The evolution of the gas content of galaxy groups

Wilcots, Eric M.

doi:10.1002/asna.200911296

Cited by 3 publications

(2 citation statements)

References 9 publications

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“…They suggested this may be due to tidal stripping of gas from disk galaxies through interactions; rather than the result of ram pressure stripping, which occurs in clusters but is not so important in groups. Wilcots (2009) argued that galaxies falling into groups are experiencing the impact of a dense environment for the first time, and that the transformation of galaxies and the inter-galactic medium (often referred to as pre-processing) may take place in the group environment prior to infall of the group into a cluster. There is, however, a maximum group size in which such pre-processing occurs.…”

Section: Minor Mergers Versus Intergalactic Gasmentioning

confidence: 99%

Fueling Active Galactic Nuclei. Ii. Spatially Resolved Molecular Inflows and Outflows

Davies

Maciejewski

Hicks

et al. 2014

ApJ

122

166

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We analyse the 2-dimensional distribution and kinematics of the stars as well as molecular and ionised gas in the central few hundred parsecs of 5 active and 5 matched inactive galaxies. The equivalent widths of the Brγ line indicate there is no on-going star formation in their nuclei, although recent (terminated) starbursts are possible in the active galaxies. The stellar velocity fields show no signs of non-circular motions, while the 1-0 S(1) H 2 kinematics exhibit significant deviations from simple circular rotation. In the active galaxies the H 2 kinematics reveal inflow and outflow superimposed on disk rotation. Steady-state circumnuclear inflow is seen in three AGN, and hydrodynamical models indicate it can be driven by a large scale bar. In three of the five AGN, molecular outflows are spatially resolved. The outflows are oriented such that they intersect, or have an edge close to, the disk -which may be the source of molecular gas in the outflow. The relatively low speeds imply the gas will fall back onto the disk; and with moderate outflow rates, they will have only a local impact on the host galaxy. H 2 was detected in two inactive galaxies. These exhibit chaotic circumnuclear dust morphologies and have molecular structures that are counter-rotating with respect to the main gas component, which could lead to gas inflow in the near future. In our sample, all four galaxies with chaotic dust morphology in the circumnuclear region exist in moderately dense groups with 10-15 members where accretion of stripped gas can easily occur.

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Section: Minor Mergers Versus Intergalactic Gasmentioning

confidence: 99%

Fueling Active Galactic Nuclei. Ii. Spatially Resolved Molecular Inflows and Outflows

Davies

Maciejewski

Hicks

et al. 2014

ApJ

122

166

View full text Add to dashboard Cite

show abstract

“…However, the majority of present-day mETGs do not reside in clusters, but in groups ( [2]), an environment where mergers and tidal interactions determine galaxy evolution ( [12]). In fact, the evolutive trend observed in groups is quite different to the one reported in clusters: old evolved groups evidence an evolution of spirals into S0's, and of these later into ellipticals with time ( [7,1]), suggesting a possible pre-processing of galaxies in groups before falling into clusters ( [18]). So, the role played by the environment in galaxy evolution (and in particular, in the assembly of mETGs) is still unsettled.…”

Section: Introductionmentioning

confidence: 78%