Where is the neutral atomic gas in Hickson groups

By L. Verdes-Montenegro, M. Yun, B. Williams, W. Huchtmeier, A. Olmo, J. Perea. 2001

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We have analyzed the total HI contents of 72 Hickson compact groups of galaxies (HCGs) and the detailed spatial distributions and kinematics of HI within a subset of 16 groups using the high angular resolution observations obtained with the VLA in order to investigate a possible evolutionary scenario for these densest systems in the present day galaxy hierarchy. For the more homogeneous subsample of 48 groups, we found a mean HI deciency of DefHI =0 :40 0:07, which corresponds to 40% of the expected HI for the optical luminosities and morphological types of the member galaxies. The individual galaxies show larger degrees of deciency than the groups globally, DefHI =0 :62 0:09 (24% of the expected HI), due in most cases to ecient gas stripping from individual galaxies into the group environment visible in the VLA maps. The degree of deciency is found to be similar to the central galaxies of Virgo and Coma cluster, and Coma I group, in spite of the signicantly dierent characteristics (number of galaxies, velocity dispersion) of these environments. It does not seem plausible that a signicant amount of extended HI has been missed by the observations. Hence phase transformation of the atomic gas should explain the HI deciency. The groups richer in early type galaxies or more compact with larger velocity dispersions show a weak tendency to be more HI decient. The detection rate of HCGs at X-ray wavelengths is larger for HI decient groups, although the hot gas distribution and hence its origin is only known for a few cases. In the evolutionary scenario we propose, the amount of detected HI would decrease further with evolution, by continuous tidal stripping and/or heating. The H2 content also tends to be lower than expected for the galaxies in HI decient groups, this may suggest that the HI stripping by frequent tidal interaction breaks the balance between the disruption of molecular clouds by star formation and the replenishment from the ambient HI.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/d47985f7e7eb047f3b1b8717f593cfb4b250c746

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Citations in the corpus

GASP. I. Gas Stripping Phenomena in Galaxies with MUSE (2017, background): “…neutral gas in nearby galaxy clusters (e.g., Haynes et al. 1984; Cayatte et al. 1990; Kenney et al. 2004; Chung et al. 2009; Vollmer et al. 2010; Jaffé et al. 2015)and sometimes also in groups (e.g., Verdes-Montenegro et al. 2001; Rasmussen et al. 2006; Rasmussen et al. 2008; Hess & Wilcots 2013).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, background): “This idea has recently received observational (Balogh et al. 1999; Lewis et al. 2002; Verdes-Montenegro et al. 2001; Jaffé et al. 2012) and theoretical support (McGee et al. 2009; De Lucia et al. 2012).”
Galaxy ecology: groups and low-density environments in the SDSS and 2dFGRS (2003, background): “Most of the work has been restricted to compact groups (e.g. Hickson 1982; Rubin et al. 1991; Iglesias-Páramo & Vı́lchez 1999; Coziol et al. 2000; Nishiura et al. 2000; Verdes-Montenegro et al. 2001; de la Rosa et al. 2001; Kelm & Focardi 2003), which are most likely to be physically bound systems.”
AN EMPIRICAL CHARACTERIZATION OF EXTENDED COOL GAS AROUND GALAXIES USING Mg ii ABSORPTION FEATURES (2010, background): “…re-distribute cold gas to larger radii (e.g. Gunn & Gott 1972; Balogh et al. 2000; Verdes-Montenegro et al. 2001), the ’group’-galaxy subsample also presents a unique opportunity to study gas kinematics in overdense galaxy environments beyond the local universe (c.f. Verdes-Montenegro et al. 2001).”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, background): “Several studies have mapped the Hi content of galaxies in groups, and found examples of Hi-deficient galaxies (e.g. Huchtmeier 1997; Verdes-Montenegro et al. 2001; Kilborn et al. 2009).”