LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at z= 0.2
Identifieur interne : 000943 ( Main/Corpus ); précédent : 000942; suivant : 000944LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at z= 0.2
Auteurs : Johan Richard ; Graham P. Smith ; Jean-Paul Kneib ; Richard S. Ellis ; A. J. R. Sanderson ; L. Pei ; T. A. Targett ; D. J. Sand ; A. M. Swinbank ; H. Dannerbauer ; P. Mazzotta ; M. Limousin ; E. Egami ; E. Jullo ; V. Hamilton-Morris ; S. M. MoranSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2010-05-01.
English descriptors
Abstract
We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution Hubble Space Telescope imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R≤ 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of 〈log10θE(z= 2)〉= 1.16 ± 0.28; (ii) we detect an X‐ray/lensing mass discrepancy of 〈MSL/MX〉= 1.3 at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm.
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DOI: 10.1111/j.1365-2966.2009.16274.x
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E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: johan.richard@durham.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Smith, Graham P" sort="Smith, Graham P" uniqKey="Smith G" first="Graham P." last="Smith">Graham P. Smith</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</mods:affiliation></affiliation></author><author><name sortKey="Kneib, Jean Aul" sort="Kneib, Jean Aul" uniqKey="Kneib J" first="Jean-Paul" last="Kneib">Jean-Paul Kneib</name><affiliation><mods:affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</mods:affiliation></affiliation></author><author><name sortKey="Ellis, Richard S" sort="Ellis, Richard S" uniqKey="Ellis R" first="Richard S." last="Ellis">Richard S. Ellis</name><affiliation><mods:affiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="Sanderson, A J R" sort="Sanderson, A J R" uniqKey="Sanderson A" first="A. J. R." last="Sanderson">A. J. R. 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Sand</name><affiliation><mods:affiliation>Harvard‐Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA02138, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: johan.richard@durham.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Swinbank, A M" sort="Swinbank, A M" uniqKey="Swinbank A" first="A. M." last="Swinbank">A. M. Swinbank</name><affiliation><mods:affiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</mods:affiliation></affiliation></author><author><name sortKey="Dannerbauer, H" sort="Dannerbauer, H" uniqKey="Dannerbauer H" first="H." last="Dannerbauer">H. Dannerbauer</name><affiliation><mods:affiliation>Max‐Planck‐Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</mods:affiliation></affiliation></author><author><name sortKey="Mazzotta, P" sort="Mazzotta, P" uniqKey="Mazzotta P" first="P." last="Mazzotta">P. Mazzotta</name><affiliation><mods:affiliation>Department of Physics, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy</mods:affiliation></affiliation></author><author><name sortKey="Limousin, M" sort="Limousin, M" uniqKey="Limousin M" first="M." last="Limousin">M. Limousin</name><affiliation><mods:affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</mods:affiliation></affiliation><affiliation><mods:affiliation>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark</mods:affiliation></affiliation></author><author><name sortKey="Egami, E" sort="Egami, E" uniqKey="Egami E" first="E." last="Egami">E. Egami</name><affiliation><mods:affiliation>Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</mods:affiliation></affiliation></author><author><name sortKey="Jullo, E" sort="Jullo, E" uniqKey="Jullo E" first="E." last="Jullo">E. Jullo</name><affiliation><mods:affiliation>Jet Propulsion Laboratory, Caltech, MS 169‐327, Oak Grove Dr, Pasadena, CA 91109, USA</mods:affiliation></affiliation></author><author><name sortKey="Hamilton Orris, V" sort="Hamilton Orris, V" uniqKey="Hamilton Orris V" first="V." last="Hamilton-Morris">V. Hamilton-Morris</name><affiliation><mods:affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</mods:affiliation></affiliation></author><author><name sortKey="Moran, S M" sort="Moran, S M" uniqKey="Moran S" first="S. M." last="Moran">S. M. Moran</name><affiliation><mods:affiliation>Johns Hopkins Deptartment of Physics and Astronomy, Baltimore, MD 21218, USA</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="ISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-05-01">2010-05-01</date><biblScope unit="volume">404</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="325">325</biblScope><biblScope unit="page" to="349">349</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">E51B0F09C42EBD306FDE252829961EABF8890EA5</idno><idno type="DOI">10.1111/j.1365-2966.2009.16274.x</idno><idno type="ArticleID">MNR16274</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>galaxies: clusters: general</term><term>gravitational