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Date and Time of the Query: 2019-06-17 T22:08:45 PDT
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Notes for object Seyfert's Sextet

8 note(s) found in NED.


1. 1996A&AS..117...39A
Re:HCG 079
Hickson 79 - Known also as Seyfert Sextet (VV 115), it is also the most compact
among Hickson's list. Hickson(1993b) attributes FIR emission to galaxy a only
(it is also a radio source). Unresolved.

2. 1995ApJ...443..514P
Re:HCG 079
HCG 79.-This group is better known as Seyfert's Sextet. Since it is a
very dense, elliptical-rich group, it might well be expected to be a
strong source of X-ray emission; unfortunately, the usable time for this
observation was so short (4.9 Ks) that there were not enough photons
detected to perform any spectral analysis. In addition, the galaxies in
the group are too close together to be individually resolved with the
PSPC even if the observation time were sufficiently long.

3. 1993AJ....105.1291B
Re:HCG 079
H 79
This group is the well-known Seyfert's Sextet (Seyfert 1951). It is
extremely interesting from the morphological point of view since it
contains galaxies which seem to experience different merging stages.
Galaxy a shows a strong major axis dust lane (see, also, Sulentic & Lorre
1983) which is probably responsible for the boxiness observed in the
inner isophotes. A bridge of matter connects this galaxy with the spiral
d, which shows the above noted "erosion" of the disk toward the big
companion. Galaxies b, b1, and c form an interacting chain. In
particular, the morphology of b1 suggests that this object is going to be
destroyed by the interaction with the galaxy b. This last galaxy is also
in close interaction with galaxy c which is characterized by strong
boxiness in the external isophotes. We classify galaxies b and c as SOs
in agreement with HKA89.
By using the UMT we were able to detect clearly the spiral structure of
galaxy e, which is a well-known case of extremely discrepant redshift
(Burbidge & Sargent 1971).

4. 1985AnTok..202.237T
Re:KUG 1556+208
Within Seyfert's Sextet the southern-most component is bluest,
the northern three components are fairly blue, while the other
two are rather red.

5. 1973UGC...C...0000N
Re:UGC 10116
VV 115, VII Zw 631
NGC 6027 0.35 x 0.18
a) (0.6 x 0.4)
b) 0.35 x 0.15
c) 0.8 x 0.15
d) 0.18 x 0.18
NGC 6027 + e) 1.0 x 0.3
(Designations from Seyfert, see P.A.S.P. 63, 72)
e) is not certainly a separate galaxy
CGCG magnitude for NGC 6027 14.7, "bar-like compact"
a) 15.1, "fuzzy E"
b) 15.3, "patchy compact"
c) 15.6, "spherical compact"
d) 16.0, "SBc"
e) 16.5, "irregular"
V = 4468, 4141, 4430, 4581 and 19930 (see O'Connell (Ed.), "Nuclei of
Galaxies", Pontificiae Academiae Scientiarum 1971), note discordant redshift
for d)

6. 1971CGPG..C...0000Z
Re:CGPG 1557.0+2055
VII Zw 631
NGC 6027
Seyfert's group of six neutral galaxies,
Total m(pg) = 13.4 [CGCG]
No. 1
Patchy compact.
m(pg) = 15.3
No. 2
Fuzzy.
m(pg) = 15.1
No. 3
SBc
m(pg) = 16.0
No. 4
Bar-like compact.
m(pg) = 14.7
No. 5
Spherical compact.
m(pg) = 15.6
No. 6
Irregular.
= +4,237 km/sec.
m(pg) = 16.5

7. 1959VV....C...0000V
Re:VV 115
= Seyfert's Group (including NGC 6027)
His stellar magnitude.
Left photograph is from Baade (Publ. A.S.P., 63, 72, 1951)

8. 1959VV....C...0000V
Re:VV 115
The whole group is in a common haze, proving that it
is not a chance projection as was assumed by Baade.


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