The RAVE survey: constraining the local Galactic escape speed
Identifieur interne : 002C85 ( Istex/Corpus ); précédent : 002C84; suivant : 002C86The RAVE survey: constraining the local Galactic escape speed
Auteurs : Martin C. Smith ; Gregory R. Ruchti ; Amina Helmi ; Rosemary F. G. Wyse ; J. P. Fulbright ; K. C. Freeman ; J. F. Navarro ; G. M. Seabroke ; M. Steinmetz ; M. Williams ; O. Bienaymé ; J. Binney ; J. Bland-Hawthorn ; W. Dehnen ; B. K. Gibson ; G. Gilmore ; E. K. Grebel ; U. Munari ; Q. A. Parker ; R. Scholz ; A. Siebert ; F. G. Watson ; T. ZwitterSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-08.
English descriptors
- KwdEn :
- Abadi, Accurate representation, Additional information, Additional stars, Archival, Archival stars, Asymptotic behaviour, Binary, Binary mass motion, Binary stars, Binary systems, Binney, Binney tremaine, Bootstrap, Bootstrap analysis, Bootstrap distribution, Bootstrap distributions, Bootstrap method, Bootstrap technique, Cent interval, Cent intervals, Centre, Chiba beers, Circ, Circular orbits, Circular velocity, Concentration parameter, Constraint, Contamination, Cosmological, Cosmological simulations, Critical density, Dark halo, Dark matter, Dark matter components, Dark matter halo, Dark matter particles, Data sets, Dehnen, Dehnen binney, Denis catalogue, Different assumptions, Disc, Disc stars, Distribution approximation, Distribution function, Elliptical galaxies, Exponential disc, Fair comparison, Fastest star, Fastest stars, Fourth column, Fractional contribution, Galactic, Galactic centre, Galactic halo, Galactic longitude, Galactocentric, Galaxies kia1, Galaxy, Globular clusters, Good agreement, Halo, Halo component, Halo giants, Halo isochrone, Halo mass, Halo masses, Halo model, Halo stars, High degree, Higher values, Hypervelocity stars, Information matrix, Isochrone, Jeffreys, Journal compilation, Kendall stuart, Kia3, Kia4, Kinematics, Kinetic energy, Large number, Large value, Last column, Likelihood, Likelihood analysis, Likelihood contours, Likelihood distribution, Likelihood equation, Likelihood estimates, Likelihood function, Lower limit, Lower panel, Mass density, Mass distribution, Maximum likelihood, Maximum likelihood analysis, Maximum likelihood method, Maximum likelihood pairs, Maximum likelihood values, Median likelihood, Milky, Minimum velocity, Mnras, More information, Motion stars, Nancial support, National science foundation, Navarro, Neighbourhood, Netherlands organization, Normal distribution, Orbital rotation, Original data, Original sample, Original sample size, Outer edge, Outer parts, Peak likelihood, Posterior distribution, Previous section, Previous studies, Previous work, Princeton univ, Probability distribution, Proper motion, Proper motions, Radial, Radial velocities, Radial velocity, Radial velocity measurements, Radius, Reference priors, Rescaled galaxies, Rescaling factor, Rotation curve, Rvir, Sample volume, Scale radius, Section name, Simulation, Solar circle, Solar motion, Solar neighbourhood, Solar radius, Solid curves, Spectroscopic binaries, Star, Star particles, Statistical arguments, Steinmetz, Stellar, Stellar halo, Stellar particles, Stellar velocities, Stellar velocity distribution, Surface brightness, Tangential, Tangential velocities, Tangential velocity, Thick disc, Thick discs, Thickdisc stars, Thin disc, Third column, Total halo mass, Total mass, Total number, Tremaine, Triangle symbols, Truncation, Typical errors, Unbound, Unbound stars, Velocity, Velocity dispersion, Velocity distribution, Velocity distributions, Velocity stars, Vesc, Vesc vmin, Virial, Virial mass, Virial radius, Virial velocity, Vmin, Vmin bootstrap, Wilkinson, Wilkinson evans.