lensing</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution Hubble Space Telescope imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R≤ 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of 〈log10θE(z= 2)〉= 1.16 ± 0.28; (ii) we detect an X‐ray/lensing mass discrepancy of 〈MSL/MX〉= 1.3 at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>Johan Richard</name><affiliations><json:string>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</json:string><json:string>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</json:string><json:string>E-mail: johan.richard@durham.ac.uk</json:string></affiliations></json:item><json:item><name>Graham P. Smith</name><affiliations><json:string>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</json:string></affiliations></json:item><json:item><name>Jean‐Paul Kneib</name><affiliations><json:string>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</json:string></affiliations></json:item><json:item><name>Richard S. Ellis</name><affiliations><json:string>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>A. J. R. Sanderson</name><affiliations><json:string>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</json:string></affiliations></json:item><json:item><name>L. Pei</name><affiliations><json:string>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>T. A. Targett</name><affiliations><json:string>University of British Columbia, Department of Physics and Astronomy, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</json:string></affiliations></json:item><json:item><name>D. J. Sand</name><affiliations><json:string>Harvard‐Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA02138, USA</json:string><json:string>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</json:string><json:string>E-mail: johan.richard@durham.ac.uk</json:string></affiliations></json:item><json:item><name>A. M. Swinbank</name><affiliations><json:string>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</json:string></affiliations></json:item><json:item><name>H. Dannerbauer</name><affiliations><json:string>Max‐Planck‐Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</json:string></affiliations></json:item><json:item><name>P. Mazzotta</name><affiliations><json:string>Department of Physics, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy</json:string></affiliations></json:item><json:item><name>M. Limousin</name><affiliations><json:string>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</json:string><json:string>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark</json:string></affiliations></json:item><json:item><name>E. Egami</name><affiliations><json:string>Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</json:string></affiliations></json:item><json:item><name>E. Jullo</name><affiliations><json:string>Jet Propulsion Laboratory, Caltech, MS 169‐327, Oak Grove Dr, Pasadena, CA 91109, USA</json:string></affiliations></json:item><json:item><name>V. Hamilton‐Morris</name><affiliations><json:string>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</json:string></affiliations></json:item><json:item><name>S. M. Moran</name><affiliations><json:string>Johns Hopkins Deptartment of Physics and Astronomy, Baltimore, MD 21218, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>gravitational lensing</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>galaxies: clusters: general</value></json:item></subject><articleId><json:string>MNR16274</json:string></articleId><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><abstract>We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution Hubble Space Telescope imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R≤ 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of 〈log10θE(z= 2)〉= 1.16 ± 0.28; (ii) we detect an X‐ray/lensing mass discrepancy of 〈MSL/MX〉= 1.3 at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. 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Journal compilation © 2010 RAS</p></availability><date>2010</date></publicationStmt><sourceDesc><biblStruct type="inbook"><analytic><title level="a" type="main" xml:lang="en">LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at z= 0.2</title><author xml:id="author-1"><persName><forename type="first">Johan</forename><surname>Richard</surname></persName><email>johan.richard@durham.ac.uk</email><affiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation><affiliation>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</affiliation></author><author xml:id="author-2"><persName><forename type="first">Graham P.</forename><surname>Smith</surname></persName><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation></author><author xml:id="author-3"><persName><forename type="first">Jean‐Paul</forename><surname>Kneib</surname></persName><affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</affiliation></author><author xml:id="author-4"><persName><forename type="first">Richard S.