Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models
Identifieur interne : 001F27 ( Istex/Corpus ); précédent : 001F26; suivant : 001F28Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models
Auteurs : A. Siebert ; O. Bienaymé ; 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 ] ; 2008-12-01.
English descriptors
- KwdEn :
- 2mass survey, Amendt cuddeford, Attening, Axis ratio, Bienaym, Binney, Binney tremaine, Black histogram, Bottom panel, Cardinal directions, Carlo, Clump, Clump candidates, Clump giants, Clump sample, Clump stars, Constraint, Contamination, Contamination fraction, Dark halo, Data points, Data release, Dehnen, Dehnen binney, Direct measurement, Disc, Distance interval, Ellipsoid, Error bars, Error budget, Error distribution, Error distributions, Error laws, Extreme cases, Famaey, Foreground, Foreground objects, Foreground population, Foreground stars, Full line, Galactic, Galactic centre, Galactic dynamics, Galactic plane, Galactic pole, Galactic potentials, Gilmore, Good agreement, Grey gaussian curve, Halo, Halo density, Inclination, Individual errors, Johns hopkins university, Journal compilation, Kuijken gilmore, Large error bars, Local velocity ellipsoid, Majewski, Mass distribution, Mass model, Mass models, Massive disc, Massive halo, Mnras, Monte carlo realization, Monte carlo sampling, Oblate, Oblate halo, Open circles, Orbit library, Original sample, Other hand, Princeton univ, Prolate, Prolate haloes, Prolate models, Proper motions, Radial velocity experiment, Random realization, Rotation curve, Same procedure, Scalelength, Second data release, Selection criteria, Selection criterion, Selection function, Short scalelength, Siebert, Single orbit, Small fraction, Solar neighbourhood, Spherical halo, Standard deviation, Stellar, Stellar disc, Stellar parameters, Substructure, Thick line, Tilt, Tilt angle, Unbiased measurement, Upper limit, Velocity, Velocity criteria, Velocity criterion, Velocity distribution, Velocity ellipsoid, Velocity error anisotropy, Velocity error distributions, Velocity errors, Velocity space, Velocity structures, Velocity substructures, Velocity trends, Velocity vector.
- Teeft :
- 2mass survey, Amendt cuddeford, Attening, Axis ratio, Bienaym, Binney, Binney tremaine, Black histogram, Bottom panel, Cardinal directions, Carlo, Clump, Clump candidates, Clump giants, Clump sample, Clump stars, Constraint, Contamination, Contamination fraction, Dark halo, Data points, Data release, Dehnen, Dehnen binney, Direct measurement, Disc, Distance interval, Ellipsoid, Error bars, Error budget, Error distribution, Error distributions, Error laws, Extreme cases, Famaey, Foreground, Foreground objects, Foreground population, Foreground stars, Full line, Galactic, Galactic centre, Galactic dynamics, Galactic plane, Galactic pole, Galactic potentials, Gilmore, Good agreement, Grey gaussian curve, Halo, Halo density, Inclination, Individual errors, Johns hopkins university, Journal compilation, Kuijken gilmore, Large error bars, Local velocity ellipsoid, Majewski, Mass distribution, Mass model, Mass models, Massive disc, Massive halo, Mnras, Monte carlo realization, Monte carlo sampling, Oblate, Oblate halo, Open circles, Orbit library, Original sample, Other hand, Princeton univ, Prolate, Prolate haloes, Prolate models, Proper motions, Radial velocity experiment, Random realization, Rotation curve, Same procedure, Scalelength, Second data release, Selection criteria, Selection criterion, Selection function, Short scalelength, Siebert, Single orbit, Small fraction, Solar neighbourhood, Spherical halo, Standard deviation, Stellar, Stellar disc, Stellar parameters, Substructure, Thick line, Tilt, Tilt angle, Unbiased measurement, Upper limit, Velocity, Velocity criteria, Velocity criterion, Velocity distribution, Velocity ellipsoid, Velocity error anisotropy, Velocity error distributions, Velocity errors, Velocity space, Velocity structures, Velocity substructures, Velocity trends, Velocity vector.
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 . 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.
