Characterization of the emitting and absorbing media around the nucleus of the active galaxy UGC11763 using XMM-Newton data

TL;DR

This study analyzes XMM-Newton data of UGC11763 to characterize its nuclear emission and absorption features, revealing a complex ionized environment with a soft excess, two-phase ionized absorbers, and emission lines.

Contribution

It provides a detailed spectral analysis of UGC11763, identifying a two-phase ionized absorber and soft excess, which enhances understanding of active galactic nucleus environments.

Findings

Power law with photon index 1.72 describes hard X-ray emission.

Soft excess modeled with black body at 0.1 keV.

Presence of two-phase ionized absorber in the line of sight.

Abstract

Aims. The detailed analysis of all data taken by the XMM-Newton satellite of UGC11763 to characterize the different components that are emitting and absorbing radiation in the vicinity of the active nucleus. Methods. The continuum emission was studied through the EPIC spectra taking profit of the spectral range of these cameras. The high resolution RGS spectra were analyzed in order to characterize the absorbing features and the emission line features that arise in the spectra of this source. Results. A power law with a photon index \Gamma = 1.72^{+0.03}_{-0.01} accounts for the continuum emission of this source in the hard X-rays from 10 down to 1 keV. At lower energies, a black body model with kT= 0.100\pm 0.003 keV provides a good description of the observed soft excess. The absorption signatures in the spectra of UGC11763 are consistent with the presence of a two phase ionized material (log U=1.65^{+0.07}_{-0.08}; 2.6\pm 0.1 and log N_{H} = 21.2\pm 0.2; 21.51\pm 0.01 cm^{-2}, respectively) in the line of sight. The physical conditions found are consistent with the two phases being in pressure equilibrium. The low ionization component is more ionized than typically found for warm absorbers in other Seyfert 1 galaxies. There are also signatures of some emission lines: Ovii He$\alpha$(r), Ovii He$\alpha$(f), a blend of the Neix He$\alpha$ triplet and Fexviii at \lambda 17.5 \AA.