Compact groups of compact galaxies. X

Baier, F. W.; Tiersch, H.

doi:10.1007/bf01006087

Cited by 13 publications

(17 citation statements)

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“…This study triggered a systematic search for this type of system. The pioneer works on Shakbazyan compact groups (Shakbazyan 1973;Baier et al 1974;Petrosian 1974Petrosian , 1978Baier & Tiersch 1975, 1976a,b, 1978, 1979 were followed by the attempt of Rose (1977) to construct a compact group catalogue, which in turn was followed by the most widely known and most frequently studied Hickson Compact Group catalogue (HCG, Hickson 1982, 1997 andreferences therein). These small systems of a few galaxies in close proximity have caused the construction of several catalogues of compact groups Appendices are available in electronic form at http://www.aanda.org…”

Section: Introductionmentioning

confidence: 99%

Where are compact groups in the local Universe?

Díaz-Giménez¹,

Zandivarez²

2015

A&A

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Aims. The purpose of this work is to perform a statistical analysis of the location of compact groups in the Universe from observational and semi-analytical points of view. Methods. We used the velocity-filtered compact group sample extracted from the Two Micron All Sky Survey for our analysis. We also used a new sample of galaxy groups identified in the 2M++ galaxy redshift catalogue as tracers of the large-scale structure. We defined a procedure to search in redshift space for compact groups that can be considered embedded in other overdense systems and applied this criterion to several possible combinations of different compact and galaxy group subsamples. We also performed similar analyses for simulated compact and galaxy groups identified in a 2M++ mock galaxy catalogue constructed from the Millennium Run Simulation I plus a semi-analytical model of galaxy formation. Results. We observed that only ∼27% of the compact groups can be considered to be embedded in larger overdense systems, that is, most of the compact groups are more likely to be isolated systems. The embedded compact groups show statistically smaller sizes and brighter surface brightnesses than non-embedded systems. No evidence was found that embedded compact groups are more likely to inhabit galaxy groups with a given virial mass or with a particular dynamical state. We found very similar results when the analysis was performed using mock compact and galaxy groups. Based on the semi-analytical studies, we predict that 70% of the embedded compact groups probably are 3D physically dense systems. Finally, real space information allowed us to reveal the bimodal behaviour of the distribution of 3D minimum distances between compact and galaxy groups. Conclusions. The location of compact groups should be carefully taken into account when comparing properties of galaxies in environments that are a priori different.

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Section: Introductionmentioning

confidence: 99%

Where are compact groups in the local Universe?

Díaz-Giménez¹,

Zandivarez²

2015

A&A

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“…They were selected on the Palomar Observatory Sky Survey (POSS) prints by visual search (Shakhbazian 1973;Baier & Tiersch 1979, and references therein). In the first list of ShCGs the groups were described as "compact groups of compact galaxies", since on the POSS E prints the images of member galaxies usually lack diffuse borders and seem to have high surface brightness.…”

Section: Introductionmentioning

confidence: 99%

Shakhbazian compact galaxy groups

Tovmassian¹,

Tiersch²,

Chavushyan³

et al. 2003

A&A

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Abstract. The results of the redshift measurements and of the detailed surface photometry in BVR of the compact group ShCG 376 are presented. The radial velocity dispersion, the virial mass, the total luminosity, the M/L ratio, and the crossing time of the group are estimated. The group consists of eight accordant redshift spiral galaxies. Four (or possibly five) of the group members have emission-line spectra. Such morphological content and the number of emission-line galaxies are very atypical for compact galaxy groups. There are signs of interaction between some members of the group. It is suggested that the irregular shape of the brightest galaxy No. 4 is probably due to interaction with other members of the group, particularly, the emission line galaxy No. 6 with a discordant redshift (∆v = 2600 km s −1 ). It is speculated that the latter galaxy may be a infalling intruder to the group.

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“…We obtained spectra of all five members of the group listed in Baier & Tiersch (1979). They all have accordant RVs with a small dispersion of ∼280 km s −1 .…”

Section: Discussionmentioning

confidence: 99%

Shakhbazian compact galaxy groups

Tovmassian¹,

Tiersch²,

Navarro³

et al. 2004

A&A

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Abstract. In 1995 we commenced a detailed spectral and photometric study of Shakhbazian compact groups. In this paper the results on groups ShCG 181, ShCG 344, ShCG 361, and ShCG 362 are presented. The redshifts of member galaxies in groups and the radial velocity dispersions, the results of the surface photometry in BVR, the profiles of the surface brightness versus semi-major axis a (or a 1/4 ) and the twisting position angle versus semi-major axis of galaxies, virial masses, luminosities and mass-to-luminosity ratios, and the crossing times of groups are given. It is shown that some members of groups are in the process of interaction. On the basis of the results obtained in this and previous works, the general properties of thirteen ShCGs are discussed.

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Compact groups of compact galaxies. X

Cited by 13 publications

References 1 publication

Where are compact groups in the local Universe?

Where are compact groups in the local Universe?

Shakhbazian compact galaxy groups

Shakhbazian compact galaxy groups

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