- Teeft :
- Abadi, Accurate representation, Additional information, Additional stars, Archival, Archival stars, Asymptotic behaviour, Binary, Binary mass motion, Binary stars, Binary systems, Binney, Binney tremaine, Bootstrap, Bootstrap analysis, Bootstrap distribution, Bootstrap distributions, Bootstrap method, Bootstrap technique, Cent interval, Cent intervals, Centre, Chiba beers, Circ, Circular orbits, Circular velocity, Concentration parameter, Constraint, Contamination, Cosmological, Cosmological simulations, Critical density, Dark halo, Dark matter, Dark matter components, Dark matter halo, Dark matter particles, Data sets, Dehnen, Dehnen binney, Denis catalogue, Different assumptions, Disc, Disc stars, Distribution approximation, Distribution function, Elliptical galaxies, Exponential disc, Fair comparison, Fastest star, Fastest stars, Fourth column, Fractional contribution, Galactic, Galactic centre, Galactic halo, Galactic longitude, Galactocentric, Galaxies kia1, Galaxy, Globular clusters, Good agreement, Halo, Halo component, Halo giants, Halo isochrone, Halo mass, Halo masses, Halo model, Halo stars, High degree, Higher values, Hypervelocity stars, Information matrix, Isochrone, Jeffreys, Journal compilation, Kendall stuart, Kia3, Kia4, Kinematics, Kinetic energy, Large number, Large value, Last column, Likelihood, Likelihood analysis, Likelihood contours, Likelihood distribution, Likelihood equation, Likelihood estimates, Likelihood function, Lower limit, Lower panel, Mass density, Mass distribution, Maximum likelihood, Maximum likelihood analysis, Maximum likelihood method, Maximum likelihood pairs, Maximum likelihood values, Median likelihood, Milky, Minimum velocity, Mnras, More information, Motion stars, Nancial support, National science foundation, Navarro, Neighbourhood, Netherlands organization, Normal distribution, Orbital rotation, Original data, Original sample, Original sample size, Outer edge, Outer parts, Peak likelihood, Posterior distribution, Previous section, Previous studies, Previous work, Princeton univ, Probability distribution, Proper motion, Proper motions, Radial, Radial velocities, Radial velocity, Radial velocity measurements, Radius, Reference priors, Rescaled galaxies, Rescaling factor, Rotation curve, Rvir, Sample volume, Scale radius, Section name, Simulation, Solar circle, Solar motion, Solar neighbourhood, Solar radius, Solid curves, Spectroscopic binaries, Star, Star particles, Statistical arguments, Steinmetz, Stellar, Stellar halo, Stellar particles, Stellar velocities, Stellar velocity distribution, Surface brightness, Tangential, Tangential velocities, Tangential velocity, Thick disc, Thick discs, Thickdisc stars, Thin disc, Third column, Total halo mass, Total mass, Total number, Tremaine, Triangle symbols, Truncation, Typical errors, Unbound, Unbound stars, Velocity, Velocity dispersion, Velocity distribution, Velocity distributions, Velocity stars, Vesc, Vesc vmin, Virial, Virial mass, Virial radius, Virial velocity, Vmin, Vmin bootstrap, Wilkinson, Wilkinson evans.
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 < vesc < 608 km s−1 (90 per cent confidence), with a median likelihood of 544 km s−1. The fact that v2esc is significantly greater than 2v2circ (where vcirc= 220 km 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 vesc 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+1.14−0.54× 1012 M⊙ and virial radius of (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.
Url:
DOI: 10.1111/j.1365-2966.2007.11964.x
Links to Exploration step
ISTEX:ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEBLe document en format XML
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Ruchti</name><affiliation><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author><author><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><affiliation><mods:affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</mods:affiliation></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><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</mods:affiliation></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><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</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>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</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, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6</mods:affiliation></affiliation></author><author><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. 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Bienaymé</name><affiliation><mods:affiliation>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 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, University of Oxford, 1 Keble Road, Oxford OX1 3NP</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, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation></affiliation></author><author><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name><affiliation><mods:affiliation>University of Leicester, University Road, Leicester LE1 7RH</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 PR1 2HE</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, University of Cambridge, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. 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Zwitter</name><affiliation><mods:affiliation>Department of Physics, University of Ljubljana, Jadranska 19, Ljubljana, Slovenia</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB</idno><date when="2007" year="2007">2007</date><idno type="doi">10.1111/j.1365-2966.2007.11964.x</idno><idno type="url">https://api.istex.fr/document/ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">002C85</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">002C85</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">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><mods:affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: msmith@astro.rug.nl</mods:affiliation></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><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author><author><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><affiliation><mods:affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</mods:affiliation></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><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</mods:affiliation></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><mods:affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</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>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</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, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6</mods:affiliation></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><mods:affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</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>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 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>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</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>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 