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Notes for object NGC 3842

7 note(s) found in NED.


1. 2010A&A...516A...1L
Re:NGC 3842
3C 264 and NGC 3842 in Abell 1367. A 1367 is an X-ray-faint and nearby
(z=0.0215) galaxy cluster. It has a secondary peak in its X-ray brightness
(Donnelly et al. 1998) located approximately 19' offset from the primary
brightness peak. This cluster is peculiar having extended trails of radio
emission behind three irregular galaxies in its periphery (Gavazzi & Jaffe
1987). It is a complex cluster currently forming at the intersection of two
filaments. NCG 3842 and NGC 3862 are its two Brightest Cluster Galaxies.
NGC 3842 is a cD galaxy, which was studied in radio band by Feretti &
Giovannini (1994). From high resolution VLA radio images, NGC 3842 exhibits a
small size WAT structure with angular size of ~55 arcsec and a flux density of
10.5 mJy corresponding to a total power at 1.4 GHz Log P_t,1.4 GHz_ = 21.72
W/Hz. In our images, it appears to be undetected above 5{sigma} (>0.7 mJy/beam).
NGC3862 is associated with the strong radio source 3C 264. In VLA images, it
has a total power of Log P=24.97 (W/Hz). On kiloparsec scales, 3C 264 has a
head-tailed morphology, prominent core, and a wiggling jet extending toward the
northeast that ends in a blob of emission at 28 arcsec (11.5 kpc) from the core
(Lara et al. 1997). There is evidence of counterjet emission in the southwest
direction from the core. Both the jet and counterjet are embedded in a vast and
diffuse region of low surface brightness emission, which seems to have been
dragged toward the north, possibly revealing the existence of a high density
intracluster medium. Simultaneous EVN and MERLIN observations at 5.0 GHz by Lara
et al. (1999); Baum et al. (1997) showed for the first time the detailed
structure of 3C 264 on sub-kiloparsec scales. It consists of a one-sided jet
with evident variations in its morphological properties with distance: i) the
strong core and innermost jet (0-10 pc); ii) a well-collimated and narrow region
(10-10 0 pc); iii) a region with strong widening, kinks, and filaments (100-300
pc); and iv) a faint and narrow region after a jet deflection (300-400 pc from
the core). In particular, in the EVN map at 5 GHz (Lara et al. 1999), the source
exhibits an unresolved core with a peak flux density ~0.126 Jy/beam and a smooth
one-sided jet, extending to 25 mas from the core along PA ~ 27^deg^.

2. 2008MNRAS.391.1009L
Re:NGC 3842
NGC 3842: this galaxy belongs to a cluster, which forms a part of the Coma
supercluster. The surface brightness profile was published by Schombert (1986)
and the HST imaging by Laine et al. (2003). The radial velocity profile of this
galaxy reveals the presence of a KDC in the centre.

3. 2001ApJS..132..129M
Re:NGC 3842
NGC 3842. - This is another E galaxy located in the Abell 1367 cluster.
It has a concentrated core detected in the MUV (Fig. 23b).

4. 1995A&A...297..643W
Re:NGC 3842
NGC 3842. This E3 galaxy is the brightest member of the cluster A1367,
and possibly a cD galaxy. A good photograph of this cluster (including
NGC 3837) is given in Arp & Gavazzi (1984). The cluster A1367 is part of
the Coma supercluster. NGC 3842 is a source of radio continuum emission
(Calvani et al. 1989). An upper limit to the HI mass of 1 x 10^8^ M_sun_
has been reported by Burns et al. (1981). We obtain an upper limit to the
H_2_ mass of 3 x 10^8^ M_sun_.

5. 1994A&A...281..375F
Re:NGC 3842
1141+202. This is another small tailed source. As in the case of
1132 + 493, it is associated with the brightest cluster member in A 1367.
This cluster is peculiar for the existence of extended trails of radio
emission behind three irregular galaxies in its periphery (Gavazzi &
Jaffe 1987). We note that the present radio galaxy is very similar to
NGC 4874, the brightest member of the Coma cluster.

6. 1976RC2...C...0000d
Re:NGC 3842
In Abell 1367.
Photometry and Spectrum:
A.J., 75, 695, 1970. (redshift is mean for galaxy and its companion =
NGC 3841 at 2.9 arcmin ).

7. 1973UGC...C...0000N
Re:UGC 06704
In a dense part of the cluster (Abell 1367)
See UGC 06697, UGC 06701
11 41.3 +20 13 at 1.0, 281, 0.22 x 0.18 + 0.10 x 0.10, separation 0.10
UGC 06705 at 4.7, 356
11 41.5 +20 16 = {NGC 3845} at 2.9, 15, 0.7 x 0.3, early, m=15.1
{UGC incorrectly notes "NGC 3841". H. Corwin}


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