Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating
Identifieur interne : 000671 ( Istex/Corpus ); précédent : 000670; suivant : 000672Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating
Auteurs : Richard R. Lane ; Lászl L. Kiss ; Geraint F. Lewis ; Rodrigo A. Ibata ; Arnaud Siebert ; Timothy R. Bedding ; Péter Székely ; Zoltán Balog ; Gyula M. SzabSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-08-21.
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, 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.
- 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:
DOI: 10.1111/j.1365-2966.2010.16874.x
Links to Exploration step
ISTEX:2290B85556B7D90BFEF26C395007389DEFFEA659Le document en format XML
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Lane</name><affiliation><mods:affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: rlane@physics.usyd.edu.au</mods:affiliation></affiliation></author><author><name sortKey="Kiss, Laszl L" sort="Kiss, Laszl L" uniqKey="Kiss L" first="Lászl L." last="Kiss">Lászl L. Kiss</name><affiliation><mods:affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</mods:affiliation></affiliation><affiliation><mods:affiliation>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary</mods:affiliation></affiliation></author><author><name sortKey="Lewis, Geraint F" sort="Lewis, Geraint F" uniqKey="Lewis G" first="Geraint F." last="Lewis">Geraint F. 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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>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><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><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>mnras</json:string><json:string>tidal</json:string><json:string>velocity dispersion</json:string><json:string>tidal radius</json:string><json:string>journal compilation</json:string><json:string>globular</json:string><json:string>kinematics</json:string><json:string>aaomega</json:string><json:string>trgb</json:string><json:string>velocity dispersions</json:string><json:string>outer regions</json:string><json:string>current paper</json:string><json:string>scarpa</json:string><json:string>metallicity</json:string><json:string>halo globular clusters</json:string><json:string>total mass</json:string><json:string>dispersion</json:string><json:string>luminosity</json:string><json:string>galactic</json:string><json:string>literature values</json:string><json:string>tidal heating</json:string><json:string>plummer</json:string><json:string>halo</json:string><json:string>central velocity dispersion</json:string><json:string>tidal radii</json:string><json:string>plummer model</json:string><json:string>plummer models</json:string><json:string>cluster</json:string><json:string>distant member</json:string><json:string>approximate axis</json:string><json:string>hungarian academy</json:string><json:string>surface brightness data</json:string><json:string>cluster centre</json:string><json:string>distant clusters</json:string><json:string>sollima nipoti</json:string><json:string>systemic velocities</json:string><json:string>newtonian gravity</json:string><json:string>galaxy</json:string><json:string>newtonian</json:string><json:string>radial velocity</json:string><json:string>radial velocities</json:string><json:string>internal kinematics</json:string><json:string>cluster members</json:string><json:string>lower panel</json:string><json:string>plummer scale radius</json:string><json:string>membership selections</json:string><json:string>distant cluster member</json:string><json:string>solid points</json:string><json:string>galactic centre</json:string><json:string>johnson pilachowski</json:string><json:string>cluster membership</json:string><json:string>globular clusters</json:string><json:string>intriguing puzzle</json:string><json:string>tidal effects</json:string><json:string>individual velocity uncertainties</json:string><json:string>stellar velocities</json:string><json:string>previous studies</json:string><json:string>newtonian dynamics</json:string><json:string>equivalent width</json:string><json:string>current study</json:string><json:string>kruijssen mieske</json:string><json:string>mass estimate</json:string><json:string>similar conclusions</json:string><json:string>scale radius</json:string><json:string>dark matter</json:string><json:string>thick line</json:string><json:string>thin lines</json:string><json:string>small radii</json:string><json:string>confusion effects</json:string><json:string>kinematic measurements</json:string><json:string>square parsec</json:string><json:string>intriguing possibility</json:string><json:string>line strengths</json:string><json:string>total luminosity</json:string><json:string>open circle</json:string><json:string>dark halo</json:string><json:string>relaxation time</json:string><json:string>calcium triplet lines</json:string><json:string>radius</json:string></teeft></keywords><author><json:item><name>Richard R. Lane</name><affiliations><json:string>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</json:string><json:string>E-mail: rlane@physics.usyd.edu.au</json:string></affiliations></json:item><json:item><name>László