AustralieFrV1, PascalFrancis, Corpus, bibRecord, 003676

Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles

Identifieur interne : 003676 ( PascalFrancis/Corpus ); précédent : 003675; suivant : 003677

Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles

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

Source :

Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2008.

RBID : Pascal:08-0168036

Descripteurs français

Pascal (Inist)
- Cinématique stellaire, Pôle galactique, Etoile K, Vitesse radiale, Dénombrement stellaire, Mouvement propre, Répartition verticale, Discontinuité, Fonction luminosité, Bras spiral, Nuage moléculaire, Mécanisme formation, Galaxies disques, Dynamique, Structure galaxies.

English descriptors

KwdEn :
- Discontinuity, Disk galaxies, Dynamics, Formation mechanism, Galactic poles, Galaxy structure, K stars, Luminosity function, Molecular clouds, Proper motion, Radial velocity, Spiral arm, Star counts, Stellar kinematics, Vertical distribution.

Abstract

We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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A08	`01`	`1`	`ENG`	`@1 Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles`
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A11	`15`	`1`		`@1 STEINMETZ (M.)`
A11	`16`	`1`		`@1 WATSON (F. G.)`
A11	`17`	`1`		`@1 WILLIAMS (M.)`
A11	`18`	`1`		`@1 WYSE (R. F. G.)`
A11	`19`	`1`		`@1 ZWITTER (T.)`
A14	`01`			`@1 Observatoire Astronomique de Strasbourg @2 Strasbourg @3 FRA @Z 1 aut. @Z 2 aut. @Z 14 aut.`
A14	`02`			`@1 RSAA, Mount Stromlo Observatory @2 Canberra @3 AUS @Z 1 aut. @Z 3 aut. @Z 17 aut.`
A14	`03`			`@1 Astrophysikalisches Institut Potsdam @2 Potsdam @3 DEU @Z 1 aut. @Z 14 aut. @Z 15 aut. @Z 17 aut.`
A14	`04`			`@1 Rudolf Peierls Centre for Theoretical Physics, University of Oxford @3 GBR @Z 4 aut.`
A14	`05`			`@1 School of Physics, University of Sydney @3 AUS @Z 5 aut.`
A14	`06`			`@1 University of Central Lancashire @2 Preston @3 GBR @Z 6 aut.`
A14	`07`			`@1 Institute of Astronomy, University of Cambridge @3 GBR @Z 7 aut. @Z 13 aut.`
A14	`08`			`@1 Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg @2 Heidelberg @3 DEU @Z 8 aut.`
A14	`09`			`@1 Astronomical Institute of the University of Basel @2 Basel @3 CHE @Z 8 aut.`
A14	`10`			`@1 Kapteyn Astronomical Institute, University of Groningen @2 Groningen @3 NLD @Z 9 aut.`
A14	`11`			`@1 INAF Osservatorio Astronomico di Padova @2 Asiago @3 ITA @Z 10 aut.`
A14	`12`			`@1 University of Victoria @2 Victoria @3 CAN @Z 11 aut.`
A14	`13`			`@1 Anglo Australian Observatory @2 Sydney @3 AUS @Z 12 aut. @Z 16 aut.`
A14	`14`			`@1 Macquarie University @2 Sydney @3 AUS @Z 12 aut.`
A14	`15`			`@1 Johns Hopkins University @2 Baltimore MD @3 USA @Z 18 aut.`
A14	`16`			`@1 University of Ljubijana, Department of Physics @2 Ljubljana @3 SVN @Z 19 aut.`
A20				`@1 753-765`
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A44				`@0 0000 @1 © 2008 INIST-CNRS. All rights reserved.`
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A64	`01`	`1`		`@0 Astronomy and astrophysics : (Berlin. Print)`
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C01	`01`		`ENG`	@0 We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.
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C03	`01`	`X`	`ENG`	`@0 Stellar kinematics @5 26`
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C03	`02`	`3`	`FRE`	`@0 Pôle galactique @5 27`
C03	`02`	`3`	`ENG`	`@0 Galactic poles @5 27`
C03	`03`	`3`	`FRE`	`@0 Etoile K @5 28`
C03	`03`	`3`	`ENG`	`@0 K stars @5 28`
C03	`04`	`3`	`FRE`	`@0 Vitesse radiale @5 29`
C03	`04`	`3`	`ENG`	`@0 Radial velocity @5 29`
C03	`05`	`3`	`FRE`	`@0 Dénombrement stellaire @5 30`
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C03	`07`	`X`	`ENG`	`@0 Vertical distribution @5 32`
C03	`07`	`X`	`SPA`	`@0 Distribución vertical @5 32`
C03	`08`	`X`	`FRE`	`@0 Discontinuité @5 33`
C03	`08`	`X`	`ENG`	`@0 Discontinuity @5 33`
C03	`08`	`X`	`SPA`	`@0 Discontinuidad @5 33`
C03	`09`	`3`	`FRE`	`@0 Fonction luminosité @5 34`
C03	`09`	`3`	`ENG`	`@0 Luminosity function @5 34`
C03	`10`	`X`	`FRE`	`@0 Bras spiral @5 35`
C03	`10`	`X`	`ENG`	`@0 Spiral arm @5 35`
C03	`10`	`X`	`SPA`	`@0 Brazo espiral @5 35`
C03	`11`	`3`	`FRE`	`@0 Nuage moléculaire @5 36`
C03	`11`	`3`	`ENG`	`@0 Molecular clouds @5 36`
C03	`12`	`X`	`FRE`	`@0 Mécanisme formation @5 37`
C03	`12`	`X`	`ENG`	`@0 Formation mechanism @5 37`
C03	`12`	`X`	`SPA`	`@0 Mecanismo formacion @5 37`
C03	`13`	`3`	`FRE`	`@0 Galaxies disques @5 38`
C03	`13`	`3`	`ENG`	`@0 Disk galaxies @5 38`
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C03	`14`	`3`	`ENG`	`@0 Dynamics @5 39`
C03	`15`	`X`	`FRE`	`@0 Structure galaxies @5 40`
C03	`15`	`X`	`ENG`	`@0 Galaxy structure @5 40`
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N21				`@1 105`
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Format Inist (serveur)