</forename><surname>Ellis</surname></persName><affiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</affiliation></author><author xml:id="author-5"><persName><forename type="first">A. J. R.</forename><surname>Sanderson</surname></persName><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation></author><author xml:id="author-6"><persName><forename type="first">L.</forename><surname>Pei</surname></persName><affiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</affiliation></author><author xml:id="author-7"><persName><forename type="first">T. A.</forename><surname>Targett</surname></persName><affiliation>University of British Columbia, Department of Physics and Astronomy, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</affiliation></author><author xml:id="author-8"><persName><forename type="first">D. J.</forename><surname>Sand</surname></persName><email>johan.richard@durham.ac.uk</email><affiliation>Harvard‐Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA02138, USA</affiliation><affiliation>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</affiliation></author><author xml:id="author-9"><persName><forename type="first">A. M.</forename><surname>Swinbank</surname></persName><affiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation></author><author xml:id="author-10"><persName><forename type="first">H.</forename><surname>Dannerbauer</surname></persName><affiliation>Max‐Planck‐Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</affiliation></author><author xml:id="author-11"><persName><forename type="first">P.</forename><surname>Mazzotta</surname></persName><affiliation>Department of Physics, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy</affiliation></author><author xml:id="author-12"><persName><forename type="first">M.</forename><surname>Limousin</surname></persName><affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</affiliation><affiliation>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark</affiliation></author><author xml:id="author-13"><persName><forename type="first">E.</forename><surname>Egami</surname></persName><affiliation>Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</affiliation></author><author xml:id="author-14"><persName><forename type="first">E.</forename><surname>Jullo</surname></persName><affiliation>Jet Propulsion Laboratory, Caltech, MS 169‐327, Oak Grove Dr, Pasadena, CA 91109, USA</affiliation></author><author xml:id="author-15"><persName><forename type="first">V.</forename><surname>Hamilton‐Morris</surname></persName><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation></author><author xml:id="author-16"><persName><forename type="first">S. M.</forename><surname>Moran</surname></persName><affiliation>Johns Hopkins Deptartment of Physics and Astronomy, Baltimore, MD 21218, USA</affiliation></author></analytic><monogr><title level="j">Monthly Notices of the Royal Astronomical Society</title><idno type="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="DOI">10.1111/(ISSN)1365-2966</idno><imprint><publisher>Blackwell Publishing Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2010-05-01"></date><biblScope unit="volume">404</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="325">325</biblScope><biblScope unit="page" to="349">349</biblScope></imprint></monogr><idno type="istex">E51B0F09C42EBD306FDE252829961EABF8890EA5</idno><idno type="DOI">10.1111/j.1365-2966.2009.16274.x</idno><idno type="ArticleID">MNR16274</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2010</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution Hubble Space Telescope imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R≤ 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of 〈log10θE(z= 2)〉= 1.16 ± 0.28; (ii) we detect an X‐ray/lensing mass discrepancy of 〈MSL/MX〉= 1.3 at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>keywords</head><item><term>gravitational lensing</term></item><item><term>galaxies: clusters: general</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2010-05-01">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/E51B0F09C42EBD306FDE252829961EABF8890EA5/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="05101"><doi origin="wiley">10.1111/mnr.2010.404.issue-1</doi><numberingGroup><numbering type="journalVolume" number="404">404</numbering><numbering type="journalIssue" number="1">1</numbering></numberingGroup><coverDate startDate="2010-05-01">May 2010</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="30" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2009.16274.x</doi><idGroup><id type="unit" value="MNR16274"></id></idGroup><countGroup><count type="pageTotal" number="25"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2010 The Authors. Journal compilation © 2010 RAS</copyright><eventGroup><event type="firstOnline" date="2010-03-08"></event><event type="publishedOnlineFinalForm" date="2010-04-21"></event><event type="publishedOnlineAcceptedOrEarlyUnpaginated" date="2010-03-08"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.4 mode:FullText source:FullText result:FullText" date="2010-12-14"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-02"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="325">325</numbering><numbering type="pageLast" number="349">349</numbering></numberingGroup><correspondenceTo><lineatedText><line> Marie‐Curie fellow.