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, University of Oxford, 1 Keble Road, Oxford OX1 3NP</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, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation></affiliation></author><author><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name><affiliation><mods:affiliation>University of Leicester, University Road, Leicester LE1 7RH</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 PR1 2HE</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, University of Cambridge, Madingley Road, Cambridge CB3 0HA</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 Institut, Universität Basel, Venusstrasse 7, Binningen CH‐4102, Switzerland</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>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8, Asiago I‐36012, Italy</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, PO Box 296, Epping, NSW 1710, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Macquarie University, Sydney, NSW 2109, Australia</mods:affiliation></affiliation></author><author><name sortKey="Scholz, R" sort="Scholz, R" uniqKey="Scholz R" first="R." last="Scholz">R. Scholz</name><affiliation><mods:affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</mods:affiliation></affiliation></author><author><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name><affiliation><mods:affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</mods:affiliation></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><mods:affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</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>Department of Physics, University of Ljubljana, Jadranska 19, 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">379</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="755">755</biblScope><biblScope unit="page" to="772">772</biblScope><biblScope unit="page-count">18</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-08">2007-08</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>Abadi</term><term>Accurate representation</term><term>Additional information</term><term>Additional stars</term><term>Archival</term><term>Archival stars</term><term>Asymptotic behaviour</term><term>Binary</term><term>Binary mass motion</term><term>Binary stars</term><term>Binary systems</term><term>Binney</term><term>Binney tremaine</term><term>Bootstrap</term><term>Bootstrap analysis</term><term>Bootstrap distribution</term><term>Bootstrap distributions</term><term>Bootstrap method</term><term>Bootstrap technique</term><term>Cent interval</term><term>Cent intervals</term><term>Centre</term><term>Chiba beers</term><term>Circ</term><term>Circular orbits</term><term>Circular velocity</term><term>Concentration parameter</term><term>Constraint</term><term>Contamination</term><term>Cosmological</term><term>Cosmological simulations</term><term>Critical density</term><term>Dark halo</term><term>Dark matter</term><term>Dark matter components</term><term>Dark matter 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stars</term><term>Information matrix</term><term>Isochrone</term><term>Jeffreys</term><term>Journal compilation</term><term>Kendall stuart</term><term>Kia3</term><term>Kia4</term><term>Kinematics</term><term>Kinetic energy</term><term>Large number</term><term>Large value</term><term>Last column</term><term>Likelihood</term><term>Likelihood analysis</term><term>Likelihood contours</term><term>Likelihood distribution</term><term>Likelihood equation</term><term>Likelihood estimates</term><term>Likelihood function</term><term>Lower limit</term><term>Lower panel</term><term>Mass density</term><term>Mass distribution</term><term>Maximum likelihood</term><term>Maximum likelihood analysis</term><term>Maximum likelihood method</term><term>Maximum likelihood pairs</term><term>Maximum likelihood values</term><term>Median likelihood</term><term>Milky</term><term>Minimum velocity</term><term>Mnras</term><term>More information</term><term>Motion stars</term><term>Nancial support</term><term>National science foundation</term><term>Navarro</term><term>Neighbourhood</term><term>Netherlands organization</term><term>Normal distribution</term><term>Orbital rotation</term><term>Original data</term><term>Original sample</term><term>Original sample size</term><term>Outer edge</term><term>Outer parts</term><term>Peak likelihood</term><term>Posterior distribution</term><term>Previous section</term><term>Previous studies</term><term>Previous work</term><term>Princeton univ</term><term>Probability distribution</term><term>Proper motion</term><term>Proper motions</term><term>Radial</term><term>Radial velocities</term><term>Radial velocity</term><term>Radial velocity measurements</term><term>Radius</term><term>Reference priors</term><term>Rescaled galaxies</term><term>Rescaling factor</term><term>Rotation curve</term><term>Rvir</term><term>Sample volume</term><term>Scale radius</term><term>Section name</term><term>Simulation</term><term>Solar circle</term><term>Solar motion</term><term>Solar neighbourhood</term><term>Solar radius</term><term>Solid curves</term><term>Spectroscopic binaries</term><term>Star</term><term>Star particles</term><term>Statistical arguments</term><term>Steinmetz</term><term>Stellar</term><term>Stellar halo</term><term>Stellar particles</term><term>Stellar velocities</term><term>Stellar velocity distribution</term><term>Surface brightness</term><term>Tangential</term><term>Tangential velocities</term><term>Tangential velocity</term><term>Thick disc</term><term>Thick discs</term><term>Thickdisc stars</term><term>Thin disc</term><term>Third column</term><term>Total halo mass</term><term>Total mass</term><term>Total number</term><term>Tremaine</term><term>Triangle symbols</term><term>Truncation</term><term>Typical errors</term><term>Unbound</term><term>Unbound stars</term><term>Velocity</term><term>Velocity dispersion</term><term>Velocity distribution</term><term>Velocity distributions</term><term>Velocity stars</term><term>Vesc</term><term>Vesc vmin</term><term>Virial</term><term>Virial mass</term><term>Virial radius</term><term>Virial velocity</term><term>Vmin</term><term>Vmin bootstrap</term><term>Wilkinson</term><term>Wilkinson evans</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Abadi</term><term>Accurate representation</term><term>Additional information</term><term>Additional stars</term><term>Archival</term><term>Archival stars</term><term>Asymptotic behaviour</term><term>Binary</term><term>Binary mass motion</term><term>Binary stars</term><term>Binary systems</term><term>Binney</term><term>Binney tremaine</term><term>Bootstrap</term><term>Bootstrap analysis</term><term>Bootstrap distribution</term><term>Bootstrap distributions</term><term>Bootstrap method</term><term>Bootstrap technique</term><term>Cent interval</term><term>Cent intervals</term><term>Centre</term><term>Chiba beers</term><term>Circ</term><term>Circular orbits</term><term>Circular velocity</term><term>Concentration parameter</term><term>Constraint</term><term>Contamination</term><term>Cosmological</term><term>Cosmological simulations</term><term>Critical density</term><term>Dark halo</term><term>Dark