X-ray analysis of the accreting supermassive black hole in the radio galaxy PKS 2251+11

• Published in: arXiv.org
• Main Authors: Ronchini, Samuele, Tombesi, Francesco, Vagnetti, Fausto, Panessa, Francesca, Bruni, Gabriele
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 17.07.2019
• Subjects: Active galactic nuclei; Black holes; Density; Deposition; Ionization; Kinematics; Luminosity; Physics - High Energy Astrophysical Phenomena; Power law; Radio galaxies; Spectra; Supermassive black holes; X ray analysis; XMM (spacecraft)
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.1903.06611

We investigate the dichotomy between jetted and non-jetted Active Galactic Nuclei (AGNs), focusing on the fundamental differences of these two classes in the accretion physics onto the central supermassive black hole (SMBH). Our aim is to study and constrain the structure, kinematics and physical state of the nuclear environment in the Broad Line Radio Galaxy (BLRG) PKS 2251+11. The high X-ray luminosity and the relative proximity make such AGN an ideal candidate for a detailed analysis of the accretion regions in radio galaxies. We performed a spectral and timing analysis of a \(\sim\)64 ks observation of PKS 2251+11 in the X-ray band with XMM-Newton. We modeled the spectrum considering an absorbed power law superimposed to a reflection component. We performed a time-resolved spectral analysis to search for variability of the X-ray flux and of the individual spectral components. We found that the power law has a photon index \(\Gamma=1.8\pm 0.1\), absorbed by an ionized partial covering medium with a column density \(N_H=(10.1\pm 0.8) \times 10^{23}\) cm\(^{-2}\), a ionization parameter \(\log{\xi}=1.3\pm 0.1\) erg s\(^{-1}\) cm and a covering factor \(f\simeq90\%\). Considering a density of the absorber typical of the Broad Line Region (BLR), its distance from the central SMBH is of the order of \(r\sim 0.1\) pc. An Fe K\(\alpha\) emission line is found at 6.4 keV, whose intensity shows variability on time scales of hours. We derived that the reflecting material is located at a distance \(r\gtrsim600r_s\), where \(r_s\) is the Schwarzschild radius. Concerning the X-ray properties, we found that PKS 2251+11 does not differ significantly from the non-jetted AGNs, confirming the validity of the unified model in describing the inner regions around the central SMBH, but the lack of information regarding the state of the very innermost disk and SMBH spin still leave unconstrained the origin of the jet.