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The 1.5 Ms observing campaign on IRAS 13224−3809 – I. X-ray spectral analysis

Jiang, J. and Parker, M. L. and Fabian, A. C. and Alston, W. N. and Buisson, D. J. K. and Cackett, E. M. and Chiang, C.-Y. and Dauser, T. and Gallo, L. C. and García, J. A. and Harrison, F. A. and Lohfink, A. M. and De Marco, B. and Kara, E. and Miller, J. M. and Miniutti, G. and Pinto, C. and Walton, D. J. and Wilkins, D. R. (2018) The 1.5 Ms observing campaign on IRAS 13224−3809 – I. X-ray spectral analysis. Monthly Notices of the Royal Astronomical Society, 477 (3). pp. 3711-3726. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20180620-154958509

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Abstract

We present a detailed spectral analysis of the recent 1.5 Ms XMM–Newton observing campaign on the narrow-line Seyfert 1 galaxy IRAS 13224−3809, taken simultaneously with 500 ks of NuSTAR data. The X-ray light curve shows three flux peaks, registering at about 100 times the minimum flux seen during the campaign, and rapid variability with a time-scale of kiloseconds. The spectra are well fit with a primary power-law continuum, two relativistic-blurred reflection components from the inner accretion disc with very high iron abundance, and a simple blackbody-shaped model for the remaining soft excess. The spectral variability is dominated by the power-law continuum from a corona region within a few gravitational radii from the black hole. Additionally, blueshifted Ne X, Mg XII, Si XIV, and S XVI absorption lines are identified in the stacked low-flux spectrum, confirming the presence of a highly ionized outflow with velocity up to v = 0.267 and 0.225 c. We fit the absorption features with xstar models and find a relatively constant velocity outflow through the whole observation. Finally, we replace the bbody and supersolar abundance reflection models by fitting the soft excess successfully with the extended reflection model relxillD, which allows for higher densities than the standard relxill model. This returns a disc electron density n_e > 10^(18.7) cm^(−3) and lowers the iron abundance from Z_(Fe) = 24^(+3)_(−4)Z_⊙ with n-e = 10^(15) cm^(-3) to Z_(Fe) = 6.6^(+0.8)_(-2.1)Z_⊙.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty836DOIArticle
https://arxiv.org/abs/1804.00349arXivDiscussion Paper
ORCID:
AuthorORCID
Fabian, A. C.0000-0002-9378-4072
Cackett, E. M.0000-0002-8294-9281
Chiang, C.-Y.0000-0002-9630-4003
García, J. A.0000-0003-3828-2448
Harrison, F. A.0000-0003-2992-8024
Pinto, C.0000-0003-2532-7379
Walton, D. J.0000-0001-5819-3552
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/about_us/legal/notices) Accepted 2018 March 28. Received 2018 March 1; in original form 2017 September 11. J.J. acknowledges support by the Cambridge Trust and the Chinese Scholarship Council Joint Scholarship Programme (201604100032). A.C.F., M.L.P., and C.P. acknowledge support by the ERC Advanced Grant 340442. B.D.M. acknowledges support by the Polish National Science Center grant Polonez 2016/21/P/ST9/04025. W.N.A. acknowledges support from the European Union Seventh Framework Program (FP7/2013–2017) under grant agreement no. 312789, StrongGravity. G.M. acknowledges support from the European Union Seventh Framework Program (FP7/2007–2013) under grant agreement no. 312789, StrongGravity and the Spanish grant ESP2015-65597-C4-1-R. D.J.K.B. is supported by the Science and Technology Facilities Council (STFC). J.A.G. acknowledges the support from the Alexander von Humboldt Foundation. D.R.W. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF6-170160, awarded by the Chandra X-ray Center, operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. D.J.W. acknowledges support from an STFC Ernest Rutherford fellowship. Based on observations obtained with XMM–Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This project has made use of the Science Analysis Software (SAS), an extensive suite to process the data collected by the XMM–Newton observatory. This work made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by NASA. This research has made use of the NuSTAR Data Analysis Software (NuSTARDAS) jointly developed by the ASI Science Data Center and the California Institute of Technology.
Group:NuSTAR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Cambridge Overseas TrustUNSPECIFIED
Chinese Scholarship Council201604100032
European Research Council (ERC)340442
National Science Centre (Poland)2016/21/P/ST9/04025
European Research Council (ERC)312789
Ministerio de Economía y Competitividad (MINECO)ESP2015-65597-C4-1-R
Science and Technology Facilities Council (STFC)UNSPECIFIED
Alexander von Humboldt FoundationUNSPECIFIED
NASA Einstein FellowshipPF6-170160
NASANAS8-03060
ESA Member States UNSPECIFIED
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:accretion, accretion discs – black hole physics, galaxies: Seyfert, X-rays: galaxies
Record Number:CaltechAUTHORS:20180620-154958509
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180620-154958509
Official Citation:J Jiang(姜嘉陈), M L Parker, A C Fabian, W N Alston, D J K Buisson, E M Cackett, C-Y Chiang, T Dauser, L C Gallo, J A García, F A Harrison, A M Lohfink, B De Marco, E Kara, J M Miller, G Miniutti, C Pinto, D J Walton, D R Wilkins; The 1.5 Ms observing campaign on IRAS 13224−3809 – I. X-ray spectral analysis, Monthly Notices of the Royal Astronomical Society, Volume 477, Issue 3, 1 July 2018, Pages 3711–3726, https://doi.org/10.1093/mnras/sty836
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87282
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:20 Jun 2018 23:17
Last Modified:20 Jun 2018 23:17

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