NO :	PASCAL 08-0168036 INIST
ET :	Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles
AU :	VELTZ (L.); BIENAYME (O.); FREEMAN (K. C.); BINNEY (J.); BLAND-HAWTHORN (J.); GIBSON (B. K.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)
AF :	Observatoire Astronomique de Strasbourg/Strasbourg/France (1 aut., 2 aut., 14 aut.); RSAA, Mount Stromlo Observatory/Canberra/Australie (1 aut., 3 aut., 17 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (1 aut., 14 aut., 15 aut., 17 aut.); Rudolf Peierls Centre for Theoretical Physics, University of Oxford/Royaume-Uni (4 aut.); School of Physics, University of Sydney/Australie (5 aut.); University of Central Lancashire/Preston/Royaume-Uni (6 aut.); Institute of Astronomy, University of Cambridge/Royaume-Uni (7 aut., 13 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg/Heidelberg/Allemagne (8 aut.); Astronomical Institute of the University of Basel/Basel/Suisse (8 aut.); Kapteyn Astronomical Institute, University of Groningen/Groningen/Pays-Bas (9 aut.); INAF Osservatorio Astronomico di Padova/Asiago/Italie (10 aut.); University of Victoria/Victoria/Canada (11 aut.); Anglo Australian Observatory/Sydney/Australie (12 aut., 16 aut.); Macquarie University/Sydney/Australie (12 aut.); Johns Hopkins University/Baltimore MD/Etats-Unis (18 aut.); University of Ljubijana, Department of Physics/Ljubljana/Slovénie (19 aut.)
DT :	Publication en série; Niveau analytique
SO :	Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 480; No. 3; Pp. 753-765; Bibl. 3/4 p.
LA :	Anglais
EA :	We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.
CC :	001E03
FD :	Cinématique stellaire; Pôle galactique; Etoile K; Vitesse radiale; Dénombrement stellaire; Mouvement propre; Répartition verticale; Discontinuité; Fonction luminosité; Bras spiral; Nuage moléculaire; Mécanisme formation; Galaxies disques; Dynamique; Structure galaxies
ED :	Stellar kinematics; Galactic poles; K stars; Radial velocity; Star counts; Proper motion; Vertical distribution; Discontinuity; Luminosity function; Spiral arm; Molecular clouds; Formation mechanism; Disk galaxies; Dynamics; Galaxy structure
SD :	Cinematica estelar; Distribución vertical; Discontinuidad; Brazo espiral; Mecanismo formacion; Estructura galaxias
LO :	INIST-14176.354000183677150170
ID :	08-0168036

