Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55
Identifieur interne : 000481 ( Istex/Corpus ); précédent : 000480; suivant : 000482Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55
Auteurs : Richard R. Lane ; Lászl L. Kiss ; Geraint F. Lewis ; Rodrigo A. Ibata ; Arnaud Siebert ; Timothy R. Bedding ; Péter SzékelySource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-02-01.
English descriptors
- KwdEn :
- 2mass cmds, Accurate metallicity calibration, Approximate axis, Arcsec, Arcsec radius, Bica dutra, Calcium triplet lines, Central velocity dispersion, Central velocity dispersions, Cluster, Cluster members, Cluster membership, Cole, Complete sample, Consecutive nights, Core mass, Current study, Current understanding, Current work, Dark matter, Dispersion, Dwarf galaxies, Edge stars, Equivalent width, Evaporation, Exhibits rotation, Galaxy, Gebhardt, Gebhardt fischer, Giant branch, Globular, Globular clusters, Gravitational interaction, Gravitational theories, Greater numbers, Horizontal branch, Hungarian academy, Hydrogen paschen lines, Isothermal distribution, Journal compilation, Kely, Kron, Kruijssen mieske, Large points, Large radii, Large uncertainty, Literature values, Marconi, Mass estimates, Metallicity, Metallicity analysis, Metallicity calibration, Meylan, Meziane colin, Mnras, Newtonian, Newtonian gravity, Outer regions, Plummer, Plummer model, Plummer models, Pryor meylan, Radial velocities, Radial velocity, Rotational axis, Scale radii, Scale radius, Scarpa, Small magellanic cloud, Straight lines, Subsequent paper, Surface brightness, Systemic velocity, Testing newtonian gravity, Tidal, Tidal radius, Tidal tails, Total mass, Total masses, Trgb, Trgb values, Triplet, Velocity dispersion, Velocity dispersion analysis, Velocity dispersions, Warren cole, Wavelength calibration.
- Teeft :
- 2mass cmds, Accurate metallicity calibration, Approximate axis, Arcsec, Arcsec radius, Bica dutra, Calcium triplet lines, Central velocity dispersion, Central velocity dispersions, Cluster, Cluster members, Cluster membership, Cole, Complete sample, Consecutive nights, Core mass, Current study, Current understanding, Current work, Dark matter, Dispersion, Dwarf galaxies, Edge stars, Equivalent width, Evaporation, Exhibits rotation, Galaxy, Gebhardt, Gebhardt fischer, Giant branch, Globular, Globular clusters, Gravitational interaction, Gravitational theories, Greater numbers, Horizontal branch, Hungarian academy, Hydrogen paschen lines, Isothermal distribution, Journal compilation, Kely, Kron, Kruijssen mieske, Large points, Large radii, Large uncertainty, Literature values, Marconi, Mass estimates, Metallicity, Metallicity analysis, Metallicity calibration, Meylan, Meziane colin, Mnras, Newtonian, Newtonian gravity, Outer regions, Plummer, Plummer model, Plummer models, Pryor meylan, Radial velocities, Radial velocity, Rotational axis, Scale radii, Scale radius, Scarpa, Small magellanic cloud, Straight lines, Subsequent paper, Surface brightness, Systemic velocity, Testing newtonian gravity, Tidal, Tidal radius, Tidal tails, Total mass, Total masses, Trgb, Trgb values, Triplet, Velocity dispersion, Velocity dispersion analysis, Velocity dispersions, Warren cole, Wavelength calibration.
Abstract
Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and K‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked increase in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.
