Catalogue of Shakhbazian compact groups of galaxies. IX

Stoll, D.; Tiersch, H.; Cordis, L.

doi:10.1002/asna.2113180206

Cited by 10 publications

(4 citation statements)

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“…A fifth galaxy, E, is also associated with this group, but its faintness did not allow us to obtain a good spectrum. This group was already known in the literature as SHK 371 (Stoll et al 1997), but its redshift was measured here for the first time. The group belongs to Class A.…”

Section: Individual Targetsmentioning

confidence: 99%

The DPOSS II compact group survey: first spectroscopically confirmed candidates

Pompei

Carvalho

Iovino

2006

A&A

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This paper presents the results of a pilot redshift survey of 18 candidate compact groups from the distant DPOSS survey that extends to redshift ∼0.2 the available surveys of compact groups of galaxies, mainly Hickson Compact Groups and Southern Compact Groups. The goal of our survey was to confirm group membership via redshift information and to measure the characteristic parameters of a representative, albeit small, sample of DPOSS survey groups. Of the 18 candidates observed, seven are found to be indeed isolated compact groups, i.e. groups with 3 or more concordant members and with no neighbouring known cluster, while 7 are chance projection configurations on the sky. Three remaining candidates, despite having 3 or more concordant member galaxies, are located in the neighbourhood of known clusters, while another candidate turned out to be a dense sub-condensation within Abell 0952. The median redshift of our 7 confirmed groups is z ∼ 0.12, to be compared with a median redshift of 0.03 for the local sample of compact groups by Hickson. The typical group size is ∼50 kpc, and the median radial velocity dispersion is 167 km s 0 , all similar to the values usually found in the literature for such structures in the local universe. The average mass-to-light ratio for our groups, M/L B , is 92h, higher than the value found for nearby Hickson compact groups but lower than that found for loose groups. Our results suggest that, once full redshift information for its members becomes available, the DPOSS sample will provide a reference sample to study the properties of compact groups beyond the local universe.

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Section: Individual Targetsmentioning

confidence: 99%

The DPOSS II compact group survey: first spectroscopically confirmed candidates

Pompei

Carvalho

Iovino

2006

A&A

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“…In the original papers the positions of groups were given with relatively low accuracy. To study the groups in detail the correct positions of member galaxies have been determined (Stoll et al 1993a(Stoll et al , 1993b(Stoll et al , 1994a(Stoll et al , 1994b(Stoll et al , 1996c(Stoll et al , 1997a(Stoll et al , 1997b(Stoll et al , 1997c.…”

Section: Introductionmentioning

confidence: 99%

Shakhbazian compact galaxy groups

Tiersch¹,

Tovmassian²,

Stoll³

et al. 2002

A&A

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Abstract. Shakhbazian compact galaxy groups belong to the interesting class of compact groups. Because of their large number (the catalogue contains 377 entries) we are able to study the groups in different stages of evolution. Here we give the results of detailed study of four groups, ShCG 154, ShCG 166, ShCG 328 and ShCG 360. We present the redshifts of individual galaxies in groups, the results of the surface photometry in BVR, the contourplots of the surface brightness versus effective radius of galaxies, the twisting postion angle versus effective radius of galaxies, the radial velocity dispersions, the crossing times, the mass-to-luminosity ratios of groups and the results of the X-ray study. The dynamical state of groups, interactions between member galaxies, and the physical parameters of groups are discussed.

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“…If a galaxy is embedded in a common halo with another galaxy, then the last undisturbed isophot The results of the photometry of the studied groups are presented in Table 1, in which the following information is given: 1, the galaxy identification number according to [26][27][28][29][30]; 2-4, the stellar magnitudes in the B, V, and R bands, respectively; 5, the axial ratio b/a; and 6, the position angle, i, of the large axis. The limiting surface brightness of galaxies with superimposed halos does not reach this value.…”

Section: Observations and Resultsmentioning

confidence: 99%

Photometric observations of nine Shakhbazian compact groups

Tovmassian

Tiersch²,

Tovmassian

et al. 2010

Astrophysics

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By observations with the 1.5m telescope at San Pedro Martir (OAN, UNAM, Mexico) the BVR magnitudes are determined for 66 member galaxies in Shakhbazian Compact Galaxy Groups ShCG 40, ShCG 176, ShCG 270, ShCG 278, ShCG 310, and ShCG 342. Three other groups were observed in two or only in oneband. Seven galaxies in ShCG 298 were observed in B and R, six galaxies in ShCG 95 were observed in V, and seven galaxies in ShCG 345 were observed in V and R. The distribution of brightness of observed galaxies is determined. Signs of interaction between galaxies are detected in some groups.

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Catalogue of Shakhbazian compact groups of galaxies. IX

Abstract: 'I'he nirieth part of t.he catalogue of Shakhbazian groups contains the positions and references of all the galaxies of the following 48 groups (north of 6 >

Cited by 10 publications

References 10 publications

The DPOSS II compact group survey: first spectroscopically confirmed candidates

The DPOSS II compact group survey: first spectroscopically confirmed candidates

Shakhbazian compact galaxy groups

Photometric observations of nine Shakhbazian compact groups

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