Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models
Identifieur interne : 003170 ( PascalFrancis/Corpus ); précédent : 003169; suivant : 003171Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models
Auteurs : A. Siebert ; O. Bienayme ; J. Binney ; J. Bland-Hawthorn ; R. Campbell ; K. C. Freeman ; B. K. Gibson ; G. Gilmore ; E. K. Grebel ; A. Helmi ; U. Munari ; J. F. Navarro ; Q. A. Parker ; G. Seabroke ; A. Siviero ; M. Steinmetz ; M. Williams ; R. F. G. Wyse ; T. ZwitterSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2008.
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Abstract
We present a measure of the inclination of the velocity ellipsoid at 1 kpc below the Galactic plane using a sample of red clump giants from the RAdial Velocity Experiment (RAVE) Data Release 2. We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of 7°.3 ± 1°8. We compare this value to computed inclinations for two mass models of the Milky Way. We find that our measurement is consistent with a short scalelength of the stellar disc (Rd ≃ 2 kpc) if the dark halo is oblate or with a long scalelength (Rd ≃ 3 kpc) if the dark halo is prolate. Once combined with independent constraints on the flattening of the halo, our measurement suggests that the scalelength is approximately halfway between these two extreme values, with a preferred range 2.5-2.7 kpc for a nearly spherical halo. Nevertheless, no model can be clearly ruled out. With the continuation of the RAVE survey, it will be possible to provide a strong constraint on the mass distribution of the Milky Way using refined measurements of the orientation of the velocity ellipsoid.
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Format Inist (serveur)
| NO : | PASCAL 08-0537612 INIST |
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| ET : | Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models |
| AU : | SIEBERT (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B. K.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G.); SIVIERO (A.); STEINMETZ (M.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.) |
| AF : | Université de Strasbourg, Observatoire Astronomique/Strasbourg/France (1 aut., 2 aut.); Astrophysikalishes Institut Potsdam/Potsdam/Allemagne (1 aut., 5 aut., 16 aut., 17 aut.); Rudolf Peierls Centre for Theoretical Physics/Oxford/Royaume-Uni (3 aut.); Anglo-Australian Observatory/Sydney/Australie (4 aut., 13 aut.); Macquary University/Sydney/Australie (5 aut., 13 aut.); Australian Natianal University/Canberra/Australie (6 aut., 17 aut.); University of Central Lancashire/Preston/Royaume-Uni (7 aut.); Institute of Astronomy/Cambridge/Royaume-Uni (8 aut., 14 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg/Heidelberg/Allemagne (9 aut.); Kapteyn Astronomical Institut/Groningen/Pays-Bas (10 aut.); Astronomical Observatory of Padova in Asiago/Asiago/Italie (11 aut., 15 aut.); University of Victoria/Victoria/Canada (12 aut.); e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University/Milton Keynes/Royaume-Uni (14 aut.); Johns Hopkins University/Baltimore, MD/Etats-Unis (18 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (19 aut.) |
| DT : | Publication en série; Niveau analytique |
| SO : | Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2008; Vol. 391; No. 2; Pp. 793-801; Bibl. 3/4 p. |
| LA : | Anglais |
| EA : | We present a measure of the inclination of the velocity ellipsoid at 1 kpc below the Galactic plane using a sample of red clump giants from the RAdial Velocity Experiment (RAVE) Data Release 2. We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of 7°.3 ± 1°8. We compare this value to computed inclinations for two mass models of the Milky Way. We find that our measurement is consistent with a short scalelength of the stellar disc (Rd ≃ 2 kpc) if the dark halo is oblate or with a long scalelength (Rd ≃ 3 kpc) if the dark halo is prolate. Once combined with independent constraints on the flattening of the halo, our measurement suggests that the scalelength is approximately halfway between these two extreme values, with a preferred range 2.5-2.7 kpc for a nearly spherical halo. Nevertheless, no model can be clearly ruled out. With the continuation of the RAVE survey, it will be possible to provide a strong constraint on the mass distribution of the Milky Way using refined measurements of the orientation of the velocity ellipsoid. |
