Narrow Results

In this work, we revisited the relationship between the subclasses of blazars (X–ray selected BL Lacertae objects (XBLs), radio selected BL Lacertae objects (RBLs), and flat spectrum radio quasars (FSRQs)) based on a sample of blazars. We found that the FSRQs–RBLs–XBLs relationship is clear in their bolometric luminosity, emission line luminosity and the accretion ratio with V_FSRQs > V_RBLs > V_XBLs, where V stands for the three parameters. However, there is no clear difference amongst their central black hole masses. The bolometric luminosity is closely correlated with the emission line luminosity and the accretion ratio.

We have analyzed the XMM-Newton RGS spectral properties of a sample of the most prominent Narrow-Line Seyfert 1 (NLS1) galaxies observed so far with previous and present X-ray missions. We have fitted the merged RGS1/RGS2 first and second order spectra for all available observations from the XMM-Newton Science Archive to test the reflection model interpretation proposed by Ross & Fabian (2005). For objects with more than one observations a combined RGS1/RGS2 first and second order spectrum has been created, resulting in exposure times ranging between about 13 and 780 ks. For the maximum possible RGS statistics we work out the progress and limitations for the spectral fitting of those NLS1 galaxies most observed with XMM-Newton. The objects 1H 0707–495 and Ark 564 can be modelled with the relativistic reflection model by Ross & Fabian (2005). For 1H 0707–495, the reflection spectrum fit suggests an inner disc radius at about 3 R_G. Assuming a standard disc where the inner disc edge is equal to the marginally stable orbit we infer a rapidly rotating black hole with spin parameter of about 0.8. The emissivity index of the power law amounts to 6.3 suggesting a centrally peaked emission. The ionization parameter is about 1000. The soft X-ray lines are therefore strongly broadened by Compton broadening effects and the emission in the strong gravity field limit. Similar values are obtained for Ark 564. The FWHM of the additional soft X-ray lines required in the fit for 1H 0707-495 are much smaller, about 0.1c, which is consistent with an origination in the weaker field limit. We find that for the prototype objects 1H 0707–495 and for Ark 564 only the relativistic reflection model provides a statistically acceptable fit. The obtained parameters from the relativistic reflection model suggest that the observed emission originates from matter very close to the central supermassive black hole.

The following sections are included:

• Estimating BH Masses

• Beyond Crude Estimates

• FWHM(MgII) as a Virial Estimator for Higher z Quasars?

• References