Compact Group selection From Redshift Surveys

Barton, Elizabeth J.; Geller, Margaret J.; Ramella, M.; Marzke, Ronald O.; Costa, L. N. da

doi:10.1086/118060

Cited by 101 publications

(187 citation statements)

References 38 publications

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“…Therefore, at least some X-rayYluminous, intermediate-redshift groups have central densities comparable to CGs. This result is consistent with the observation that many CGs at low redshift are actually associated with larger galaxy systems (Ramella et al 1994;Barton et al 1996;de Carvalho et al 1997;Ribeiro et al 1998;Tovmassian et al 2006). This is also consistent with the fact that many CGs are luminous in X-rays, although typically with lower luminosities than the groups studied here (Ponman et al 1996).…”

Section: Brightest Group Galaxiessupporting

confidence: 92%

“…As rich systems, our groups do not meet this final isolation criterion; however, a few of them do have several galaxies closely spaced in projection. The galaxies in CGs typically lie within radii of around 100 h À1 70 kpc ( Hickson 1982;Iovino 2002;Iovino et al 2003;Pompei et al 2006;Focardi & Kelm 2002;Barton et al 1996;Allam & Tucker 2000;Lee et al 2004). In column (8) of Table 4, we list the number of galaxies in each group within 100 h À1 70 kpc of the group center and with magnitudes within 3 mag of the BGG.…”

Section: Brightest Group Galaxiesmentioning

confidence: 99%

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The Evolution of Galaxies in X‐Ray–luminous Groups

Jeltema

Mulchaey

Lubin

et al. 2007

ApJ

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We investigate the galaxy populations in seven X-rayYselected, intermediate-redshift groups (0:2 < z < 0:6). Overall, the galaxy populations in these systems are similar to those in clusters at the same redshift; they have large fractions of early-type galaxies ( f e $ 70%) and small fractions of galaxies with significant star formation ( f ½O ii $ 30%). We do not observe a strong evolution in the galaxy populations from those seen in X-rayYluminous groups at low redshift. Both f e and f ½O ii are correlated with radius but do not reach the field value out to $r 500 . However, we find significant variation in the galaxy populations between groups, with some groups having fieldlike populations. Comparisons between the morphological and spectral properties of group galaxies reveal both gas-poor mergers and a population of passive spirals. Unlike low-redshift, X-rayYemitting groups, in some of these groups the brightest galaxy does not lie at the center of the X-ray emission, and in several of the groups that do have a central BGG, the BGG has multiple components. These groups appear to represent a range of evolutionary stages in the formation of the BGG. Some groups have relatively large central galaxy densities, and one group contains a string of seven bright galaxies within a radius of 200 kpc that have a lower velocity dispersion than the rest of the system. None of the central galaxies, including those with multiple components, have significant [O ii] emission. These observations support a scenario in which BGGs are formed relatively late through gas-poor mergers.

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Section: Brightest Group Galaxiessupporting

confidence: 92%

Section: Brightest Group Galaxiesmentioning

confidence: 99%

The Evolution of Galaxies in X‐Ray–luminous Groups

Jeltema

Mulchaey

Lubin

et al. 2007

ApJ

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“…Barton et al (1996) also find a similar space density for nearby CGs, 3:8 ; 10 À5 h 3 Mpc À3 . These two estimates are consistent with each other and were determined using totally different algorithms.…”

Section: The Space Density Of Our Samplesupporting

confidence: 69%

A Catalog of Distant Compact Groups Using the Digitized Second Palomar Observatory Sky Survey

et al. 2005

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In this paper we present an objectively defined catalog of 459 small, high-density groups of galaxies out to z $ 0:2 in a region of $6260 deg 2 in the northern sky derived from the Digitized Second Palomar Observatory Sky Survey. Our catalog extends down to r ¼ 19:0 and has a median redshift of z med ¼ 0:12, making it complementary to Hickson's catalog for the nearby universe (z med ¼ 0:03). The depth and angular coverage of this catalog makes it valuable for studies of the general characteristics of small groups of galaxies and how galaxies evolve in and around them. We also examine the relationship between compact groups and large-scale structure.

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“…In spite of concerns about selection biases in the Hickson catalog (Mamon 1994;Ribeiro et al 1998), it has been shown that several characteristic properties of HCG galaxies are comparable to median galaxy values (e.g., surface brightness and linear or angular diameters, Lee et al 2004, T14). One of our CGs comes from the catalog of Redshift Survey Compact Groups (RSCGs, Barton et al 1996). This RSCG is part of a larger sample selected by Walker et al (2012) to have properties similar to those of HCGs.…”

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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Compact Group selection From Redshift Surveys

Cited by 101 publications

References 38 publications

The Evolution of Galaxies in X‐Ray–luminous Groups

The Evolution of Galaxies in X‐Ray–luminous Groups

A Catalog of Distant Compact Groups Using the Digitized Second Palomar Observatory Sky Survey

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

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