A wide Chandra view of the core of the Perseus cluster
Identifieur interne : 002A19 ( Istex/Corpus ); précédent : 002A18; suivant : 002A20A wide Chandra view of the core of the Perseus cluster
Auteurs : A. C. Fabian ; J. S. Sanders ; S. W. Allen ; R. E. A. Canning ; E. Churazov ; C. S. Crawford ; W. Forman ; J. Gabany ; J. Hlavacek-Larrondo ; R. M. Johnstone ; H. R. Russell ; C. S. Reynolds ; P. Salomé ; G. B. Taylor ; A. J. YoungSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-12-21.
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- KwdEn :
Abstract
We present new Chandra images of the X‐ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s−1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. It separates an inner disturbed region dominated by the activity of the active nucleus of NGC 1275 from the outer region where a subcluster merger dominates.
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DOI: 10.1111/j.1365-2966.2011.19402.x
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ISTEX:F9648690C09CCD45C081ECE3629BA1661B286C73Le document en format XML
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Fabian</name><affiliation><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: acf@ast.cam.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Sanders, J S" sort="Sanders, J S" uniqKey="Sanders J" first="J. S." last="Sanders">J. S. Sanders</name><affiliation><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation></affiliation></author><author><name sortKey="Allen, S W" sort="Allen, S W" uniqKey="Allen S" first="S. W." last="Allen">S. W. 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Taylor</name><affiliation><mods:affiliation>Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: acf@ast.cam.ac.uk</mods:affiliation></affiliation></author><author><name sortKey="Young, A J" sort="Young, A J" uniqKey="Young A" first="A. J." last="Young">A. J. Young</name><affiliation><mods:affiliation>H. H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 3HG</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="2011-12-21">2011-12-21</date><biblScope unit="volume">418</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="2154">2154</biblScope><biblScope unit="page" to="2164">2164</biblScope></imprint><idno type="ISSN">0035-8711</idno></series><idno type="istex">F9648690C09CCD45C081ECE3629BA1661B286C73</idno><idno type="DOI">10.1111/j.1365-2966.2011.19402.x</idno><idno type="ArticleID">MNR19402</idno></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>X‐rays: galaxies</term><term>galaxies: clusters: general</term><term>galaxies: individual: NGC 1275</term><term>intergalactic medium</term></keywords></textClass><langUsage><language ident="en">en</language></langUsage></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">We present new Chandra images of the X‐ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s−1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. It separates an inner disturbed region dominated by the activity of the active nucleus of NGC 1275 from the outer region where a subcluster merger dominates.</div></front></TEI><istex><corpusName>wiley</corpusName><author><json:item><name>A. C. 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The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s−1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. 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S.</forename><surname>Crawford</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-7"><persName><forename type="first">W.</forename><surname>Forman</surname></persName><affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA</affiliation></author><author xml:id="author-8"><persName><forename type="first">J.</forename><surname>GaBany</surname></persName><affiliation>Blackbird 2 Observatory, Alder Springs, CA 93602, USA</affiliation></author><author xml:id="author-9"><persName><forename type="first">J.</forename><surname>Hlavacek‐Larrondo</surname></persName><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation></author><author xml:id="author-10"><persName><forename type="first">R. 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B.</forename><surname>Taylor</surname></persName><email>acf@ast.cam.ac.uk</email><affiliation>Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA</affiliation></author><author xml:id="author-15"><persName><forename type="first">A. J.</forename><surname>Young</surname></persName><affiliation>H. H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 3HG</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="2011-12-21"></date><biblScope unit="volume">418</biblScope><biblScope unit="issue">4</biblScope><biblScope unit="page" from="2154">2154</biblScope><biblScope unit="page" to="2164">2164</biblScope></imprint></monogr><idno type="istex">F9648690C09CCD45C081ECE3629BA1661B286C73</idno><idno type="DOI">10.1111/j.1365-2966.2011.19402.x</idno><idno type="ArticleID">MNR19402</idno></biblStruct></sourceDesc></fileDesc><profileDesc><creation><date>2011</date></creation><langUsage><language ident="en">en</language></langUsage><abstract xml:lang="en"><p>We present new Chandra images of the X‐ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s−1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. 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Received 2011 July 5; in original form 2011 May 24</unparsedEditorialHistory><countGroup><count type="figureTotal" number="17"></count><count type="tableTotal" number="0"></count><count type="formulaTotal" number="7"></count><count type="referenceTotal" number="50"></count><count type="linksCrossRef" number="138"></count></countGroup><titleGroup><title type="main">A wide <i>Chandra</i> view of the core of the Perseus cluster</title><title type="shortAuthors"><i>A. C. Fabian et al.</i></title><title type="short"><i>A wider view of the Perseus cluster</i></title></titleGroup><creators><creator creatorRole="author" xml:id="cr1" affiliationRef="#a1" corresponding="yes"><personName><givenNames>A. C.</givenNames><familyName>Fabian</familyName></personName></creator><creator creatorRole="author" xml:id="cr2" affiliationRef="#a1"><personName><givenNames>J. 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J.