Far-infrared emission from Shakhbazian Compact Galaxy Groups

Tovmassian, H. M.; Mazzarella, J. M.; Tovmassian, G.; Stoll, D.; Tiersch, H.

doi:10.1051/aas:1998225

Cited by 16 publications

(22 citation statements)

References 35 publications

(49 reference statements)

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“…The spiral arms, if any, are apparently distorted. This galaxy has also FIR (Tovmassian et al 1998) and radio emission (Tovmassian et al 1999). Its luminosity at 1.4 GHz is 1.1 × 10 43 erg s −1 .…”

Section: Discussionmentioning

confidence: 99%

“…In many ShCGs the space density reaches Send offprint requests to: H. M. Tovmassian, e-mail: hrant@inaoep.mx the values of about 10 4 −10 5 galaxies per Mpc 3 . However, since these groups are, on average, at least three times farther than HCGs (Tiersch et al 1996;Tovmassian et al 1998), and member galaxies are sufficiently faint, only a few of them have been investigated in detail until recently. About two dozen ShCGs have been observed spectroscopically (Robinson & Wampler 1973;Arp et al 1973;Mirzoyan et al 1975;Kirshner & Malamuth 1980;Amirkhanian 1989;Kodaira et al 1988Kodaira et al , 1990Kodaira & Sekiguchi 1991;Lynds et al 1990;del Olmo & Moles 1991).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Shakhbazian compact galaxy groups

Tovmassian¹,

Tiersch²,

Chavushyan³

et al. 2003

A&A

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“…These clusters contain a combined total of 64 O-type stars including one of the most massive and spectacular stars known, η Car (Feinstein 1995). Located at a distance of 2.2 kpc (Tovmassian 1995), the Carina Nebula is an excellent region in which to study the effect massive stars have on their natal GMC.…”

Section: Introductionmentioning

confidence: 99%

The giant pillars of the Carina Nebula

Rathborne

Brooks

Burton

et al. 2004

A&A

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Abstract.Results are presented from a multi-wavelength study of the giant pillars within the Carina Nebula. Using near-IR data from 2MASS, mid-IR data from MSX, 843 MHz radio continuum maps from the MOST and molecular line and continuum observations from the SEST, we investigate the nature of the pillars and search for evidence of ongoing star formation within them. Photodissociation regions (PDRs) exist across the whole nebula and trace the giant pillars, as well as many ridges, filaments and condensations (A v > 7 mag). Morphological similarities between emission features at 21 µm and 843 MHz adjacent to the PDRs, suggests that the molecular material has been carved by the intense stellar winds and UV radiation from the nearby massive stars. In addition, star forming cores are found at the tips of several of the pillars. Using a stellar density distribution, several candidate embedded clusters are also found. One is clearly seen in the 2MASS images and is located within a dense core (G287.84-0.82). A search for massive young stellar objects and compact H II regions using mid-IR colour criteria, reveal twelve candidates across the complex. Grey-body fits to SEDs for four of these objects are suggestive of OB-stars. We find that massive star formation in the Carina Nebula is occurring across the whole complex and confirm it has been continuous over the past 3 Myrs.

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“…• 25 20.0 (Tovmassian et al 1998). Another infrared source, IRAS F14234+4729, at ≈30 north-west from the center of the group may probably be associated with either member.…”

Section: Discussionmentioning

confidence: 98%

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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Far-infrared emission from Shakhbazian Compact Galaxy Groups

Cited by 16 publications

References 35 publications

Shakhbazian compact galaxy groups

Shakhbazian compact galaxy groups

The giant pillars of the Carina Nebula

Shakhbazian compact galaxy groups

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