The RAVE survey: constraining the local Galactic escape speed
Identifieur interne : 009083 ( Main/Exploration ); précédent : 009082; suivant : 009084The 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. Bienaymé [France] ; J. Binney [Royaume-Uni] ; J. Bland-Hawthorn [Australie] ; W. Dehnen ; B. K. Gibson ; G. Gilmore [Royaume-Uni] ; E. K. Grebel [Suisse] ; U. Munari [Italie] ; Q. A. Parker [Australie] ; R. Scholz [Allemagne] ; A. Siebert [Allemagne] ; F. G. Watson [Australie] ; T. Zwitter [Slovénie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-08.
Descripteurs français
- Pascal (Inist)
- Wicri :
- topic : Simulation.
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, Circle, 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, Disk galaxies, Distribution approximation, Distribution function, Dynamics, Elliptical galaxies, Escape velocity, Exponential disc, Fair comparison, Fastest star, Fastest stars, Fourth column, Fractional contribution, Galactic, Galactic centre, Galactic halo, Galactic halos, Galactic longitude, Galactocentric, Galaxies kia1, Galaxy, Galaxy formation, Galaxy halo, Globular clusters, Good agreement, Halo, Halo component, Halo giants, Halo isochrone, Halo mass, Halo masses, Halo model, Halo stars, High degree, High velocity star, 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, Milky Way, Minimum velocity, Mnras, Models, 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:
- https://api.istex.fr/document/ED8060E2435B35A0ABBEB8ADC7D1E2FB87BFCBEB/fulltext/pdf
- https://api.istex.fr/document/2B601EE5E952B20A4850DA4FA04082437F33EB5A/fulltext/pdf
DOI: 10.1111/j.1365-2966.2007.11964.x
Affiliations:
- Allemagne, Australie, Canada, France, Italie, Pays-Bas, Royaume-Uni, Slovénie, Suisse, États-Unis
- Alsace (région administrative), Angleterre, Angleterre de l'Est, Canton de Bâle-Ville, Grand Est, Groningue (province), Maryland, Oxfordshire
- Bâle, Cambridge, Groningue (ville), Oxford, Strasbourg
- Université d'Oxford, Université de Bâle, Université de Cambridge, Université de Groningue
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Siebert</name><affiliation wicri:level="1"><country xml:lang="fr">Allemagne</country><wicri:regionArea>Astrophysikalisches Institut Potsdam, An der Sterwarte 16, D‐14482 Potsdam</wicri:regionArea><wicri:noRegion>14482 Potsdam</wicri:noRegion><wicri:noRegion>D‐14482 Potsdam</wicri:noRegion></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"><country xml:lang="fr">Australie</country><wicri:regionArea>Anglo‐Australian Observatory, PO Box 296, Epping, NSW 1710</wicri:regionArea><wicri:noRegion>NSW 1710</wicri:noRegion></affiliation></author><author><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name><affiliation wicri:level="1"><country xml:lang="fr">Slovénie</country><wicri:regionArea>Department of Physics, University of Ljubljana, Jadranska 19, Ljubljana</wicri:regionArea><wicri:noRegion>Ljubljana</wicri:noRegion></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>Circle</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>Disk galaxies</term><term>Distribution approximation</term><term>Distribution function</term><term>Dynamics</term><term>Elliptical galaxies</term><term>Escape velocity</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 halos</term><term>Galactic longitude</term><term>Galactocentric</term><term>Galaxies kia1</term><term>Galaxy</term><term>Galaxy formation</term><term>Galaxy halo</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>High velocity star</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>Milky Way</term><term>Minimum velocity</term><term>Mnras</term><term>Models</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="Pascal" xml:lang="fr"><term>Cercle</term><term>Cinématique</term><term>Distribution vitesse</term><term>Dynamique</term><term>Etoile grande vitesse</term><term>Formation galaxies</term><term>Galaxies disques</term><term>Halo galactique</term><term>Halo galaxies</term><term>Masse viriel</term><term>Modèle</term><term>Vitesse fuite</term><term>Voie lactée</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><keywords