Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating
Identifieur interne : 007273 ( Main/Exploration ); précédent : 007272; suivant : 007274Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating
Auteurs : Richard R. Lane [Australie] ; Lászl L. Kiss [Australie, Hongrie] ; Geraint F. Lewis [Australie] ; Rodrigo A. Ibata [France] ; Arnaud Siebert [France] ; Timothy R. Bedding [Australie] ; Péter Székely [Hongrie] ; Zoltán Balog [Allemagne] ; Gyula M. Szab [Hongrie]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-08-21.
Descripteurs français
- Pascal (Inist)
English descriptors
- KwdEn :
- Aaomega, Approximate axis, Calcium triplet lines, Central velocity dispersion, Cluster, Cluster centre, Cluster members, Cluster membership, Confusion effects, Current paper, Current study, Dark halo, Dark matter, Dispersion, Distant cluster member, Distant clusters, Distant member, Equivalent width, Flattening, Galactic, Galactic centre, Galactic disks, Galactic halos, Galaxy, Globular, Globular clusters, Gravitation, Gravity, Halo, Halo globular clusters, Hungarian academy, Individual velocity uncertainties, Internal kinematics, Intriguing possibility, Intriguing puzzle, Johnson pilachowski, Journal compilation, Kinematic measurements, Kinematics, Kruijssen mieske, Line strengths, Literature values, Lower panel, Luminosity, Mass estimate, Membership selections, Metallicity, Milky Way, Mnras, Newtonian, Newtonian dynamics, Newtonian gravity, Open circle, Outer regions, Plummer, Plummer model, Plummer models, Plummer scale radius, Previous studies, Radial velocities, Radial velocity, Radius, Relaxation time, Scale radius, Scarpa, Similar conclusions, Small radii, Solid points, Sollima nipoti, Spectroscopical observation, Square parsec, Star clusters, Stellar dynamics, Stellar velocities, Surface brightness data, Systemic velocities, Thick line, Thin lines, Tidal, Tidal effects, Tidal heating, Tidal radii, Tidal radius, Total luminosity, Total mass, Trgb, Velocity dispersion, Velocity dispersions.
- Teeft :
- Aaomega, Approximate axis, Calcium triplet lines, Central velocity dispersion, Cluster, Cluster centre, Cluster members, Cluster membership, Confusion effects, Current paper, Current study, Dark halo, Dark matter, Dispersion, Distant cluster member, Distant clusters, Distant member, Equivalent width, Galactic, Galactic centre, Galaxy, Globular, Globular clusters, Halo, Halo globular clusters, Hungarian academy, Individual velocity uncertainties, Internal kinematics, Intriguing possibility, Intriguing puzzle, Johnson pilachowski, Journal compilation, Kinematic measurements, Kinematics, Kruijssen mieske, Line strengths, Literature values, Lower panel, Luminosity, Mass estimate, Membership selections, Metallicity, Mnras, Newtonian, Newtonian dynamics, Newtonian gravity, Open circle, Outer regions, Plummer, Plummer model, Plummer models, Plummer scale radius, Previous studies, Radial velocities, Radial velocity, Radius, Relaxation time, Scale radius, Scarpa, Similar conclusions, Small radii, Solid points, Sollima nipoti, Square parsec, Stellar velocities, Surface brightness data, Systemic velocities, Thick line, Thin lines, Tidal, Tidal effects, Tidal heating, Tidal radii, Tidal radius, Total luminosity, Total mass, Trgb, Velocity dispersion, Velocity dispersions.
Abstract
Globular clusters (GCs) have proven to be essential to our understanding of many important astrophysical phenomena. Here, we analyse spectroscopic observations of 10 halo GCs to determine their dark matter (DM) content, their tidal heating by the Galactic disc and halo, describe their metallicities and the likelihood that Newtonian dynamics explains their kinematics. We analyse a large number of members in all clusters, allowing us to address all these issues together, and we have included NGC 288 and M30 to overlap with previous studies. We find that any flattening of the velocity dispersion profiles in the outer regions of our clusters can be explained by tidal heating. We also find that all our GCs have M/LV≲ 5, therefore, we infer the observed dynamics do not require DM, or a modification of gravity. We suggest that the lack of tidal heating signatures in distant clusters indicates the halo is not triaxial. The isothermal rotations of each cluster are measured, with M4 and NGC 288 exhibiting rotation at a level of 0.9 ± 0.1 km s−1 and 0.25 ± 0.15 km s−1, respectively. We also indirectly measure the tidal radius of NGC 6752, determining a more realistic figure for this cluster than current literature values. Lastly, an unresolved and intriguing puzzle is uncovered with regard to the cooling of the outer regions of all ten clusters.
