The RAVE survey : constraining the local Galactic escape speed
Identifieur interne : 002595 ( PascalFrancis/Curation ); précédent : 002594; suivant : 002596The RAVE survey : constraining the local Galactic escape speed
Auteurs : Martin C. Smith [Pays-Bas] ; Gregory R. Ruchti [États-Unis] ; Amina Helmi [Pays-Bas] ; Rosemary F. G. Wyse [États-Unis] ; J. P. Fulbright [États-Unis] ; K. C. Freeman [Australie] ; J. F. Navarro [Canada] ; G. M. Seabroke [Royaume-Uni] ; M. Steinmetz [Allemagne] ; M. Williams [Australie] ; O. Bienayme [France] ; J. Binney [Royaume-Uni] ; J. Bland-Hawthorn [Australie] ; W. Dehnen [Royaume-Uni] ; B. K. Gibson [Royaume-Uni] ; G. Gilmore [Royaume-Uni] ; E. K. Grebel [Suisse] ; U. Munari [Italie] ; Q. A. Parker [Australie] ; R.-D. Scholz [Allemagne] ; A. Siebert [Allemagne] ; F. G. Watson [Australie] ; T. Zwitter [Slovénie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007.
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Abstract
We report new constraints on the local escape speed of our Galaxy. Our analysis is based on a sample of high-velocity stars from the RAVE survey and two previously published data sets. We use cosmological simulations of disc galaxy formation to motivate our assumptions on the shape of the velocity distribution, allowing for a significantly more precise measurement of the escape velocity compared to previous studies. We find that the escape velocity lies within the range 498 < ùesc < 608 km s-1 (90 per cent confidence), with a median likelihood of 544 km s-1. The fact that ù2esc is significantly greater than 2ù2circ (where ùcirc = 220km s-1 is the local circular velocity) implies that there must be a significant amount of mass exterior to the solar circle, that is, this convincingly demonstrates the presence of a dark halo in the Galaxy. We use our constraints on ùesc to determine the mass of the Milky Way halo for three halo profiles. For example, an adiabatically contracted NFW halo model results in a virial mass of 1.42+1.44-0.54 x 1012 M◦. and virial radius of 305+66-45 kpc (90 per cent confidence). For this model the circular velocity at the virial radius is 142+31-21 km s-1. Although our halo masses are model dependent, we find that they are in good agreement with each other.
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Williams</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Observatoire de Strasbourg, 11 Rue de L'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, I Keble Road</s1><s2>Oxford OX1 3NP</s2><s3>GBR</s3><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="11"><s1>University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="12"><s1>Astronomisches Institut, Universität Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>17 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>18 aut.</sZ></inist:fA14><country>Italie</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>19 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Scholz, R D" sort="Scholz, R D" uniqKey="Scholz R" first="R.-D." last="Scholz">R.-D. Scholz</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 aut.</sZ></inist:fA14><country>Slovénie</country></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">INIST</idno><idno type="inist">07-0361816</idno><date when="2007">2007</date><idno type="stanalyst">PASCAL 07-0361816 INIST</idno><idno type="RBID">Pascal:07-0361816</idno><idno type="wicri:Area/PascalFrancis/Corpus">003A93</idno><idno type="wicri:Area/PascalFrancis/Curation">002595</idno></publicationStmt><sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">The RAVE survey : constraining the local Galactic escape speed</title><author><name sortKey="Smith, Martin C" sort="Smith, Martin C" uniqKey="Smith M" first="Martin C." last="Smith">Martin C. Smith</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Ruchti, Gregory R" sort="Ruchti, Gregory R" uniqKey="Ruchti G" first="Gregory R." last="Ruchti">Gregory R. Ruchti</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ></inist:fA14><country>Pays-Bas</country></affiliation></author><author><name sortKey="Wyse, Rosemary F G" sort="Wyse, Rosemary F G" uniqKey="Wyse R" first="Rosemary F. G." last="Wyse">Rosemary F. G. Wyse</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></affiliation></author><author><name sortKey="Fulbright, J P" sort="Fulbright, J P" uniqKey="Fulbright J" first="J. P." last="Fulbright">J. P. Fulbright</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></inist:fA14><country>États-Unis</country></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 wicri:level="1"><inist:fA14 i1="03"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Australie</country></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 wicri:level="1"><inist:fA14 i1="04"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC, V8W 3P6</s2><s3>CAN</s3><sZ>7 aut.