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Date and Time of the Query: 2019-07-23 T17:16:59 PDT
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Notes for object VV 698

4 note(s) found in NED.


1. 2007AJ....134.1522J
Re:HCG 090
The SEDs for the galaxies in HCG 90 are shown in Figure 26. This group is
classified as type III according to log(M_dyn_)/ log(M_HI_), indicating that the
group is relatively gas-poor. Ribeiro et al. (1998) identify HCG 90 as being
part of a loose group. Due to the close interaction between galaxies B and D,
they were not separable at low contour levels and their photometry was combined
into a single data point. Galaxy D fell off the detector in the 24 micron
observations, and is therefore lacking this data point. Galaxy A (NGC 7172) is
somewhat disturbed and has clumpy infrared emission throughout the galaxy.
Galaxies B (NGC 7176) and C (NGC 7173) are dominated by stellar light, with
little evidence for recent activity. Galaxy D (NGC 7174) is fairly disturbed,
with a spur of infrared emission originating from its western edge. The nuclear
region of galaxy D is also a luminous 24 micron source. These results are
consistent with the kinematic H{alpha} observations of Plana et al. (1998), who
conclude that galaxy D is a warm-gas reservoir in the group. Galaxies A and D
have been identified as active galaxies by Coziol et al. (1998) and these are
the outlying type III galaxies in Figures 11-13.

2. 1996A&AS..117...39A
Re:HCG 090
Hickson 90 - Strongly interacting system. Galaxy a is well resolved in all four
IRAS bands. A second FIR source coincides with galaxies b, c and d. Since
detailed multiband CCD photometry shows no signs of cold dust in galaxies b and
c, the FIR emission very likely originates from galaxy d (i.e. NGC 7174: a late
type spiral heavily disrupted by the ongoing interaction with galaxy c, namely
NGC 7173) only.

3. 1994A&A...282..418L
Re:HCG 090
The Hickson group No. 90
Hickson group 90 (known also as Klemola 34) is a Southern compact group
formed by four bright galaxies, all NGC objects: two early-type galaxies
NGC 7173 and NGC 7176, the early-type spiral NGC 7172. and the late-type
spiral NGC 7174. The most relevant data for these galaxies are given in
Table 1. The average brightness of the group is 22.1 mag arcsec^-2^ and
only 15 groups in Hickson's list are more compact.
The detailed deep photometric study presented in Paper II shows that
all four galaxies in the group are, at different degrees, perturbed (see
also Sharples et al. 1984): the galaxies are embedded into an extended,
strongly distorted envelope and display the whole repertory of faint
tails, archs, bridges which is typical of interacting systems. The group
was first studied by Rubin (1974), who obtained low dispersion spectra
for all the members of the group and suggested the existence of possible
links with another nearby chain of galaxies (NGC 7201-7203-7204). The
fact that Hickson 90 may belong to a more extended and looser group has
been confirmed by two recently published catalogues of nearby groups and
associations (Maia et al. 1989; Fouque et al. 1992) and by Vennik et al.
(1992).
The observed angular diameter of Hickson 90 is 7.4 arcmin. and its
distance, obtained independently from surface brightness fluctuations
(Capaccioli et al. 1993) and from the matching of the globular cluster
luminosity function is (Grimaldi et al. 1992) 28.2+/-2.0 Mpc.

4. 1969AJ.....74..804K
Re:KLEMOLA 34
Object 34. Four bright galaxies but no fainter members in group.
Probably unrelated to group are five or six considerably fainter
galaxies one-third degree to the East. Northern member of main group is
spiral (magnitude 13) with well-defined absorbing lanes. To the South is
spiral (magnitude 13) and elliptical (magnitude 12), which appear
interconnected possibly by an arm. Middle member of group is elliptical
of magnitude 12.


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