Url:
DOI: 10.1111/j.1365-2966.2008.13912.x
Links to Exploration step
ISTEX:A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00ELe document en format XML
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Bienaymé</name><affiliation><mods:affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</mods:affiliation></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><mods:affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford</mods:affiliation></affiliation></author><author><name sortKey="Bland Awthorn, J" sort="Bland Awthorn, J" uniqKey="Bland Awthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, Australia</mods:affiliation></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><mods:affiliation>Australian Natianal University, Canberra, Australia</mods:affiliation></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><mods:affiliation>University of Central Lancashire, Preston</mods:affiliation></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. 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Seabroke</name><affiliation><mods:affiliation>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University, Milton Keynes</mods:affiliation></affiliation><affiliation><mods:affiliation>Institute of Astronomy, Cambridge</mods:affiliation></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><mods:affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy</mods:affiliation></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. 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Zwitter</name><affiliation><mods:affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E</idno><date when="2008" year="2008">2008</date><idno type="doi">10.1111/j.1365-2966.2008.13912.x</idno><idno type="url">https://api.istex.fr/document/A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">001F27</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">001F27</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">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><mods:affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</mods:affiliation></affiliation><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: siebert@astro.u‐strasbg.fr</mods:affiliation></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienaymé">O. Bienaymé</name><affiliation><mods:affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</mods:affiliation></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation><mods:affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford</mods:affiliation></affiliation></author><author><name sortKey="Bland Awthorn, J" sort="Bland Awthorn, J" uniqKey="Bland Awthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><affiliation><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation></author><author><name sortKey="Campbell, R" sort="Campbell, R" uniqKey="Campbell R" first="R." last="Campbell">R. Campbell</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, Australia</mods:affiliation></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><mods:affiliation>Australian Natianal University, Canberra, Australia</mods:affiliation></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><mods:affiliation>University of Central Lancashire, Preston</mods:affiliation></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation><mods:affiliation>Institute of Astronomy, Cambridge</mods:affiliation></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><mods:affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany</mods:affiliation></affiliation></author><author><name sortKey="Helmi, A" sort="Helmi, A" uniqKey="Helmi A" first="A." last="Helmi">A. Helmi</name><affiliation><mods:affiliation>Kapteyn Astronomical Institut, Groningen, the Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation><mods:affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy</mods:affiliation></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><mods:affiliation>University of Victoria, Victoria, Canada</mods:affiliation></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><mods:affiliation>Anglo‐Australian Observatory, Sydney, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquary University, Sydney, Australia</mods:affiliation></affiliation></author><author><name sortKey="Seabroke, G" sort="Seabroke, G" uniqKey="Seabroke G" first="G." last="Seabroke">G. Seabroke</name><affiliation><mods:affiliation>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University, Milton Keynes</mods:affiliation></affiliation><affiliation><mods:affiliation>Institute of Astronomy, Cambridge</mods:affiliation></affiliation></author><author><name sortKey="Siviero, A" sort="Siviero, A" uniqKey="Siviero A" first="A." last="Siviero">A. Siviero</name><affiliation><mods:affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy</mods:affiliation></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation><mods:affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</mods:affiliation></affiliation><affiliation><mods:affiliation>Australian Natianal University, Canberra, Australia</mods:affiliation></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><mods:affiliation>Johns Hopkins University, Baltimore, MD, USA</mods:affiliation></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation><mods:affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><biblScope