Url:
- https://api.istex.fr/document/2290B85556B7D90BFEF26C395007389DEFFEA659/fulltext/pdf
- https://api.istex.fr/document/80B07FF241F395F13E2E495F1B074D027FB79238/fulltext/pdf
DOI: 10.1111/j.1365-2966.2010.16874.x
Affiliations:
- Allemagne, Australie, France, Hongrie
- Alsace (région administrative), Bade-Wurtemberg, District de Karlsruhe, Grand Est, Nouvelle-Galles du Sud
- Heidelberg, Strasbourg, Sydney
- Université de Strasbourg, Université de Sydney
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Szab</name><affiliation wicri:level="1"><country xml:lang="fr">Hongrie</country><wicri:regionArea>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest</wicri:regionArea><wicri:noRegion>H‐1525 Budapest</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">406</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="2732">2732</biblScope><biblScope unit="page" to="2742">2742</biblScope><biblScope unit="page-count">11</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-08-21">2010-08-21</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>Aaomega</term><term>Approximate axis</term><term>Calcium triplet lines</term><term>Central velocity dispersion</term><term>Cluster</term><term>Cluster centre</term><term>Cluster members</term><term>Cluster membership</term><term>Confusion effects</term><term>Current paper</term><term>Current study</term><term>Dark halo</term><term>Dark matter</term><term>Dispersion</term><term>Distant cluster member</term><term>Distant clusters</term><term>Distant member</term><term>Equivalent width</term><term>Flattening</term><term>Galactic</term><term>Galactic centre</term><term>Galactic disks</term><term>Galactic halos</term><term>Galaxy</term><term>Globular</term><term>Globular clusters</term><term>Gravitation</term><term>Gravity</term><term>Halo</term><term>Halo globular clusters</term><term>Hungarian academy</term><term>Individual velocity uncertainties</term><term>Internal kinematics</term><term>Intriguing possibility</term><term>Intriguing puzzle</term><term>Johnson pilachowski</term><term>Journal compilation</term><term>Kinematic measurements</term><term>Kinematics</term><term>Kruijssen mieske</term><term>Line strengths</term><term>Literature values</term><term>Lower panel</term><term>Luminosity</term><term>Mass estimate</term><term>Membership selections</term><term>Metallicity</term><term>Milky Way</term><term>Mnras</term><term>Newtonian</term><term>Newtonian dynamics</term><term>Newtonian gravity</term><term>Open circle</term><term>Outer regions</term><term>Plummer</term><term>Plummer model</term><term>Plummer models</term><term>Plummer scale radius</term><term>Previous studies</term><term>Radial velocities</term><term>Radial velocity</term><term>Radius</term><term>Relaxation time</term><term>Scale radius</term><term>Scarpa</term><term>Similar conclusions</term><term>Small radii</term><term>Solid points</term><term>Sollima nipoti</term><term>Spectroscopical observation</term><term>Square parsec</term><term>Star clusters</term><term>Stellar dynamics</term><term>Stellar velocities</term><term>Surface brightness data</term><term>Systemic velocities</term><term>Thick line</term><term>Thin lines</term><term>Tidal</term><term>Tidal effects</term><term>Tidal heating</term><term>Tidal radii</term><term>Tidal radius</term><term>Total luminosity</term><term>Total mass</term><term>Trgb</term><term>Velocity dispersion</term><term>Velocity dispersions</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Amas globulaire</term><term>Amas stellaire</term><term>Aplatissement</term><term>Cinématique</term><term>Dispersion vitesse</term><term>Disque galactique</term><term>Dynamique stellaire</term><term>Gravitation</term><term>Gravité</term><term>Halo galactique</term><term>Matière sombre</term><term>Métallicité</term><term>Observation spectroscopique</term><term>Voie lactée</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Aaomega</term><term>Approximate axis</term><term>Calcium triplet lines</term><term>Central velocity dispersion</term><term>Cluster</term><term>Cluster centre</term><term>Cluster members</term><term>Cluster membership</term><term>Confusion effects</term><term>Current paper</term><term>Current study</term><term>Dark halo</term><term>Dark matter</term><term>Dispersion</term><term>Distant cluster member</term><term>Distant clusters</term><term>Distant member</term><term>Equivalent width</term><term>Galactic</term><term>Galactic centre</term><term>Galaxy</term><term>Globular</term><term>Globular clusters</term><term>Halo</term><term>Halo globular clusters</term><term>Hungarian academy</term><term>Individual velocity uncertainties</term><term>Internal kinematics</term><term>Intriguing possibility</term><term>Intriguing puzzle</term><term>Johnson pilachowski</term><term>Journal compilation</term><term>Kinematic