Catalogue of Shakhbazian compact groups of galaxies. V.

Stoll, D.; Tiersch, H.; Braun, M.

doi:10.1002/asna.2113170403

Cited by 16 publications

(11 citation statements)

References 15 publications

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“…The coordinates of the centers of the studied groups given in Table 1 are taken from Stoll et al (1996). In the last column of Table 1 the Galactic extinction in R (taken from the NED, Schlegel et al 1998) is given.…”

Section: Observations and Resultsmentioning

confidence: 99%

“…According to the original list (Shakhbazian 1973;Stoll et al 1996) the group consists of seven galaxies. Spectral observations revealed, however, that one of the supposed members of this group, No.…”

Section: Discussionmentioning

confidence: 99%

“…Spectral observations showed that galaxy No. 7 located at about 1.5 to the south of the group and not included in the original list (Shakhbazian 1973;Stoll et al 1996) belongs to the group, so that the group consists of seven accordant redshift members. Though the group is a sufficiently dense one, the isophotes (Fig.…”

Section: Discussionmentioning

confidence: 99%

“…The latter are chosen arbitrarily to reveal possible signs of interaction between member galaxies. The units of isophotes for each group are given in corresponding figure captions, where the galaxy identification numbers are from Stoll et al (1996). Magnitudes are calibrated in the Kron-Cousins photometric system, and the star cluster NGC 4147 served as a standard.…”

Section: Direct Imaging and Photometrymentioning

confidence: 99%

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Shakhbazian compact galaxy groups

Tovmassian

Tiersch²,

Chavushyan

et al. 2005

A&A

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Abstract. We present the results of a detailed spectroscopic and photometric study of four Shakhbazian compact groups: ShCG 8, ShCG 14, ShCG 19, and ShCG 22. We determined the redshifts of member galaxies and radial velocity dispersions of groups. We also studied the distribution of the surface brightness of member galaxies in R and determined their morphological types. The profiles of the surface brightness versus semi-major axis, the curves of isophotal twisting, and Fourier parameter a 4 are constructed. We found that some members of groups are in the process of interaction. We determined physical parameters of groups: virial masses, luminosities, mass-to-luminosity ratios, and the crossing times. On the basis of the results obtained in this and our previous works, the general properties of 22 ShCGs are discussed.Key words. galaxies: clusters: general -galaxies: distances and redshifts -galaxies: interactions -galaxies: generalgalaxies: kinematics and dynamics -galaxies: photometry IntroductionIn 1995 we commenced a spectroscopic and detailed photometric study of Shakhbazian compact groups (ShCGs). The list of ShCGs contains 377 groups (Shakhbazian 1973;Petrosian 1974Petrosian , 1978Baier et al. 1974;Baier & Tiersch 1975, 1976a, 1976b, 1978, 1979. ShCGs were found by an eye inspection of the POSS prints. They were selected as dense groups of mainly red galaxies, the images of many of which were often hard to distinguish from those of stars. Through follow-up spectral observations (Tiersch et al. 2002, hereafter Paper I;Tovmassian et al. 2003a, hereafter Paper II, 2003b, hereafter Paper III, 2004a, hereafter Paper IV, 2004b, hereafter Paper V) it was found that some objects in the area of groups which were assumed in original papers to be stars, are in reality galaxies. On the other hand, only a Figures 1 and 3-10 are only available in electronic form at http://www.edpsciences.org few assumed members of ShCGs turned out to be stars. Hence, the great majority of the assumed members of these groups are galaxies.Many ShCGs, like ShCG 19 and ShCG 38 (Fig. 1), are very dense formations. Probably due to the compactness of images of the member galaxies, which on the POSS prints are almost indistinguishable from those of stars, these two groups and also some others were missed in other compact group lists, e.g. HCG list (1982). ShCGs generally consist of up to 15 members, while the distances between member galaxies are typically 3−5 times their diameters. The space density of many of ShCGs reaches about 10 4 −10 5 galaxies per Mpc 3 . The groups have a "cigar"-like, prolate spheroid configuration (Oleak et al. 1995). Numerical N-body simulations have showen that compact groups should undergo fast dynamical evolution, which will result in coalescence of member galaxies to one giant elliptical galaxy (Barnes 1985(Barnes , 1989Mamon 1986;Bode et al. 1993). It means that processes of dynamical Article published by EDP Sciences and available at http://www.edpsciences.org/aa or http://dx

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Section: Observations and Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Direct Imaging and Photometrymentioning

confidence: 99%

See 2 more Smart Citations

Shakhbazian compact galaxy groups

Tovmassian

Tiersch²,

Chavushyan

et al. 2005

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…-VIII." (Stoll et al 1993a(Stoll et al , 1993b(Stoll et al , 1994a(Stoll et al , 1994b(Stoll et al , 1996a(Stoll et al , 1996b(Stoll et al , 1996c.…”

Section: Introductionmentioning

confidence: 99%