</givenNames><familyName>Young</familyName></personName></creator></creators><affiliationGroup><affiliation xml:id="a1"><unparsedAffiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</unparsedAffiliation></affiliation><affiliation xml:id="a2"><unparsedAffiliation>Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, 452 Lomita Mall, Stanford, CA 94305‐4085</unparsedAffiliation></affiliation><affiliation xml:id="a3" countryCode="US"><unparsedAffiliation>SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA</unparsedAffiliation></affiliation><affiliation xml:id="a4" countryCode="DE"><unparsedAffiliation>Max‐Planck‐Institut for Astrophysics, Karl‐Schwarzschild‐str. 1, 85741 Garching, Germany</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="US"><unparsedAffiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="US"><unparsedAffiliation>Blackbird 2 Observatory, Alder Springs, CA 93602, USA</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="CA"><unparsedAffiliation>Department of Physics and Astronomy, University of Waterloo, ON N2L 3G1, Canada</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="US"><unparsedAffiliation>Department of Astronomy, University of Maryland, College Park, MD 20742, USA</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="FR"><unparsedAffiliation>LERMA, Observatoire de Paris, UMR 8112 du CNRS, 75014 Paris, France</unparsedAffiliation></affiliation><affiliation xml:id="a10" countryCode="US"><unparsedAffiliation>Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA</unparsedAffiliation></affiliation><affiliation xml:id="a11"><unparsedAffiliation>H. H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 3HG</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">galaxies: clusters: general</keyword><keyword xml:id="k2">galaxies: individual: NGC 1275</keyword><keyword xml:id="k3">intergalactic medium</keyword><keyword xml:id="k4">X‐rays: galaxies</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>We present new <i>Chandra</i> images of the X‐ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s<sup>−1</sup>. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. It separates an inner disturbed region dominated by the activity of the active nucleus of NGC 1275 from the outer region where a subcluster merger dominates.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>A wide Chandra view of the core of the Perseus cluster</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>A wider view of the Perseus cluster</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>A wide Chandra view of the core of the Perseus cluster</title></titleInfo><name type="personal"><namePart type="given">A. C.</namePart><namePart type="family">Fabian</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><affiliation>E-mail: acf@ast.cam.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. S.</namePart><namePart type="family">Sanders</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S. W.</namePart><namePart type="family">Allen</namePart><affiliation>Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics, Stanford University, 452 Lomita Mall, Stanford, CA 94305‐4085</affiliation><affiliation>SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, CA 94025, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. E. A.</namePart><namePart type="family">Canning</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">E.</namePart><namePart type="family">Churazov</namePart><affiliation>Max‐Planck‐Institut for Astrophysics, Karl‐Schwarzschild‐str. 1, 85741 Garching, Germany</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C. S.</namePart><namePart type="family">Crawford</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">W.</namePart><namePart type="family">Forman</namePart><affiliation>Harvard–Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">GaBany</namePart><affiliation>Blackbird 2 Observatory, Alder Springs, CA 93602, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Hlavacek‐Larrondo</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R. M.</namePart><namePart type="family">Johnstone</namePart><affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H. R.</namePart><namePart type="family">Russell</namePart><affiliation>Department of Physics and Astronomy, University of Waterloo, ON N2L 3G1, Canada</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C. S.</namePart><namePart type="family">Reynolds</namePart><affiliation>Department of Astronomy, University of Maryland, College Park, MD 20742, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Salomé</namePart><affiliation>LERMA, Observatoire de Paris, UMR 8112 du CNRS, 75014 Paris, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G. B.</namePart><namePart type="family">Taylor</namePart><affiliation>Department of Physics and Astronomy, University of New Mexico, Albuquerque, NM 87131, USA</affiliation><affiliation>E-mail: acf@ast.cam.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A. J.</namePart><namePart type="family">Young</namePart><affiliation>H. H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 3HG</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">2011-12-21</dateIssued><edition>Accepted 2011 July 7. Received 2011 July 5; in original form 2011 May 24</edition><copyrightDate encoding="w3cdtf">2011</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">17</extent><extent unit="formulas">7</extent><extent unit="references">50</extent></physicalDescription><abstract lang="en">We present new Chandra images of the X‐ray emission from the core of the Perseus cluster of galaxies. The total observation time is now 1.4 Ms. New depressions in X‐ray surface brightness are discovered to the north of NGC 1275, which we interpret as old rising bubbles. They imply that bubbles are long‐lived and do not readily breakup when rising in the hot cluster atmosphere. The existence of a 300 kpc long NNW–SSW bubble axis means there cannot be significant transverse large‐scale flows exceeding 100 km s−1. Interesting spatial correlations are seen along that axis in early deep radio maps. A semicircular cold front about 100 kpc west of the nucleus is seen. It separates an inner disturbed region dominated by the activity of the active nucleus of NGC 1275 from the outer region where a subcluster merger dominates.</abstract><subject lang="en"><genre>keywords</genre><topic>galaxies: clusters: general</topic><topic>galaxies: individual: NGC 1275</topic><topic>intergalactic medium</topic><topic>X‐rays: galaxies</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>2011</date><detail type="volume"><caption>vol.</caption><number>418</number></detail><detail type="issue"><caption>no.</caption><number>4</number></detail><extent unit="pages"><start>2154</start><end>2164</end><total>11</total></extent></part></relatedItem><identifier type="istex">F9648690C09CCD45C081ECE3629BA1661B286C73</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.19402.x</identifier><identifier type="ArticleID">MNR19402</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition><recordInfo><recordContentSource>WILEY</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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