Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag
The narrow-line Seyfert 1 galaxy IRAS 13224−3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe − K and L emission features which are interpreted as arising from reflection from the inner parts of an...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2013-03, Vol.429 (4), p.2917-2923 |
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| creator | Fabian, A. C. Kara, E. Walton, D. J. Wilkins, D. R. Ross, R. R. Lozanov, K. Uttley, P. Gallo, L. C. Zoghbi, A. Miniutti, G. Boller, T. Brandt, W. N. Cackett, E. M. Chiang, C.-Y. Dwelly, T. Malzac, J. Miller, J. M. Nardini, E. Ponti, G. Reis, R. C. Reynolds, C. S. Steiner, J. F. Tanaka, Y. Young, A. J. |
| description | The narrow-line Seyfert 1 galaxy IRAS 13224−3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe − K
and L emission features which are interpreted as arising from reflection from the inner parts of an accretion disc around a rapidly spinning black hole. Assuming a power law emissivity for the reflected flux and that the innermost radius corresponds to the innermost stable circular orbit, the black hole spin is measured to be 0.989 with a statistical precision better than 1 per cent. Systematic uncertainties are discussed. A soft X-ray lag of 100 s confirms this scenario. The bulk of the power-law continuum source is located at a radius of 2-3 gravitational radii. |
| doi_str_mv | 10.1093/mnras/sts504 |
| format | Article |
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and L emission features which are interpreted as arising from reflection from the inner parts of an accretion disc around a rapidly spinning black hole. Assuming a power law emissivity for the reflected flux and that the innermost radius corresponds to the innermost stable circular orbit, the black hole spin is measured to be 0.989 with a statistical precision better than 1 per cent. Systematic uncertainties are discussed. A soft X-ray lag of 100 s confirms this scenario. The bulk of the power-law continuum source is located at a radius of 2-3 gravitational radii.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/sts504</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Astrophysics ; Black holes ; Gravity ; Star & galaxy formation ; Uncertainty</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2013-03, Vol.429 (4), p.2917-2923</ispartof><rights>2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2013</rights><rights>Copyright Oxford University Press, UK Mar 11, 2013</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c399t-398f3040f5aed2ec68a82ed85118efe60a73c4eacec3f20fde85cb7b71dc1a5b3</citedby><cites>FETCH-LOGICAL-c399t-398f3040f5aed2ec68a82ed85118efe60a73c4eacec3f20fde85cb7b71dc1a5b3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,1598,27901,27902</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/sts504$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Fabian, A. C.</creatorcontrib><creatorcontrib>Kara, E.</creatorcontrib><creatorcontrib>Walton, D. J.</creatorcontrib><creatorcontrib>Wilkins, D. R.</creatorcontrib><creatorcontrib>Ross, R. R.</creatorcontrib><creatorcontrib>Lozanov, K.</creatorcontrib><creatorcontrib>Uttley, P.</creatorcontrib><creatorcontrib>Gallo, L. C.</creatorcontrib><creatorcontrib>Zoghbi, A.</creatorcontrib><creatorcontrib>Miniutti, G.</creatorcontrib><creatorcontrib>Boller, T.</creatorcontrib><creatorcontrib>Brandt, W. N.</creatorcontrib><creatorcontrib>Cackett, E. M.</creatorcontrib><creatorcontrib>Chiang, C.-Y.</creatorcontrib><creatorcontrib>Dwelly, T.</creatorcontrib><creatorcontrib>Malzac, J.</creatorcontrib><creatorcontrib>Miller, J. M.</creatorcontrib><creatorcontrib>Nardini, E.</creatorcontrib><creatorcontrib>Ponti, G.</creatorcontrib><creatorcontrib>Reis, R. C.</creatorcontrib><creatorcontrib>Reynolds, C. S.</creatorcontrib><creatorcontrib>Steiner, J. F.</creatorcontrib><creatorcontrib>Tanaka, Y.</creatorcontrib><creatorcontrib>Young, A. J.</creatorcontrib><title>Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>The narrow-line Seyfert 1 galaxy IRAS 13224−3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe − K
and L emission features which are interpreted as arising from reflection from the inner parts of an accretion disc around a rapidly spinning black hole. Assuming a power law emissivity for the reflected flux and that the innermost radius corresponds to the innermost stable circular orbit, the black hole spin is measured to be 0.989 with a statistical precision better than 1 per cent. Systematic uncertainties are discussed. A soft X-ray lag of 100 s confirms this scenario. The bulk of the power-law continuum source is located at a radius of 2-3 gravitational radii.</description><subject>Astrophysics</subject><subject>Black holes</subject><subject>Gravity</subject><subject>Star & galaxy formation</subject><subject>Uncertainty</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNp90L1OwzAUhmELgUQpbFzAkRhYGmrHcX7YKsRPpVZIFCS26CSxU1dpHOy0JXfAzCVyJRTCzHSWR-eTXkLOGb1iNOHjdW3RjV3rBA0OyIDxUHh-EoaHZEApF14cMXZMTpxbUUoD7ocDspuZuoTX-RxM5qTdYqtNDUZBu5RQo7Vm51W6lrCQnZK2BQYlVvjewfRpsgDGfT_4-vjkMU2uwWKjC9ii1ZjpSrfdCJa6XIJrdA1YF4DgjGqhwvKUHCmsnDz7u0Pycnf7fPPgzR7vpzeTmZfzJGk9nsSK04AqgbLwZR7GGPuyiAVjsVQypBjxPJCYy5wrn6pCxiLPoixiRc5QZHxILvq_jTVvG-nadGU2tt5PpoyLIOBUBOFejXqVW-OclSptrF6j7VJG05-06W_atE-755c9N5vmf_kNeXl79g</recordid><startdate>20130311</startdate><enddate>20130311</enddate><creator>Fabian, A. 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J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2013-03-11</date><risdate>2013</risdate><volume>429</volume><issue>4</issue><spage>2917</spage><epage>2923</epage><pages>2917-2923</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>The narrow-line Seyfert 1 galaxy IRAS 13224−3809 has been observed with XMM-Newton for 500 ks. The source is rapidly variable on time-scales down to a few 100 s. The spectrum shows strong broad Fe − K
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| subjects | Astrophysics Black holes Gravity Star & galaxy formation Uncertainty |
| title | Long XMM observation of the narrow-line Seyfert 1 galaxy IRAS 13224−3809: rapid variability, high spin and a soft lag |
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