; Numerical method; Statistical method; Galaxies; Dynamics; Galaxy structure; Star clusters
SD :	Metalicidad; Magnitud absoluta; Incertidumbre; Subestructura; Elipsoide; Método numérico; Método estadístico; Estructura galaxias
LO :	INIST-14176.354000182126301000
ID :	10-0258264

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Pascal:10-0258264

Le document en format XML

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<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="08"><s1>RSAA, Australian National University</s1>
<s2>Canberra</s2>
<s3>AUS</s3>
<sZ>10 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>University of Central Lancashire</s1>
<s2>Preston</s2>
<s3>GBR</s3>
<sZ>11 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="03"><s1>Institute of Astronomy, University of Cambridge</s1>
<s2>Cambridge</s2>
<s3>GBR</s3>
<sZ>2 aut.</sZ>
<sZ>12 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="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1>
<s2>Heidelberg</s2>
<s3>DEU</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="11"><s1>INAF, Astronomical Observatory of Padova</s1>
<s2>Asiago station</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>19 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</s1>
<s2>Victoria</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="13"><s1>Macquarie University</s1>
<s2>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="14"><s1>ECentre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1>
<s2>Milton Keynes</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="04"><s1>Université de Strasbourg, Observatoire Astronomique</s1>
<s2>Strasbourg</s2>
<s3>FRA</s3>
<sZ>4 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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="11"><s1>INAF, Astronomical Observatory of Padova</s1>
<s2>Asiago station</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 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="06"><s1>Anglo-Australian Observatory</s1>
<s2>Sydney</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
<sZ>21 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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 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="15"><s1>Johns Hopkins University</s1>
<s2>Baltimore, MD</s2>
<s3>USA</s3>
<sZ>23 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="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1>
<s2>Ljubljana</s2>
<s3>SVN</s3>
<sZ>24 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">10-0258264</idno>
<date when="2010">2010</date>
<idno type="stanalyst">PASCAL 10-0258264 INIST</idno>
<idno type="RBID">Pascal:10-0258264</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">002665</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Distance determination for RAVE stars using stellar models</title>
<author><name sortKey="Breddels, M A" sort="Breddels, M A" uniqKey="Breddels M" first="M. A." last="Breddels">M. A. Breddels</name>
<affiliation><inist:fA14 i1="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1>
<s2>9700 AV Groningen</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smith, M C" sort="Smith, M C" uniqKey="Smith M" first="M. C." last="Smith">M. C. Smith</name>
<affiliation><inist:fA14 i1="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1>
<s2>9700 AV Groningen</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>Kavli Institute for Astronomy and Astrophysics, Peking University</s1>
<s2>Beijing 100871</s2>
<s3>CHN</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="03"><s1>Institute of Astronomy, University of Cambridge</s1>
<s2>Cambridge</s2>
<s3>GBR</s3>
<sZ>2 aut.</sZ>
<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="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1>
<s2>9700 AV Groningen</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 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="04"><s1>Université de Strasbourg, Observatoire Astronomique</s1>
<s2>Strasbourg</s2>
<s3>FRA</s3>
<sZ>4 aut.</sZ>
<sZ>18 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="05"><s1>Rudolf Peierls Centre for Theoretical Physics</s1>
<s2>Oxford</s2>
<s3>GBR</s3>
<sZ>5 aut.</sZ>
<sZ>8 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="06"><s1>Anglo-Australian Observatory</s1>
<s2>Sydney</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
<sZ>21 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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Burnett, B C M" sort="Burnett, B C M" uniqKey="Burnett B" first="B. C. M." last="Burnett">B. C. M. Burnett</name>
<affiliation><inist:fA14 i1="05"><s1>Rudolf Peierls Centre for Theoretical Physics</s1>
<s2>Oxford</s2>
<s3>GBR</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name>
<affiliation><inist:fA14 i1="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 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="08"><s1>RSAA, Australian National University</s1>
