Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures
Identifieur interne : 001F23 ( Istex/Corpus ); précédent : 001F22; suivant : 001F24Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures
Auteurs : Geraint F. Lewis ; Rodrigo A. IbataSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2006-04.
English descriptors
- KwdEn :
- Accretion disc, Blrs, Bottom panel, Bottorff, Bottorff ferland, Coherent velocity structure, Einstein radii, Einstein radius, Emission line, Emission lines, Extensive nature, External shear, Ferland, Fractal, Fractal blrs, Fractal distribution, Fractal hierarchies, Fractal hierarchy, Fractal structure, Fractal structures, Gravitational microlensing, Highest fractal hierarchy, Individual clouds, Journal compilation, Kinematic, Kinematic properties, Lewis ibata, Lewis irwin, Light curve, Light curves, Lower fractal hierarchies, Maximum fractal hierarchy, Maximum hierarchy, Microlensed, Microlensed quasar, Microlensing, Microlensing light curve, Mnras, Particular fractal hierarchy, Particular velocity, Pixel, Quasar, Reverberation mapping, Same keplerian velocity, Smallest structures, Solar mass star, Spatial structure, Velocity elements, Wambsganss, Wambsganss paczynski.
- Teeft :
- Accretion disc, Blrs, Bottom panel, Bottorff, Bottorff ferland, Coherent velocity structure, Einstein radii, Einstein radius, Emission line, Emission lines, Extensive nature, External shear, Ferland, Fractal, Fractal blrs, Fractal distribution, Fractal hierarchies, Fractal hierarchy, Fractal structure, Fractal structures, Gravitational microlensing, Highest fractal hierarchy, Individual clouds, Journal compilation, Kinematic, Kinematic properties, Lewis ibata, Lewis irwin, Light curve, Light curves, Lower fractal hierarchies, Maximum fractal hierarchy, Maximum hierarchy, Microlensed, Microlensed quasar, Microlensing, Microlensing light curve, Mnras, Particular fractal hierarchy, Particular velocity, Pixel, Quasar, Reverberation mapping, Same keplerian velocity, Smallest structures, Solar mass star, Spatial structure, Velocity elements, Wambsganss, Wambsganss paczynski.
Abstract
Recent models for the emission clouds within the broad‐line region (BLR) of quasars suggest that they are due to transient overdensities within an overall turbulent medium. If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.
Url:
DOI: 10.1111/j.1365-2966.2006.10042.x
Links to Exploration step
ISTEX:A4E7793426EA6F3243EAD70902B2D3F362E9BB84Le document en format XML
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If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.</div></front></TEI><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>fractal</json:string><json:string>quasar</json:string><json:string>microlensing</json:string><json:string>mnras</json:string><json:string>light curves</json:string><json:string>light curve</json:string><json:string>blrs</json:string><json:string>pixel</json:string><json:string>microlensed</json:string><json:string>fractal structure</json:string><json:string>wambsganss</json:string><json:string>gravitational microlensing</json:string><json:string>ferland</json:string><json:string>bottorff</json:string><json:string>kinematic</json:string><json:string>bottorff ferland</json:string><json:string>emission line</json:string><json:string>fractal hierarchy</json:string><json:string>einstein radius</json:string><json:string>journal compilation</json:string><json:string>emission lines</json:string><json:string>einstein radii</json:string><json:string>fractal hierarchies</json:string><json:string>microlensed quasar</json:string><json:string>accretion disc</json:string><json:string>fractal distribution</json:string><json:string>maximum fractal hierarchy</json:string><json:string>external shear</json:string><json:string>particular velocity</json:string><json:string>spatial structure</json:string><json:string>reverberation mapping</json:string><json:string>wambsganss paczynski</json:string><json:string>lewis ibata</json:string><json:string>solar mass star</json:string><json:string>individual clouds</json:string><json:string>microlensing light curve</json:string><json:string>extensive nature</json:string><json:string>bottom panel</json:string><json:string>lewis irwin</json:string><json:string>smallest structures</json:string><json:string>highest fractal hierarchy</json:string><json:string>lower fractal hierarchies</json:string><json:string>maximum hierarchy</json:string><json:string>fractal structures</json:string><json:string>velocity elements</json:string><json:string>kinematic properties</json:string><json:string>particular fractal hierarchy</json:string><json:string>same keplerian velocity</json:string><json:string>coherent velocity structure</json:string><json:string>fractal blrs</json:string></teeft></keywords><author><json:item><name>Geraint F. 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If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.