scheme="Wicri" type="topic" xml:lang="fr"><term>Simulation</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><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>Canada</li><li>France</li><li>Italie</li><li>Pays-Bas</li><li>Royaume-Uni</li><li>Slovénie</li><li>Suisse</li><li>États-Unis</li></country><region><li>Alsace (région administrative)</li><li>Angleterre</li><li>Angleterre de l'Est</li><li>Canton de Bâle-Ville</li><li>Grand Est</li><li>Groningue (province)</li><li>Maryland</li><li>Oxfordshire</li></region><settlement><li>Bâle</li><li>Cambridge</li><li>Groningue (ville)</li><li>Oxford</li><li>Strasbourg</li></settlement><orgName><li>Université d'Oxford</li><li>Université de Bâle</li><li>Université de Cambridge</li><li>Université de Groningue</li></orgName></list><tree><noCountry><name sortKey="Dehnen, W" sort="Dehnen, W" uniqKey="Dehnen W" first="W." last="Dehnen">W. Dehnen</name><name sortKey="Gibson, B K" sort="Gibson, B K" uniqKey="Gibson B" first="B. K." last="Gibson">B. K. Gibson</name></noCountry><country name="Pays-Bas"><region name="Groningue (province)"><name sortKey="Smith, Martin C" sort="Smith, Martin C" uniqKey="Smith M" first="Martin C." last="Smith">Martin C. Smith</name></region><name sortKey="Helmi, Amina" sort="Helmi, Amina" uniqKey="Helmi A" first="Amina" last="Helmi">Amina Helmi</name><name sortKey="Smith, Martin C" sort="Smith, Martin C" uniqKey="Smith M" first="Martin C." last="Smith">Martin C. Smith</name></country><country name="États-Unis"><region name="Maryland"><name sortKey="Ruchti, Gregory R" sort="Ruchti, Gregory R" uniqKey="Ruchti G" first="Gregory R." last="Ruchti">Gregory R. Ruchti</name></region><name sortKey="Fulbright, J P" sort="Fulbright, J P" uniqKey="Fulbright J" first="J. P." last="Fulbright">J. P. Fulbright</name><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></country><country name="Australie"><noRegion><name sortKey="Freeman, K C" sort="Freeman, K C" uniqKey="Freeman K" first="K. C." last="Freeman">K. C. Freeman</name></noRegion><name sortKey="Bland Awthorn, J" sort="Bland Awthorn, J" uniqKey="Bland Awthorn J" first="J." last="Bland-Hawthorn">J. Bland-Hawthorn</name><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><name sortKey="Parker, Q A" sort="Parker, Q A" uniqKey="Parker Q" first="Q. A." last="Parker">Q. A. Parker</name><name sortKey="Watson, F G" sort="Watson, F G" uniqKey="Watson F" first="F. G." last="Watson">F. G. Watson</name><name sortKey="Williams, M" sort="Williams, M" uniqKey="Williams M" first="M." last="Williams">M. Williams</name></country><country name="Canada"><noRegion><name sortKey="Navarro, J F" sort="Navarro, J F" uniqKey="Navarro J" first="J. F." last="Navarro">J. F. Navarro</name></noRegion></country><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Seabroke, G M" sort="Seabroke, G M" uniqKey="Seabroke G" first="G. M." last="Seabroke">G. M. Seabroke</name></region><name sortKey="Binney, J" sort="Binney, J" uniqKey="Binney J" first="J." last="Binney">J. Binney</name><name sortKey="Gilmore, G" sort="Gilmore, G" uniqKey="Gilmore G" first="G." last="Gilmore">G. Gilmore</name></country><country name="Allemagne"><noRegion><name sortKey="Steinmetz, M" sort="Steinmetz, M" uniqKey="Steinmetz M" first="M." last="Steinmetz">M. Steinmetz</name></noRegion><name sortKey="Scholz, R" sort="Scholz, R" uniqKey="Scholz R" first="R." last="Scholz">R. Scholz</name><name sortKey="Siebert, A" sort="Siebert, A" uniqKey="Siebert A" first="A." last="Siebert">A. Siebert</name></country><country name="France"><region name="Grand Est"><name sortKey="Bienayme, O" sort="Bienayme, O" uniqKey="Bienayme O" first="O." last="Bienaymé">O. Bienaymé</name></region></country><country name="Suisse"><region name="Canton de Bâle-Ville"><name sortKey="Grebel, E K" sort="Grebel, E K" uniqKey="Grebel E" first="E. K." last="Grebel">E. K. Grebel</name></region></country><country name="Italie"><noRegion><name sortKey="Munari, U" sort="Munari, U" uniqKey="Munari U" first="U." last="Munari">U. Munari</name></noRegion></country><country name="Slovénie"><noRegion><name sortKey="Zwitter, T" sort="Zwitter, T" uniqKey="Zwitter T" first="T." last="Zwitter">T. Zwitter</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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