High‐resolution imaging of the anomalous flux ratio gravitational lens system CLASS B2045+265: dark or luminous satellites?
Identifieur interne : 000616 ( Main/Corpus ); précédent : 000615; suivant : 000617High‐resolution imaging of the anomalous flux ratio gravitational lens system CLASS B2045+265: dark or luminous satellites?
Auteurs : J. P. Mckean ; L. V. E. Koopmans ; C. E. Flack ; C. D. Fassnacht ; D. Thompson ; K. Matthews ; R. D. Blandford ; A. C. S. Readhead ; B. T. SoiferSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007-06-11.
English descriptors
Abstract
The existence of flux ratio anomalies between fold and cusp images in galaxy‐scale strong‐lens systems has led to an interpretation based on the presence of a high mass fraction of cold dark matter (CDM) substructures around galaxies, as predicted by numerical N‐body simulations. These substructures can cause large perturbations of the image magnifications, leading to changes in the image flux ratios. The flux ratio anomaly is particularly evident in the radio‐loud quadruple gravitational lens system CLASS B2045+265. In this paper, new high‐resolution radio, optical and infrared imaging of B2045+265 is presented which sheds more light on this anomaly and its possible causes. First, deep Very Long Baseline Array observations show very compact images, possibly with a hint of a jet, but with no evidence for differential scattering or scatter broadening. Hence, the flux ratio anomaly is unlikely to be caused by refractive scattering in either the Milky Way or the lens galaxy. Secondly, optical and infrared observations with the Hubble Space Telescope and through adaptive optics imaging with the W. M. Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O ii] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional and flux ratio constraints, without the need for additional CDM substructure. Although the model is peculiar in that the dwarf galaxy must be highly flattened, the model is very similar to recently proposed mass models based on high‐order multipole expansions.
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DOI: 10.1111/j.1365-2966.2007.11744.x
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Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O ii] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional and flux ratio constraints, without the need for additional CDM substructure. 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These substructures can cause large perturbations of the image magnifications, leading to changes in the image flux ratios. The flux ratio anomaly is particularly evident in the radio‐loud quadruple gravitational lens system CLASS B2045+265. In this paper, new high‐resolution radio, optical and infrared imaging of B2045+265 is presented which sheds more light on this anomaly and its possible causes. First, deep Very Long Baseline Array observations show very compact images, possibly with a hint of a jet, but with no evidence for differential scattering or scatter broadening. Hence, the flux ratio anomaly is unlikely to be caused by refractive scattering in either the Milky Way or the lens galaxy. Secondly, optical and infrared observations with the Hubble Space Telescope and through adaptive optics imaging with the W. M. Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O ii] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional and flux ratio constraints, without the need for additional CDM substructure. 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P.</forename><surname>McKean</surname></persName><note type="correspondence"><p>Correspondence: E‐mail:</p></note><affiliation>Department of Physics, University of California, Davis, CA 95616, USA</affiliation><affiliation>Max‐Planck‐Institut für Radioastronomie, Auf dem Hügel 69, D‐53121 Bonn, Germany</affiliation></author><author xml:id="author-2"><persName><forename type="first">L. V. E.</forename><surname>Koopmans</surname></persName><affiliation>Kapteyn Astronomical Institute, Postbus 800, NL‐9700 AV Groningen, the Netherlands</affiliation></author><author xml:id="author-3"><persName><forename type="first">C. E.</forename><surname>Flack</surname></persName><affiliation>Department of Physics, University of California, Davis, CA 95616, USA</affiliation><affiliation>Bemidji State University, Bemidji, MN 56601, USA</affiliation></author><author xml:id="author-4"><persName><forename type="first">C. 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These substructures can cause large perturbations of the image magnifications, leading to changes in the image flux ratios. The flux ratio anomaly is particularly evident in the radio‐loud quadruple gravitational lens system CLASS B2045+265. In this paper, new high‐resolution radio, optical and infrared imaging of B2045+265 is presented which sheds more light on this anomaly and its possible causes. First, deep Very Long Baseline Array observations show very compact images, possibly with a hint of a jet, but with no evidence for differential scattering or scatter broadening. Hence, the flux ratio anomaly is unlikely to be caused by refractive scattering in either the Milky Way or the lens galaxy. Secondly, optical and infrared observations with the Hubble Space Telescope and through adaptive optics imaging with the W. M. Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O ii] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional and flux ratio constraints, without the need for additional CDM substructure. Although the model is peculiar in that the dwarf galaxy must be highly flattened, the model is very similar to recently proposed mass models based on high‐order multipole expansions.