unit="vol">391</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="793">793</biblScope><biblScope unit="page" to="801">801</biblScope><biblScope unit="page-count">9</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-12-01">2008-12-01</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>2mass survey</term><term>Amendt cuddeford</term><term>Attening</term><term>Axis ratio</term><term>Bienaym</term><term>Binney</term><term>Binney tremaine</term><term>Black histogram</term><term>Bottom panel</term><term>Cardinal directions</term><term>Carlo</term><term>Clump</term><term>Clump candidates</term><term>Clump giants</term><term>Clump sample</term><term>Clump stars</term><term>Constraint</term><term>Contamination</term><term>Contamination fraction</term><term>Dark halo</term><term>Data points</term><term>Data release</term><term>Dehnen</term><term>Dehnen binney</term><term>Direct measurement</term><term>Disc</term><term>Distance interval</term><term>Ellipsoid</term><term>Error bars</term><term>Error budget</term><term>Error distribution</term><term>Error distributions</term><term>Error laws</term><term>Extreme cases</term><term>Famaey</term><term>Foreground</term><term>Foreground objects</term><term>Foreground population</term><term>Foreground stars</term><term>Full line</term><term>Galactic</term><term>Galactic centre</term><term>Galactic dynamics</term><term>Galactic plane</term><term>Galactic pole</term><term>Galactic potentials</term><term>Gilmore</term><term>Good agreement</term><term>Grey gaussian curve</term><term>Halo</term><term>Halo density</term><term>Inclination</term><term>Individual errors</term><term>Johns hopkins university</term><term>Journal compilation</term><term>Kuijken gilmore</term><term>Large error bars</term><term>Local velocity ellipsoid</term><term>Majewski</term><term>Mass distribution</term><term>Mass model</term><term>Mass models</term><term>Massive disc</term><term>Massive halo</term><term>Mnras</term><term>Monte carlo realization</term><term>Monte carlo sampling</term><term>Oblate</term><term>Oblate halo</term><term>Open circles</term><term>Orbit library</term><term>Original sample</term><term>Other hand</term><term>Princeton univ</term><term>Prolate</term><term>Prolate haloes</term><term>Prolate models</term><term>Proper motions</term><term>Radial velocity experiment</term><term>Random realization</term><term>Rotation curve</term><term>Same procedure</term><term>Scalelength</term><term>Second data release</term><term>Selection criteria</term><term>Selection criterion</term><term>Selection function</term><term>Short scalelength</term><term>Siebert</term><term>Single orbit</term><term>Small fraction</term><term>Solar neighbourhood</term><term>Spherical halo</term><term>Standard deviation</term><term>Stellar</term><term>Stellar disc</term><term>Stellar parameters</term><term>Substructure</term><term>Thick line</term><term>Tilt</term><term>Tilt angle</term><term>Unbiased measurement</term><term>Upper limit</term><term>Velocity</term><term>Velocity criteria</term><term>Velocity criterion</term><term>Velocity distribution</term><term>Velocity ellipsoid</term><term>Velocity error anisotropy</term><term>Velocity error distributions</term><term>Velocity errors</term><term>Velocity space</term><term>Velocity structures</term><term>Velocity substructures</term><term>Velocity trends</term><term>Velocity vector</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>2mass survey</term><term>Amendt cuddeford</term><term>Attening</term><term>Axis ratio</term><term>Bienaym</term><term>Binney</term><term>Binney tremaine</term><term>Black histogram</term><term>Bottom panel</term><term>Cardinal directions</term><term>Carlo</term><term>Clump</term><term>Clump candidates</term><term>Clump giants</term><term>Clump sample</term><term>Clump stars</term><term>Constraint</term><term>Contamination</term><term>Contamination fraction</term><term>Dark halo</term><term>Data points</term><term>Data release</term><term>Dehnen</term><term>Dehnen binney</term><term>Direct measurement</term><term>Disc</term><term>Distance interval</term><term>Ellipsoid</term><term>Error bars</term><term>Error budget</term><term>Error distribution</term><term>Error distributions</term><term>Error laws</term><term>Extreme cases</term><term>Famaey</term><term>Foreground</term><term>Foreground objects</term><term>Foreground population</term><term>Foreground stars</term><term>Full line</term><term>Galactic</term><term>Galactic centre</term><term>Galactic dynamics</term><term>Galactic plane</term><term>Galactic pole</term><term>Galactic potentials</term><term>Gilmore</term><term>Good agreement</term><term>Grey gaussian curve</term><term>Halo</term><term>Halo density</term><term>Inclination</term><term>Individual errors</term><term>Johns hopkins university</term><term>Journal compilation</term><term>Kuijken gilmore</term><term>Large error bars</term><term>Local velocity ellipsoid</term><term>Majewski</term><term>Mass distribution</term><term>Mass model</term><term>Mass models</term><term>Massive disc</term><term>Massive halo</term><term>Mnras</term><term>Monte carlo realization</term><term>Monte carlo sampling</term><term>Oblate</term><term>Oblate halo</term><term>Open circles</term><term>Orbit library</term><term>Original sample</term><term>Other hand</term><term>Princeton univ</term><term>Prolate</term><term>Prolate haloes</term><term>Prolate