Photometric catalogue of Shakhbazian compact groups of galaxies. II

Stoll, D.; Tiersch, H.; Oleak, H.; Baier, F. W.; MacGillivray, H. T.

doi:10.1002/asna.2113140502

Cited by 15 publications

(4 citation statements)

References 5 publications

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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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Section: Introductionmentioning

confidence: 99%

Shakhbazian compact galaxy groups

Tiersch¹,

Tovmassian²,

Stoll³

et al. 2002

A&A

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“…214 SHK groups lie in the sky area covered by the SDSS DR5. Among these 214 groups, we selected those for which a first order estimate of the distance was possible, averaging either spectroscopic redshifts from literature or spectroscopic redshifts available in the SDSS DR5, for all galaxies contained in the catalogue by (Stoll et al 1993a,b,; Stoll, Tiersch & Braun 1996a,b,c; Stoll, Tiersch & Cordes 1997a; Stoll, Tiersch & Braun 1997b; Stoll, Tiersch & Cordis 1997c). 2 The same process has been used to derive the centroids of the groups using the coordinates of the single galaxies in the catalogue by Stoll et al…”

Section: The Datamentioning

confidence: 99%

The properties of the heterogeneous Shakhbazyan groups of galaxies in the SDSS

Capozzi

Filippis

Paolillo

et al. 2009

Monthly Notices of the Royal Astronomical Society

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We present a systematic study of the subsample of Shakhbazyan (SHK) groups covered by the Sloan Digital Sky Survey Data Release 5 (SDSS DR5). SHK groups probe an environment with characteristics which are intermediate between those of loose and very compact groups. Surprisingly, we found that several groups identifying algorithms, e. g. Berlind et al. and Tago et al., miss this type of structures. Using the SDSS DR5 spectroscopic data and the photometric redshifts derived in D'Abrusco et al., we identified possible group members in photometric redshift space and derived, for each group, several individual properties (richness, size, mean photometric redshift, fraction of red galaxies, etc.). We also combined pointed and stacked Rosat All Sky Survey (RASS) data to investigate the X-ray luminosities of these systems. Our study confirms that the majority of groups are physical entities with richness in the range 3-13 galaxies, and properties ranging between those of loose and compact groups. We confirm that SHK groups are richer in early-type galaxies than the surrounding environment and the field, as expected from the morphology - density relation and from the selection of groups of red galaxies. Furthermore, our work supports the existence of two subclasses of structures, the first one being formed by compact and isolated groups and the second formed by extended structures. We suggest that while the first class of objects dwells in less dense regions like the outer parts of clusters or the field, possibly sharing the properties of Hickson Compact Groups, the more extended structures represent a mixture of [core + halo] configurations and cores of rich clusters. X-ray luminosities for SHK groups are generally consistent with these results and with the expectations for the L(X)-sigma(v) relation, but also suggest the velocity dispersions reported in literature are underestimated for some of the richest systems

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“…Each image is a superposition of three frames (of one 20 min and two min exposures). The galaxy identification numbers are given from Stoll et al (1993), Stoll, Tiersch, & Braun (1996) 7 . The images were processed with the MIDAS image processing package.…”

Section: Direct Imaging and Photometrymentioning

confidence: 99%