matter</term><term>Dark matter components</term><term>Dark matter halo</term><term>Dark matter particles</term><term>Data sets</term><term>Dehnen</term><term>Dehnen binney</term><term>Denis catalogue</term><term>Different assumptions</term><term>Disc</term><term>Disc stars</term><term>Distribution approximation</term><term>Distribution function</term><term>Elliptical galaxies</term><term>Exponential disc</term><term>Fair comparison</term><term>Fastest star</term><term>Fastest stars</term><term>Fourth column</term><term>Fractional contribution</term><term>Galactic</term><term>Galactic centre</term><term>Galactic halo</term><term>Galactic longitude</term><term>Galactocentric</term><term>Galaxies kia1</term><term>Galaxy</term><term>Globular clusters</term><term>Good agreement</term><term>Halo</term><term>Halo component</term><term>Halo giants</term><term>Halo isochrone</term><term>Halo mass</term><term>Halo masses</term><term>Halo model</term><term>Halo stars</term><term>High degree</term><term>Higher values</term><term>Hypervelocity stars</term><term>Information matrix</term><term>Isochrone</term><term>Jeffreys</term><term>Journal compilation</term><term>Kendall stuart</term><term>Kia3</term><term>Kia4</term><term>Kinematics</term><term>Kinetic energy</term><term>Large number</term><term>Large value</term><term>Last column</term><term>Likelihood</term><term>Likelihood analysis</term><term>Likelihood contours</term><term>Likelihood distribution</term><term>Likelihood equation</term><term>Likelihood estimates</term><term>Likelihood function</term><term>Lower limit</term><term>Lower panel</term><term>Mass density</term><term>Mass distribution</term><term>Maximum likelihood</term><term>Maximum likelihood analysis</term><term>Maximum likelihood method</term><term>Maximum likelihood pairs</term><term>Maximum likelihood values</term><term>Median likelihood</term><term>Milky</term><term>Minimum velocity</term><term>Mnras</term><term>More information</term><term>Motion stars</term><term>Nancial support</term><term>National science foundation</term><term>Navarro</term><term>Neighbourhood</term><term>Netherlands organization</term><term>Normal distribution</term><term>Orbital rotation</term><term>Original data</term><term>Original sample</term><term>Original sample size</term><term>Outer edge</term><term>Outer parts</term><term>Peak likelihood</term><term>Posterior distribution</term><term>Previous section</term><term>Previous studies</term><term>Previous work</term><term>Princeton univ</term><term>Probability distribution</term><term>Proper motion</term><term>Proper motions</term><term>Radial</term><term>Radial velocities</term><term>Radial velocity</term><term>Radial velocity measurements</term><term>Radius</term><term>Reference priors</term><term>Rescaled galaxies</term><term>Rescaling factor</term><term>Rotation curve</term><term>Rvir</term><term>Sample volume</term><term>Scale radius</term><term>Section name</term><term>Simulation</term><term>Solar circle</term><term>Solar motion</term><term>Solar neighbourhood</term><term>Solar radius</term><term>Solid curves</term><term>Spectroscopic binaries</term><term>Star</term><term>Star particles</term><term>Statistical arguments</term><term>Steinmetz</term><term>Stellar</term><term>Stellar halo</term><term>Stellar particles</term><term>Stellar velocities</term><term>Stellar velocity distribution</term><term>Surface brightness</term><term>Tangential</term><term>Tangential velocities</term><term>Tangential velocity</term><term>Thick disc</term><term>Thick discs</term><term>Thickdisc stars</term><term>Thin disc</term><term>Third column</term><term>Total halo mass</term><term>Total mass</term><term>Total number</term><term>Tremaine</term><term>Triangle symbols</term><term>Truncation</term><term>Typical errors</term><term>Unbound</term><term>Unbound stars</term><term>Velocity</term><term>Velocity dispersion</term><term>Velocity distribution</term><term>Velocity distributions</term><term>Velocity stars</term><term>Vesc</term><term>Vesc vmin</term><term>Virial</term><term>Virial mass</term><term>Virial radius</term><term>Virial velocity</term><term>Vmin</term><term>Vmin bootstrap</term><term>Wilkinson</term><term>Wilkinson evans</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 < vesc < 608 km s−1 (90 per cent confidence), with a median likelihood of 544 km s−1. The fact that v2esc is significantly greater than 2v2circ (where vcirc= 220 km 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 vesc 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+1.14−0.54× 1012 M⊙ and virial radius of (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.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>bootstrap</json:string><json:string>vesc</json:string><json:string>mnras</json:string><json:string>velocity distribution</json:string><json:string>halo</json:string><json:string>stellar</json:string><json:string>journal compilation</json:string><json:string>bootstrap distribution</json:string><json:string>radial velocities</json:string><json:string>steinmetz</json:string><json:string>virial</json:string><json:string>stellar particles</json:string><json:string>binary</json:string><json:string>abadi</json:string><json:string>tremaine</json:string><json:string>cosmological simulations</json:string><json:string>binney</json:string><json:string>navarro</json:string><json:string>maximum likelihood values</json:string><json:string>jeffreys</json:string><json:string>distribution function</json:string><json:string>galaxy</json:string><json:string>total mass</json:string><json:string>solar radius</json:string><json:string>rvir</json:string><json:string>virial radius</json:string><json:string>truncation</json:string><json:string>circular velocity</json:string><json:string>thin disc</json:string><json:string>galactic</json:string><json:string>kinematics</json:string><json:string>thick disc</json:string><json:string>kia4</json:string><json:string>dehnen</json:string><json:string>kia3</json:string><json:string>isochrone</json:string><json:string>constraint</json:string><json:string>tangential</json:string><json:string>simulation</json:string><json:string>vmin</json:string><json:string>circ</json:string><json:string>solar circle</json:string><json:string>archival</json:string><json:string>galactocentric</json:string><json:string>proper motion</json:string><json:string>maximum likelihood</json:string><json:string>stellar velocities</json:string><json:string>cent 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distributions</json:string><json:string>peak likelihood</json:string><json:string>unbound stars</json:string><json:string>reference priors</json:string><json:string>total number</json:string><json:string>binary stars</json:string><json:string>velocity stars</json:string><json:string>previous work</json:string><json:string>hypervelocity stars</json:string><json:string>virial mass</json:string><json:string>globular clusters</json:string><json:string>rotation curve</json:string><json:string>radial velocity measurements</json:string><json:string>information matrix</json:string><json:string>halo