Links to Exploration step

Pascal:08-0168036

Le document en format XML

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<author><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name>
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<author><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name>
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<author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name>
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<author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name>
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<author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name>
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<author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name>
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<author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name>
<affiliation><inist:fA14 i1="02"><s1>RSAA, Mount Stromlo Observatory</s1>
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<affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam</s1>
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<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>
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</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>University of Ljubijana, Department of Physics</s1>
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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles</title>
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<author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name>
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<author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name>
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<author><name sortKey="Bland Hawthorn, J" sort="Bland Hawthorn, J" uniqKey="Bland Hawthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name>
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<author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name>
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<affiliation><inist:fA14 i1="08"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg</s1>
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<author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name>
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<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 Osservatorio Astronomico di Padova</s1>
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<s3>ITA</s3>
<sZ>10 aut.</sZ>
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<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>11 aut.</sZ>
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</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>Anglo Australian Observatory</s1>
<s2>Sydney</s2>
<s3>AUS</s3>
<sZ>12 aut.</sZ>
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<affiliation><inist:fA14 i1="14"><s1>Macquarie University</s1>
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<author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name>
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<author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name>
<affiliation><inist:fA14 i1="01"><s1>Observatoire Astronomique de Strasbourg</s1>
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<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
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<affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam</s1>
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<sZ>1 aut.</sZ>
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<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</s1>
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<sZ>1 aut.</sZ>
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<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="13"><s1>Anglo Australian Observatory</s1>
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<author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name>
<affiliation><inist:fA14 i1="02"><s1>RSAA, Mount Stromlo Observatory</s1>
<s2>Canberra</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>17 aut.</sZ>
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<affiliation><inist:fA14 i1="03"><s1>Astrophysikalisches Institut Potsdam</s1>
<s2>Potsdam</s2>
<s3>DEU</s3>
<sZ>1 aut.</sZ>
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<sZ>15 aut.</sZ>
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<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>18 aut.</sZ>
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</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>University of Ljubijana, Department of Physics</s1>
<s2>Ljubljana</s2>
<s3>SVN</s3>
<sZ>19 aut.</sZ>
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<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="2008">2008</date>
</imprint>
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<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>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Discontinuity</term>