measurements</term><term>Kinematics</term><term>Kruijssen mieske</term><term>Line strengths</term><term>Literature values</term><term>Lower panel</term><term>Luminosity</term><term>Mass estimate</term><term>Membership selections</term><term>Metallicity</term><term>Mnras</term><term>Newtonian</term><term>Newtonian dynamics</term><term>Newtonian gravity</term><term>Open circle</term><term>Outer regions</term><term>Plummer</term><term>Plummer model</term><term>Plummer models</term><term>Plummer scale radius</term><term>Previous studies</term><term>Radial velocities</term><term>Radial velocity</term><term>Radius</term><term>Relaxation time</term><term>Scale radius</term><term>Scarpa</term><term>Similar conclusions</term><term>Small radii</term><term>Solid points</term><term>Sollima nipoti</term><term>Square parsec</term><term>Stellar velocities</term><term>Surface brightness data</term><term>Systemic velocities</term><term>Thick line</term><term>Thin lines</term><term>Tidal</term><term>Tidal effects</term><term>Tidal heating</term><term>Tidal radii</term><term>Tidal radius</term><term>Total luminosity</term><term>Total mass</term><term>Trgb</term><term>Velocity dispersion</term><term>Velocity dispersions</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Globular clusters (GCs) have proven to be essential to our understanding of many important astrophysical phenomena. Here, we analyse spectroscopic observations of 10 halo GCs to determine their dark matter (DM) content, their tidal heating by the Galactic disc and halo, describe their metallicities and the likelihood that Newtonian dynamics explains their kinematics. We analyse a large number of members in all clusters, allowing us to address all these issues together, and we have included NGC 288 and M30 to overlap with previous studies. We find that any flattening of the velocity dispersion profiles in the outer regions of our clusters can be explained by tidal heating. We also find that all our GCs have M/LV≲ 5, therefore, we infer the observed dynamics do not require DM, or a modification of gravity. We suggest that the lack of tidal heating signatures in distant clusters indicates the halo is not triaxial. The isothermal rotations of each cluster are measured, with M4 and NGC 288 exhibiting rotation at a level of 0.9 ± 0.1 km s−1 and 0.25 ± 0.15 km s−1, respectively. We also indirectly measure the tidal radius of NGC 6752, determining a more realistic figure for this cluster than current literature values. Lastly, an unresolved and intriguing puzzle is uncovered with regard to the cooling of the outer regions of all ten clusters.</div></front></TEI><affiliations><list><country><li>Allemagne</li><li>Australie</li><li>France</li><li>Hongrie</li></country><region><li>Alsace (région administrative)</li><li>Bade-Wurtemberg</li><li>District de Karlsruhe</li><li>Grand Est</li><li>Nouvelle-Galles du Sud</li></region><settlement><li>Heidelberg</li><li>Strasbourg</li><li>Sydney</li></settlement><orgName><li>Université de Strasbourg</li><li>Université de Sydney</li></orgName></list><tree><country name="Australie"><region name="Nouvelle-Galles du Sud"><name sortKey="Lane, Richard R" sort="Lane, Richard R" uniqKey="Lane R" first="Richard R." last="Lane">Richard R. Lane</name></region><name sortKey="Bedding, Timothy R" sort="Bedding, Timothy R" uniqKey="Bedding T" first="Timothy R." last="Bedding">Timothy R. Bedding</name><name sortKey="Kiss, Laszl L" sort="Kiss, Laszl L" uniqKey="Kiss L" first="Lászl L." last="Kiss">Lászl L. Kiss</name><name sortKey="Lane, Richard R" sort="Lane, Richard R" uniqKey="Lane R" first="Richard R." last="Lane">Richard R. Lane</name><name sortKey="Lewis, Geraint F" sort="Lewis, Geraint F" uniqKey="Lewis G" first="Geraint F." last="Lewis">Geraint F. Lewis</name></country><country name="Hongrie"><noRegion><name sortKey="Kiss, Laszl L" sort="Kiss, Laszl L" uniqKey="Kiss L" first="Lászl L." last="Kiss">Lászl L. Kiss</name></noRegion><name sortKey="Szab, Gyula M" sort="Szab, Gyula M" uniqKey="Szab G" first="Gyula M." last="Szab">Gyula M. Szab</name><name sortKey="Szekely, Peter" sort="Szekely, Peter" uniqKey="Szekely P" first="Péter" last="Székely">Péter Székely</name></country><country name="France"><region name="Grand Est"><name sortKey="Ibata, Rodrigo A" sort="Ibata, Rodrigo A" uniqKey="Ibata R" first="Rodrigo A." last="Ibata">Rodrigo A. Ibata</name></region><name sortKey="Siebert, Arnaud" sort="Siebert, Arnaud" uniqKey="Siebert A" first="Arnaud" last="Siebert">Arnaud Siebert</name></country><country name="Allemagne"><region name="Bade-Wurtemberg"><name sortKey="Balog, Zoltan" sort="Balog, Zoltan" uniqKey="Balog Z" first="Zoltán" last="Balog">Zoltán Balog</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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