L. Kiss</name><affiliations><json:string>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</json:string><json:string>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary</json:string></affiliations></json:item><json:item><name>Geraint F. Lewis</name><affiliations><json:string>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Rodrigo A. Ibata</name><affiliations><json:string>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>Arnaud Siebert</name><affiliations><json:string>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France</json:string></affiliations></json:item><json:item><name>Timothy R. Bedding</name><affiliations><json:string>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia</json:string></affiliations></json:item><json:item><name>Péter Székely</name><affiliations><json:string>Department of Experimental Physics, University of Szeged, Szeged 6720, Hungary</json:string></affiliations></json:item><json:item><name>Zoltán Balog</name><affiliations><json:string>Max‐Planck Institut für Astronomie, Königstuhl 17, D‐69117 Heidelberg, Germany</json:string></affiliations></json:item><json:item><name>Gyula M. Szabó</name><affiliations><json:string>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>gravitation</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>stellar dynamics</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>globular clusters: individual</value></json:item></subject><articleId><json:string>MNR16874</json:string></articleId><arkIstex>ark:/67375/WNG-P3ZT53GK-3</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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.</abstract><qualityIndicators><refBibsNative>true</refBibsNative><abstractWordCount>220</abstractWordCount><abstractCharCount>1356</abstractCharCount><keywordCount>3</keywordCount><score>9.64</score><pdfWordCount>6776</pdfWordCount><pdfCharCount>35798</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>11</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize></qualityIndicators><title>Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating</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>406</volume><issue>4</issue><pages><first>2732</first><last>2742</last><total>11</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>1700</json:string><json:string>2006</json:string><json:string>2007</json:string><json:string>2010</json:string></date><geogName></geogName><orgName><json:string>Department of Experimental Physics, University of Szeged, Szeged</json:string><json:string>University of Sydney</json:string><json:string>Hungarian Academy of Sciences</json:string><json:string>Research Fellowship of the Hungarian Academy</json:string><json:string>Australia Observatory of the Hungarian Academy of Sciences, PO Box</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Sky Survey</json:string><json:string>Arnaud Siebert</json:string><json:string>Rodrigo A. 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(2007a)</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-P3ZT53GK-3</json:string></ark><categories><wos><json:string>1 - science</json:string><json:string>2 - astronomy & astrophysics</json:string></wos><scienceMetrix><json:string>1 - natural sciences</json:string><json:string>2 - physics & astronomy</json:string><json:string>3 - astronomy & astrophysics</json:string></scienceMetrix><scopus><json:string>1 - Physical Sciences</json:string><json:string>2 - Earth and Planetary Sciences</json:string><json:string>3 - Space and Planetary Science</json:string><json:string>1 - Physical Sciences</json:string><json:string>2 - Physics and Astronomy</json:string><json:string>3 - Astronomy and Astrophysics</json:string></scopus><inist><json:string>1 - sciences appliquees, technologies et medecines</json:string><json:string>2 - sciences biologiques et medicales</json:string><json:string>3 - sciences biologiques fondamentales et appliquees. psychologie</json:string><json:string>4 - vertebres: systeme nerveux et organes des sens</json:string></inist></categories><publicationDate>2010</publicationDate><copyrightDate>2010</copyrightDate><doi><json:string>10.1111/j.1365-2966.2010.16874.x</json:string></doi><id>2290B85556B7D90BFEF26C395007389DEFFEA659</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/2290B85556B7D90BFEF26C395007389DEFFEA659/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/2290B85556B7D90BFEF26C395007389DEFFEA659/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/2290B85556B7D90BFEF26C395007389DEFFEA659/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2010 The Authors. Journal compilation © 2010 RAS</licence></availability><date type="published" when="2010-08-21"></date></publicationStmt><notesStmt><note type="content-type" subtype="article" source="article" scheme="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</note><note type="publication-type" subtype="journal" scheme="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</note></notesStmt><sourceDesc><biblStruct type="article"><analytic><title level="a" type="main">Halo globular clusters observed with AAOmega: dark matter content, metallicity and tidal heating</title><title level="a" type="short">Halo globular clusters</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Richard R.