Chandra View of the LINER-type Nucleus in the Radio-loud Galaxy CGCG 292-057: Ionized Iron Line and Jet-ISM Interactions
Abstract
We present an analysis of the new, deep (94 ksec) Chandra ACIS-S observation of radio-loud active galaxy CGCG 292-057, characterized by a LINER-type nucleus and a complex radio structure that indicates intermittent jet activity. On the scale of the host galaxy bulge, we detected excess X-ray emission with a spectrum best fit by a thermal plasma model with a temperature of ∼0.8 keV. We argue that this excess emission results from compression and heating of the hot diffuse fraction of the interstellar medium displaced by the expanding inner, ∼20 kpc-scale lobes observed in this restarted radio galaxy. The nuclear X-ray spectrum of the target clearly displays an ionized iron line at ∼6.7 keV, and is best fitted with a phenomenological model consisting of a power-law (photon index ≃ 1.8) continuum absorbed by a relatively large amount of cold matter (hydrogen column density ≃0.7 × 1023 cm-2), and partly scattered (fraction ∼3%) by ionized gas, giving rise to a soft excess component and Kα line from iron ions. We demonstrate that the observed X-ray spectrum, particularly the equivalent width of Fe XXV Kα (of order 0.3 keV) can in principle, be explained in a scenario involving a Compton-thin gas located at the scale of the broad-lined region in this source and photoionized by nuclear illumination. We compare the general spectral properties of the CGCG 292-057 nucleus, with those of other nearby LINERs studied in X-rays.
- Publication:
-
The Astrophysical Journal
- Pub Date:
- December 2020
- DOI:
- 10.3847/1538-4357/abc4e2
- arXiv:
- arXiv:2006.03717
- Bibcode:
- 2020ApJ...905..148B
- Keywords:
-
- X-ray active galactic nuclei;
- Low-luminosity active galactic nuclei;
- Active galaxies;
- Relativistic jets;
- Intergalactic medium;
- LINER galaxies;
- Radio galaxies;
- 2035;
- 2033;
- 17;
- 1390;
- 813;
- 925;
- 1343;
- Astrophysics - High Energy Astrophysical Phenomena
- E-Print:
- revised version, accepted for publication in the Astrophysical Journal