| CC : | 001E03 |
| FD : | Ellipsoïde; Modèle; Plan galactique; Géante rouge; Vitesse radiale; Voie lactée; Aplatissement; Valeur extrême; Distribution masse; Cinématique stellaire; Galaxies; Dynamique |
| ED : | Ellipsoid; Models; Galactic planes; Red giant stars; Radial velocity; Milky Way; Flattening; Extreme value; Mass distribution; Stellar kinematics; Galaxies; Dynamics |
| SD : | Elipsoide; Modelo; Aplanamiento; Valor extremo; Cinematica estelar |
| LO : | INIST-2067.354000184351160260 |
| ID : | 08-0537612 |
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Parker</name><affiliation><inist:fA14 i1="04"><s1>Anglo-Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Macquary University</s1><s2>Sydney</s2><s3>AUS</s3><sZ>5 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name><affiliation><inist:fA14 i1="08"><s1>Institute of Astronomy</s1><s2>Cambridge</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1><s2>Milton Keynes</s2><s3>GBR</s3><sZ>14 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="11"><s1>Astronomical Observatory of Padova in Asiago</s1><s2>Asiago</s2><s3>ITA</s3><sZ>11 aut.</sZ><sZ>15 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="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 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="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Australian Natianal University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>17 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="14"><s1>Johns Hopkins University</s1><s2>Baltimore, MD</s2><s3>USA</s3><sZ>18 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="15"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">08-0537612</idno><date when="2008">2008</date><idno type="stanalyst">PASCAL 08-0537612 INIST</idno><idno type="RBID">Pascal:08-0537612</idno><idno type="wicri:Area/PascalFrancis/Corpus">003170</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><inist:fA14 i1="01"><s1>Université de Strasbourg, Observatoire Astronomique</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 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="01"><s1>Université de Strasbourg, Observatoire Astronomique</s1><s2>Strasbourg</s2><s3>FRA</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="03"><s1>Rudolf Peierls Centre for Theoretical Physics</s1><s2>Oxford</s2><s3>GBR</s3><sZ>3 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="04"><s1>Anglo-Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>13 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="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Macquary University</s1><s2>Sydney</s2><s3>AUS</s3><sZ>5 aut.</sZ><sZ>13 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="06"><s1>Australian Natianal University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Gibson, B K" sort="Gibson, B K" uniqKey="Gibson B" first="B. K." last="Gibson">B. K. Gibson</name><affiliation><inist:fA14 i1="07"><s1>University of Central Lancashire</s1><s2>Preston</s2><s3>GBR</s3><sZ>7 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="08"><s1>Institute of Astronomy</s1><s2>Cambridge</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>14 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="09"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg</s1><s2>Heidelberg</s2><s3>DEU</s3><sZ>9 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="10"><s1>Kapteyn Astronomical Institut</s1><s2>Groningen</s2><s3>NLD</s3><sZ>10 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>Astronomical Observatory of Padova in Asiago</s1><s2>Asiago</s2><s3>ITA</s3><sZ>11 aut.</sZ><sZ>15 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>12 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="04"><s1>Anglo-Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="05"><s1>Macquary University</s1><s2>Sydney</s2><s3>AUS</s3><sZ>5 aut.</sZ><sZ>13 aut.