models</term><term>Proper motions</term><term>Radial velocity experiment</term><term>Random realization</term><term>Rotation curve</term><term>Same procedure</term><term>Scalelength</term><term>Second data release</term><term>Selection criteria</term><term>Selection criterion</term><term>Selection function</term><term>Short scalelength</term><term>Siebert</term><term>Single orbit</term><term>Small fraction</term><term>Solar neighbourhood</term><term>Spherical halo</term><term>Standard deviation</term><term>Stellar</term><term>Stellar disc</term><term>Stellar parameters</term><term>Substructure</term><term>Thick line</term><term>Tilt</term><term>Tilt angle</term><term>Unbiased measurement</term><term>Upper limit</term><term>Velocity</term><term>Velocity criteria</term><term>Velocity criterion</term><term>Velocity distribution</term><term>Velocity ellipsoid</term><term>Velocity error anisotropy</term><term>Velocity error distributions</term><term>Velocity errors</term><term>Velocity space</term><term>Velocity structures</term><term>Velocity substructures</term><term>Velocity trends</term><term>Velocity vector</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 . 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.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>velocity ellipsoid</json:string><json:string>mnras</json:string><json:string>ellipsoid</json:string><json:string>scalelength</json:string><json:string>galactic</json:string><json:string>famaey</json:string><json:string>galactic plane</json:string><json:string>attening</json:string><json:string>direct measurement</json:string><json:string>prolate</json:string><json:string>bienaym</json:string><json:string>binney</json:string><json:string>dehnen</json:string><json:string>standard deviation</json:string><json:string>tilt angle</json:string><json:string>oblate</json:string><json:string>journal 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Siebert</name><affiliations><json:string>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</json:string><json:string>Astrophysikalishes Institut Potsdam, Potsdam, Germany</json:string><json:string>E-mail: siebert@astro.u‐strasbg.fr</json:string></affiliations></json:item><json:item><name>O. Bienaymé</name><affiliations><json:string>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</json:string></affiliations></json:item><json:item><name>J. Binney</name><affiliations><json:string>Rudolf Peierls Centre for Theoretical Physics, Oxford</json:string></affiliations></json:item><json:item><name>J. Bland‐Hawthorn</name><affiliations><json:string>Anglo‐Australian Observatory, Sydney, Australia</json:string></affiliations></json:item><json:item><name>R. Campbell</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, Potsdam, Germany</json:string><json:string>Macquary University, Sydney, Australia</json:string></affiliations></json:item><json:item><name>K. C. Freeman</name><affiliations><json:string>Australian Natianal University, Canberra, Australia</json:string></affiliations></json:item><json:item><name>B. K. Gibson</name><affiliations><json:string>University of Central Lancashire, Preston</json:string></affiliations></json:item><json:item><name>G. Gilmore</name><affiliations><json:string>Institute of Astronomy, Cambridge</json:string></affiliations></json:item><json:item><name>E. K. Grebel</name><affiliations><json:string>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany</json:string></affiliations></json:item><json:item><name>A. Helmi</name><affiliations><json:string>Kapteyn Astronomical Institut, Groningen, the Netherlands</json:string></affiliations></json:item><json:item><name>U. Munari</name><affiliations><json:string>Astronomical Observatory of Padova in Asiago, Asiago, Italy</json:string></affiliations></json:item><json:item><name>J. F. Navarro</name><affiliations><json:string>University of Victoria, Victoria, Canada</json:string></affiliations></json:item><json:item><name>Q. A. Parker</name><affiliations><json:string>Anglo‐Australian Observatory, Sydney, Australia</json:string><json:string>Macquary University, Sydney, Australia</json:string></affiliations></json:item><json:item><name>G. Seabroke</name><affiliations><json:string>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University, Milton Keynes</json:string><json:string>Institute of Astronomy, Cambridge</json:string></affiliations></json:item><json:item><name>A. Siviero</name><affiliations><json:string>Astronomical Observatory of Padova in Asiago, Asiago, Italy</json:string></affiliations></json:item><json:item><name>M. Steinmetz</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, Potsdam, Germany</json:string></affiliations></json:item><json:item><name>M. Williams</name><affiliations><json:string>Astrophysikalishes Institut Potsdam, Potsdam, Germany</json:string><json:string>Australian Natianal University, Canberra, Australia</json:string></affiliations></json:item><json:item><name>R. F. G. Wyse</name><affiliations><json:string>Johns Hopkins University, Baltimore, MD, USA</json:string></affiliations></json:item><json:item><name>T. Zwitter</name><affiliations><json:string>Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stars: kinematics</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxy: fundamental parameters</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxy: kinematics and dynamics</value></json:item></subject><articleId><json:string>MNR13912</json:string></articleId><arkIstex>ark:/67375/WNG-5NGQWGQC-Q</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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 . 