Url:
DOI: 10.1111/j.1365-2966.2009.15827.x
Links to Exploration step
ISTEX:1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2Le document en format XML
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width</term><term>Evaporation</term><term>Exhibits rotation</term><term>Galaxy</term><term>Gebhardt</term><term>Gebhardt fischer</term><term>Giant branch</term><term>Globular</term><term>Globular clusters</term><term>Gravitational interaction</term><term>Gravitational theories</term><term>Greater numbers</term><term>Horizontal branch</term><term>Hungarian academy</term><term>Hydrogen paschen lines</term><term>Isothermal distribution</term><term>Journal compilation</term><term>Kely</term><term>Kron</term><term>Kruijssen mieske</term><term>Large points</term><term>Large radii</term><term>Large uncertainty</term><term>Literature values</term><term>Marconi</term><term>Mass estimates</term><term>Metallicity</term><term>Metallicity analysis</term><term>Metallicity calibration</term><term>Meylan</term><term>Meziane colin</term><term>Mnras</term><term>Newtonian</term><term>Newtonian gravity</term><term>Outer regions</term><term>Plummer</term><term>Plummer model</term><term>Plummer models</term><term>Pryor meylan</term><term>Radial velocities</term><term>Radial velocity</term><term>Rotational axis</term><term>Scale radii</term><term>Scale radius</term><term>Scarpa</term><term>Small magellanic cloud</term><term>Straight lines</term><term>Subsequent paper</term><term>Surface brightness</term><term>Systemic velocity</term><term>Testing newtonian gravity</term><term>Tidal</term><term>Tidal radius</term><term>Tidal tails</term><term>Total mass</term><term>Total masses</term><term>Trgb</term><term>Trgb values</term><term>Triplet</term><term>Velocity dispersion</term><term>Velocity dispersion analysis</term><term>Velocity dispersions</term><term>Warren cole</term><term>Wavelength calibration</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>2mass cmds</term><term>Accurate metallicity calibration</term><term>Approximate axis</term><term>Arcsec</term><term>Arcsec radius</term><term>Bica dutra</term><term>Calcium triplet lines</term><term>Central velocity dispersion</term><term>Central velocity dispersions</term><term>Cluster</term><term>Cluster members</term><term>Cluster membership</term><term>Cole</term><term>Complete sample</term><term>Consecutive nights</term><term>Core mass</term><term>Current study</term><term>Current understanding</term><term>Current work</term><term>Dark matter</term><term>Dispersion</term><term>Dwarf galaxies</term><term>Edge stars</term><term>Equivalent width</term><term>Evaporation</term><term>Exhibits rotation</term><term>Galaxy</term><term>Gebhardt</term><term>Gebhardt fischer</term><term>Giant branch</term><term>Globular</term><term>Globular clusters</term><term>Gravitational interaction</term><term>Gravitational theories</term><term>Greater numbers</term><term>Horizontal branch</term><term>Hungarian academy</term><term>Hydrogen paschen lines</term><term>Isothermal distribution</term><term>Journal compilation</term><term>Kely</term><term>Kron</term><term>Kruijssen mieske</term><term>Large points</term><term>Large radii</term><term>Large uncertainty</term><term>Literature values</term><term>Marconi</term><term>Mass estimates</term><term>Metallicity</term><term>Metallicity analysis</term><term>Metallicity calibration</term><term>Meylan</term><term>Meziane colin</term><term>Mnras</term><term>Newtonian</term><term>Newtonian gravity</term><term>Outer regions</term><term>Plummer</term><term>Plummer model</term><term>Plummer models</term><term>Pryor meylan</term><term>Radial velocities</term><term>Radial velocity</term><term>Rotational axis</term><term>Scale radii</term><term>Scale radius</term><term>Scarpa</term><term>Small magellanic cloud</term><term>Straight lines</term><term>Subsequent paper</term><term>Surface brightness</term><term>Systemic velocity</term><term>Testing newtonian gravity</term><term>Tidal</term><term>Tidal radius</term><term>Tidal tails</term><term>Total mass</term><term>Total masses</term><term>Trgb</term><term>Trgb values</term><term>Triplet</term><term>Velocity dispersion</term><term>Velocity dispersion analysis</term><term>Velocity dispersions</term><term>Warren cole</term><term>Wavelength calibration</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and K‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked increase in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>velocity dispersion</json:string><json:string>mnras</json:string><json:string>kron</json:string><json:string>trgb</json:string><json:string>metallicity</json:string><json:string>meylan</json:string><json:string>arcsec</json:string><json:string>journal compilation</json:string><json:string>dispersion</json:string><json:string>globular</json:string><json:string>marconi</json:string><json:string>scarpa</json:string><json:string>kely</json:string><json:string>gebhardt</json:string><json:string>velocity dispersions</json:string><json:string>tidal</json:string><json:string>calcium triplet lines</json:string><json:string>newtonian gravity</json:string><json:string>triplet</json:string><json:string>warren cole</json:string><json:string>radial velocity</json:string><json:string>testing newtonian gravity</json:string><json:string>tidal radius</json:string><json:string>equivalent width</json:string><json:string>large points</json:string><json:string>systemic velocity</json:string><json:string>plummer model</json:string><json:string>cluster members</json:string><json:string>tidal tails</json:string><json:string>large radii</json:string><json:string>outer regions</json:string><json:string>core mass</json:string><json:string>globular clusters</json:string><json:string>newtonian</json:string><json:string>giant branch</json:string><json:string>gebhardt fischer</json:string><json:string>dwarf galaxies</json:string><json:string>central velocity dispersions</json:string><json:string>total masses</json:string><json:string>total mass</json:string><json:string>literature values</json:string><json:string>gravitational interaction</json:string><json:string>scale radius</json:string><json:string>cluster</json:string><json:string>cole</json:string><json:string>plummer</json:string><json:string>evaporation</json:string><json:string>galaxy</json:string><json:string>complete