</sZ></inist:fA14></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name><affiliation><inist:fA14 i1="08"><s1>Institute of Astronomy</s1><s2>Cambridge</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="13"><s1>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1><s2>Milton Keynes</s2><s3>GBR</s3><sZ>14 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="11"><s1>Astronomical Observatory of Padova in Asiago</s1><s2>Asiago</s2><s3>ITA</s3><sZ>11 aut.</sZ><sZ>15 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="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 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="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ></inist:fA14></affiliation><affiliation><inist:fA14 i1="06"><s1>Australian Natianal University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>17 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="14"><s1>Johns Hopkins University</s1><s2>Baltimore, MD</s2><s3>USA</s3><sZ>18 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="15"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></inist:fA14></affiliation></author></analytic><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno><imprint><date when="2008">2008</date></imprint></series></biblStruct></sourceDesc><seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Dynamics</term><term>Ellipsoid</term><term>Extreme value</term><term>Flattening</term><term>Galactic planes</term><term>Galaxies</term><term>Mass distribution</term><term>Milky Way</term><term>Models</term><term>Radial velocity</term><term>Red giant stars</term><term>Stellar kinematics</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Ellipsoïde</term><term>Modèle</term><term>Plan galactique</term><term>Géante rouge</term><term>Vitesse radiale</term><term>Voie lactée</term><term>Aplatissement</term><term>Valeur extrême</term><term>Distribution masse</term><term>Cinématique stellaire</term><term>Galaxies</term><term>Dynamique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present a measure of the inclination of the velocity ellipsoid at 1 kpc below the Galactic plane using a sample of red clump giants from the RAdial Velocity Experiment (RAVE) Data Release 2. We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of 7°.3 ± 1°8. We compare this value to computed inclinations for two mass models of the Milky Way. We find that our measurement is consistent with a short scalelength of the stellar disc (R<sub>d</sub> ≃ 2 kpc) if the dark halo is oblate or with a long scalelength (R<sub>d</sub> ≃ 3 kpc) if the dark halo is prolate. Once combined with independent constraints on the flattening of the halo, our measurement suggests that the scalelength is approximately halfway between these two extreme values, with a preferred range 2.5-2.7 kpc for a nearly spherical halo. Nevertheless, no model can be clearly ruled out. With the continuation of the RAVE survey, it will be possible to provide a strong constraint on the mass distribution of the Milky Way using refined measurements of the orientation of the velocity ellipsoid.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>391</s2></fA05><fA06><s2>2</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</s1></fA08><fA11 i1="01" i2="1"><s1>SIEBERT (A.)</s1></fA11><fA11 i1="02" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="03" i2="1"><s1>BINNEY (J.)</s1></fA11><fA11 i1="04" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="05" i2="1"><s1>CAMPBELL (R.)</s1></fA11><fA11 i1="06" i2="1"><s1>FREEMAN (K. C.)</s1></fA11><fA11 i1="07" i2="1"><s1>GIBSON (B. K.)</s1></fA11><fA11 i1="08" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="09" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="10" i2="1"><s1>HELMI (A.)</s1></fA11><fA11 i1="11" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="12" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="13" i2="1"><s1>PARKER (Q. A.)</s1></fA11><fA11 i1="14" i2="1"><s1>SEABROKE (G.)</s1></fA11><fA11 i1="15" i2="1"><s1>SIVIERO (A.)</s1></fA11><fA11 i1="16" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA11 i1="17" i2="1"><s1>WILLIAMS (M.)</s1></fA11><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>Université de Strasbourg, Observatoire Astronomique</s1><s2>Strasbourg</s2><s3>FRA</s3><sZ>1 aut.</sZ><sZ>2 aut.</sZ></fA14><fA14 i1="02"><s1>Astrophysikalishes Institut Potsdam</s1><s2>Potsdam</s2><s3>DEU</s3><sZ>1 aut.