A blind ATCA HI survey of the Fornax galaxy cluster: properties of the HI detections
arXiv:2102.01185 · doi:10.1051/0004-6361/202039803
Abstract
We present the first interferometric blind HI survey of the Fornax galaxy cluster, which covers an area of 15 deg out to the cluster . The survey has a resolution of 67''x95'' and 6.6 km with a 3 sensitivity of N(HI)~2x10 cm and MHI 2x10 M. We detect 16 galaxies out of 200 spectroscopically confirmed Fornax cluster members. The detections cover ~3 orders of magnitude in HI mass, from 8x10 to 1.5x10 M. They avoid the central, virialised region of the cluster both on the sky and in projected phase-space, showing that they are recent arrivals and that, in Fornax, HI is lost within a crossing time, ~2 Gyr. Half of these galaxies exhibit a disturbed HI morphology, including several cases of asymmetries, tails, offsets between HI and optical centres, and a case of a truncated HI disc suggesting that they have been interacting within or on their way to Fornax. Our HI detections are HI-poorer and form stars at a lower rate than non-cluster galaxies in the same range. Low mass galaxies are more strongly affected throughout their infall towards the cluster. The MHI/ ratio of Fornax galaxies is comparable to that in the Virgo cluster. At fixed , our HI detections follow the non-cluster relation between MHI and the star formation rate, and we argue that this implies that so far they have lost their HI on a timescale 1-2 Gyr. Deeper inside the cluster HI removal is likely to proceed faster, as confirmed by a population of HI-undetected but H-detected star-forming galaxies. Based on ALMA data, we find a large scatter in H-to-HI mass ratio, with several galaxies showing an unusually high ratio that is probably caused by faster HI removal. We identify an HI-rich subgroup of possible interacting galaxies dominated by NGC 1365, where pre-processing is likey to have taken place.
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