</abstract><qualityIndicators><score>7.144</score><pdfWordCount>3680</pdfWordCount><pdfCharCount>20496</pdfCharCount><pdfVersion>1.3</pdfVersion><pdfPageCount>5</pdfPageCount><pdfPageSize>612 x 792 pts (letter)</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>122</abstractWordCount><abstractCharCount>823</abstractCharCount><keywordCount>3</keywordCount></qualityIndicators><title>Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</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>367</volume><issue>3</issue><pages><first>1217</first><last>1221</last></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>2006</json:string><json:string>1000</json:string></date><geogName></geogName><orgName></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Rodrigo A. 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(1995)</json:string><json:string>Lewis & Irwin 1996</json:string><json:string>Lewis (2004)</json:string><json:string>Wandel et al. 1999</json:string><json:string>Schmidt, Webster & Lewis 1998</json:string><json:string>Wambsganss & Paczynski 1991</json:string><json:string>Lewis & Irwin 1995</json:string><json:string>Kayser et al. 1986</json:string><json:string>Peterson, Crenshaw & Meyers 1985</json:string><json:string>Davidson & Netzer 1979</json:string><json:string>Lewis & Ibata 2004</json:string></ref_bibl><bibl></bibl></unitex></namedEntities><ark><json:string>ark:/67375/WNG-G6SL9ZM5-B</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 exactes et technologie</json:string><json:string>3 - terre, ocean, espace</json:string><json:string>4 - astronomie</json:string></inist></categories><publicationDate>2006</publicationDate><copyrightDate>2006</copyrightDate><doi><json:string>10.1111/j.1365-2966.2006.10042.x</json:string></doi><id>A4E7793426EA6F3243EAD70902B2D3F362E9BB84</id><score>1</score><fulltext><json:item><extension>pdf</extension><original>true</original><mimetype>application/pdf</mimetype><uri>https://api.istex.fr/document/A4E7793426EA6F3243EAD70902B2D3F362E9BB84/fulltext/pdf</uri></json:item><json:item><extension>zip</extension><original>false</original><mimetype>application/zip</mimetype><uri>https://api.istex.fr/document/A4E7793426EA6F3243EAD70902B2D3F362E9BB84/fulltext/zip</uri></json:item><istex:fulltextTEI uri="https://api.istex.fr/document/A4E7793426EA6F3243EAD70902B2D3F362E9BB84/fulltext/tei"><teiHeader><fileDesc><titleStmt><title level="a" type="main">Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</title></titleStmt><publicationStmt><authority>ISTEX</authority><publisher>Blackwell Publishing Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2006-04"></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">Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</title><title level="a" type="short">Microlensing of fractal BLRs</title><author xml:id="author-0000" role="corresp"><persName><forename type="first">Geraint F.</forename><surname>Lewis</surname></persName><affiliation>Institute of Astronomy, School of Physics, University of Sydney, NSW 2006, Australia<address><country key="AU"></country></address></affiliation><affiliation>E‐mail: gfl@physics.usyd.edu.au (GFL); ibata@astro.u‐strasbg.fr (RAI)</affiliation></author><author xml:id="author-0001" role="corresp"><persName><forename type="first">Rodrigo A.</forename><surname>Ibata</surname></persName><affiliation>Observatoire de Strasbourg, 11 Rue de l'Universite, F‐6700 Strasbourg, France<address><country key="FR"></country></address></affiliation><affiliation>E‐mail: gfl@physics.usyd.edu.au (GFL); ibata@astro.u‐strasbg.fr (RAI)</affiliation></author><idno type="istex">A4E7793426EA6F3243EAD70902B2D3F362E9BB84</idno><idno type="ark">ark:/67375/WNG-G6SL9ZM5-B</idno><idno type="DOI">10.1111/j.1365-2966.2006.10042.x</idno><idno type="unit">MNR10042</idno><idno type="supplier">mnr10042</idno><idno type="toTypesetVersion">file:MNR.MNR10042.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.2006.367.issue-3</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</idno><imprint><biblScope unit="vol">367</biblScope><biblScope unit="issue">3</biblScope><biblScope unit="page" from="1217">1217</biblScope><biblScope unit="page" to="1221">1221</biblScope><publisher>Blackwell Publishing Ltd</publisher><pubPlace> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2006-04"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>Recent models for the emission clouds within the broad‐line region (BLR) of quasars suggest that they are due to transient overdensities within an overall turbulent medium. If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">gravitational lensing</term><term xml:id="k2">quasars: absorption lines</term><term xml:id="k3">quasars: emission lines</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/A4E7793426EA6F3243EAD70902B2D3F362E9BB84/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> 23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803 </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="04003"><doi origin="wiley">10.1111/mnr.2006.367.issue-3</doi><numberingGroup><numbering type="journalVolume" number="367">367</numbering><numbering type="journalIssue" number="3">3</numbering></numberingGroup><coverDate startDate="2006-04">April 2006</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="34" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2006.10042.x</doi><idGroup><id type="unit" value="MNR10042"></id><id type="supplier" value="mnr10042"></id></idGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><eventGroup><event type="firstOnline" date="2006-02-13"></event><event type="publishedOnlineFinalForm" date="2006-02-13"></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="1217">1217</numbering><numbering type="pageLast" number="1221">1221</numbering></numberingGroup><correspondenceTo>