</forename><surname>Lane</surname></persName><affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation><affiliation>E‐mail: rlane@physics.usyd.edu.au</affiliation></author><author xml:id="author-0001"><persName><forename type="first">László L.</forename><surname>Kiss</surname></persName><affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation><affiliation>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary<address><country key="HU"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">Geraint F.</forename><surname>Lewis</surname></persName><affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0003"><persName><forename type="first">Rodrigo A.</forename><surname>Ibata</surname></persName><affiliation>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">Arnaud</forename><surname>Siebert</surname></persName><affiliation>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">Timothy R.</forename><surname>Bedding</surname></persName><affiliation>Sydney Institute for Astronomy, School of Physics, A28, The University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">Péter</forename><surname>Székely</surname></persName><affiliation>Department of Experimental Physics, University of Szeged, Szeged 6720, Hungary<address><country key="HU"></country></address></affiliation></author><author xml:id="author-0007"><persName><forename type="first">Zoltán</forename><surname>Balog</surname></persName><affiliation>Max‐Planck Institut für Astronomie, Königstuhl 17, D‐69117 Heidelberg, Germany<address><country key="DE"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">Gyula M.</forename><surname>Szabó</surname></persName><affiliation>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary<address><country key="HU"></country></address></affiliation></author><idno type="istex">2290B85556B7D90BFEF26C395007389DEFFEA659</idno><idno type="ark">ark:/67375/WNG-P3ZT53GK-3</idno><idno type="DOI">10.1111/j.1365-2966.2010.16874.x</idno><idno type="unit">MNR16874</idno><idno type="toTypesetVersion">file:MNR.MNR16874.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.2010.406.issue-4</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</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"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>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/L<emph><span><hi rend="subscript">V</hi>≲ 5</span></emph>, 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 <emph><span>0.9 ± 0.1 km s<hi rend="superscript">−1</hi></span></emph> and <emph><span>0.25 ± 0.15 km s<hi rend="superscript">−1</hi></span></emph>, 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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">gravitation</term><term xml:id="k2">stellar dynamics</term><term xml:id="k3">globular clusters: individual</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/2290B85556B7D90BFEF26C395007389DEFFEA659/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="08104"><doi origin="wiley">10.1111/mnr.2010.406.issue-4</doi><numberingGroup><numbering type="journalVolume" number="406">406</numbering><numbering type="journalIssue" number="4">4</numbering></numberingGroup><coverDate startDate="2010-08-21">August 2010</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="48" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2010.16874.x</doi><idGroup><id type="unit" value="MNR16874"></id></idGroup><countGroup><count type="pageTotal" number="11"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2010 The Authors. 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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/L<span type="mathematics"><sub>V</sub>≲ 5</span>, 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 <span type="mathematics">0.9 ± 0.1 km s<sup>−1</sup></span> and <span type="mathematics">0.25 ± 0.15 km s<sup>−1</sup></span>, respectively. We also indirectly measure the tidal radius of NGC 6752, determining a more realistic figure for this cluster than current literature values. 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Received 2010 April 13; in original form 2009 November 18</edition><copyrightDate encoding="w3cdtf">2010</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">8</extent><extent unit="tables">1</extent><extent unit="formulas">151</extent><extent unit="references">62</extent><extent unit="linksCrossRef">129</extent></physicalDescription><abstract 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.</abstract><subject lang="en"><genre>keywords</genre><topic>gravitation</topic><topic>stellar dynamics</topic><topic>globular clusters: individual</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>2010</date><detail type="volume"><caption>vol.</caption><number>406</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>2732</start><end>2742</end><total>11</total></extent></part></relatedItem><identifier type="istex">2290B85556B7D90BFEF26C395007389DEFFEA659</identifier><identifier type="ark">ark:/67375/WNG-P3ZT53GK-3</identifier><identifier type="DOI">10.1111/j.1365-2966.2010.16874.x</identifier><identifier type="ArticleID">MNR16874</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2010 The Authors. 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