Open AccessMultiwavelength XMM–Newton observations of the Laor et al. sample of PG quasars
Author(s) -
Brocksopp C.,
Starling R. L. C.,
Schady P.,
Mason K. O.,
RomeroColmenero E.,
Puchnarewicz E. M.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09772.x
Subject(s) - physics , astrophysics , spectral line , power law , quasar , photon , emission spectrum , line (geometry) , thermal , full width at half maximum , equivalent width , epic , law , astronomy , optics , galaxy , geometry , art , statistics , mathematics , literature , meteorology , political science
We present XMM–Newton /EPIC spectra for the Laor et al. sample of Palomar Green (PG) quasars. We find that a power law provides a reasonable fit to the 2–5 keV region of the spectra. Excess soft X‐ray emission below 2 keV is present for all objects, with the exception of those known to contain a warm absorber. However, a single power law is a poor fit to the 0.3–10.0 keV spectrum and instead we find that a simple model, consisting of a broken power law (plus an iron line), provides a reasonable fit in most cases. The equivalent width of the emission line is constrained in just 12 objects but with low (<2σ) significance in most cases. For the sources whose spectra are well fitted by the broken‐power‐law model, we find that various optical and X‐ray line and continuum parameters are well correlated; in particular, the power‐law photon index is well correlated with the FWHM of the Hβ line and the photon indices of the low‐ and high‐energy components of the broken power law are well correlated with each other. These results suggest that the 0.3–10 keV X‐ray emission shares a common (presumably non‐thermal) origin, as opposed to suggestions that the soft excess is directly produced by thermal disc emission or via an additional spectral component. We present XMM–Newton Optical Monitor (OM) data, which we combine with the X‐ray spectra so as to produce broad‐band spectral energy distributions (SEDs), free from uncertainties due to long‐term variability in non‐simultaneous data. Fitting these optical–UV spectra with a Comptonized disc model indicates that the soft X‐ray excess is independent of the accretion disc, confirming our interpretation of the tight correlation between the hard and soft X‐ray spectra.