giants</json:string><json:string>unbound</json:string><json:string>wilkinson</json:string><json:string>disc</json:string><json:string>radial</json:string><json:string>centre</json:string><json:string>cosmological</json:string><json:string>star</json:string><json:string>fractional contribution</json:string><json:string>likelihood analysis</json:string><json:string>posterior distribution</json:string><json:string>bootstrap analysis</json:string><json:string>likelihood function</json:string><json:string>halo stars</json:string><json:string>critical density</json:string><json:string>tangential velocities</json:string><json:string>halo component</json:string><json:string>stellar halo</json:string><json:string>kinetic energy</json:string><json:string>likelihood estimates</json:string><json:string>minimum velocity</json:string><json:string>chiba beers</json:string><json:string>mass density</json:string><json:string>binary systems</json:string><json:string>solar motion</json:string><json:string>halo mass</json:string><json:string>lower panel</json:string><json:string>galactic halo</json:string><json:string>maximum likelihood analysis</json:string><json:string>probability distribution</json:string><json:string>third column</json:string><json:string>fourth column</json:string><json:string>last column</json:string><json:string>princeton univ</json:string><json:string>distribution approximation</json:string><json:string>bootstrap distributions</json:string><json:string>likelihood</json:string><json:string>contamination</json:string><json:string>radius</json:string><json:string>dehnen binney</json:string><json:string>outer parts</json:string><json:string>galaxies kia1</json:string><json:string>higher values</json:string><json:string>original sample</json:string><json:string>kendall stuart</json:string><json:string>orbital rotation</json:string><json:string>statistical arguments</json:string><json:string>additional information</json:string><json:string>original sample size</json:string><json:string>outer edge</json:string><json:string>large value</json:string><json:string>maximum likelihood pairs</json:string><json:string>rescaling factor</json:string><json:string>high degree</json:string><json:string>thickdisc stars</json:string><json:string>rescaled galaxies</json:string><json:string>normal distribution</json:string><json:string>likelihood distribution</json:string><json:string>halo model</json:string><json:string>large number</json:string><json:string>spectroscopic binaries</json:string><json:string>motion stars</json:string><json:string>binney tremaine</json:string><json:string>denis catalogue</json:string><json:string>binary mass motion</json:string><json:string>section name</json:string><json:string>galactic longitude</json:string><json:string>additional stars</json:string><json:string>circular orbits</json:string><json:string>maximum likelihood method</json:string><json:string>likelihood contours</json:string><json:string>star particles</json:string><json:string>typical errors</json:string><json:string>fair comparison</json:string><json:string>proper motions</json:string><json:string>stellar velocity distribution</json:string><json:string>dark matter components</json:string><json:string>accurate representation</json:string><json:string>thick discs</json:string><json:string>vmin bootstrap</json:string><json:string>previous section</json:string><json:string>original data</json:string><json:string>solid curves</json:string><json:string>more information</json:string><json:string>fastest stars</json:string><json:string>halo masses</json:string><json:string>triangle symbols</json:string><json:string>surface brightness</json:string><json:string>velocity dispersion</json:string><json:string>different assumptions</json:string><json:string>halo isochrone</json:string><json:string>scale radius</json:string><json:string>concentration parameter</json:string><json:string>fastest star</json:string><json:string>dark matter halo</json:string><json:string>virial velocity</json:string><json:string>national science foundation</json:string><json:string>netherlands organization</json:string><json:string>exponential disc</json:string><json:string>elliptical galaxies</json:string><json:string>previous studies</json:string><json:string>nancial support</json:string><json:string>asymptotic behaviour</json:string><json:string>vesc vmin</json:string><json:string>likelihood equation</json:string></teeft></keywords><author><json:item><name>Martin C. Smith</name><affiliations><json:string>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</json:string><json:string>E-mail: msmith@astro.rug.nl</json:string></affiliations></json:item><json:item><name>Gregory R. Ruchti</name><affiliations><json:string>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</json:string></affiliations></json:item><json:item><name>Amina Helmi</name><affiliations><json:string>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</json:string></affiliations></json:item><json:item><name>Rosemary F. G. Wyse</name><affiliations><json:string>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</json:string></affiliations></json:item><json:item><name>J. P. Fulbright</name><affiliations><json:string>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</json:string></affiliations></json:item><json:item><name>K. C. Freeman</name><affiliations><json:string>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</json:string></affiliations></json:item><json:item><name>J. F. Navarro</name><affiliations><json:string>University of Victoria, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6</json:string></affiliations></json:item><json:item><name>G. M. Seabroke</name><affiliations><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>M. Steinmetz</name><affiliations><json:string>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>M. Williams</name><affiliations><json:string>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</json:string></affiliations></json:item><json:item><name>O. Bienaymé</name><affiliations><json:string>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>J. Binney</name><affiliations><json:string>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP</json:string></affiliations></json:item><json:item><name>J. Bland‐Hawthorn</name><affiliations><json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</json:string></affiliations></json:item><json:item><name>W. Dehnen</name><affiliations><json:string>University of Leicester, University Road, Leicester LE1 7RH</json:string></affiliations></json:item><json:item><name>B. K. Gibson</name><affiliations><json:string>University of Central Lancashire, Preston PR1 2HE</json:string></affiliations></json:item><json:item><name>G. Gilmore</name><affiliations><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</json:string></affiliations></json:item><json:item><name>E. K. Grebel</name><affiliations><json:string>Astronomisches Institut, Universität Basel, Venusstrasse 7, Binningen CH‐4102, Switzerland</json:string></affiliations></json:item><json:item><name>U. Munari</name><affiliations><json:string>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8, Asiago I‐36012, Italy</json:string></affiliations></json:item><json:item><name>Q. A. Parker</name><affiliations><json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</json:string><json:string>Macquarie University, Sydney, NSW 2109, Australia</json:string></affiliations></json:item><json:item><name>R.