sample</json:string><json:string>2mass cmds</json:string><json:string>metallicity analysis</json:string><json:string>consecutive nights</json:string><json:string>isothermal distribution</json:string><json:string>straight lines</json:string><json:string>metallicity calibration</json:string><json:string>large uncertainty</json:string><json:string>exhibits rotation</json:string><json:string>hydrogen paschen lines</json:string><json:string>accurate metallicity calibration</json:string><json:string>current study</json:string><json:string>radial velocities</json:string><json:string>velocity dispersion analysis</json:string><json:string>gravitational theories</json:string><json:string>rotational axis</json:string><json:string>approximate axis</json:string><json:string>edge stars</json:string><json:string>wavelength calibration</json:string><json:string>central velocity dispersion</json:string><json:string>cluster membership</json:string><json:string>dark matter</json:string><json:string>arcsec radius</json:string><json:string>small magellanic cloud</json:string><json:string>scale radii</json:string><json:string>mass estimates</json:string><json:string>pryor meylan</json:string><json:string>meziane colin</json:string><json:string>kruijssen mieske</json:string><json:string>plummer models</json:string><json:string>greater numbers</json:string><json:string>horizontal branch</json:string><json:string>bica dutra</json:string><json:string>subsequent paper</json:string><json:string>current understanding</json:string><json:string>surface brightness</json:string><json:string>hungarian academy</json:string><json:string>trgb values</json:string><json:string>current work</json:string></teeft></keywords><author><json:item><name>Richard R. Lane</name><affiliations><json:string>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</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, A29, University of Sydney, NSW, Australia 2006</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, A29, University of Sydney, NSW, Australia 2006</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, A29, University of Sydney, NSW, Australia 2006</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></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>MNR15827</json:string></articleId><arkIstex>ark:/67375/WNG-0Q7GK4XT-L</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and K‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked increase in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.</abstract><qualityIndicators><score>10</score><pdfWordCount>6829</pdfWordCount><pdfCharCount>36497</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>10</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>250</abstractWordCount><abstractCharCount>1607</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55</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>401</volume><issue>4</issue><pages><first>2521</first><last>2530</last><total>10</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2009</json:string><json:string>2010</json:string><json:string>2241</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></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. Ibata</json:string><json:string>L. Kiss</json:string><json:string>Richard R. Lane</json:string><json:string>F. Lewis</json:string><json:string>Roberto Gilmozzi</json:string><json:string>Observatory</json:string><json:string>By</json:string><json:string>Tuc</json:string></persName><placeName><json:string>Monaco</json:string><json:string>Australia</json:string><json:string>Metallicity</json:string><json:string>Strasbourg</json:string><json:string>Wales</json:string><json:string>Manchester</json:string><json:string>San Francisco</json:string><json:string>Velocity</json:string><json:string>France</json:string><json:string>Hungary</json:string><json:string>Budapest</json:string></placeName><ref_url><json:string>http://pos.sissa.it</json:string></ref_url><ref_bibl><json:string>Lane et al. 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(2007)</json:string><json:string>Navarro, Frenk & White 1997</json:string><json:string>Meylan & Mayor 1986</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-0Q7GK4XT-L</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></inist></categories><publicationDate>2010</publicationDate><copyrightDate>2010</copyrightDate><doi><json:string>10.1111/j.1365-2966.2009.15827.x</json:string></doi><id>1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><availability><licence>© 2009 The Authors. Journal compilation © 2009 RAS</licence></availability><date type="published" when="2010-02-01"></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">Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55</title><title level="a" type="short">Testing Newtonian gravity with 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, A29, University of Sydney, NSW, Australia 2006<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, A29, University of Sydney, NSW, Australia 2006<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, A29, University of Sydney, NSW, Australia 2006<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, A29, University of Sydney, NSW, Australia 2006<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><idno type="istex">1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2</idno><idno type="ark">ark:/67375/WNG-0Q7GK4XT-L</idno><idno type="DOI">10.1111/j.1365-2966.2009.15827.x</idno><idno type="unit">MNR15827</idno><idno type="toTypesetVersion">file:MNR.MNR15827.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.2010.401.issue-4</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">401</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="2521">2521</biblScope><biblScope unit="page" to="2530">2530</biblScope><biblScope unit="page-count">10</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-02-01"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and <hi rend="italic">K</hi>‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked <hi rend="italic">increase</hi> in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.