</p></abstract><textClass xml:lang="en"><keywords scheme="keyword"><list><head>keywords</head><item><term>gravitational lensing</term></item><item><term>quasars: individual: CLASS B2045+265</term></item><item><term>cosmology: observations</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2007-06-11">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/3CC88ADE9D906CD4F2B3A970DED28BEDD54805F3/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="06001"><doi origin="wiley">10.1111/mnr.2007.378.issue-1</doi><numberingGroup><numbering type="journalVolume" number="378">378</numbering><numbering type="journalIssue" number="1">1</numbering></numberingGroup><coverDate startDate="2007-06-11">June 2007</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="10" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2007.11744.x</doi><idGroup><id type="unit" value="MNR11744"></id></idGroup><countGroup><count type="pageTotal" number="10"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2007-05-07"></event><event type="publishedOnlineFinalForm" date="2007-05-10"></event><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.3.6 mode:FullText source:FullText result:FullText" date="2010-04-21"></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="109">109</numbering><numbering type="pageLast" number="118">118</numbering></numberingGroup><correspondenceTo> E‐mail: <email normalForm="mckean@mpifr-bonn.mpg.de">mckean@mpifr‐bonn.mpg.de</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR11744.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2007 March 16. Received 2007 March 15; in original form 2006 October 23</unparsedEditorialHistory><countGroup><count type="figureTotal" number="6"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="89"></count><count type="referenceTotal" number="51"></count><count type="linksCrossRef" number="140"></count></countGroup><titleGroup><title type="main">High‐resolution imaging of the anomalous flux ratio gravitational lens system CLASS B2045+265: dark or luminous satellites?</title><title type="shortAuthors"><i>J. P. McKean et al.</i></title><title type="short"><i>High‐resolution imaging of CLASS B2045+265</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1 #a2" corresponding="yes"><personName><givenNames>J. P.</givenNames><familyName>McKean</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a3"><personName><givenNames>L. V. E.</givenNames><familyName>Koopmans</familyName></personName></creator><creator creatorRole="author" xml:id="cr3" affiliationRef="#a1 #a4"><personName><givenNames>C. E.</givenNames><familyName>Flack</familyName></personName></creator><creator creatorRole="author" xml:id="cr4" affiliationRef="#a1"><personName><givenNames>C. D.</givenNames><familyName>Fassnacht</familyName></personName></creator><creator creatorRole="author" xml:id="cr5" affiliationRef="#a5"><personName><givenNames>D.</givenNames><familyName>Thompson</familyName></personName></creator><creator creatorRole="author" xml:id="cr6" affiliationRef="#a5"><personName><givenNames>K.</givenNames><familyName>Matthews</familyName></personName></creator><creator creatorRole="author" xml:id="cr7" affiliationRef="#a6"><personName><givenNames>R. D.</givenNames><familyName>Blandford</familyName></personName></creator><creator creatorRole="author" xml:id="cr8" affiliationRef="#a7"><personName><givenNames>A. C. S.</givenNames><familyName>Readhead</familyName></personName></creator><creator creatorRole="author" xml:id="cr9" affiliationRef="#a5"><personName><givenNames>B. T.</givenNames><familyName>Soifer</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="US"><unparsedAffiliation>Department of Physics, University of California, Davis, CA 95616, USA</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut für Radioastronomie, Auf dem Hügel 69, D‐53121 Bonn, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="NL"><unparsedAffiliation>Kapteyn Astronomical Institute, Postbus 800, NL‐9700 AV Groningen, the Netherlands</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="US"><unparsedAffiliation>Bemidji State University, Bemidji, MN 56601, USA</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="US"><unparsedAffiliation>KIPAC, Stanford University, 2575 Sand Hill Road, Menlo Park, CA 94025, USA</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="US"><unparsedAffiliation>Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">gravitational lensing</keyword><keyword xml:id="k2">quasars: individual: CLASS B2045+265</keyword><keyword xml:id="k3">cosmology: observations</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>The existence of flux ratio anomalies between fold and cusp images in galaxy‐scale strong‐lens systems has led to an interpretation based on the presence of a high mass fraction of cold dark matter (CDM) substructures around galaxies, as predicted by numerical <i>N</i>‐body simulations. These substructures can cause large perturbations of the image magnifications, leading to changes in the image flux ratios. The flux ratio anomaly is particularly evident in the radio‐loud quadruple gravitational lens system CLASS B2045+265. In this paper, new high‐resolution radio, optical and infrared imaging of B2045+265 is presented which sheds more light on this anomaly and its possible causes. First, deep Very Long Baseline Array observations show very compact images, possibly with a hint of a jet, but with no evidence for differential scattering or scatter broadening. Hence, the flux ratio anomaly is unlikely to be caused by refractive scattering in either the Milky Way or the lens galaxy. Secondly, optical and infrared observations with the <i>Hubble Space Telescope</i> and through adaptive optics imaging with the W. M. Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O <sc>ii</sc>] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional <i>and</i> flux ratio constraints, without the need for additional CDM substructure. Although the model is peculiar in that the dwarf galaxy must be highly flattened, the model is very similar to recently proposed mass models based on high‐order multipole expansions.