‐D. Scholz</name><affiliations><json:string>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>A. Siebert</name><affiliations><json:string>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</json:string></affiliations></json:item><json:item><name>F. G. Watson</name><affiliations><json:string>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</json:string></affiliations></json:item><json:item><name>T. Zwitter</name><affiliations><json:string>Department of Physics, University of Ljubljana, Jadranska 19, Ljubljana, Slovenia</json:string></affiliations></json:item></author><subject><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>MNR11964</json:string></articleId><arkIstex>ark:/67375/WNG-HWGF1B7G-F</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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 > vesc > 608 km s−1 (90 per cent confidence), with a median likelihood of 544 km s−1. The fact that v2esc is significantly greater than 2v2circ (where vcirc= 220 km 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 vesc 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+1.14−0.54× 1012 M⊙ and virial radius of (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.</abstract><qualityIndicators><score>9.52</score><pdfWordCount>16853</pdfWordCount><pdfCharCount>88828</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>18</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>210</abstractWordCount><abstractCharCount>1285</abstractCharCount><keywordCount>2</keywordCount></qualityIndicators><title>The RAVE survey: constraining the local Galactic escape speed</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>379</volume><issue>2</issue><pages><first>755</first><last>772</last><total>18</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>1920s</json:string><json:string>the 20th century</json:string><json:string>2007</json:string><json:string>2010</json:string><json:string>1359</json:string></date><geogName></geogName><orgName><json:string>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB</json:string><json:string>University of Oxford</json:string><json:string>Department of Physics, University of Ljubljana, Jadranska</json:string><json:string>Netherlands Research School for Astronomy, Natural Sciences and Engineering</json:string><json:string>Research School of Astronomy and Astrophysics</json:string><json:string>The Johns Hopkins University</json:string><json:string>Astrophysical Institute Potsdam, Australian Research Council, German Research Foundation, National Institute for Astrophysics</json:string><json:string>Slovenian Research Agency</json:string><json:string>Macquarie University</json:string><json:string>University of Victoria</json:string><json:string>University of Central Lancashire</json:string><json:string>Research, Particle Physics and Astronomy</json:string><json:string>United Kingdom Schmidt Telescope of the Anglo-Australian Observatory</json:string><json:string>University of Leicester</json:string><json:string>Netherlands Hopkins University</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>U. Munari</json:string><json:string>Gregory R. Ruchti</json:string><json:string>K. C. Freeman</json:string><json:string>A. Siebert</json:string><json:string>F. G. Wyse</json:string><json:string>T. Zwitter</json:string><json:string>F. Navarro</json:string><json:string>M. Seabroke</json:string><json:string>G. Gilmore</json:string><json:string>E. K. Grebel</json:string><json:string>A. Parker</json:string><json:string>Amina Helmi</json:string><json:string>To</json:string><json:string>K. Gibson</json:string><json:string>F. G. Watson</json:string><json:string>Charles Street</json:string><json:string>D. Scholz</json:string><json:string>P. Fulbright</json:string><json:string>Martin C. Smith</json:string></persName><placeName><json:string>Groningen</json:string><json:string>Potsdam</json:string><json:string>Germany</json:string><json:string>Ljubljana</json:string><json:string>Australia</json:string><json:string>Mexico</json:string><json:string>UK</json:string><json:string>Canada</json:string><json:string>Slovenia</json:string><json:string>Canberra</json:string><json:string>Strasbourg</json:string><json:string>Baltimore</json:string><json:string>Basel</json:string><json:string>MD</json:string><json:string>Chiba</json:string><json:string>Velocity</json:string><json:string>France</json:string><json:string>Cambridge</json:string><json:string>Italy</json:string></placeName><ref_url></ref_url><ref_bibl><json:string>Bloomberg Center, 3400</json:string><json:string>Jahreiß & Wielen 1997</json:string><json:string>Tonry & Davis 1979</json:string><json:string>Navarro et al. 1996</json:string><json:string>Abadi et al. 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G.</forename><surname>Wyse</surname></persName><affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">J. P.</forename><surname>Fulbright</surname></persName><affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">K. C.</forename><surname>Freeman</surname></persName><affiliation>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">J. F.</forename><surname>Navarro</surname></persName><affiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6<address><country key="CA"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">G. M.</forename><surname>Seabroke</surname></persName><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-0008"><persName><forename type="first">M.</forename><surname>Steinmetz</surname></persName><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">M.</forename><surname>Williams</surname></persName><affiliation>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">O.</forename><surname>Bienaymé</surname></persName><affiliation>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">J.</forename><surname>Binney</surname></persName><affiliation>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP</affiliation></author><author xml:id="author-0012"><persName><forename type="first">J.</forename><surname>Bland‐Hawthorn</surname></persName><affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">W.</forename><surname>Dehnen</surname></persName><affiliation>University of Leicester, University Road, Leicester LE1 7RH</affiliation></author><author xml:id="author-0014"><persName><forename type="first">B. K.</forename><surname>Gibson</surname></persName><affiliation>University of Central Lancashire, Preston PR1 2HE</affiliation></author><author xml:id="author-0015"><persName><forename type="first">G.</forename><surname>Gilmore</surname></persName><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-0016"><persName><forename type="first">E. K.</forename><surname>Grebel</surname></persName><affiliation>Astronomisches Institut, Universität Basel, Venusstrasse 7, Binningen CH‐4102, Switzerland<address><country key="CH"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">U.