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.</abstract><qualityIndicators><score>9.184</score><pdfWordCount>7861</pdfWordCount><pdfCharCount>42045</pdfCharCount><pdfVersion>1.5</pdfVersion><pdfPageCount>9</pdfPageCount><pdfPageSize>595 x 782 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>182</abstractWordCount><abstractCharCount>1071</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>391</volume><issue>2</issue><pages><first>793</first><last>801</last><total>9</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>5000</json:string><json:string>6500</json:string><json:string>1000</json:string><json:string>2008</json:string></date><geogName></geogName><orgName><json:string>Space Sciences Research Institute, The Open University, Milton Keynes</json:string><json:string>Netherlands Research School for Astronomy, the Natural Sciences and Engineering</json:string><json:string>Astrophysical Institute Potsdam, the Australian Research Council, the German Research</json:string><json:string>Research, the Particle Physics and Astronomy</json:string><json:string>Johns Hopkins University</json:string><json:string>National Institute for Astrophysics</json:string><json:string>The Johns Hopkins University</json:string><json:string>Australian Natianal University</json:string><json:string>Slovenian Research Agency</json:string><json:string>Macquary University</json:string><json:string>University of Victoria</json:string><json:string>University of Central Lancashire</json:string><json:string>Institute of Astronomy, Cambridge</json:string><json:string>Netherlands Organization for Scienti</json:string><json:string>University of Ljubljana</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>U. 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(2007)</json:string><json:string>Read & Moore 2005</json:string><json:string>Odenkirchen et al. 2003</json:string><json:string>Famaey et al. (2005)</json:string><json:string>Seabroke et al. (2008)</json:string><json:string>Famaey et al.</json:string><json:string>Schlegel, Finkbeiner & Davis 1998</json:string><json:string>Binney 1983</json:string><json:string>Ollongren 1962</json:string><json:string>Ibata et al. 2001</json:string><json:string>Ojha (2001)</json:string><json:string>Hawley (1996)</json:string><json:string>Seabroke & Gilmore 2007</json:string><json:string>Amendt & Cuddeford 1991</json:string><json:string>Newberg et al. (2006)</json:string><json:string>Chereul et al. 1998</json:string><json:string>Majewski et al. (2003)</json:string><json:string>Binney & Tremaine 1987</json:string><json:string>Veltz et al. 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(2008)</json:string><json:string>Zhao, Qiu & Zhang 2000</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-5NGQWGQC-Q</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - astronomie</json:string></inist></categories><publicationDate>2008</publicationDate><copyrightDate>2008</copyrightDate><doi><json:string>10.1111/j.1365-2966.2008.13912.x</json:string></doi><id>A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2008 The Authors. Journal compilation © 2008 RAS</licence></availability><date type="published" when="2008-12-01"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title><title level="a" type="short">The tilt of the velocity ellipsoid from RAVE</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">A.</forename><surname>Siebert</surname></persName><affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France<address><country key="FR"></country></address></affiliation><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany<address><country key="DE"></country></address></affiliation><affiliation>E‐mail: siebert@astro.u‐strasbg.fr</affiliation></author><author xml:id="author-0001"><persName><forename type="first">O.</forename><surname>Bienaymé</surname></persName><affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">J.</forename><surname>Binney</surname></persName><affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford</affiliation></author><author xml:id="author-0003"><persName><forename type="first">J.</forename><surname>Bland‐Hawthorn</surname></persName><affiliation>Anglo‐Australian Observatory, Sydney, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">R.</forename><surname>Campbell</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany<address><country key="DE"></country></address></affiliation><affiliation>Macquary University, Sydney, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">K. C.</forename><surname>Freeman</surname></persName><affiliation>Australian Natianal University, Canberra, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">B. K.</forename><surname>Gibson</surname></persName><affiliation>University of Central Lancashire, Preston</affiliation></author><author xml:id="author-0007"><persName><forename type="first">G.</forename><surname>Gilmore</surname></persName><affiliation>Institute of Astronomy, Cambridge</affiliation></author><author xml:id="author-0008"><persName><forename type="first">E. K.</forename><surname>Grebel</surname></persName><affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">A.