Chandra View of the LINER-type Nucleus in the Radio-Loud Galaxy CGCG 292-057: Ionized Iron Line and Jet-ISM Interactions. (arXiv:2006.03717v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Balasubramaniam_K/0/1/0/all/0/1">K. Balasubramaniam</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Stawarz_L/0/1/0/all/0/1">L. Stawarz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marchenko_V/0/1/0/all/0/1">V. Marchenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sobolewska_M/0/1/0/all/0/1">M. Sobolewska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cheung_C/0/1/0/all/0/1">C.C. Cheung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siemiginowska_A/0/1/0/all/0/1">A. Siemiginowska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thimmappa_R/0/1/0/all/0/1">R. Thimmappa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kosmaczewski_E/0/1/0/all/0/1">E. Kosmaczewski</a>
We present an analysis of the new, deep (94,ksec) {it 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 $sim 0.8$,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, $sim 20$, kpc-scale lobes observed in this restarted
radio galaxy. The nuclear X-ray spectrum of the target clearly displays an
ionized iron line at $sim 6.7$,keV, and is best fitted with a
phenomenological model consisting of a power-law (photon index $simeq 1.8$)
continuum absorbed by a relatively large amount of cold matter (hydrogen column
density $simeq 0.7 times 10^{23}$,cm$^{-2}$), and partly scattered (fraction
$sim 3%$) by ionized gas, giving rise to a soft excess component and
K$alpha$ line from iron ions. We demonstrate that the observed X-ray spectrum,
particularly the equivalent width of Fe,texttt{XXV} K$alpha$ (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$-$057 nucleus, with those of other nearby LINERs
studied in X-rays.
We present an analysis of the new, deep (94,ksec) {it Chandra} ACIS-S
observation of radio-loud active galaxy CGCG,292$-$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 $sim 0.8$,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, $sim 20$, kpc-scale lobes observed in this restarted
radio galaxy. The nuclear X-ray spectrum of the target clearly displays an
ionized iron line at $sim 6.7$,keV, and is best fitted with a
phenomenological model consisting of a power-law (photon index $simeq 1.8$)
continuum absorbed by a relatively large amount of cold matter (hydrogen column
density $simeq 0.7 times 10^{23}$,cm$^{-2}$), and partly scattered (fraction
$sim 3%$) by ionized gas, giving rise to a soft excess component and
K$alpha$ line from iron ions. We demonstrate that the observed X-ray spectrum,
particularly the equivalent width of Fe,texttt{XXV} K$alpha$ (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.
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