<term>Disk galaxies</term>
<term>Dynamics</term>
<term>Formation mechanism</term>
<term>Galactic poles</term>
<term>Galaxy structure</term>
<term>K stars</term>
<term>Luminosity function</term>
<term>Molecular clouds</term>
<term>Proper motion</term>
<term>Radial velocity</term>
<term>Spiral arm</term>
<term>Star counts</term>
<term>Stellar kinematics</term>
<term>Vertical distribution</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Cinématique stellaire</term>
<term>Pôle galactique</term>
<term>Etoile K</term>
<term>Vitesse radiale</term>
<term>Dénombrement stellaire</term>
<term>Mouvement propre</term>
<term>Répartition verticale</term>
<term>Discontinuité</term>
<term>Fonction luminosité</term>
<term>Bras spiral</term>
<term>Nuage moléculaire</term>
<term>Mécanisme formation</term>
<term>Galaxies disques</term>
<term>Dynamique</term>
<term>Structure galaxies</term>
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<front><div type="abstract" xml:lang="en">We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.</div>
</front>
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<fA08 i1="01" i2="1" l="ENG"><s1>Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles</s1>
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<fA11 i1="03" i2="1"><s1>FREEMAN (K. C.)</s1>
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<fA11 i1="10" i2="1"><s1>MUNARI (U.)</s1>
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<fA11 i1="11" i2="1"><s1>NAVARRO (J. F.)</s1>
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<fA11 i1="12" i2="1"><s1>PARKER (Q. A.)</s1>
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<fA11 i1="13" i2="1"><s1>SEABROKE (G. M.)</s1>
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<fA11 i1="14" i2="1"><s1>SIEBERT (A.)</s1>
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<fA11 i1="16" i2="1"><s1>WATSON (F. G.)</s1>
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<fA11 i1="17" i2="1"><s1>WILLIAMS (M.)</s1>
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<fA11 i1="18" i2="1"><s1>WYSE (R. F. G.)</s1>
</fA11>
<fA11 i1="19" i2="1"><s1>ZWITTER (T.)</s1>
</fA11>
<fA14 i1="01"><s1>Observatoire Astronomique de Strasbourg</s1>
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<sZ>3 aut.</sZ>
<sZ>17 aut.</sZ>
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<s2>Potsdam</s2>
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<sZ>1 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>17 aut.</sZ>
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<sZ>9 aut.</sZ>
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<fA14 i1="11"><s1>INAF Osservatorio Astronomico di Padova</s1>
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<sZ>10 aut.</sZ>
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<sZ>11 aut.</sZ>
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<fA14 i1="13"><s1>Anglo Australian Observatory</s1>
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<sZ>12 aut.</sZ>
<sZ>16 aut.</sZ>
</fA14>
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<s3>AUS</s3>
<sZ>12 aut.</sZ>
</fA14>
<fA14 i1="15"><s1>Johns Hopkins University</s1>
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<sZ>18 aut.</sZ>
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<fC01 i1="01" l="ENG"><s0>We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
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<s5>26</s5>
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<s5>26</s5>
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<s5>27</s5>
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<s5>27</s5>
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<fC03 i1="03" i2="3" l="FRE"><s0>Etoile K</s0>
<s5>28</s5>
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<s5>28</s5>
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<s5>29</s5>
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<fC03 i1="04" i2="3" l="ENG"><s0>Radial velocity</s0>
<s5>29</s5>
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<fC03 i1="05" i2="3" l="FRE"><s0>Dénombrement stellaire</s0>
<s5>30</s5>
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<fC03 i1="05" i2="3" l="ENG"><s0>Star counts</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Mouvement propre</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Proper motion</s0>
<s5>31</s5>
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<fC03 i1="07" i2="X" l="FRE"><s0>Répartition verticale</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Vertical distribution</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Distribución vertical</s0>
<s5>32</s5>
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<s5>33</s5>
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<fC03 i1="08" i2="X" l="ENG"><s0>Discontinuity</s0>
<s5>33</s5>
