An enormous molecular gas flow in the RXJ0821+0752 galaxy cluster. (arXiv:1811.09653v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vantyghem_A/0/1/0/all/0/1">A. N. Vantyghem</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. R. Russell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edge_A/0/1/0/all/0/1">A. C. Edge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nulsen_P/0/1/0/all/0/1">P. E. J. Nulsen</a>, <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:+Fabian_A/0/1/0/all/0/1">A. C. Fabian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDonald_M/0/1/0/all/0/1">M. McDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salome_P/0/1/0/all/0/1">P. Salome</a>
We present recent {it Chandra} X-ray observations of the RXJ0821.0+0752
galaxy cluster in addition to ALMA observations of the CO(1-0) and CO(3-2) line
emission tracing the molecular gas in its central galaxy. All of the CO line
emission, originating from a $10^{10},M_{odot}$ molecular gas reservoir, is
located several kpc away from the nucleus of the central galaxy. The cold gas
is concentrated into two main clumps surrounded by a diffuse envelope. They
form a wide filament coincident with a plume of bright X-ray emission emanating
from the cluster core. This plume encompasses a putative X-ray cavity that is
only large enough to have uplifted a few percent of the molecular gas. Unlike
other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift
low entropy cluster gas until it becomes thermally unstable, cannot have
produced the observed gas reservoir. Instead, the molecular gas has likely
formed as a result of sloshing motions in the intracluster medium induced by a
nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic
center. This gas has the shortest cooling time, so will condense if disrupted
for long enough.
We present recent {it Chandra} X-ray observations of the RXJ0821.0+0752
galaxy cluster in addition to ALMA observations of the CO(1-0) and CO(3-2) line
emission tracing the molecular gas in its central galaxy. All of the CO line
emission, originating from a $10^{10},M_{odot}$ molecular gas reservoir, is
located several kpc away from the nucleus of the central galaxy. The cold gas
is concentrated into two main clumps surrounded by a diffuse envelope. They
form a wide filament coincident with a plume of bright X-ray emission emanating
from the cluster core. This plume encompasses a putative X-ray cavity that is
only large enough to have uplifted a few percent of the molecular gas. Unlike
other brightest cluster galaxies, stimulated cooling, where X-ray cavities lift
low entropy cluster gas until it becomes thermally unstable, cannot have
produced the observed gas reservoir. Instead, the molecular gas has likely
formed as a result of sloshing motions in the intracluster medium induced by a
nearby galaxy. Sloshing can emulate uplift by dislodging gas from the galactic
center. This gas has the shortest cooling time, so will condense if disrupted
for long enough.
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