</sZ><sZ>5 aut.</sZ><sZ>16 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="03"><s1>Rudolf Peierls Centre for Theoretical Physics</s1><s2>Oxford</s2><s3>GBR</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>Anglo-Australian Observatory</s1><s2>Sydney</s2><s3>AUS</s3><sZ>4 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="05"><s1>Macquary University</s1><s2>Sydney</s2><s3>AUS</s3><sZ>5 aut.</sZ><sZ>13 aut.</sZ></fA14><fA14 i1="06"><s1>Australian Natianal University</s1><s2>Canberra</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>17 aut.</sZ></fA14><fA14 i1="07"><s1>University of Central Lancashire</s1><s2>Preston</s2><s3>GBR</s3><sZ>7 aut.</sZ></fA14><fA14 i1="08"><s1>Institute of Astronomy</s1><s2>Cambridge</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>14 aut.</sZ></fA14><fA14 i1="09"><s1>Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg</s1><s2>Heidelberg</s2><s3>DEU</s3><sZ>9 aut.</sZ></fA14><fA14 i1="10"><s1>Kapteyn Astronomical Institut</s1><s2>Groningen</s2><s3>NLD</s3><sZ>10 aut.</sZ></fA14><fA14 i1="11"><s1>Astronomical Observatory of Padova in Asiago</s1><s2>Asiago</s2><s3>ITA</s3><sZ>11 aut.</sZ><sZ>15 aut.</sZ></fA14><fA14 i1="12"><s1>University of Victoria</s1><s2>Victoria</s2><s3>CAN</s3><sZ>12 aut.</sZ></fA14><fA14 i1="13"><s1>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University</s1><s2>Milton Keynes</s2><s3>GBR</s3><sZ>14 aut.</sZ></fA14><fA14 i1="14"><s1>Johns Hopkins University</s1><s2>Baltimore, MD</s2><s3>USA</s3><sZ>18 aut.</sZ></fA14><fA14 i1="15"><s1>Faculty of Mathematics and Physics, University of Ljubljana</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>19 aut.</sZ></fA14><fA20><s1>793-801</s1></fA20><fA21><s1>2008</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000184351160260</s5></fA43><fA44><s0>0000</s0><s1>© 2008 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>08-0537612</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>We present a measure of the inclination of the velocity ellipsoid at 1 kpc below the Galactic plane using a sample of red clump giants from the RAdial Velocity Experiment (RAVE) Data Release 2. We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of 7°.3 ± 1°8. We compare this value to computed inclinations for two mass models of the Milky Way. We find that our measurement is consistent with a short scalelength of the stellar disc (R<sub>d</sub> ≃ 2 kpc) if the dark halo is oblate or with a long scalelength (R<sub>d</sub> ≃ 3 kpc) if the dark halo is prolate. Once combined with independent constraints on the flattening of the halo, our measurement suggests that the scalelength is approximately halfway between these two extreme values, with a preferred range 2.5-2.7 kpc for a nearly spherical halo. Nevertheless, no model can be clearly ruled out. With the continuation of the RAVE survey, it will be possible to provide a strong constraint on the mass distribution of the Milky Way using refined measurements of the orientation of the velocity ellipsoid.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="X" l="FRE"><s0>Ellipsoïde</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="ENG"><s0>Ellipsoid</s0><s5>26</s5></fC03><fC03 i1="01" i2="X" l="SPA"><s0>Elipsoide</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Modèle</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Models</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Modelo</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Plan galactique</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Galactic planes</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Géante rouge</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Red giant stars</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Vitesse radiale</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Radial velocity</s0><s5>30</s5></fC03><fC03 i1="06" i2="3" l="FRE"><s0>Voie lactée</s0><s5>31</s5></fC03><fC03 i1="06" i2="3" l="ENG"><s0>Milky Way</s0><s5>31</s5></fC03><fC03 i1="07" i2="X" l="FRE"><s0>Aplatissement</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="ENG"><s0>Flattening</s0><s5>32</s5></fC03><fC03 i1="07" i2="X" l="SPA"><s0>Aplanamiento</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Valeur