</forename><surname>Munari</surname></persName><affiliation>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8, Asiago I‐36012, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0018"><persName><forename type="first">Q. A.</forename><surname>Parker</surname></persName><affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation><affiliation>Macquarie University, Sydney, NSW 2109, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0019"><persName><forename type="first">R.‐D.</forename><surname>Scholz</surname></persName><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0020"><persName><forename type="first">A.</forename><surname>Siebert</surname></persName><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0021"><persName><forename type="first">F. G.</forename><surname>Watson</surname></persName><affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0022"><persName><forename type="first">T.</forename><surname>Zwitter</surname></persName><affiliation>Department of Physics, University of Ljubljana, Jadranska 19, Ljubljana, Slovenia<address><country key="SI"></country></address></affiliation></author><idno type="istex">ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB</idno><idno type="ark">ark:/67375/WNG-HWGF1B7G-F</idno><idno type="DOI">10.1111/j.1365-2966.2007.11964.x</idno><idno type="unit">MNR11964</idno><idno type="toTypesetVersion">file:MNR.MNR11964.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.2007.379.issue-2</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">379</biblScope><biblScope unit="issue">2</biblScope><biblScope unit="page" from="755">755</biblScope><biblScope unit="page" to="772">772</biblScope><biblScope unit="page-count">18</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-08"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>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 <emph><span>498 < <hi rend="italic">v</hi><hi rend="subscript">esc</hi> < 608 km s<hi rend="superscript">−1</hi></span></emph> (90 per cent confidence), with a median likelihood of 544 km s<hi rend="superscript">−1</hi>. The fact that <hi rend="italic">v</hi><hi rend="superscript">2</hi><hi rend="subscript">esc</hi> is significantly greater than 2<hi rend="italic">v</hi><hi rend="superscript">2</hi><hi rend="subscript">circ</hi> (where <hi rend="italic">v</hi><hi rend="subscript">circ</hi>= 220 km s<hi rend="superscript">−1</hi> 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 <hi rend="italic">v</hi><hi rend="subscript">esc</hi> 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 <emph><span>1.42<hi rend="superscript">+1.14</hi><hi rend="subscript">−0.54</hi>× 10<hi rend="superscript">12</hi> M<hi rend="subscript">⊙</hi></span></emph> and virial radius of <graphic url="equation/MNR_11964_mu1.gif" rend="inline image"></graphic> (90 per cent confidence). For this model the circular velocity at the virial radius is 142<hi rend="superscript">+31</hi><hi rend="subscript">−21</hi> km s<hi rend="superscript">−1</hi>. Although our halo masses are model dependent, we find that they are in good agreement with each other.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">Galaxy: fundamental parameters</term><term xml:id="k2">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/ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB/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="08002"><doi origin="wiley">10.1111/mnr.2007.379.issue-2</doi><numberingGroup><numbering type="journalVolume" number="379">379</numbering><numbering type="journalIssue" number="2">2</numbering></numberingGroup><coverDate startDate="2007-08">August 2007</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="23" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2007.11964.x</doi><idGroup><id type="unit" value="MNR11964"></id></idGroup><countGroup><count type="pageTotal" number="18"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2007-07-05"></event><event type="publishedOnlineFinalForm" date="2007-07-11"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.6 mode:FullText source:FullText result:FullText" date="2010-04-21"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-11-01"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="755">755</numbering><numbering type="pageLast" number="772">772</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>msmith@astro.rug.nl</email></correspondenceTo><objectNameGroup><objectName elementName="appendix">Appendices</objectName></objectNameGroup><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR11964.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2007 May 9. Received 2007 April 17; in original form 2006 November 21</unparsedEditorialHistory><countGroup><count type="figureTotal" number="9"></count><count type="tableTotal" number="6"></count><count type="formulaTotal" number="103"></count><count type="referenceTotal" number="72"></count><count type="linksCrossRef" number="299"></count></countGroup><titleGroup><title type="main">The RAVE survey: constraining the local Galactic escape speed</title><title type="shortAuthors"><i>M. C. Smith et al.</i></title><title type="short"><i>Constraining the local Galactic escape speed</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Martin C.</givenNames><familyName>Smith</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>Gregory R.</givenNames><familyName>Ruchti</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a1"><personName><givenNames>Amina</givenNames><familyName>Helmi</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a2"><personName><givenNames>Rosemary F. G.</givenNames><familyName>Wyse</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a2"><personName><givenNames>J. P.</givenNames><familyName>Fulbright</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a3"><personName><givenNames>K. C.</givenNames><familyName>Freeman</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a4"><personName><givenNames>J. F.</givenNames><familyName>Navarro</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a5"><personName><givenNames>G. 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A.</givenNames><familyName>Parker</familyName></personName></creator><creator creatorRole="author" xml:id="cr20" affiliationRef="#a6"><personName><givenNames>R.‐D.</givenNames><familyName>Scholz</familyName></personName></creator><creator creatorRole="author" xml:id="cr21" affiliationRef="#a6"><personName><givenNames>A.</givenNames><familyName>Siebert</familyName></personName></creator><creator creatorRole="author" xml:id="cr22" affiliationRef="#a9"><personName><givenNames>F. G.</givenNames><familyName>Watson</familyName></personName></creator><creator creatorRole="author" xml:id="cr23" affiliationRef="#a15"><personName><givenNames>T.