<s2>Canberra</s2>
<s3>AUS</s3>
<sZ>10 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>University of Central Lancashire</s1>
<s2>Preston</s2>
<s3>GBR</s3>
<sZ>11 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="03"><s1>Institute of Astronomy, University of Cambridge</s1>
<s2>Cambridge</s2>
<s3>GBR</s3>
<sZ>2 aut.</sZ>
<sZ>12 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="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1>
<s2>Heidelberg</s2>
<s3>DEU</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="11"><s1>INAF, Astronomical Observatory of Padova</s1>
<s2>Asiago station</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>19 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</s1>
<s2>Victoria</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="13"><s1>Macquarie University</s1>
<s2>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="14"><s1>ECentre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1>
<s2>Milton Keynes</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="04"><s1>Université de Strasbourg, Observatoire Astronomique</s1>
<s2>Strasbourg</s2>
<s3>FRA</s3>
<sZ>4 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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="11"><s1>INAF, Astronomical Observatory of Padova</s1>
<s2>Asiago station</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 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="06"><s1>Anglo-Australian Observatory</s1>
<s2>Sydney</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
<sZ>21 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="07"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 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="15"><s1>Johns Hopkins University</s1>
<s2>Baltimore, MD</s2>
<s3>USA</s3>
<sZ>23 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="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1>
<s2>Ljubljana</s2>
<s3>SVN</s3>
<sZ>24 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="2010">2010</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>Absolute magnitude</term>
<term>Astronomical catalogues</term>
<term>Distance measurement</term>
<term>Dwarf stars</term>
<term>Dynamics</term>
<term>Effective temperature</term>
<term>Ellipsoid</term>
<term>Galactic planes</term>
<term>Galaxies</term>
<term>Galaxy structure</term>
<term>Giant stars</term>
<term>Kinematics</term>
<term>Main sequence stars</term>
<term>Metallicity</term>
<term>Nearby stars</term>
<term>Numerical method</term>
<term>Open clusters</term>
<term>Phase space</term>
<term>Photometry</term>
<term>Proper motion</term>
<term>Radial velocity</term>
<term>Star clusters</term>
<term>Star models</term>
<term>Statistical method</term>
<term>Substructure</term>
<term>Surface gravity</term>
<term>Uncertainty</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Mesure distance</term>
<term>Modèle stellaire</term>
<term>Espace phase</term>
<term>Température effective</term>
<term>Gravité surface</term>
<term>Métallicité</term>
<term>Photométrie</term>
<term>Magnitude absolue</term>
<term>Mouvement propre</term>
<term>Vitesse radiale</term>
<term>Amas ouvert</term>
<term>Etoile séquence principale</term>
<term>Etoile géante</term>
<term>Incertitude</term>
<term>Plan galactique</term>
<term>Cinématique</term>
<term>Sous structure</term>
<term>Etoile proche</term>
<term>Etoile naine</term>
<term>Ellipsoïde</term>
<term>Catalogue astronomique</term>
<term>Méthode numérique</term>
<term>Méthode statistique</term>
<term>Galaxies</term>
<term>Dynamique</term>
<term>Structure galaxies</term>
<term>Amas stellaire</term>
</keywords>
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</teiHeader>
<front><div type="abstract" xml:lang="en">Aims. We develop a method for deriving distances from spectroscopic data and obtaining full 6D phase-space coordinates for the RAVE survey's second data release. Methods. We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J - K<sub>s</sub>
) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able to derive the full 6D phase-space coordinates for a large sample of RAVE stars. This method is tested with artificial data, Hipparcos trigonometric parallaxes and observations of the open cluster M 67. Results. When we applied our method to a set of 16 146 stars, we found that 25% (4037) of the stars have relative (statistical) distance errors of <35%, while 50% (8073) and 75% (12 110) have relative (statistical) errors smaller than 45% and 50%, respectively. Our various tests show that we can reliably estimate distances for main-sequence stars, but there is an indication of potential systematic problems with giant stars owing to uncertainties in the underlying stellar models. For the main-sequence star sample (defined as those with log(g) > 4), 25% (1744) have relative