Kinematics of quasars and AGN
Identifieur interne : 000796 ( Main/Corpus ); précédent : 000795; suivant : 000797Kinematics of quasars and AGN
Auteurs : K. I Kellermann ; R. C Vermeulen ; J. A Zensus ; M. H Cohen ; A. WestSource :
- New Astronomy Reviews [ 1387-6473 ] ; 1999.
Abstract
The VLBA has been used over a period of four years to study the internal motions within a sample of quasars and AGN. In most sources, features appear to propagate away from the central engine along a well collimated radio jet with apparent transverse velocities between zero and 10c, with some evidence for apparent accelerations and decelerations. The distribution of apparent velocity is not consistent with any simple ballistic model and appears to require either a spread in intrinsic velocity or a difference between the bulk velocity and pattern velocity. The dependence of apparent angular velocity with redshift is consistent with standard Friedmann world models. Further observations of a larger source sample, especially at large redshift may lead to meaningful constraints on world models.
Url:
DOI: 10.1016/S1387-6473(99)00093-7
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ISTEX:A229CFBEEE61B5EBC7F9918FCB69A99E5FC53673Le document en format XML
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A Zensus</name><affiliation><mods:affiliation>MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany</mods:affiliation></affiliation></author><author><name sortKey="Cohen, M H" sort="Cohen, M H" uniqKey="Cohen M" first="M. H" last="Cohen">M. H Cohen</name><affiliation><mods:affiliation>Department of Astronomy. Mail-Stop 105-24, Caltech, Pasadena, CA 91125, USA</mods:affiliation></affiliation></author><author><name sortKey="West, A" sort="West, A" uniqKey="West A" first="A" last="West">A. 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I Kellermann</name><affiliation><mods:affiliation>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</mods:affiliation></affiliation></author><author><name sortKey="Vermeulen, R C" sort="Vermeulen, R C" uniqKey="Vermeulen R" first="R. C" last="Vermeulen">R. C Vermeulen</name><affiliation><mods:affiliation>NFRA, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</mods:affiliation></affiliation></author><author><name sortKey="Zensus, J A" sort="Zensus, J A" uniqKey="Zensus J" first="J. A" last="Zensus">J. A Zensus</name><affiliation><mods:affiliation>MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany</mods:affiliation></affiliation></author><author><name sortKey="Cohen, M H" sort="Cohen, M H" uniqKey="Cohen M" first="M. H" last="Cohen">M. H Cohen</name><affiliation><mods:affiliation>Department of Astronomy. 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West</name><affiliation><mods:affiliation>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">New Astronomy Reviews</title><title level="j" type="abbrev">ASTREV</title><idno type="ISSN">1387-6473</idno><imprint><publisher>ELSEVIER</publisher><date type="published" when="1999">1999</date><biblScope unit="volume">43</biblScope><biblScope unit="issue">8–10</biblScope><biblScope unit="page" from="757">757</biblScope><biblScope unit="page" to="760">760</biblScope></imprint><idno type="ISSN">1387-6473</idno></series><idno type="istex">A229CFBEEE61B5EBC7F9918FCB69A99E5FC53673</idno><idno type="DOI">10.1016/S1387-6473(99)00093-7</idno><idno type="PII">S1387-6473(99)00093-7</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">1387-6473</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The VLBA has been used over a period of four years to study the internal motions within a sample of quasars and AGN. In most sources, features appear to propagate away from the central engine along a well collimated radio jet with apparent transverse velocities between zero and 10c, with some evidence for apparent accelerations and decelerations. The distribution of apparent velocity is not consistent with any simple ballistic model and appears to require either a spread in intrinsic velocity or a difference between the bulk velocity and pattern velocity. The dependence of apparent angular velocity with redshift is consistent with standard Friedmann world models. Further observations of a larger source sample, especially at large redshift may lead to meaningful constraints on world models.</div></front></TEI><istex><corpusName>elsevier</corpusName><author><json:item><name>K.I Kellermann</name><affiliations><json:string>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</json:string></affiliations></json:item><json:item><name>R.C Vermeulen</name><affiliations><json:string>NFRA, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</json:string></affiliations></json:item><json:item><name>J.A Zensus</name><affiliations><json:string>MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany</json:string></affiliations></json:item><json:item><name>M.H Cohen</name><affiliations><json:string>Department of Astronomy. Mail-Stop 105-24, Caltech, Pasadena, CA 91125, USA</json:string></affiliations></json:item><json:item><name>A West</name><affiliations><json:string>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>98.54.