</forename><surname>Helmi</surname></persName><affiliation>Kapteyn Astronomical Institut, Groningen, the Netherlands<address><country key="NL"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">U.</forename><surname>Munari</surname></persName><affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">J. F.</forename><surname>Navarro</surname></persName><affiliation>University of Victoria, Victoria, Canada<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0012"><persName><forename type="first">Q. A.</forename><surname>Parker</surname></persName><affiliation>Anglo‐Australian Observatory, Sydney, Australia<address><country key="AU"></country></address></affiliation><affiliation>Macquary University, Sydney, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">G.</forename><surname>Seabroke</surname></persName><affiliation>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University, Milton Keynes</affiliation><affiliation>Institute of Astronomy, Cambridge</affiliation></author><author xml:id="author-0014"><persName><forename type="first">A.</forename><surname>Siviero</surname></persName><affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">M.</forename><surname>Steinmetz</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0016"><persName><forename type="first">M.</forename><surname>Williams</surname></persName><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany<address><country key="DE"></country></address></affiliation><affiliation>Australian Natianal University, Canberra, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">R. F. G.</forename><surname>Wyse</surname></persName><affiliation>Johns Hopkins University, Baltimore, MD, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0018"><persName><forename type="first">T.</forename><surname>Zwitter</surname></persName><affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia<address><country key="SI"></country></address></affiliation></author><idno type="istex">A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E</idno><idno type="ark">ark:/67375/WNG-5NGQWGQC-Q</idno><idno type="DOI">10.1111/j.1365-2966.2008.13912.x</idno><idno type="unit">MNR13912</idno><idno type="toTypesetVersion">file:MNR.MNR13912.pdf</idno></analytic><monogr><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title><title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2008.391.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">391</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="793">793</biblScope><biblScope unit="page" to="801">801</biblScope><biblScope unit="page-count">9</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2008-12-01"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>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 <graphic url="equation/MNR_13912_mu1.gif" rend="inline image"></graphic>. 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 <emph><span>(<hi rend="italic">R</hi><hi rend="subscript">d</hi>≃ 2 kpc)</span></emph> if the dark halo is oblate or with a long scalelength <emph><span>(<hi rend="italic">R</hi><hi rend="subscript">d</hi>≃ 3 kpc)</span></emph> 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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">stars: kinematics</term><term xml:id="k2">galaxy: fundamental parameters</term><term xml:id="k3">galaxy: kinematics and dynamics</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="12002"><doi origin="wiley">10.1111/mnr.2008.391.issue-2</doi><numberingGroup><numbering type="journalVolume" number="391">391</numbering><numbering type="journalIssue" number="2">2</numbering></numberingGroup><coverDate startDate="2008-12-01">December 2008</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="26" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2008.13912.x</doi><idGroup><id type="unit" value="MNR13912"></id></idGroup><countGroup><count type="pageTotal" number="9"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2008 The Authors. 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E‐mail: <email normalForm="siebert@astro.u-strasbg.fr">siebert@astro.u‐strasbg.fr</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR13912.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2008 September 2. Received 2008 August 28; in original form 2008 August 7</unparsedEditorialHistory><countGroup><count type="figureTotal" number="9"></count><count type="tableTotal" number="2"></count><count type="formulaTotal" number="103"></count><count type="referenceTotal" number="57"></count><count type="linksCrossRef" number="134"></count></countGroup><titleGroup><title type="main">Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title><title type="shortAuthors"><i>A. Siebert et al.</i></title><title type="short"><i>The tilt of the velocity ellipsoid from RAVE</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2" corresponding="yes"><personName><givenNames>A.</givenNames><familyName>Siebert</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>O.</givenNames><familyName>Bienaymé</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>J.</givenNames><familyName>Binney</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a4"><personName><givenNames>J.</givenNames><familyName>Bland‐Hawthorn</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a2 #a5"><personName><givenNames>R.