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|Title:||XMM–Newton observations of high-luminosity radio-quiet quasi-stellar objects|
|Authors:||Page, Kim L.|
Reeves, J. N.
O'Brien, Paul T.
Turner, Martin J. L.
Worrall, D. M.
|Publisher:||Oxford University Press (OUP) on behalf of the Royal Astronomical Society|
|Citation:||Monthly Notices of the Royal Astronomical Society, 2004, 353 (1), pp. 133-142|
|Abstract:||XMM–Newton observations of five high-luminosity radio-quiet quasi-stellar objects (QSOs; Q 0144−3938, UM 269, PG 1634+706, SBS 0909+532 and PG 1247+267) are presented. Spectral energy distributions were calculated from the XMM–Newton European Photon Imaging Camera (EPIC) and Optical Monitor (OM) data, with bolometric luminosities estimated in the range from 7 × 10[superscript 45] to 2 × 10[superscript 48] erg s[superscript −1] for the sample, peaking in the ultraviolet. At least four of the QSOs show a similar soft excess, which can be well modelled by either one or two blackbody components, in addition to the hard X-ray power law. The temperatures of these blackbodies (∼100–500 eV) are too high to be direct thermal emission from the accretion disc, so Comptonization is suggested. Two populations of Comptonizing electrons, with different temperatures, are needed to model the broad-band spectrum. The hotter of these produces what is seen as the hard X-ray power law, while the cooler (∼0.25–0.5 keV) population models the spectral curvature at low energies. Only one of the QSOs shows evidence for an absorption component, while three of the five show neutral iron emission. Of these, PG 1247+267 seems to have a broad line (with an equivalent width of ∼250 eV), with a strong, associated reflection component (R ∼ 2), measured out to 30 keV in the rest frame of the QSO. Finally, it is concluded that the X-ray continuum shape of active galactic nuclei remains essentially constant over a wide range of black hole mass and luminosity.|
|Rights:||Copyright © 2004 The Authors. Journal compilation © 2004 RAS. Deposited with reference to the publisher’s open access archiving policy.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
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