</line><line> E‐mail: <email>johan.richard@durham.ac.uk</email></line><line> Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</line></lineatedText></correspondenceTo><objectNameGroup><objectName elementName="appendix">Appendices</objectName></objectNameGroup><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR16274.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2010 January 4. Received 2009 December 17; in original form 2009 August 12</unparsedEditorialHistory><countGroup><count type="figureTotal" number="14"></count><count type="tableTotal" number="9"></count><count type="formulaTotal" number="464"></count><count type="referenceTotal" number="91"></count><count type="linksCrossRef" number="253"></count></countGroup><titleGroup><title type="main">LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at <i>z</i>= 0.2</title><title type="shortAuthors"><i>J. Richard et al.</i></title><title type="short"><i>LoCuSS: strong‐lensing clusters</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Johan</givenNames><familyName>Richard</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2"><personName><givenNames>Graham P.</givenNames><familyName>Smith</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a3"><personName><givenNames>Jean‐Paul</givenNames><familyName>Kneib</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a4"><personName><givenNames>Richard S.</givenNames><familyName>Ellis</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a2"><personName><givenNames>A. J. 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M.</givenNames><familyName>Swinbank</familyName></personName></creator><creator creatorRole="author" xml:id="cr10" affiliationRef="#a7"><personName><givenNames>H.</givenNames><familyName>Dannerbauer</familyName></personName></creator><creator creatorRole="author" xml:id="cr11" affiliationRef="#a8"><personName><givenNames>P.</givenNames><familyName>Mazzotta</familyName></personName></creator><creator creatorRole="author" xml:id="cr12" affiliationRef="#a3 #a9"><personName><givenNames>M.</givenNames><familyName>Limousin</familyName></personName></creator><creator creatorRole="author" xml:id="cr13" affiliationRef="#a10"><personName><givenNames>E.</givenNames><familyName>Egami</familyName></personName></creator><creator creatorRole="author" xml:id="cr14" affiliationRef="#a11"><personName><givenNames>E.</givenNames><familyName>Jullo</familyName></personName></creator><creator creatorRole="author" xml:id="cr15" affiliationRef="#a2"><personName><givenNames>V.</givenNames><familyName>Hamilton‐Morris</familyName></personName></creator><creator creatorRole="author" xml:id="cr16" affiliationRef="#a12"><personName><givenNames>S. M.</givenNames><familyName>Moran</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</unparsedAffiliation></affiliation><affiliation xml:id="a2"><unparsedAffiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="FR"><unparsedAffiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="CA"><unparsedAffiliation>University of British Columbia, Department of Physics and Astronomy, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="US"><unparsedAffiliation>Harvard‐Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA02138, USA</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="IT"><unparsedAffiliation>Department of Physics, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="DK"><unparsedAffiliation>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark</unparsedAffiliation></affiliation><affiliation xml:id="a10" countryCode="US"><unparsedAffiliation>Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</unparsedAffiliation></affiliation><affiliation xml:id="a11" countryCode="US"><unparsedAffiliation>Jet Propulsion Laboratory, Caltech, MS 169‐327, Oak Grove Dr, Pasadena, CA 91109, USA</unparsedAffiliation></affiliation><affiliation xml:id="a12" countryCode="US"><unparsedAffiliation>Johns Hopkins Deptartment of Physics and Astronomy, Baltimore, MD 21218, USA</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">gravitational lensing</keyword><keyword xml:id="k2">galaxies: clusters: general</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution <i>Hubble Space Telescope</i> imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within <span type="mathematics"><i>R</i>≤ 250 kpc</span>. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of <span type="mathematics">〈log<sub>10</sub>θ<sub>E</sub>(<i>z</i>= 2)〉= 1.16 ± 0.28</span>; (ii) we detect an X‐ray/lensing mass discrepancy of <span type="mathematics">〈<i>M</i><sub>SL</sub>/<i>M</i><sub>X</sub>〉= 1.3</span> at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at z= 0.2</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>LoCuSS: strong‐lensing clusters</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>LoCuSS: first results from strong‐lensing analysis of 20 massive galaxy clusters at z= 0.2</title></titleInfo><name type="personal"><namePart type="given">Johan</namePart><namePart type="family">Richard</namePart><affiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation><affiliation>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</affiliation><affiliation>E-mail: johan.richard@durham.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Graham P.</namePart><namePart type="family">Smith</namePart><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Jean‐Paul</namePart><namePart type="family">Kneib</namePart><affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Richard S.</namePart><namePart type="family">Ellis</namePart><affiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. J. R.</namePart><namePart type="family">Sanderson</namePart><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Pei</namePart><affiliation>California Institute of Technology, Mail Code 105‐24, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T. A.</namePart><namePart type="family">Targett</namePart><affiliation>University of British Columbia, Department of Physics and Astronomy, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D. J.</namePart><namePart type="family">Sand</namePart><affiliation>Harvard‐Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge MA02138, USA</affiliation><affiliation>Marie‐Curie fellow. E‐mail: Harvard Center for Astrophysics and Las Cumbres Observatory Global Telescope Network fellow.</affiliation><affiliation>E-mail: johan.richard@durham.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. M.</namePart><namePart type="family">Swinbank</namePart><affiliation>Institute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Dannerbauer</namePart><affiliation>Max‐Planck‐Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Mazzotta</namePart><affiliation>Department of Physics, Universitá di Roma Tor Vergata, via della Ricerca Scientifica, 1, 00133 Roma, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Limousin</namePart><affiliation>Laboratoire d'Astrophysique de Marseille, CNRS – Université Aix‐Marseille, 38 rue Frédéric Joliot‐Curie, 13388 Marseille Cedex 13, France</affiliation><affiliation>Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Egami</namePart><affiliation>Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Jullo</namePart><affiliation>Jet Propulsion Laboratory, Caltech, MS 169‐327, Oak Grove Dr, Pasadena, CA 91109, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">V.</namePart><namePart type="family">Hamilton‐Morris</namePart><affiliation>School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. M.</namePart><namePart type="family">Moran</namePart><affiliation>Johns Hopkins Deptartment of Physics and Astronomy, Baltimore, MD 21218, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2010-05-01</dateIssued><edition>Accepted 2010 January 4. Received 2009 December 17; in original form 2009 August 12</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><internetMediaType>text/html</internetMediaType><extent unit="figures">14</extent><extent unit="tables">9</extent><extent unit="formulas">464</extent><extent unit="references">91</extent></physicalDescription><abstract lang="en">We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high‐resolution Hubble Space Telescope imaging of the cluster cores and follow‐up spectroscopic observations using the Keck‐I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R≤ 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X‐ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1σ width of 〈log10θE(z= 2)〉= 1.16 ± 0.28; (ii) we detect an X‐ray/lensing mass discrepancy of 〈MSL/MX〉= 1.3 at 3σ significance – clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster–cluster mergers and gas cooling. Overall our results are consistent with the view that cluster–cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm.</abstract><subject lang="en"><genre>keywords</genre><topic>gravitational lensing</topic><topic>galaxies: clusters: general</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal">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>404</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>325</start><end>349</end><total>25</total></extent></part></relatedItem><identifier type="istex">E51B0F09C42EBD306FDE252829961EABF8890EA5</identifier><identifier type="DOI">10.1111/j.1365-2966.2009.16274.x</identifier><identifier type="ArticleID">MNR16274</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2010 The Authors. 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