distance errors <31%, while 50% (3488) and 75% (5231) have relative errors smaller than 36% and 42%, respectively. Our full dataset shows the expected decrease in the metallicity of stars as a function of distance from the Galactic plane. The known kinematic substructures in the U and V velocity components of nearby dwarf stars are apparent in our dataset, confirming the accuracy of our data and the reliability of our technique. We provide independent measurements of the orientation of the UV velocity ellipsoid and of the solar motion, and they are in very good agreement with previous work. Conclusions. The distance catalogue for the RAVE second data release is available at http: //www. astro. rug. nl/∼rave, and will be updated in the future to include new data releases.</div>
</front>
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<fA08 i1="01" i2="1" l="ENG"><s1>Distance determination for RAVE stars using stellar models</s1>
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<fA11 i1="01" i2="1"><s1>BREDDELS (M. A.)</s1>
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<s3>CHN</s3>
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</fA14>
<fA14 i1="03"><s1>Institute of Astronomy, University of Cambridge</s1>
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<sZ>2 aut.</sZ>
<sZ>12 aut.</sZ>
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<fA14 i1="04"><s1>Université de Strasbourg, Observatoire Astronomique</s1>
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<sZ>4 aut.</sZ>
<sZ>18 aut.</sZ>
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<sZ>6 aut.</sZ>
<sZ>21 aut.</sZ>
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<fA14 i1="07"><s1>Astrophysikalisches Institut Potsdam</s1>
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<sZ>7 aut.</sZ>
<sZ>9 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>22 aut.</sZ>
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<fA14 i1="08"><s1>RSAA, Australian National University</s1>
<s2>Canberra</s2>
<s3>AUS</s3>
<sZ>10 aut.</sZ>
</fA14>
<fA14 i1="09"><s1>University of Central Lancashire</s1>
<s2>Preston</s2>
<s3>GBR</s3>
<sZ>11 aut.</sZ>
</fA14>
<fA14 i1="10"><s1>Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg</s1>
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<s3>DEU</s3>
<sZ>13 aut.</sZ>
</fA14>
<fA14 i1="11"><s1>INAF, Astronomical Observatory of Padova</s1>
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<sZ>14 aut.</sZ>
<sZ>19 aut.</sZ>
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<fA14 i1="12"><s1>University of Victoria</s1>
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<s3>CAN</s3>
<sZ>15 aut.</sZ>
</fA14>
<fA14 i1="13"><s1>Macquarie University</s1>
<s2>Sydney</s2>
<s3>AUS</s3>
<sZ>16 aut.</sZ>
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<fA14 i1="14"><s1>ECentre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1>
<s2>Milton Keynes</s2>
<s3>GBR</s3>
<sZ>17 aut.</sZ>
</fA14>
<fA14 i1="15"><s1>Johns Hopkins University</s1>
<s2>Baltimore, MD</s2>
<s3>USA</s3>
<sZ>23 aut.</sZ>
</fA14>
<fA14 i1="16"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1>
<s2>Ljubljana</s2>
<s3>SVN</s3>
<sZ>24 aut.</sZ>
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<fA20><s2>511A90.1-511A90.16</s2>
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<fA47 i1="01" i2="1"><s0>10-0258264</s0>
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<fC01 i1="01" l="ENG"><s0>Aims. We develop a method for deriving distances from spectroscopic data and obtaining full 6D phase-space coordinates for the RAVE survey's second data release. Methods. We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J - K<sub>s</sub>
) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able to derive the full 6D phase-space coordinates for a large sample of RAVE stars. This method is tested with artificial data, Hipparcos trigonometric parallaxes and observations of the open cluster M 67. Results. When we applied our method to a set of 16 146 stars, we found that 25% (4037) of the stars have relative (statistical) distance errors of <35%, while 50% (8073) and 75% (12 110) have relative (statistical) errors smaller than 45% and 50%, respectively. Our various tests show that we can reliably estimate distances for main-sequence stars, but there is an indication of potential systematic problems with giant stars owing to uncertainties in the underlying stellar models. For the main-sequence star sample (defined as those with log(g) > 4), 25% (1744) have relative distance errors <31%, while 50% (3488) and 75% (5231) have relative errors smaller than 36% and 42%, respectively. Our full dataset shows the expected decrease in the metallicity of stars as a function of distance from the Galactic plane. The known kinematic substructures in the U and V velocity components of nearby dwarf stars are apparent in our dataset, confirming the accuracy of our data and the reliability of our technique. We provide independent measurements of the orientation of the UV velocity ellipsoid and of the solar motion, and they are in very good agreement with previous work. Conclusions. The distance catalogue for the RAVE second data release is available at http: //www. astro. rug. nl/∼rave, and will be updated in the future to include new data releases.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Mesure distance</s0>