</givenNames><familyName>Zwitter</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="NL"><unparsedAffiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="US"><unparsedAffiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="AU"><unparsedAffiliation>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="CA"><unparsedAffiliation>University of Victoria, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6</unparsedAffiliation></affiliation><affiliation xml:id="a5"><unparsedAffiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="DE"><unparsedAffiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a8"><unparsedAffiliation>Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="AU"><unparsedAffiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a10"><unparsedAffiliation>University of Leicester, University Road, Leicester LE1 7RH</unparsedAffiliation></affiliation><affiliation xml:id="a11"><unparsedAffiliation>University of Central Lancashire, Preston PR1 2HE</unparsedAffiliation></affiliation><affiliation xml:id="a12" countryCode="CH"><unparsedAffiliation>Astronomisches Institut, Universität Basel, Venusstrasse 7, Binningen CH‐4102, Switzerland</unparsedAffiliation></affiliation><affiliation xml:id="a13" countryCode="IT"><unparsedAffiliation>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8, Asiago I‐36012, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a14" countryCode="AU"><unparsedAffiliation>Macquarie University, Sydney, NSW 2109, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a15" countryCode="SI"><unparsedAffiliation>Department of Physics, University of Ljubljana, Jadranska 19, Ljubljana, Slovenia</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">Galaxy: fundamental parameters</keyword><keyword xml:id="k2">Galaxy: kinematics and dynamics</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>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 <span type="mathematics">498 < <i>v</i><sub>esc</sub> < 608 km s<sup>−1</sup></span> (90 per cent confidence), with a median likelihood of 544 km s<sup>−1</sup>. The fact that <i>v</i><sup>2</sup><sub>esc</sub> is significantly greater than 2<i>v</i><sup>2</sup><sub>circ</sub> (where <i>v</i><sub>circ</sub>= 220 km 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 <i>v</i><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 <span type="mathematics">1.42<sup>+1.14</sup><sub>−0.54</sub>× 10<sup>12</sup> M<sub>⊙</sub></span> and virial radius of <inlineGraphic alt="inline image" location="equation/MNR_11964_mu1.gif" href=""></inlineGraphic> (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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>The RAVE survey: constraining the local Galactic escape speed</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Constraining the local Galactic escape speed</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>The RAVE survey: constraining the local Galactic escape speed</title></titleInfo><name type="personal"><namePart type="given">Martin C.</namePart><namePart type="family">Smith</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><affiliation>E-mail: msmith@astro.rug.nl</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Gregory R.</namePart><namePart type="family">Ruchti</namePart><affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Amina</namePart><namePart type="family">Helmi</namePart><affiliation>Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Rosemary F. G.</namePart><namePart type="family">Wyse</namePart><affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. P.</namePart><namePart type="family">Fulbright</namePart><affiliation>Johns Hopkins University, 366 Bloomberg Center, 3400 North Charles Street, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K. C.</namePart><namePart type="family">Freeman</namePart><affiliation>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</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, PO Box 3055, Station CSC, Victoria, BC, Canada V8W 3P6</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G. M.</namePart><namePart type="family">Seabroke</namePart><affiliation>Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Steinmetz</namePart><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 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>Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Cotter Road, Weston Creek, Canberra, ACT 72611, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">O.</namePart><namePart type="family">Bienaymé</namePart><affiliation>Observatoire de Strasbourg, 11 Rue de L'Université, 67000 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, University of Oxford, 1 Keble Road, Oxford OX1 3NP</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, PO Box 296, Epping, NSW 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">W.</namePart><namePart type="family">Dehnen</namePart><affiliation>University of Leicester, University Road, Leicester LE1 7RH</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 PR1 2HE</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, University of Cambridge, Madingley Road, Cambridge CB3 0HA</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 Institut, Universität Basel, Venusstrasse 7, Binningen CH‐4102, Switzerland</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">U.</namePart><namePart type="family">Munari</namePart><affiliation>INAF Osservatorio Astronomico di Padova, Via dell'Osservatorio 8, Asiago I‐36012, Italy</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, PO Box 296, Epping, NSW 1710, Australia</affiliation><affiliation>Macquarie University, Sydney, NSW 2109, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.‐D.</namePart><namePart type="family">Scholz</namePart><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Siebert</namePart><affiliation>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">F. G.</namePart><namePart type="family">Watson</namePart><affiliation>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Zwitter</namePart><affiliation>Department of Physics, University of Ljubljana, Jadranska 19, 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">2007-08</dateIssued><edition>Accepted 2007 May 9. Received 2007 April 17; in original form 2006 November 21</edition><copyrightDate encoding="w3cdtf">2007</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">6</extent><extent unit="formulas">103</extent><extent unit="references">72</extent><extent unit="linksCrossRef">299</extent></physicalDescription><abstract 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 < vesc < 608 km s−1 (90 per cent confidence), with a median likelihood of 544 km s−1. The fact that v2esc is significantly greater than 2v2circ (where vcirc= 220 km 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 vesc 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+1.14−0.54× 1012 M⊙ and virial radius of (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.</abstract><subject lang="en"><genre>keywords</genre><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>2007</date><detail type="volume"><caption>vol.</caption><number>379</number></detail><detail type="issue"><caption>no.</caption><number>2</number></detail><extent unit="pages"><start>755</start><end>772</end><total>18</total></extent></part></relatedItem><identifier type="istex">ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB</identifier><identifier type="ark">ark:/67375/WNG-HWGF1B7G-F</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.11964.x</identifier><identifier type="ArticleID">MNR11964</identifier><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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