</sZ></inist:fA14><country>Canada</country></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienayme">O. Bienayme</name><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Observatoire de Strasbourg, 11 Rue de L'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>11 aut.</sZ></inist:fA14><country>France</country></affiliation></author><author><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, I Keble Road</s1><s2>Oxford OX1 3NP</s2><s3>GBR</s3><sZ>12 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name><affiliation wicri:level="1"><inist:fA14 i1="10"><s1>University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>14 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="11"><s1>University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>15 aut.</sZ></inist:fA14><country>Royaume-Uni</country></affiliation></author><author><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name><affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ></inist:fA14><country>Royaume-Uni</country></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 wicri:level="1"><inist:fA14 i1="12"><s1>Astronomisches Institut, Universität Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>17 aut.</sZ></inist:fA14><country>Suisse</country></affiliation></author><author><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name><affiliation wicri:level="1"><inist:fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>18 aut.</sZ></inist:fA14><country>Italie</country></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 wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation><affiliation wicri:level="1"><inist:fA14 i1="14"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>19 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Scholz, R D" sort="Scholz, R D" uniqKey="Scholz R" first="R.-D." last="Scholz">R.-D. Scholz</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></inist:fA14><country>Allemagne</country></affiliation></author><author><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></inist:fA14><country>Australie</country></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation wicri:level="1"><inist:fA14 i1="15"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 aut.</sZ></inist:fA14><country>Slovénie</country></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="2007">2007</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>Circle</term><term>Disk galaxies</term><term>Dynamics</term><term>Escape velocity</term><term>Galactic halos</term><term>Galaxy formation</term><term>Galaxy halo</term><term>High velocity star</term><term>Kinematics</term><term>Milky Way</term><term>Models</term><term>Velocity distribution</term><term>Virial mass</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Galaxies disques</term><term>Etoile grande vitesse</term><term>Formation galaxies</term><term>Distribution vitesse</term><term>Vitesse fuite</term><term>Cercle</term><term>Halo galactique</term><term>Modèle</term><term>Masse viriel</term><term>Cinématique</term><term>Dynamique</term><term>Voie lactée</term><term>Halo galaxies</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We report new constraints on the local escape speed of our Galaxy. Our analysis is based on a sample of high-velocity stars from the RAVE survey and two previously published data sets. We use cosmological simulations of disc galaxy formation to motivate our assumptions on the shape of the velocity distribution, allowing for a significantly more precise measurement of the escape velocity compared to previous studies. We find that the escape velocity lies within the range 498 < ù<sub>esc</sub> < 608 km s<sup>-1</sup> (90 per cent confidence), with a median likelihood of 544 km s<sup>-1</sup>. The fact that ù<sup>2</sup><sub>esc</sub> is significantly greater than 2ù<sup>2</sup><sub>circ</sub> (where ù<sub>circ</sub> = 220km s<sup>-1</sup> is the local circular velocity) implies that there must be a significant amount of mass exterior to the solar circle, that is, this convincingly demonstrates the presence of a dark halo in the Galaxy. We use our constraints on ù<sub>esc</sub> to determine the mass of the Milky Way halo for three halo profiles. For example, an adiabatically contracted NFW halo model results in a virial mass of 1.42<sup>+1.44</sup><sub>-0.54</sub> x 1012 M<sub>◦.