</givenNames><familyName>Campbell</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a6"><personName><givenNames>K. 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We find that the velocity ellipsoid is tilted towards the Galactic plane with an inclination of <inlineGraphic alt="inline image" location="equation/MNR_13912_mu1.gif" href=""></inlineGraphic>. 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 <span type="mathematics">(<i>R</i><sub>d</sub>≃ 2 kpc)</span> if the dark halo is oblate or with a long scalelength <span type="mathematics">(<i>R</i><sub>d</sub>≃ 3 kpc)</span> 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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>The tilt of the velocity ellipsoid from RAVE</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Estimation of the tilt of the stellar velocity ellipsoid from RAVE and implications for mass models</title></titleInfo><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siebert</namePart><affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</affiliation><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</affiliation><affiliation>E-mail: siebert@astro.u‐strasbg.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">O.</namePart><namePart type="family">Bienaymé</namePart><affiliation>Université de Strasbourg, Observatoire Astronomique, Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Binney</namePart><affiliation>Rudolf Peierls Centre for Theoretical Physics, Oxford</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Bland‐Hawthorn</namePart><affiliation>Anglo‐Australian Observatory, Sydney, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Campbell</namePart><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</affiliation><affiliation>Macquary University, Sydney, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K. C.</namePart><namePart type="family">Freeman</namePart><affiliation>Australian Natianal University, Canberra, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B. K.</namePart><namePart type="family">Gibson</namePart><affiliation>University of Central Lancashire, Preston</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Gilmore</namePart><affiliation>Institute of Astronomy, Cambridge</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E. K.</namePart><namePart type="family">Grebel</namePart><affiliation>Astronomisches Rechen‐Institut, Zentrum für Astronomie der Universität Heidelberg, Heidelberg, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Helmi</namePart><affiliation>Kapteyn Astronomical Institut, Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">U.</namePart><namePart type="family">Munari</namePart><affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. F.</namePart><namePart type="family">Navarro</namePart><affiliation>University of Victoria, Victoria, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Q. A.</namePart><namePart type="family">Parker</namePart><affiliation>Anglo‐Australian Observatory, Sydney, Australia</affiliation><affiliation>Macquary University, Sydney, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G.</namePart><namePart type="family">Seabroke</namePart><affiliation>e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, The Open University, Milton Keynes</affiliation><affiliation>Institute of Astronomy, Cambridge</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siviero</namePart><affiliation>Astronomical Observatory of Padova in Asiago, Asiago, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Steinmetz</namePart><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Williams</namePart><affiliation>Astrophysikalishes Institut Potsdam, Potsdam, Germany</affiliation><affiliation>Australian Natianal University, Canberra, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. F. G.</namePart><namePart type="family">Wyse</namePart><affiliation>Johns Hopkins University, Baltimore, MD, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Zwitter</namePart><affiliation>Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2008-12-01</dateIssued><edition>Accepted 2008 September 2. Received 2008 August 28; in original form 2008 August 7</edition><copyrightDate encoding="w3cdtf">2008</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">9</extent><extent unit="tables">2</extent><extent unit="formulas">103</extent><extent unit="references">57</extent><extent unit="linksCrossRef">134</extent></physicalDescription><abstract 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 . 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.</abstract><subject lang="en"><genre>keywords</genre><topic>stars: kinematics</topic><topic>galaxy: fundamental parameters</topic><topic>galaxy: kinematics and dynamics</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2008</date><detail type="volume"><caption>vol.</caption><number>391</number></detail><detail type="issue"><caption>no.</caption><number>2</number></detail><extent unit="pages"><start>793</start><end>801</end><total>9</total></extent></part></relatedItem><identifier type="istex">A51AFD5C6FE24B5C1719D5B4F68EA3B33DF6F00E</identifier><identifier type="ark">ark:/67375/WNG-5NGQWGQC-Q</identifier><identifier type="DOI">10.1111/j.1365-2966.2008.13912.x</identifier><identifier type="ArticleID">MNR13912</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2008 The Authors. 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