Detecting compact dark matter in galaxy clusters via gravitational microlensing: A2218 and A370
Identifieur interne : 000529 ( Main/Corpus ); précédent : 000528; suivant : 000530Detecting compact dark matter in galaxy clusters via gravitational microlensing: A2218 and A370
Auteurs : A. V. Tuntsov ; G. F. Lewis ; R. A. Ibata ; J. KneibSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2004-09.
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- KwdEn :
Abstract
After decades of searching, the true nature of dark matter still eludes us. One potential probe of the form of dark matter in galaxy clusters is to search for microlensing variability in the giant arcs and arclets. In this paper, a simple method is introduced to characterize pixel variability in the limit of high optical depth to microlensing. Expanding on earlier work, the expected microlensing signal for two massive clusters, A2218 and A370 is calculated. It is found that the microlensing signal depends sensitively upon the mix of smooth and compact dark matter in the cluster. Comparison of two deep exposures taken with James Webb Space Telescope or 2‐h exposures taken with a 30‐m class telescope in two epochs separated by a few years will possibly detect a few dozen pixels that show strong variability due to microlensing at the 5σ level, revealing a wealth of information on the microlensing population.
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DOI: 10.1111/j.1365-2966.2004.08115.x
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ISTEX:9138203D911634C86D195A490CFDE5092E8D0C6ALe document en format XML
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Belin, 31400 Toulouse, France</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">gravitational lensing</keyword><keyword xml:id="k2">dark matter</keyword><keyword xml:id="k3">galaxies: clusters: individual: A370</keyword><keyword xml:id="k4">galaxies: clusters: individual: A2218.</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>After decades of searching, the true nature of dark matter still eludes us. One potential probe of the form of dark matter in galaxy clusters is to search for microlensing variability in the giant arcs and arclets. In this paper, a simple method is introduced to characterize pixel variability in the limit of high optical depth to microlensing. Expanding on earlier work, the expected microlensing signal for two massive clusters, A2218 and A370 is calculated. It is found that the microlensing signal depends sensitively upon the mix of smooth and compact dark matter in the cluster. Comparison of two deep exposures taken with <i>James Webb Space Telescope</i> or 2‐h exposures taken with a 30‐m class telescope in two epochs separated by a few years will possibly detect a few dozen pixels that show strong variability due to microlensing at the 5σ level, revealing a wealth of information on the microlensing population.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Detecting compact dark matter in galaxy clusters via gravitational microlensing: A2218 and A370</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Compact dark matter in galaxy clusters</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Detecting compact dark matter in galaxy clusters via gravitational microlensing: A2218 and A370</title></titleInfo><name type="personal"><namePart type="given">A. V.</namePart><namePart type="family">Tuntsov</namePart><affiliation>A29, School of Physics, University of Sydney, NSW 2006, Australia</affiliation><affiliation>E‐mail: (AVT); (GFL); (RAI); (JPK) On leave at: Caltech, Astronomy, 105‐24, Pasadena, CA 91125, USA.</affiliation><affiliation>E-mail: tyomich@physics.usyd.edu.augfl@physics.usyd.edu.auibata@pleiades.u‐strasbg.frkneib@ast.obs‐mip.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G. F.</namePart><namePart type="family">Lewis</namePart><affiliation>A29, School of Physics, University of Sydney, NSW 2006, Australia</affiliation><affiliation>E‐mail: (AVT); (GFL); (RAI); (JPK) On leave at: Caltech, Astronomy, 105‐24, Pasadena, CA 91125, USA.</affiliation><affiliation>E-mail: tyomich@physics.usyd.edu.augfl@physics.usyd.edu.auibata@pleiades.u‐strasbg.frkneib@ast.obs‐mip.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. A.</namePart><namePart type="family">Ibata</namePart><affiliation>Observatoire de Strasbourg, 11 rue de l'Universite, F‐67000 Strasbourg, France</affiliation><affiliation>E‐mail: (AVT); (GFL); (RAI); (JPK) On leave at: Caltech, Astronomy, 105‐24, Pasadena, CA 91125, USA.</affiliation><affiliation>E-mail: tyomich@physics.usyd.edu.augfl@physics.usyd.edu.auibata@pleiades.u‐strasbg.frkneib@ast.obs‐mip.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.‐P.</namePart><namePart type="family">Kneib</namePart><affiliation>Observatoire Midi‐Pyrénées, 14 Av. E. Belin, 31400 Toulouse, France</affiliation><affiliation>E‐mail: (AVT); (GFL); (RAI); (JPK) On leave at: Caltech, Astronomy, 105‐24, Pasadena, CA 91125, USA.</affiliation><affiliation>E-mail: tyomich@physics.usyd.edu.augfl@physics.usyd.edu.auibata@pleiades.u‐strasbg.frkneib@ast.obs‐mip.fr</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article"></genre><originInfo><publisher>Blackwell Science Ltd</publisher><place><placeTerm type="text">23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803</placeTerm></place><dateIssued encoding="w3cdtf">2004-09</dateIssued><edition>Accepted 2004 June 9. Received 2004 June 8; in original form 2004 March 11</edition><copyrightDate encoding="w3cdtf">2004</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">5</extent><extent unit="formulas">318</extent><extent unit="references">49</extent></physicalDescription><abstract lang="en">After decades of searching, the true nature of dark matter still eludes us. One potential probe of the form of dark matter in galaxy clusters is to search for microlensing variability in the giant arcs and arclets. In this paper, a simple method is introduced to characterize pixel variability in the limit of high optical depth to microlensing. Expanding on earlier work, the expected microlensing signal for two massive clusters, A2218 and A370 is calculated. It is found that the microlensing signal depends sensitively upon the mix of smooth and compact dark matter in the cluster. Comparison of two deep exposures taken with James Webb Space Telescope or 2‐h exposures taken with a 30‐m class telescope in two epochs separated by a few years will possibly detect a few dozen pixels that show strong variability due to microlensing at the 5σ level, revealing a wealth of information on the microlensing population.</abstract><subject lang="en"><genre>keywords</genre><topic>gravitational lensing</topic><topic>dark matter</topic><topic>galaxies: clusters: individual: A370</topic><topic>galaxies: clusters: individual: A2218.</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>2004</date><detail type="volume"><caption>vol.</caption><number>353</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>853</start><end>866</end></extent></part></relatedItem><identifier type="istex">9138203D911634C86D195A490CFDE5092E8D0C6A</identifier><identifier type="DOI">10.1111/j.1365-2966.2004.08115.x</identifier><identifier type="ArticleID">MNR8115</identifier><recordInfo><recordContentSource>WILEY</recordContentSource><recordOrigin>Blackwell Science Ltd</recordOrigin></recordInfo></mods></metadata><enrichments><json:item><type>multicat</type><uri>https://api.istex.fr/document/9138203D911634C86D195A490CFDE5092E8D0C6A/enrichments/multicat</uri></json:item></enrichments><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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