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<s5>26</s5>
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<s5>28</s5>
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<s5>29</s5>
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<s5>30</s5>
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<s5>30</s5>
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<s5>31</s5>
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<s5>32</s5>
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<s5>32</s5>
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<fC03 i1="08" i2="X" l="FRE"><s0>Magnitude absolue</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Absolute magnitude</s0>
<s5>33</s5>
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<fC03 i1="08" i2="X" l="SPA"><s0>Magnitud absoluta</s0>
<s5>33</s5>
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<fC03 i1="09" i2="3" l="FRE"><s0>Mouvement propre</s0>
<s5>34</s5>
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<fC03 i1="09" i2="3" l="ENG"><s0>Proper motion</s0>
<s5>34</s5>
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<fC03 i1="10" i2="3" l="FRE"><s0>Vitesse radiale</s0>
<s5>35</s5>
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<fC03 i1="10" i2="3" l="ENG"><s0>Radial velocity</s0>
<s5>35</s5>
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<s5>36</s5>
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<s5>37</s5>
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<fC03 i1="14" i2="X" l="SPA"><s0>Incertidumbre</s0>
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<s5>40</s5>
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<s5>40</s5>
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<s5>41</s5>
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<s5>42</s5>
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<s5>43</s5>
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<fC03 i1="18" i2="3" l="ENG"><s0>Nearby stars</s0>
<s5>43</s5>
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<fC03 i1="19" i2="3" l="FRE"><s0>Etoile naine</s0>
<s5>44</s5>
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<fC03 i1="19" i2="3" l="ENG"><s0>Dwarf stars</s0>
<s5>44</s5>
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<fC03 i1="20" i2="X" l="FRE"><s0>Ellipsoïde</s0>
<s5>45</s5>
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<s5>45</s5>
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<s5>47</s5>
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<s5>47</s5>
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<s5>48</s5>
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<fC03 i1="23" i2="X" l="ENG"><s0>Statistical method</s0>
<s5>48</s5>
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<s5>48</s5>
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<fC03 i1="24" i2="3" l="FRE"><s0>Galaxies</s0>
<s5>49</s5>
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<s5>49</s5>
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<s5>50</s5>
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<fC03 i1="25" i2="3" l="ENG"><s0>Dynamics</s0>
<s5>50</s5>
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<fC03 i1="26" i2="X" l="FRE"><s0>Structure galaxies</s0>
<s5>90</s5>
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<fC03 i1="26" i2="X" l="ENG"><s0>Galaxy structure</s0>
<s5>90</s5>
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<fC03 i1="26" i2="X" l="SPA"><s0>Estructura galaxias</s0>
<s5>90</s5>
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<s5>91</s5>
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<fC03 i1="27" i2="3" l="ENG"><s0>Star clusters</s0>
<s5>91</s5>
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<fN21><s1>172</s1>
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<server><NO>PASCAL 10-0258264 INIST</NO>
<ET>Distance determination for RAVE stars using stellar models</ET>
<AU>BREDDELS (M. A.); SMITH (M. C.); HELMI (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); BOECHE (C.); BURNETT (B. C. M.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B.); GILMORE (G.); GREBEL (E. K.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); SIVIERO (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)</AU>