</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/1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2/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="02104"><doi origin="wiley">10.1111/mnr.2010.401.issue-4</doi><numberingGroup><numbering type="journalVolume" number="401">401</numbering><numbering type="journalIssue" number="4">4</numbering></numberingGroup><coverDate startDate="2010-02-01">February 2010</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="30" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.15827.x</doi><idGroup><id type="unit" value="MNR15827"></id></idGroup><countGroup><count type="pageTotal" number="10"></count></countGroup><titleGroup><title type="tocHeading1">PAPERS</title></titleGroup><copyright>© 2009 The Authors. 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Lane et al.</i></title><title type="short"><i>Testing Newtonian gravity with globular clusters</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Richard R.</givenNames><familyName>Lane</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1 #a2"><personName><givenNames>László L.</givenNames><familyName>Kiss</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a1"><personName><givenNames>Geraint F.</givenNames><familyName>Lewis</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a3"><personName><givenNames>Rodrigo A.</givenNames><familyName>Ibata</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a3"><personName><givenNames>Arnaud</givenNames><familyName>Siebert</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a1"><personName><givenNames>Timothy R.</givenNames><familyName>Bedding</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a4"><personName><givenNames>Péter</givenNames><familyName>Székely</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="AU"><unparsedAffiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="HU"><unparsedAffiliation>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="HU"><unparsedAffiliation>Department of Experimental Physics, University of Szeged, Szeged 6720, Hungary</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">gravitation</keyword><keyword xml:id="k2">stellar dynamics</keyword><keyword xml:id="k3">globular clusters: individual</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and <i>K</i>‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked <i>increase</i> in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Testing Newtonian gravity with globular clusters</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Testing Newtonian gravity with AAOmega: mass‐to‐light profiles and metallicity calibrations from 47 Tuc and M55</title></titleInfo><name type="personal"><namePart type="given">Richard R.</namePart><namePart type="family">Lane</namePart><affiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</affiliation><affiliation>E-mail: rlane@physics.usyd.edu.au</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">László L.</namePart><namePart type="family">Kiss</namePart><affiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</affiliation><affiliation>Konkoly Observatory of the Hungarian Academy of Sciences, PO Box 67, H‐1525 Budapest, Hungary</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Geraint F.</namePart><namePart type="family">Lewis</namePart><affiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Rodrigo A.</namePart><namePart type="family">Ibata</namePart><affiliation>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Arnaud</namePart><namePart type="family">Siebert</namePart><affiliation>Observatoire Astronomique, Universite de Strasbourg, CNRS, 67000 Strasbourg, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Timothy R.</namePart><namePart type="family">Bedding</namePart><affiliation>Sydney Institute for Astronomy, School of Physics, A29, University of Sydney, NSW, Australia 2006</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Péter</namePart><namePart type="family">Székely</namePart><affiliation>Department of Experimental Physics, University of Szeged, Szeged 6720, Hungary</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">2010-02-01</dateIssued><edition>Accepted 2009 October 4. Received 2009 October 2; in original form 2009 September 1</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">12</extent><extent unit="tables">4</extent><extent unit="formulas">104</extent><extent unit="references">61</extent><extent unit="linksCrossRef">153</extent></physicalDescription><abstract lang="en">Globular clusters (GCs) are an important test bed for Newtonian gravity in the weak‐acceleration regime, which is vital to our understanding of the nature of the gravitational interaction. Recent claims have been made that the velocity dispersion profiles of GCs flatten out at large radii, despite an apparent paucity of dark matter (DM) in such objects, indicating the need for a modification of gravitational theories. We continue our investigation of this claim, with the largest spectral samples ever obtained of 47 Tucanae (47 Tuc) and M55. Furthermore, this large sample allows for an accurate metallicity calibration based on the equivalent widths of the calcium triplet lines and K‐band magnitude of the Tip of the Red Giant Branch. Assuming an isothermal distribution, the rotations of each cluster are also measured with both clusters exhibiting clear rotation signatures. The global velocity dispersions of NGC 121 and Kron 3, two GCs in the Small Magellanic Cloud, are also calculated. By applying a simple dynamical model to the velocity dispersion profiles of 47 Tuc and M55, we calculate their mass‐to‐light profiles, total masses and central velocity dispersions. We find no statistically significant flattening of the velocity dispersion at large radii for M55, and a marked increase in the profile of 47 Tuc for radii greater than approximately half the tidal radius. We interpret this increase as an evaporation signature, indicating that 47 Tuc is undergoing, or has undergone, core‐collapse, but find no requirement for DM or a modification of gravitational theories in either cluster.</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>401</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>2521</start><end>2530</end><total>10</total></extent></part></relatedItem><identifier type="istex">1925AC5E2FC17CB54BB28F656D4FDCE3547EC9E2</identifier><identifier type="ark">ark:/67375/WNG-0Q7GK4XT-L</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.15827.x</identifier><identifier type="ArticleID">MNR15827</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2009 The Authors. 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