Dynamical properties of compact groups of galaxies

Hickson, Paul; Oliveira, C. Mendes de; Huchra, J. P.; Palumbo, G. G. C.

doi:10.1086/171932

Cited by 324 publications

(601 citation statements)

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“…This appears to contrast to the fact that galaxies in compact groups do experience more interactions from their close neighbors, either major or minor mergers, than a single galaxy by its companion. A possible explanation could be that the higher velocity dispersion of compact groups (∼330 km s −1 , Hickson et al 1992), compared to typical values seen in near parabolic prograde encounters of galaxy pairs, reduces the gravitational Fig. 7.…”

Section: Star Formation Activity In Hickson Compact Groupsmentioning

confidence: 96%

A mid-IR study of Hickson compact groups

Bitsakis¹,

Charmandaris

Floc’h

et al. 2010

A&A

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Hickson compact groups (HCGs) are among the densest galaxy environments of the local universe. To examine the effects of the environment on the infrared properties of these systems, we present an analysis of Spitzer and ISO mid-infrared imaging, as well as of deep ground-based near-infrared imaging of 14 HCGs containing a total of 69 galaxies. Based on mid-infrared color diagnostics we identify the galaxies that appear to host an active nucleus, while using a suite of templates, and fit the complete infrared spectral energy distribution for each group member. We compare our estimates of galaxy mass, star formation rate, total infrared luminosities, and specific star formation rates (sSFR) for our HCG sample to samples of isolated galaxies and interacting pairs and find that overall there is no discernible difference among them. However, HCGs that can be considered as dynamically "old" host late-type galaxies with a slightly lower sSFR than the one found in dynamically "young" groups. This could be attributed to multiple past interactions among the galaxies in old groups, that have led to the build up of their stellar mass. It is also consistent with our prediction of the presence of diffuse cold dust in the intergalactic medium of 9 of the dynamically "old" groups.

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Section: Star Formation Activity In Hickson Compact Groupsmentioning

confidence: 96%

A mid-IR study of Hickson compact groups

Bitsakis¹,

Charmandaris

Floc’h

et al. 2010

A&A

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“…The majority of the CGs analyzed here are from the catalog of 92 CGs that have been spectroscopically confirmed by Hickson et al (1992). As in Tzanavaris et al (2010) and Tzanavaris et al (2014) the selection criteria for this sample aimed to allow observations with a range of telescopes and instruments, both space and ground-based.…”

Section: Sample Selectionmentioning

confidence: 99%

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Tzanavaris

Hornschemeier²,

Gallagher

et al. 2016

ApJ

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We obtain total galaxy X-ray luminosities, L X , originating from individually detected point sources in a sample of 47 galaxies in 15 compact groups of galaxies (CGs). For the great majority of our galaxies, we find that the detected point sources most likely are local to their associated galaxy, and are thus extragalactic X-ray binaries (XRBs) or nuclear active galactic nuclei (AGNs). For spiral and irregular galaxies, we find that, after accounting for AGNs and nuclear sources, most CG galaxies are either within the ±1σ scatter of the Mineo et al. L X -star formation rate (SFR) correlation or have higher L X than predicted by this correlation for their SFR. We discuss how these "excesses" may be due to low metallicities and high interaction levels. For elliptical and S0 galaxies, after accounting for AGNs and nuclear sources, most CG galaxies are consistent with the Boroson et al. L X -stellar mass correlation for low-mass XRBs, with larger scatter, likely due to residual effects such as AGN activity or hot gas. Assuming non-nuclear sources are low-or high-mass XRBs, we use appropriate XRB luminosity functions to estimate the probability that stochastic effects can lead to such extreme L X values. We find that, although stochastic effects do not in general appear to be important, for some galaxies there is a significant probability that high L X values can be observed due to strong XRB variability.

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“…With the aim of comparing the approach of identifying galaxy groups using catalogues of UV emitting galaxies with the approach of searching groups in catalogues of optically and near-infrared selected galaxies, we apply the same methodology described in this work over the sample of group galaxies from the HCG catalogue (Hickson et al 1992) consisting of 463 galaxies. We take the HCG sample as the prototype of the optically or near-infrared selected group samples, assuming that similar results should be expected for others (e.g.…”

Section: Results From An Ultraviolet Search Over the Galaxy Cataloguementioning

confidence: 99%

“…Section 2 describes the selection of a sample of this type, starting from catalogues of pure UV sources and also presents the final sample including observational information and basic properties. In Section 3, several aspects of the SFCG sample are analyzed and compared with three other prototypical compact group samples: the optically-selected Hickson Compact Group (HCG, Hickson 1982;Hickson et al 1992) sample, the near-infraredselected and velocity-filtered 2MASS Compact Group (2MCG, Díaz-Giménez et al 2012) sample and the catalogue A of compact groups selected in the Sloan Digital Sky Survey by McConnachie et al (SCGA, 2009). Section 4 places the SFCG sample in the context of the Local Universe providing additional information about their galaxy members, cluster and group counterparts and also, the close surroundings of its groups.…”

Section: Introductionmentioning

confidence: 99%

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Star-forming compact groups (SFCGs): an ultraviolet search for a local sample

Hernández-Fernández

Oliveira

2015

Mon. Not. R. Astron. Soc.

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We present a local sample (z<0.15) of 280 Star-Forming Compact Groups (SFCGs) of galaxies identified in the ultraviolet Galaxy Evolution EXplorer (GALEX) All-sky Imaging Survey (AIS). So far, just one prototypical example of SFCG, the Blue Infalling Group, has been studied in detail in the Local Universe. The sample of SFCGs is mainly the result of applying a Friendsof-Friends group finder in the space of celestial coordinates with a maximum linking-length of 1.5 arcmin and choosing groups with a minimum number of four members of bright UV-emitting 17

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Dynamical properties of compact groups of galaxies

Cited by 324 publications

References 0 publications

A mid-IR study of Hickson compact groups

A mid-IR study of Hickson compact groups

Exploring X-Ray Binary Populations in Compact Group Galaxies With Chandra

Star-forming compact groups (SFCGs): an ultraviolet search for a local sample

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