A molecular absorption line survey toward the AGN of Hydra-A. (arXiv:2005.10252v1 [astro-ph.GA])

A molecular absorption line survey toward the AGN of Hydra-A. (arXiv:2005.10252v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rose_T/0/1/0/all/0/1">Tom Rose</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Edge_A/0/1/0/all/0/1">A. C. Edge</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Combes_F/0/1/0/all/0/1">F. Combes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hamer_S/0/1/0/all/0/1">S. Hamer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McNamara_B/0/1/0/all/0/1">B. R. McNamara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Russell_H/0/1/0/all/0/1">H. Russell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaspari_M/0/1/0/all/0/1">M. Gaspari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salome_P/0/1/0/all/0/1">P. Salom&#xe9;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sarazin_C/0/1/0/all/0/1">C. Sarazin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tremblay_G/0/1/0/all/0/1">G. R. Tremblay</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baum_S/0/1/0/all/0/1">S. A. Baum</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bremer_M/0/1/0/all/0/1">M. N. Bremer</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>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferland_G/0/1/0/all/0/1">G. Ferland</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nesvadba_N/0/1/0/all/0/1">N. Nesvadba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+ODea_C/0/1/0/all/0/1">C. O&#x27;Dea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oonk_J/0/1/0/all/0/1">J. B. R. Oonk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peck_A/0/1/0/all/0/1">A. B. Peck</a> ((1) Centre for Extragalactic Astronomy, Durham University)

We present Atacama Large Millimeter/submillimeter Array observations of the
brightest cluster galaxy Hydra-A, a nearby ($z=0.054$) giant elliptical galaxy
with powerful and extended radio jets. The observations reveal CO(1-0),
CO(2-1), $^{13}$CO(2-1), CN(2-1), SiO(5-4), HCO$^{+}$(1-0), HCO$^{+}$(2-1),
HCN(1-0), HCN(2-1), HNC(1-0) and H$_{2}$CO(3-2) absorption lines against the
galaxy’s bright and compact active galactic nucleus. These absorption features
are due to at least 12 individual molecular clouds which lie close to the
centre of the galaxy and have velocities of approximately $-50$ to $+10$ km/s
relative to its recession velocity, where negative values correspond to inward
motion. The absorption profiles are evidence of a clumpy interstellar medium
within brightest cluster galaxies composed of clouds with similar column
densities, velocity dispersions and excitation temperatures to those found at
radii of several kpc in the Milky Way. We also show potential variation in a
$sim 10$ km/s wide section of the absorption profile over a two year
timescale, most likely caused by relativistic motions in the hot spots of the
continuum source which change the background illumination of the absorbing
clouds.

We present Atacama Large Millimeter/submillimeter Array observations of the
brightest cluster galaxy Hydra-A, a nearby ($z=0.054$) giant elliptical galaxy
with powerful and extended radio jets. The observations reveal CO(1-0),
CO(2-1), $^{13}$CO(2-1), CN(2-1), SiO(5-4), HCO$^{+}$(1-0), HCO$^{+}$(2-1),
HCN(1-0), HCN(2-1), HNC(1-0) and H$_{2}$CO(3-2) absorption lines against the
galaxy’s bright and compact active galactic nucleus. These absorption features
are due to at least 12 individual molecular clouds which lie close to the
centre of the galaxy and have velocities of approximately $-50$ to $+10$ km/s
relative to its recession velocity, where negative values correspond to inward
motion. The absorption profiles are evidence of a clumpy interstellar medium
within brightest cluster galaxies composed of clouds with similar column
densities, velocity dispersions and excitation temperatures to those found at
radii of several kpc in the Milky Way. We also show potential variation in a
$sim 10$ km/s wide section of the absorption profile over a two year
timescale, most likely caused by relativistic motions in the hot spots of the
continuum source which change the background illumination of the absorbing
clouds.

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