</sub> and virial radius of 305<sup>+66</sup><sub>-45</sub> kpc (90 per cent confidence). For this model the circular velocity at the virial radius is 142<sup>+31</sup><sub>-21</sub> km s<sup>-1</sup>. Although our halo masses are model dependent, we find that they are in good agreement with each other.</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>379</s2></fA05><fA06><s2>2</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>The RAVE survey : constraining the local Galactic escape speed</s1></fA08><fA11 i1="01" i2="1"><s1>SMITH (Martin C.)</s1></fA11><fA11 i1="02" i2="1"><s1>RUCHTI (Gregory R.)</s1></fA11><fA11 i1="03" i2="1"><s1>HELMI (Amina)</s1></fA11><fA11 i1="04" i2="1"><s1>WYSE (Rosemary F. G.)</s1></fA11><fA11 i1="05" i2="1"><s1>FULBRIGHT (J. P.)</s1></fA11><fA11 i1="06" i2="1"><s1>FREEMAN (K. C.)</s1></fA11><fA11 i1="07" i2="1"><s1>NAVARRO (J. F.)</s1></fA11><fA11 i1="08" i2="1"><s1>SEABROKE (G. M.)</s1></fA11><fA11 i1="09" i2="1"><s1>STEINMETZ (M.)</s1></fA11><fA11 i1="10" i2="1"><s1>WILLIAMS (M.)</s1></fA11><fA11 i1="11" i2="1"><s1>BIENAYME (O.)</s1></fA11><fA11 i1="12" i2="1"><s1>BINNEY (J.)</s1></fA11><fA11 i1="13" i2="1"><s1>BLAND-HAWTHORN (J.)</s1></fA11><fA11 i1="14" i2="1"><s1>DEHNEN (W.)</s1></fA11><fA11 i1="15" i2="1"><s1>GIBSON (B. K.)</s1></fA11><fA11 i1="16" i2="1"><s1>GILMORE (G.)</s1></fA11><fA11 i1="17" i2="1"><s1>GREBEL (E. K.)</s1></fA11><fA11 i1="18" i2="1"><s1>MUNARI (U.)</s1></fA11><fA11 i1="19" i2="1"><s1>PARKER (Q. A.)</s1></fA11><fA11 i1="20" i2="1"><s1>SCHOLZ (R.-D.)</s1></fA11><fA11 i1="21" i2="1"><s1>SIEBERT (A.)</s1></fA11><fA11 i1="22" i2="1"><s1>WATSON (F. G.)</s1></fA11><fA11 i1="23" i2="1"><s1>ZWITTER (T.)</s1></fA11><fA14 i1="01"><s1>Kapteyn Astronomical Institute, University of Groningen, PO Box 800</s1><s2>9700 AV Groningen</s2><s3>NLD</s3><sZ>1 aut.</sZ><sZ>3 aut.</sZ></fA14><fA14 i1="02"><s1>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street</s1><s2>Baltimore, MD 21218</s2><s3>USA</s3><sZ>2 aut.</sZ><sZ>4 aut.</sZ><sZ>5 aut.</sZ></fA14><fA14 i1="03"><s1>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek</s1><s2>Canberra, ACT 72611</s2><s3>AUS</s3><sZ>6 aut.</sZ><sZ>10 aut.</sZ></fA14><fA14 i1="04"><s1>University of Victoria, PO Box 3055, Station CSC</s1><s2>Victoria, BC, V8W 3P6</s2><s3>CAN</s3><sZ>7 aut.</sZ></fA14><fA14 i1="05"><s1>Institute of Astronomy, University of Cambridge, Madingley Road</s1><s2>Cambridge CB3 0HA</s2><s3>GBR</s3><sZ>8 aut.</sZ><sZ>16 aut.</sZ></fA14><fA14 i1="06"><s1>Astrophysikalisches Institut Potsdam, An der Sterwarte 16</s1><s2>14482 Potsdam</s2><s3>DEU</s3><sZ>9 aut.</sZ><sZ>20 aut.</sZ><sZ>21 aut.</sZ></fA14><fA14 i1="07"><s1>Observatoire de Strasbourg, 11 Rue de L'Université</s1><s2>67000 Strasbourg</s2><s3>FRA</s3><sZ>11 aut.</sZ></fA14><fA14 i1="08"><s1>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, I Keble Road</s1><s2>Oxford OX1 3NP</s2><s3>GBR</s3><sZ>12 aut.</sZ></fA14><fA14 i1="09"><s1>Anglo-Australian Observatory, PO Box 296</s1><s2>Epping, NSW 1710</s2><s3>AUS</s3><sZ>13 aut.</sZ><sZ>19 aut.</sZ><sZ>22 aut.</sZ></fA14><fA14 i1="10"><s1>University of Leicester, University Road</s1><s2>Leicester LE1 7RH</s2><s3>GBR</s3><sZ>14 aut.</sZ></fA14><fA14 i1="11"><s1>University of Central Lancashire</s1><s2>Preston PR1 2HE</s2><s3>GBR</s3><sZ>15 aut.</sZ></fA14><fA14 i1="12"><s1>Astronomisches Institut, Universität Basel, Venusstrasse 7</s1><s2>Binningen 4102</s2><s3>CHE</s3><sZ>17 aut.</sZ></fA14><fA14 i1="13"><s1>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8</s1><s2>Asiago 36012</s2><s3>ITA</s3><sZ>18 aut.</sZ></fA14><fA14 i1="14"><s1>Macquarie University</s1><s2>Sydney, NSW 2109</s2><s3>AUS</s3><sZ>19 aut.