The hard X-ray perspective on the soft X-ray excess

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dc.creator Vasudevan, Ranjan V.
dc.creator Mushotzky, Richard F.
dc.creator Reynolds, Christopher S.
dc.creator Fabian, Andrew C.
dc.creator Lohfink, Anne M.
dc.creator Zoghbi, Abderahmen
dc.creator Gallo, Luigi C.
dc.creator Walton, Dominic
dc.date.accessioned 2018-04-04T13:34:31Z
dc.date.available 2018-04-04T13:34:31Z
dc.date.issued 2014-04-10
dc.identifier.issn 0004-637X
dc.identifier.uri http://library2.smu.ca/handle/01/27395
dc.description Publisher's Version/PDF
dc.description.abstract The X-ray spectra of many active galactic nuclei exhibit a “soft excess” below 1 keV, whose physical origin remains unclear. Diverse models have been suggested to account for it, including ionized reflection of X-rays from the inner part of the accretion disk, ionized winds/absorbers, and Comptonization. The ionized reflection model suggests a natural link between the prominence of the soft excess and the Compton reflection hump strength above 10 keV, but it has not been clear what hard X-ray signatures, if any, are expected from the other soft X-ray candidate models. Additionally, it has not been possible up until recently to obtain high-quality simultaneous measurements of both soft and hard X-ray emission necessary to distinguish these models but upcoming joint XMM–NuSTAR programs provide precisely this opportunity. In this paper, we present an extensive analysis of simulations of XMM–NuSTAR observations, using two candidate soft excess models as inputs, to determine whether such campaigns can disambiguate between them by using hard and soft X-ray observations in tandem. The simulated spectra are fit with the simplest “observer’s model” of a blackbody and neutral reflection to characterize the strength of the soft and hard excesses. A plot of the strength of the hard excess against the soft excess strength provides a diagnostic plot which allows the soft excess production mechanism to be determined in individual sources and samples using current state-of-the-art and next generation hard X-ray enabled observatories. This approach can be straightforwardly extended to other candidate models for the soft excess. en_CA
dc.language.iso en en_CA
dc.publisher IOP Publishing Limited en_CA
dc.relation.uri https://dx.doi.org/10.1088/0004-637X/785/1/30
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Accretion (Astrophysics)
dc.subject.lcsh Active galaxies
dc.subject.lcsh X-ray sources, Galactic
dc.title The hard X-ray perspective on the soft X-ray excess en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal 785(1), 30. (2014) en_CA


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Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: https://dx.doi.org/10.1088/0004-637X/785/1/30
 
 

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