-h</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>98.54.Cm</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>98.70.Dk</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxies: active</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxies: jets</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxies: kinematics</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Galaxies: nuclei</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>Quasars: general</value></json:item></subject><language><json:string>eng</json:string></language><originalGenre><json:string>Review article</json:string></originalGenre><abstract>The VLBA has been used over a period of four years to study the internal motions within a sample of quasars and AGN. In most sources, features appear to propagate away from the central engine along a well collimated radio jet with apparent transverse velocities between zero and 10c, with some evidence for apparent accelerations and decelerations. The distribution of apparent velocity is not consistent with any simple ballistic model and appears to require either a spread in intrinsic velocity or a difference between the bulk velocity and pattern velocity. The dependence of apparent angular velocity with redshift is consistent with standard Friedmann world models. 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In most sources, features appear to propagate away from the central engine along a well collimated radio jet with apparent transverse velocities between zero and 10c, with some evidence for apparent accelerations and decelerations. The distribution of apparent velocity is not consistent with any simple ballistic model and appears to require either a spread in intrinsic velocity or a difference between the bulk velocity and pattern velocity. The dependence of apparent angular velocity with redshift is consistent with standard Friedmann world models. Further observations of a larger source sample, especially at large redshift may lead to meaningful constraints on world models.</p></abstract><textClass><keywords scheme="keyword"><list><head>PACS</head><item><term>98.54.-h</term></item><item><term>98.54.Cm</term></item><item><term>98.70.Dk</term></item></list></keywords></textClass><textClass><keywords scheme="keyword"><list><head>Keywords</head><item><term>Galaxies: active</term></item><item><term>Galaxies: jets</term></item><item><term>Galaxies: kinematics</term></item><item><term>Galaxies: nuclei</term></item><item><term>Quasars: general</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="1999">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><original>false</original><mimetype>text/plain</mimetype><extension>txt</extension><uri>https://api.istex.fr/document/A229CFBEEE61B5EBC7F9918FCB69A99E5FC53673/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Elsevier, elements deleted: ce:floats; body; tail"><istex:xmlDeclaration>version="1.0" encoding="utf-8"</istex:xmlDeclaration><istex:docType PUBLIC="-//ES//DTD journal article DTD version 4.5.2//EN//XML" URI="art452.dtd" name="istex:docType"><istex:entity SYSTEM="gr1" NDATA="IMAGE" name="gr1"></istex:entity></istex:docType><istex:document><converted-article version="4.5.2" docsubtype="rev"><item-info><jid>ASTREV</jid><aid>186</aid><ce:pii>S1387-6473(99)00093-7</ce:pii><ce:doi>10.1016/S1387-6473(99)00093-7</ce:doi><ce:copyright year="1999" type="full-transfer">Elsevier Science B.V.</ce:copyright></item-info><head><ce:title>Kinematics of quasars and AGN</ce:title><ce:author-group><ce:author><ce:given-name>K.I</ce:given-name><ce:surname>Kellermann</ce:surname><ce:cross-ref refid="AFF1">a</ce:cross-ref></ce:author><ce:author><ce:given-name>R.C</ce:given-name><ce:surname>Vermeulen</ce:surname><ce:cross-ref refid="AFF2">b</ce:cross-ref></ce:author><ce:author><ce:given-name>J.A</ce:given-name><ce:surname>Zensus</ce:surname><ce:cross-ref refid="AFF3">c</ce:cross-ref></ce:author><ce:author><ce:given-name>M.H</ce:given-name><ce:surname>Cohen</ce:surname><ce:cross-ref refid="AFF4">d</ce:cross-ref></ce:author><ce:author><ce:given-name>A</ce:given-name><ce:surname>West</ce:surname><ce:cross-ref refid="AFF1">a</ce:cross-ref></ce:author><ce:affiliation id="AFF1"><ce:label>a</ce:label><ce:textfn>NRAO<ce:footnote id="FN1"><ce:label>1</ce:label><ce:note-para>The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.</ce:note-para></ce:footnote><ce:cross-ref refid="FN1"><ce:sup>1</ce:sup></ce:cross-ref>, Edgemont Rd., Charolottesville, VA 22903, USA</ce:textfn></ce:affiliation><ce:affiliation id="AFF2"><ce:label>b</ce:label><ce:textfn>NFRA, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</ce:textfn></ce:affiliation><ce:affiliation id="AFF3"><ce:label>c</ce:label><ce:textfn>MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany</ce:textfn></ce:affiliation><ce:affiliation id="AFF4"><ce:label>d</ce:label><ce:textfn>Department of Astronomy. 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Further observations of a larger source sample, especially at large redshift may lead to meaningful constraints on world models.