The ALMA Fornax Cluster Survey I: stirring and stripping of the molecular gas in cluster galaxies. (arXiv:1811.11759v1 [astro-ph.GA])

The ALMA Fornax Cluster Survey I: stirring and stripping of the molecular gas in cluster galaxies. (arXiv:1811.11759v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zabel_N/0/1/0/all/0/1">Nikki Zabel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davis_T/0/1/0/all/0/1">Timothy A. Davis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_M/0/1/0/all/0/1">Matthew W. L. Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maddox_N/0/1/0/all/0/1">Natasha Maddox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bendo_G/0/1/0/all/0/1">George J. Bendo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peletier_R/0/1/0/all/0/1">Reynier Peletier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iodice_E/0/1/0/all/0/1">Enrichetta Iodice</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baes_M/0/1/0/all/0/1">Maarten Baes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_J/0/1/0/all/0/1">Jonathan I. Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Looze_I/0/1/0/all/0/1">Ilse de Looze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gomez_H/0/1/0/all/0/1">Haley Gomez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grossi_M/0/1/0/all/0/1">Marco Grossi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kenney_J/0/1/0/all/0/1">Jeffrey D. P. Kenney</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Serra_P/0/1/0/all/0/1">Paolo Serra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Voort_F/0/1/0/all/0/1">Freeke van de Voort</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vlahakis_C/0/1/0/all/0/1">Catherine Vlahakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Young_L/0/1/0/all/0/1">Lisa M. Young</a>

We present the first results of the ALMA Fornax Cluster Survey (AlFoCS): a
complete ALMA survey of all members of the Fornax galaxy cluster that were
detected in HI or in the far infrared with Herschel. The sample consists of a
wide variety of galaxy types, ranging from giant ellipticals to spiral galaxies
and dwarfs, located in all (projected) areas of the cluster. It spans a mass
range of 10^(~8.5 – 11) M_Sun. The CO(1-0) line was targeted as a tracer for
the cold molecular gas, along with the associated 3 mm continuum. CO was
detected in 15 of the 30 galaxies observed. All 8 detected galaxies with
stellar masses below 3×10^9 M_Sun have disturbed molecular gas reservoirs, only
6 galaxies are regular/undisturbed. This implies that Fornax is still a very
active environment, having a significant impact on its members. Both detections
and non-detections occur at all projected locations in the cluster. Based on
visual inspection, and the detection of molecular gas tails in alignment with
the direction of the cluster centre, in some cases ram pressure stripping is a
possible candidate for disturbing the molecular gas morphologies and
kinematics. Derived gas fractions in almost all galaxies are lower than
expected for field objects with the same mass, especially for the galaxies with
disturbed molecular gas, with differences of sometimes more than an order of
magnitude. The detection of these disturbed molecular gas reservoirs reveals
the importance of the cluster environment for even the tightly bound molecular
gas phase.

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