Powerful AGN jets and unbalanced cooling in the hot atmosphere of IC 4296. (arXiv:1903.03198v1 [astro-ph.GA])

Powerful AGN jets and unbalanced cooling in the hot atmosphere of IC 4296. (arXiv:1903.03198v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Grossova_R/0/1/0/all/0/1">R. Grossova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Werner_N/0/1/0/all/0/1">N. Werner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rajpurohit_K/0/1/0/all/0/1">K. Rajpurohit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mernier_F/0/1/0/all/0/1">F. Mernier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lakhchaura_K/0/1/0/all/0/1">K. Lakhchaura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gabanyi_K/0/1/0/all/0/1">K. Gabanyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canning_R/0/1/0/all/0/1">R. E. A. Canning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_P/0/1/0/all/0/1">P. Nulsen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Massaro_F/0/1/0/all/0/1">F. Massaro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sun_M/0/1/0/all/0/1">M. Sun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Connor_T/0/1/0/all/0/1">T. Connor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+King_A/0/1/0/all/0/1">A. King</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_S/0/1/0/all/0/1">S. W. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frisbie_R/0/1/0/all/0/1">R. Lyn-Salmon Frisbie</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Donahue_M/0/1/0/all/0/1">M. Donahue</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fabian_A/0/1/0/all/0/1">A. C. Fabian</a>

We present new Karl G. Jansky Very Large Array (VLA, 1-2 GHz) radio data of
the giant elliptical galaxy IC 4296, supported by archival radio, X-ray
(Chandra, XMM-Newton) and optical (SOAR, HST) observations. The galaxy hosts
powerful radio jets piercing through the inner hot X-ray emitting atmosphere,
depositing most of the energy into the ambient intra-cluster medium (ICM).
Whereas the radio surface brightness of the A configuration image is consistent
with a Fanaroff-Riley Class I (FR I) system, the D configuration image reveals
two large (diameter ~160 kpc), well-defined lobes (one of which is associated
with an X-ray cavity) at a projected distance r~230 kpc. The total enthalpy of
the radio lobes is $sim7times10^{59},rm{erg}$ and the mechanical power
output of the jets is $sim 10^{44},rm{erg,s}^{-1}$. The jets are mildly
curved, possibly re-brightened by the relative motion of the galaxy and the
ICM, and terminate with sharp edges, suggesting the presence of bow shocks,
which would classify this as a transitional state of a supersonic FR I radio
source. The central entropy and cooling time of the X-ray gas are unusually
low, the cooling rate is consistent with $dot{M}sim5~M_{odot}$ yr$^{-1}$,
and the nucleus hosts a warm H$alpha$+[NII] nebula and a cold molecular CO
disk. Because most of the energy of the jets is deposited far from the nucleus,
the atmosphere of the galaxy continues to cool, apparently feeding the central
supermassive black hole and powering the jet activity.

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