extrême</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Extreme value</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Valor extremo</s0><s5>33</s5></fC03><fC03 i1="09" i2="3" l="FRE"><s0>Distribution masse</s0><s5>34</s5></fC03><fC03 i1="09" i2="3" l="ENG"><s0>Mass distribution</s0><s5>34</s5></fC03><fC03 i1="10" i2="X" l="FRE"><s0>Cinématique stellaire</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Stellar kinematics</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Cinematica estelar</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Galaxies</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Galaxies</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Dynamique</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Dynamics</s0><s5>37</s5></fC03><fN21><s1>350</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard><server><NO>PASCAL 08-0537612 INIST</NO><ET>Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</ET><AU>SIEBERT (A.); BIENAYME (O.); BINNEY (J.); BLAND-HAWTHORN (J.); CAMPBELL (R.); FREEMAN (K. C.); GIBSON (B. K.); GILMORE (G.); GREBEL (E. K.); HELMI (A.); MUNARI (U.); NAVARRO (J. F.); PARKER (Q. A.); SEABROKE (G.); SIVIERO (A.); STEINMETZ (M.); WILLIAMS (M.); WYSE (R. F. G.); ZWITTER (T.)</AU><AF>Université de Strasbourg, Observatoire Astronomique/Strasbourg/France (1 aut., 2 aut.); Astrophysikalishes Institut Potsdam/Potsdam/Allemagne (1 aut., 5 aut., 16 aut., 17 aut.); Rudolf Peierls Centre for Theoretical Physics/Oxford/Royaume-Uni (3 aut.); Anglo-Australian Observatory/Sydney/Australie (4 aut., 13 aut.); Macquary University/Sydney/Australie (5 aut., 13 aut.); Australian Natianal University/Canberra/Australie (6 aut., 17 aut.); University of Central Lancashire/Preston/Royaume-Uni (7 aut.); Institute of Astronomy/Cambridge/Royaume-Uni (8 aut., 14 aut.); Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg/Heidelberg/Allemagne (9 aut.); Kapteyn Astronomical Institut/Groningen/Pays-Bas (10 aut.); Astronomical Observatory of Padova in Asiago/Asiago/Italie (11 aut., 15 aut.); University of Victoria/Victoria/Canada (12 aut.); e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University/Milton Keynes/Royaume-Uni (14 aut.); Johns Hopkins University/Baltimore, MD/Etats-Unis (18 aut.); Faculty of Mathematics and Physics, University of Ljubljana/Ljubljana/Slovénie (19 aut.)</AF><DT>Publication en série; Niveau analytique</DT><SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2008; Vol. 391; No. 2; Pp. 793-801; Bibl. 3/4 p.</SO><LA>Anglais</LA><EA>We present a measure of the inclination of the velocity ellipsoid at 1 kpc below the Galactic plane using a sample of red clump giants from the RAdial Velocity Experiment (RAVE) Data Release 2. We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of 7°.3 ± 1°8. We compare this value to computed inclinations for two mass models of the Milky Way. We find that our measurement is consistent with a short scalelength of the stellar disc (R<sub>d</sub> ≃ 2 kpc) if the dark halo is oblate or with a long scalelength (R<sub>d</sub> ≃ 3 kpc) if the dark halo is prolate. Once combined with independent constraints on the flattening of the halo, our measurement suggests that the scalelength is approximately halfway between these two extreme values, with a preferred range 2.5-2.7 kpc for a nearly spherical halo. Nevertheless, no model can be clearly ruled out. With the continuation of the RAVE survey, it will be possible to provide a strong constraint on the mass distribution of the Milky Way using refined measurements of the orientation of the velocity ellipsoid.</EA><CC>001E03</CC><FD>Ellipsoïde; Modèle; Plan galactique; Géante rouge; Vitesse radiale; Voie lactée; Aplatissement; Valeur extrême; Distribution masse; Cinématique stellaire; Galaxies; Dynamique</FD><ED>Ellipsoid; Models; Galactic planes; Red giant stars; Radial velocity; Milky Way; Flattening; Extreme value; Mass distribution; Stellar kinematics; Galaxies; Dynamics</ED><SD>Elipsoide; Modelo; Aplanamiento; Valor extremo; Cinematica estelar</SD><LO>INIST-2067.354000184351160260</LO><ID>08-0537612</ID></server></inist></record>Pour manipuler ce document sous Unix (Dilib)
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