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>High‐resolution imaging of the anomalous flux ratio gravitational lens system CLASS B2045+265: dark or luminous satellites?</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>High‐resolution imaging of CLASS B2045+265</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>High‐resolution imaging of the anomalous flux ratio gravitational lens system CLASS B2045+265: dark or luminous satellites?</title></titleInfo><name type="personal"><namePart type="given">J. P.</namePart><namePart type="family">McKean</namePart><affiliation>Department of Physics, University of California, Davis, CA 95616, USA</affiliation><affiliation>Max‐Planck‐Institut für Radioastronomie, Auf dem Hügel 69, D‐53121 Bonn, Germany</affiliation><description>Correspondence: E‐mail: </description><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L. V. E.</namePart><namePart type="family">Koopmans</namePart><affiliation>Kapteyn Astronomical Institute, Postbus 800, NL‐9700 AV Groningen, the Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C. E.</namePart><namePart type="family">Flack</namePart><affiliation>Department of Physics, University of California, Davis, CA 95616, USA</affiliation><affiliation>Bemidji State University, Bemidji, MN 56601, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C. D.</namePart><namePart type="family">Fassnacht</namePart><affiliation>Department of Physics, University of California, Davis, CA 95616, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Thompson</namePart><affiliation>Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K.</namePart><namePart type="family">Matthews</namePart><affiliation>Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. D.</namePart><namePart type="family">Blandford</namePart><affiliation>KIPAC, Stanford University, 2575 Sand Hill Road, Menlo Park, CA 94025, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. C. S.</namePart><namePart type="family">Readhead</namePart><affiliation>Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">B. T.</namePart><namePart type="family">Soifer</namePart><affiliation>Caltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, 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">2007-06-11</dateIssued><edition>Accepted 2007 March 16. Received 2007 March 15; in original form 2006 October 23</edition><copyrightDate encoding="w3cdtf">2007</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">6</extent><extent unit="tables">3</extent><extent unit="formulas">89</extent><extent unit="references">51</extent></physicalDescription><abstract lang="en">The existence of flux ratio anomalies between fold and cusp images in galaxy‐scale strong‐lens systems has led to an interpretation based on the presence of a high mass fraction of cold dark matter (CDM) substructures around galaxies, as predicted by numerical N‐body simulations. These substructures can cause large perturbations of the image magnifications, leading to changes in the image flux ratios. The flux ratio anomaly is particularly evident in the radio‐loud quadruple gravitational lens system CLASS B2045+265. In this paper, new high‐resolution radio, optical and infrared imaging of B2045+265 is presented which sheds more light on this anomaly and its possible causes. First, deep Very Long Baseline Array observations show very compact images, possibly with a hint of a jet, but with no evidence for differential scattering or scatter broadening. Hence, the flux ratio anomaly is unlikely to be caused by refractive scattering in either the Milky Way or the lens galaxy. Secondly, optical and infrared observations with the Hubble Space Telescope and through adaptive optics imaging with the W. M. Keck Telescope, show a previously undiscovered object – interpreted as a (tidally disrupted) dwarf satellite based on its colours and slight extension – between the main lens galaxy and the three anomalous flux ratio images. Thirdly, colour variations in the early‐type lens galaxy indicate recent star formation, possibly the result of secondary infall of gas‐rich satellites. A population of such galaxies around the lens system could explain the previously discovered strong [O ii] emission. However, spiral structure and/or normal star formation in the lens galaxy cannot be excluded. In light of these new data, we propose a lens model for the system, including the observed dwarf satellite, which reproduces all positional and flux ratio constraints, without the need for additional CDM substructure. Although the model is peculiar in that the dwarf galaxy must be highly flattened, the model is very similar to recently proposed mass models based on high‐order multipole expansions.</abstract><subject lang="en"><genre>keywords</genre><topic>gravitational lensing</topic><topic>quasars: individual: CLASS B2045+265</topic><topic>cosmology: observations</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>2007</date><detail type="volume"><caption>vol.</caption><number>378</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>109</start><end>118</end><total>10</total></extent></part></relatedItem><identifier type="istex">3CC88ADE9D906CD4F2B3A970DED28BEDD54805F3</identifier><identifier type="DOI">10.1111/j.1365-2966.2007.11744.x</identifier><identifier type="ArticleID">MNR11744</identifier><recordInfo><recordContentSource>WILEY</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods></metadata><enrichments><json:item><type>multicat</type><uri>https://api.istex.fr/document/3CC88ADE9D906CD4F2B3A970DED28BEDD54805F3/enrichments/multicat</uri></json:item></enrichments><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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