Show simple item record

dc.contributor.authorAlston, Williamen
dc.contributor.authorFabian, Andrewen
dc.contributor.authorBuisson, DJKen
dc.contributor.authorKara, Een
dc.contributor.authorParker, Michaelen
dc.contributor.authorLohfink, AMen
dc.contributor.authorUttley, Pen
dc.contributor.authorWilkins, DRen
dc.contributor.authorPinto, Ciroen
dc.contributor.authorDe Marco, Ben
dc.contributor.authorCackett, EMen
dc.contributor.authorMiddleton, MJen
dc.contributor.authorWalton, Dominicen
dc.contributor.authorReynolds, Christopheren
dc.contributor.authorJiang, Jiachenen
dc.contributor.authorGallo, LCen
dc.contributor.authorZogbhi, Aen
dc.contributor.authorMiniutti, Gen
dc.contributor.authorDovciak, Men
dc.contributor.authorYoung, AJen
dc.date.accessioned2019-02-08T00:30:53Z
dc.date.available2019-02-08T00:30:53Z
dc.date.issued2019-01-11en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/288910
dc.description.abstract© Crown copyright 2018. We present a detailed X-ray timing analysis of the highly variable narrow-line Seyfert 1 (NLS1) galaxy IRAS 13224-3809. The source was recently monitored for 1.5 Ms with XMM-Newton, which, combined with 500 ks archival data, makes this the best-studied NLS1 galaxy in X-rays to date. We apply standard time- and Fourier-domain techniques in order to understand the underlying variability process. The source flux is not distributed lognormally, as expected for all types of accreting sources. The first non-linear rms-flux relation for any accreting source in any waveband is found, with rms ∝ flux2/3. The light curves exhibit significant strong non-stationarity, in addition to that caused by the rms-flux relation, and are fractionally more variable at lower source flux. The power spectrum is estimated down to ∼10−7 Hz and consists of multiple peaked components: a low-frequency break at ∼10−5 Hz, with slope α < 1 down to low frequencies, and an additional component breaking at ∼10−3 Hz. Using the high-frequency break, we estimate the black hole mass MBH = [0.5-2] × 106 M☉ and mass accretion rate in Eddington units, m Edd ≳ 1. The broad-band power spectral density (PSD) and accretion rate make IRAS 13224-3809 a likely analogue of very high/intermediate-state black hole X-ray binaries. The non-stationarity is manifest in the PSD with the normalization of the peaked components increasing with decreasing source flux, as well as the low-frequency peak moving to higher frequencies. We also detect a narrow coherent feature in the soft-band PSD at 7 × 10−4 Hz; modelled with a Lorentzian the feature has Q ∼ 8 and an rms ∼3 per cent. We discuss the implication of these results for accretion of matter on to black holes.
dc.titleThe remarkable X-ray variability of IRAS 13224-3809 - I. The variability processen
dc.typeArticle
prism.endingPage2106
prism.issueIdentifier2en
prism.publicationDate2019en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage2088
prism.volume482en
dc.identifier.doi10.17863/CAM.36173
dcterms.dateAccepted2018-09-13en
rioxxterms.versionofrecord10.1093/mnras/sty2527en
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2019-01-11en
dc.contributor.orcidAlston, William [0000-0003-2658-6559]
dc.contributor.orcidFabian, Andrew [0000-0002-9378-4072]
dc.contributor.orcidParker, Michael [0000-0002-8466-7317]
dc.contributor.orcidPinto, Ciro [0000-0003-2532-7379]
dc.contributor.orcidWalton, Dominic [0000-0001-5819-3552]
dc.contributor.orcidReynolds, Christopher [0000-0002-1510-4860]
dc.contributor.orcidJiang, Jiachen [0000-0002-9639-4352]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSTFC (ST/R000867/1)
pubs.funder-project-idEC FP7 CP (312789)
pubs.funder-project-idSCIENCE & TECHNOLOGY FACILITIES COUNCIL (ST/N000927/1)


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record