</sZ></fA14><fA14 i1="15"><s1>Department of Physics, University of Ljubljana, Jadranska 19</s1><s2>Ljubljana</s2><s3>SVN</s3><sZ>23 aut.</sZ></fA14><fA20><s1>755-772</s1></fA20><fA21><s1>2007</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000149977960230</s5></fA43><fA44><s0>0000</s0><s1>© 2007 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>3/4 p.</s0></fA45><fA47 i1="01" i2="1"><s0>07-0361816</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 report new constraints on the local escape speed of our Galaxy. Our analysis is based on a sample of high-velocity stars from the RAVE survey and two previously published data sets. We use cosmological simulations of disc galaxy formation to motivate our assumptions on the shape of the velocity distribution, allowing for a significantly more precise measurement of the escape velocity compared to previous studies. We find that the escape velocity lies within the range 498 < ù<sub>esc</sub> < 608 km s<sup>-1</sup> (90 per cent confidence), with a median likelihood of 544 km s<sup>-1</sup>. The fact that ù<sup>2</sup><sub>esc</sub> is significantly greater than 2ù<sup>2</sup><sub>circ</sub> (where ù<sub>circ</sub> = 220km s<sup>-1</sup> is the local circular velocity) implies that there must be a significant amount of mass exterior to the solar circle, that is, this convincingly demonstrates the presence of a dark halo in the Galaxy. We use our constraints on ù<sub>esc</sub> to determine the mass of the Milky Way halo for three halo profiles. For example, an adiabatically contracted NFW halo model results in a virial mass of 1.42<sup>+1.44</sup><sub>-0.54</sub> x 1012 M<sub>◦.</sub> and virial radius of 305<sup>+66</sup><sub>-45</sub> kpc (90 per cent confidence). For this model the circular velocity at the virial radius is 142<sup>+31</sup><sub>-21</sub> km s<sup>-1</sup>. Although our halo masses are model dependent, we find that they are in good agreement with each other.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Galaxies disques</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Disk galaxies</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Etoile grande vitesse</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>High velocity star</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Estrella gran velocidad</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Formation galaxies</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Galaxy formation</s0><s5>28</s5></fC03><fC03 i1="04" i2="3" l="FRE"><s0>Distribution vitesse</s0><s5>29</s5></fC03><fC03 i1="04" i2="3" l="ENG"><s0>Velocity distribution</s0><s5>29</s5></fC03><fC03 i1="05" i2="3" l="FRE"><s0>Vitesse fuite</s0><s5>30</s5></fC03><fC03 i1="05" i2="3" l="ENG"><s0>Escape velocity</s0><s5>30</s5></fC03><fC03 i1="06" i2="X" l="FRE"><s0>Cercle</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="ENG"><s0>Circle</s0><s5>31</s5></fC03><fC03 i1="06" i2="X" l="SPA"><s0>Circulo</s0><s5>31</s5></fC03><fC03 i1="07" i2="3" l="FRE"><s0>Halo galactique</s0><s5>32</s5></fC03><fC03 i1="07" i2="3" l="ENG"><s0>Galactic halos</s0><s5>32</s5></fC03><fC03 i1="08" i2="X" l="FRE"><s0>Modèle</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="ENG"><s0>Models</s0><s5>33</s5></fC03><fC03 i1="08" i2="X" l="SPA"><s0>Modelo</s0><s5>33</s5></fC03><fC03 i1="09" i2="X" l="FRE"><s0>Masse viriel</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="ENG"><s0>Virial mass</s0><s5>34</s5></fC03><fC03 i1="09" i2="X" l="SPA"><s0>Masa virial</s0><s5>34</s5></fC03><fC03 i1="10" i2="3" l="FRE"><s0>Cinématique</s0><s5>35</s5></fC03><fC03 i1="10" i2="3" l="ENG"><s0>Kinematics</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Dynamique</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Dynamics</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Voie lactée</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Milky Way</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Halo galaxies</s0><s4>CD</s4><s5>96</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>Galaxy halo</s0><s4>CD</s4><s5>96</s5></fC03><fC03 i1="13" i2="3" l="SPA"><s0>Halo galaxia</s0><s4>CD</s4><s5>96</s5></fC03><fN21><s1>232</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist></record>Pour manipuler ce document sous Unix (Dilib)
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