<AF>Kapteyn Astronomical Institute, University of Groningen, PO Box 800/9700 AV Groningen/Pays-Bas (1 aut., 2 aut., 3 aut.); Kavli Institute for Astronomy and Astrophysics, Peking University/Beijing 100871/Chine (2 aut.); Institute of Astronomy, University of Cambridge/Cambridge/Royaume-Uni (2 aut., 12 aut.); Université de Strasbourg, Observatoire Astronomique/Strasbourg/France (4 aut., 18 aut.); Rudolf Peierls Centre for Theoretical Physics/Oxford/Royaume-Uni (5 aut., 8 aut.); Anglo-Australian Observatory/Sydney/Australie (6 aut., 21 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (7 aut., 9 aut., 19 aut., 20 aut., 22 aut.); RSAA, Australian National University/Canberra/Australie (10 aut.); University of Central Lancashire/Preston/Royaume-Uni (11 aut.); Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg/Heidelberg/Allemagne (13 aut.); INAF, Astronomical Observatory of Padova/Asiago station/Italie (14 aut., 19 aut.); University of Victoria/Victoria/Canada (15 aut.); Macquarie University/Sydney/Australie (16 aut.); ECentre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University/Milton Keynes/Royaume-Uni (17 aut.); Johns Hopkins University/Baltimore, MD/Etats-Unis (23 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (24 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2010; Vol. 511; 511A90.1-511A90.16; Bibl. 1/2 p.</SO>
<LA>Anglais</LA>
<EA>Aims. We develop a method for deriving distances from spectroscopic data and obtaining full 6D phase-space coordinates for the RAVE survey's second data release. Methods. We used stellar models combined with atmospheric properties from RAVE (effective temperature, surface gravity and metallicity) and (J - K<sub>s</sub>
) photometry from archival sources to derive absolute magnitudes. In combination with apparent magnitudes, sky coordinates, proper motions from a variety of sources and radial velocities from RAVE, we are able to derive the full 6D phase-space coordinates for a large sample of RAVE stars. This method is tested with artificial data, Hipparcos trigonometric parallaxes and observations of the open cluster M 67. Results. When we applied our method to a set of 16 146 stars, we found that 25% (4037) of the stars have relative (statistical) distance errors of <35%, while 50% (8073) and 75% (12 110) have relative (statistical) errors smaller than 45% and 50%, respectively. Our various tests show that we can reliably estimate distances for main-sequence stars, but there is an indication of potential systematic problems with giant stars owing to uncertainties in the underlying stellar models. For the main-sequence star sample (defined as those with log(g) > 4), 25% (1744) have relative distance errors <31%, while 50% (3488) and 75% (5231) have relative errors smaller than 36% and 42%, respectively. Our full dataset shows the expected decrease in the metallicity of stars as a function of distance from the Galactic plane. The known kinematic substructures in the U and V velocity components of nearby dwarf stars are apparent in our dataset, confirming the accuracy of our data and the reliability of our technique. We provide independent measurements of the orientation of the UV velocity ellipsoid and of the solar motion, and they are in very good agreement with previous work. Conclusions. The distance catalogue for the RAVE second data release is available at http: //www. astro. rug. nl/∼rave, and will be updated in the future to include new data releases.</EA>
<CC>001E03</CC>
<FD>Mesure distance; Modèle stellaire; Espace phase; Température effective; Gravité surface; Métallicité; Photométrie; Magnitude absolue; Mouvement propre; Vitesse radiale; Amas ouvert; Etoile séquence principale; Etoile géante; Incertitude; Plan galactique; Cinématique; Sous structure; Etoile proche; Etoile naine; Ellipsoïde; Catalogue astronomique; Méthode numérique; Méthode statistique; Galaxies; Dynamique; Structure galaxies; Amas stellaire</FD>
<ED>Distance measurement; Star models; Phase space; Effective temperature; Surface gravity; Metallicity; Photometry; Absolute magnitude; Proper motion; Radial velocity; Open clusters; Main sequence stars; Giant stars; Uncertainty; Galactic planes; Kinematics; Substructure; Nearby stars; Dwarf stars; Ellipsoid; Astronomical catalogues; Numerical method; Statistical method; Galaxies; Dynamics; Galaxy structure; Star clusters</ED>
<SD>Metalicidad; Magnitud absoluta; Incertidumbre; Subestructura; Elipsoide; Método numérico; Método estadístico; Estructura galaxias</SD>
<LO>INIST-14176.354000182126301000</LO>
<ID>10-0258264</ID>
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	Serveur d'exploration sur les relations entre la France et l'Australie
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Serveur d'exploration sur les relations entre la France et l'Australie

Distance determination for RAVE stars using stellar models

Distance determination for RAVE stars using stellar models

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