</ce:simple-para></ce:abstract-sec></ce:abstract><ce:keywords class="pacs"><ce:section-title>PACS</ce:section-title><ce:keyword><ce:text>98.54.-h</ce:text></ce:keyword><ce:keyword><ce:text>98.54.Cm</ce:text></ce:keyword><ce:keyword><ce:text>98.70.Dk</ce:text></ce:keyword></ce:keywords><ce:keywords><ce:section-title>Keywords</ce:section-title><ce:keyword><ce:text>Galaxies: active</ce:text></ce:keyword><ce:keyword><ce:text>Galaxies: jets</ce:text></ce:keyword><ce:keyword><ce:text>Galaxies: kinematics</ce:text></ce:keyword><ce:keyword><ce:text>Galaxies: nuclei</ce:text></ce:keyword><ce:keyword><ce:text>Quasars: general</ce:text></ce:keyword></ce:keywords></head></converted-article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>Kinematics of quasars and AGN</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>Kinematics of quasars and AGN</title></titleInfo><name type="personal"><namePart type="given">K.I</namePart><namePart type="family">Kellermann</namePart><affiliation>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.C</namePart><namePart type="family">Vermeulen</namePart><affiliation>NFRA, Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.A</namePart><namePart type="family">Zensus</namePart><affiliation>MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.H</namePart><namePart type="family">Cohen</namePart><affiliation>Department of Astronomy. Mail-Stop 105-24, Caltech, Pasadena, CA 91125, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A</namePart><namePart type="family">West</namePart><affiliation>NRAO1 The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under cooperative Agreement with the National Science Foundation.1, Edgemont Rd., Charolottesville, VA 22903, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="review-article" displayLabel="Review article"></genre><originInfo><publisher>ELSEVIER</publisher><dateIssued encoding="w3cdtf">1999</dateIssued><copyrightDate encoding="w3cdtf">1999</copyrightDate></originInfo><language><languageTerm type="code" authority="iso639-2b">eng</languageTerm><languageTerm type="code" authority="rfc3066">en</languageTerm></language><physicalDescription><internetMediaType>text/html</internetMediaType></physicalDescription><abstract lang="en">The VLBA has been used over a period of four years to study the internal motions within a sample of quasars and AGN. In most sources, features appear to propagate away from the central engine along a well collimated radio jet with apparent transverse velocities between zero and 10c, with some evidence for apparent accelerations and decelerations. The distribution of apparent velocity is not consistent with any simple ballistic model and appears to require either a spread in intrinsic velocity or a difference between the bulk velocity and pattern velocity. The dependence of apparent angular velocity with redshift is consistent with standard Friedmann world models. Further observations of a larger source sample, especially at large redshift may lead to meaningful constraints on world models.</abstract><note type="content">Fig. 1: Observed distribution of v/c for 72 sources with asymmetric structure and well determined velocity.</note><subject><genre>PACS</genre><topic>98.54.-h</topic><topic>98.54.Cm</topic><topic>98.70.Dk</topic></subject><subject><genre>Keywords</genre><topic>Galaxies: active</topic><topic>Galaxies: jets</topic><topic>Galaxies: kinematics</topic><topic>Galaxies: nuclei</topic><topic>Quasars: general</topic></subject><relatedItem type="host"><titleInfo><title>New Astronomy Reviews</title></titleInfo><titleInfo type="abbreviated"><title>ASTREV</title></titleInfo><genre type="journal">journal</genre><originInfo><dateIssued encoding="w3cdtf">199911</dateIssued></originInfo><identifier type="ISSN">1387-6473</identifier><identifier type="PII">S1387-6473(00)X0011-5</identifier><part><date>199911</date><detail type="volume"><number>43</number><caption>vol.</caption></detail><detail type="issue"><number>8–10</number><caption>no.</caption></detail><extent unit="issue pages"><start>503</start><end>798</end></extent><extent unit="pages"><start>757</start><end>760</end></extent></part></relatedItem><identifier type="istex">A229CFBEEE61B5EBC7F9918FCB69A99E5FC53673</identifier><identifier type="DOI">10.1016/S1387-6473(99)00093-7</identifier><identifier type="PII">S1387-6473(99)00093-7</identifier><accessCondition type="use and reproduction" contentType="copyright">©1999 Elsevier Science B.V.</accessCondition><recordInfo><recordContentSource>ELSEVIER</recordContentSource><recordOrigin>Elsevier Science B.V., ©1999</recordOrigin></recordInfo></mods></metadata><enrichments><istex:catWosTEI uri="https://api.istex.fr/document/A229CFBEEE61B5EBC7F9918FCB69A99E5FC53673/enrichments/catWos"><teiHeader><profileDesc><textClass><classCode scheme="WOS">ASTRONOMY & ASTROPHYSICS</classCode></textClass></profileDesc></teiHeader></istex:catWosTEI></enrichments><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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