Shakhbazian compact groups: Poor clusters of galaxies

Tovmassian, H. M.; Tiersch, H.

doi:10.1051/0004-6361:20011221

Cited by 11 publications

(10 citation statements)

References 43 publications

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“…However, its spectrum obtained with 6 m telescope shows that it belongs to the cluster. Tovmassian (2001) and Tovmassian & Tiersch (2001) showed that compact groups generally contain fainter objects distributed in narrow strips along the elongation of the proper group. Therefore, it is quite possible that the other faint objects in the field of A1097-ShCG 191 belong to it.…”

Section: Discussionmentioning

confidence: 99%

Spectroscopy and photometry of ShCG 191 - Abell 1097

Tovmassian

Tiersch²,

Tovmassian

et al. 2005

Astron. Nachr.

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Abstract. In the course of investigation of Shakhbazian compact groups we studied the group ShCG 191 which has been identified also as the Abell cluster A1097. By its richness it may be classified as a rich compact group or a poor cluster. We determined redshifts of 14 objects in the area of the cluster and found that two of the supposed members of the group are stars. Redshifts of 12 galaxies show that the system is gravitationally bound. The V and R magnitudes of 23 member galaxies and their morphological types are determined. We present in this paper also the surface brightness contours of member galaxies in the central area of the cluster, the curves of isophotal twisting and the Fourier parameter a4. It is shown that some galaxies in the cluster are interacting with each other. Physical parameters of the group are close to those of ShCGs.

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Section: Discussionmentioning

confidence: 99%

Spectroscopy and photometry of ShCG 191 - Abell 1097

Tovmassian

Tiersch²,

Tovmassian

et al. 2005

Astron. Nachr.

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“…Such a form of the extension may obviously be due to a tidal interaction between both galaxies. Tovmassian & Tiersch (2001) showed that ShCGs are generally embedded in loose groups, members of which are distributed along the elongation determined by the proper members of corresponding groups. Therefore, a member of a group may have a RV exceeding the limit assumed for compact groups with smaller masses.…”

Section: Discussionmentioning

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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“…It means that members of CGs and LGs move along the elongation of corresponding group. It has been shown by Tovmassian (2001aTovmassian ( , 2001b and that out of three possibilities of such movement: flying out of galaxies from the center of the group in opposite directions, infalling from opposite directions, and regular rotation of member galaxies in elongated orbits around the gravitational center of each system, the latter possibility is the more realistic one. The rotation time is less than ∼ 3 × 10 9 years, so CG+LG systems may well be virialized.…”

Section: Introductionmentioning

confidence: 99%