Compton reflection and iron fluorescence in BeppoSAX observations of Seyfert type 1 galaxies

By G. Perola, G. Matt, M. Cappi, Fabrizio Fiore, M. Guainazzi, L. Maraschi, P. Petrucci, L. Piro. 2002

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A sample of nine bright Seyfert 1 and NELG type galaxies, observed with BeppoSAX, is analyzed to assess on a truly broad band basis (0.1{200 keV) the issue of the spectral contributions of Compton reflection and iron line fluorescence from circumnuclear gas. The empirical description adopted for the direct continuum is the commonly used power law with an exponential cut{o. The most direct test of the theoretical predictions, namely that the equivalent width of the line, W, and the strength R of the reflection relative to the direct continuum are closely related to each other, gives a substantially positive result, that is their mean ratio is very close to expectation, and only a modest spread in the iron abundance seems implied. The existence of a steep correlation between R and the slope of the power law is not conrmed. A weak evidence is found that the existence of a very shallow trend to increase on average with cannot be altogether excluded in both R and W, but needs to be tested with a larger sample. The energy Ef in the exponential cut{o spans a range from about 80 to more than 300 keV. A possible correlation is found, with Ef increasing on average with : if ignored, for instance by keeping Ef at a xed value in a sample study, it could be cause of articial steepening in a correlation between R and .

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/e3a2d476b18f865518fc83f3af2b76f28ca698af

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THE CORES OF THE Fe Kα LINES IN ACTIVE GALACTIC NUCLEI: AN EXTENDED CHANDRA HIGH ENERGY GRATING SAMPLE (2010, background): “…the X-ray spectrum of active galactic nuclei (AGNs) that have a 2–10 keV X-ray luminosity less than ∼1045 erg s−1 (e.g., Sulentic et al. 1998; Lubiński & Zdziarski 2001; Weaver et al. 2001; Perola et al. 2002; Yaqoob & Padmanabhan 2004 (hereafter YP04); Levenson et al. 2006; Winter et al. 2009).”
The synthesis of the cosmic X-ray background in the Chandra and XMM-Newton era (2006, background): “The most recent results indicate a relatively large spread inEc from about 50 keV up to about 500 keV (Perola et al. 2002, Molina et al. 2006).”
THE SPACE DENSITY OF COMPTON-THICK ACTIVE GALACTIC NUCLEUS AND THE X-RAY BACKGROUND (2009, methodology): “A similar value of R≃1 was reported by Perola et al. (2002) based on BeppoSAX observations of a sample of 9 Seyfert 1 galaxies.”
Quasars: the characteristic spectrum and the induced radiative heating (2003, methodology): “Perola et al. (2002) have recently presented a sample of broad-band (0.1–200 keV) spectra obtained with the BeppoSAX satellite for nine Seyfert 1s with LX ranging from 5 × 1042 to 1044 erg s−1.”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “…above yields a best-fit uncorrelated dispersion component 0.1 dex, consistent with observational estimates of the scatter in band luminosities owing to these effects (e.g., Elvis et al.1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Richards et al. 2003; Hopkins et al. 2004).”
A Physical Model for the Origin of Quasar Lifetimes (2005, methodology): “…= ǫṀc2, we model the form of the intrinsic quasar continuum SED following Marconi et al. (2004), based on optical through hard X-ray observations (e.g., Elvis et al. 1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Telfer et al. 2002; Ueda et al. 2003; Vignali et al. 2003).”
Black Holes in Galaxy Mergers: Evolution of Quasars (2005, methodology): “…= ǫrṀc2, we model the form of the intrinsic quasar continuum SED following Marconi et al. (2004), based on optical through hard X-ray observations (e.g., Elvis et al. 1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Telfer et al. 2002; Ueda et al. 2003; Vignali et al. 2003).”
X-ray obscuration and obscured AGN in the local universe (2005, methodology): “No high-energy cut-off for the intrinsic power-law continuum emission has been imposed, as it normally lays beyond the sensitive bandpass of the XMM-Newton/EPIC or Chandra/ACIS cameras (Perola et al. 2002).”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, methodology): “…Marconi et al. (2004), based on optical through hard X-ray observations (e.g., Elvis et al. 1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Telfer et al. 2002; Ueda et al. 2003; Vignali et al. 2003), with an Xray reflection component generated by the PEXRAV model…”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, methodology): “…Marconi et al. (2004), based on optical through hard X-ray observations (e.g., Elvis et al. 1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Telfer et al. 2002; Ueda et al. 2003; Vignali et al. 2003), with a reflection component generated by the PEXRAV model (Magdziarz…”
THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION (2013, background): “Previous studies (e.g., Perola et al. 2002) indicate coronal temperatures in the 50-200 keV range, as derived from the measurement of high-energy cut-offs observed in the power-law continua of several AGN.”
A long hard look at MCG–6-30-15 with XMM-Newton (2002, background): “The presence of the reflection hump has since been confirmed byCGRO (e.g. Zdziarski et al. 1995) andBeppoSAX(e.g. Perola et al. 2002).”
X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue (2014, methodology): “The high-energy cutoff observed in the energy range 80− 300 keV (Perola et al. 2002) lies well above the energy range used in this work (< 10 keV) even at moderate redshifts.”
Local supermassive black holes, relics of active galactic nuclei and the X-ray background (2003, background): “The powerlaw has the typical photon index Γ = 1.9 (e.g. George et al. 1998; Perola et al. 2002) and an exponential cutoff at Ec = 500 keV.”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, methodology): “…Marconi et al. (2004) based on optical through hard X-ray observations (e.g., Elvis et al. 1994; George et al. 1998; Vanden Berk et al. 2001; Perola et al. 2002; Telfer et al. 2002; Ueda et al. 2003; Vignali et al. 2003), with a hard X-ray reflection component generated by the PEXRAV model…”