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<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Fonction luminosité</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Luminosity function</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Bras spiral</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Spiral arm</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Brazo espiral</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Nuage moléculaire</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Molecular clouds</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE"><s0>Mécanisme formation</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG"><s0>Formation mechanism</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA"><s0>Mecanismo formacion</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="3" l="FRE"><s0>Galaxies disques</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="3" l="ENG"><s0>Disk galaxies</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="3" l="FRE"><s0>Dynamique</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="3" l="ENG"><s0>Dynamics</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="X" l="FRE"><s0>Structure galaxies</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="ENG"><s0>Galaxy structure</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="SPA"><s0>Estructura galaxias</s0>
<s5>40</s5>
</fC03>
<fN21><s1>105</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 08-0168036 INIST</NO>
<ET>Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles</ET>
<AU>VELTZ (L.); BIENAYME (O.); FREEMAN (K. C.); BINNEY (J.); BLAND-HAWTHORN (J.); GIBSON (B. K.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G. M.); SIEBERT (A.); STEINMETZ (M.); WATSON (F. G.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)</AU>
<AF>Observatoire Astronomique de Strasbourg/Strasbourg/France (1 aut., 2 aut., 14 aut.); RSAA, Mount Stromlo Observatory/Canberra/Australie (1 aut., 3 aut., 17 aut.); Astrophysikalisches Institut Potsdam/Potsdam/Allemagne (1 aut., 14 aut., 15 aut., 17 aut.); Rudolf Peierls Centre for Theoretical Physics, University of Oxford/Royaume-Uni (4 aut.); School of Physics, University of Sydney/Australie (5 aut.); University of Central Lancashire/Preston/Royaume-Uni (6 aut.); Institute of Astronomy, University of Cambridge/Royaume-Uni (7 aut., 13 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg/Heidelberg/Allemagne (8 aut.); Astronomical Institute of the University of Basel/Basel/Suisse (8 aut.); Kapteyn Astronomical Institute, University of Groningen/Groningen/Pays-Bas (9 aut.); INAF Osservatorio Astronomico di Padova/Asiago/Italie (10 aut.); University of Victoria/Victoria/Canada (11 aut.); Anglo Australian Observatory/Sydney/Australie (12 aut., 16 aut.); Macquarie University/Sydney/Australie (12 aut.); Johns Hopkins University/Baltimore MD/Etats-Unis (18 aut.); University of Ljubijana, Department of Physics/Ljubljana/Slovénie (19 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Astronomy and astrophysics : (Berlin. Print); ISSN 0004-6361; Coden AAEJAF; France; Da. 2008; Vol. 480; No. 3; Pp. 753-765; Bibl. 3/4 p.</SO>
<LA>Anglais</LA>
<EA>We analyze the distribution of G and K type stars towards the Galactic poles using RAVE and ELODIE radial velocities, 2MASS photometric star counts, and UCAC2 proper motions. The combination of photometric and 3D kinematic data allows us to disentangle and describe the vertical distribution of dwarfs, sub-giants and giants and their kinematics. We identify discontinuities within the kinematics and magnitude counts that separate the thin disk, thick disk and a hotter component. The respective scale heights of the thin disk and thick disk are 225 ± 10 pc and 1048 ± 36 pc. We also constrain the luminosity function and the kinematic distribution function. The existence of a kinematic gap between the thin and thick disks is incompatible with the thick disk having formed from the thin disk by a continuous process, such as scattering of stars by spiral arms or molecular clouds. Other mechanisms of formation of the thick disk such as "created on the spot" or smoothly "accreted" remain compatible with our findings.</EA>
<CC>001E03</CC>
<FD>Cinématique stellaire; Pôle galactique; Etoile K; Vitesse radiale; Dénombrement stellaire; Mouvement propre; Répartition verticale; Discontinuité; Fonction luminosité; Bras spiral; Nuage moléculaire; Mécanisme formation; Galaxies disques; Dynamique; Structure galaxies</FD>
<ED>Stellar kinematics; Galactic poles; K stars; Radial velocity; Star counts; Proper motion; Vertical distribution; Discontinuity; Luminosity function; Spiral arm; Molecular clouds; Formation mechanism; Disk galaxies; Dynamics; Galaxy structure</ED>
<SD>Cinematica estelar; Distribución vertical; Discontinuidad; Brazo espiral; Mecanismo formacion; Estructura galaxias</SD>
<LO>INIST-14176.354000183677150170</LO>
<ID>08-0168036</ID>
</server>
</inist>
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Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles

Galactic kinematics with RAVE data I. The distribution of stars towards the Galactic poles

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