E‐mail: <email>gfl@physics.usyd.edu.au</email> (GFL); <email normalForm="ibata@astro.u-strasbg.fr">ibata@astro.u‐strasbg.fr</email> (RAI)</correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR10042.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2006 January 1. Received 2005 November 24; in original form 2005 July 26</unparsedEditorialHistory><countGroup><count type="figureTotal" number="5"></count><count type="tableTotal" number="0"></count><count type="formulaTotal" number="57"></count><count type="referenceTotal" number="26"></count><count type="linksCrossRef" number="65"></count></countGroup><titleGroup><title type="main">Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</title><title type="shortAuthors"><i>G. F. Lewis and R. A. Ibata</i></title><title type="short"><i>Microlensing of fractal BLRs</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>Geraint F.</givenNames><familyName>Lewis</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a2" corresponding="yes"><personName><givenNames>Rodrigo A.</givenNames><familyName>Ibata</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1" countryCode="AU"><unparsedAffiliation>Institute of Astronomy, School of Physics, University of Sydney, NSW 2006, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a2" countryCode="FR"><unparsedAffiliation>Observatoire de Strasbourg, 11 Rue de l'Universite, F‐6700 Strasbourg, France</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">gravitational lensing</keyword><keyword xml:id="k2">quasars: absorption lines</keyword><keyword xml:id="k3">quasars: emission lines</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>Recent models for the emission clouds within the broad‐line region (BLR) of quasars suggest that they are due to transient overdensities within an overall turbulent medium. If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Microlensing of fractal BLRs</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>Gravitational microlensing of quasar broad‐line regions: the influence of fractal structures</title></titleInfo><name type="personal"><namePart type="given">Geraint F.</namePart><namePart type="family">Lewis</namePart><affiliation>Institute of Astronomy, School of Physics, University of Sydney, NSW 2006, Australia</affiliation><affiliation>E-mail: gfl@physics.usyd.edu.au</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 de Strasbourg, 11 Rue de l'Universite, F‐6700 Strasbourg, France</affiliation><affiliation>E-mail: gfl@physics.usyd.edu.au</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">23 Ainslie Place , Edinburgh EH3 6AJ , UK . Telephone (0131) 226 7232 Fax (0131) 226 3803</placeTerm></place><dateIssued encoding="w3cdtf">2006-04</dateIssued><edition>Accepted 2006 January 1. Received 2005 November 24; in original form 2005 July 26</edition><copyrightDate encoding="w3cdtf">2006</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">5</extent><extent unit="tables">0</extent><extent unit="formulas">57</extent><extent unit="references">26</extent><extent unit="linksCrossRef">65</extent></physicalDescription><abstract lang="en">Recent models for the emission clouds within the broad‐line region (BLR) of quasars suggest that they are due to transient overdensities within an overall turbulent medium. If this were the case, the broad‐line emission would spatially appear fractal, possessing structure on a range of scales. This paper examines the influence of such fractal structure when a quasar is microlensed by a population of intervening masses. It is found that while the highest fractal levels can undergo significant microlensing magnification, when these light curves are superimposed to create an emission‐line profile, the resultant emission‐line profile remains relatively constant for physical models of the BLR. It is concluded that the detection of the possible fractal structure of BLRs via gravitational microlensing is not practical.</abstract><subject lang="en"><genre>keywords</genre><topic>gravitational lensing</topic><topic>quasars: absorption lines</topic><topic>quasars: emission lines</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>2006</date><detail type="volume"><caption>vol.</caption><number>367</number></detail><detail type="issue"><caption>no.</caption><number>3</number></detail><extent unit="pages"><start>1217</start><end>1221</end></extent></part></relatedItem><identifier type="istex">A4E7793426EA6F3243EAD70902B2D3F362E9BB84</identifier><identifier type="ark">ark:/67375/WNG-G6SL9ZM5-B</identifier><identifier type="DOI">10.1111/j.1365-2966.2006.10042.x</identifier><identifier type="ArticleID">MNR10042</identifier><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/A4E7793426EA6F3243EAD70902B2D3F362E9BB84/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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