Date and Time of the Query: 2019-06-16 T10:35:18 PDT
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Notes for object NGC 3862

15 note(s) found in NED.

1. 2010A&A...516A...1L
Re:3C 264
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. 2008ApJS..177..148F
Re:3C 264
4.2.3. 3C 264; z = 0.021718; 3C 264 is a tailed radio source in the cluster
Abell 1367.12 On the arcsec scale there is a bright one-sided jet that is
detected in the radio (Baum et al. 1997; Lara et al. 1999), optical (Crane et
al. 1993), and X-ray (Tilak 2006; Padgett et al. 2005). Baum et al. (1997) note
the existence of an inner dusty disk that causes an apparent ring in the galaxy
surface brightness where the disk ends. The NICMOS image shows a bright nucleus,
the jet and the ring noted by Baum et al. The data were previously published by
Capetti et al. (2000b).

3. 2006ApJ...642...96E
Re:3C 264
The nuclear spectrum is well modeled by a single unabsorbed power law of photon
index 2.34^+0.07^_-0.08_. For this fit, we found the value of {chi}^2^ to be
123.0 for 147 dof. No improvement to the fit was achieved with more complex
spectral models, such as an intrinsically absorbed power law or the addition of
thermal emission: in every case, the values of absorption and thermal
normalization tended to zero. We compared the results of our spectral fitting to
that from an XMM-Newton observation (Donato et al. 2004). The power-law photon
indices are approximately consistent ({GAMMA} = 2.34^+0.07^_-0.08_ for Chandra
and {GAMMA} = 2.48+/-0.04 for XMM-Newton), as are the integrated X-ray

4. 2003ApJS..148..419N
Re:NGC 3862
NGC 3862 (UGC 6723).-This elliptical galaxy has a nuclear dust disk (b/a
~ 0.99). It has a core-jet radio morphology on VLBA and VLA scales. The
STIS slits were aligned approximately perpendicular to the radio jet as
the nuclear isophotal position angles are poorly constrained. The
central kinematic and flux properties are listed in Table 15; the gas
does not exhibit a regular rotation profile. The fit to the central
spectrum is improved by the addition of a broad component, which appears
to represent a nonflat continuum in this case. Data for this galaxy are
shown in Figure 11 (see key in Fig. 1 for an explanation of these

5. 2002AJ....124..675C
Re:UGC 06723
3C 264 in Abell 1367.

6. 2001ApJ...552..508G
Re:3C 264
1142+20 (3C 264). - We discussed the properties of this source in
Lara et al. (1997), Baum et al. (1997), Lara et al. (1999), and
Lara et al. 2001, in preparation. We assume here as jet dynamics the
results given in Baum et al. (1997). This source is classified as a
low-luminosity BL Lac by Rector, Stocke, & Perlman (1999).

7. 2000ApJS..129...33D
Re:3C 264
3C 264 (NGC 3862), z = 0.0208. - This object lies in a dense part
of the cluster Abell 1367. Figure 15 shows a face-on dust disk with an
optical jet projected on it. The dust disk appears to have its physical
boundary at the same distance from the nucleus as the projected optical
jet. A radio jet coincides with the optical jet. Baum et al. (1997) have
described in detail the relation between the optical jet, dust disk and
radio jet.

8. 2000AJ....120.2950X
Re:UGC 06723
UGC 06723 (NGC 3862=3C 264).-The overall radio structure of this
galaxy is very unusual. It consists of three structural components: a
small-diameter core, a one-sided jet, and a large amorphous emission
plateau (Bridle & Vallee 1981). Optical synchrotron emission is
associated with the jet (Crane et al. 1993; Baum et al. 1997). Recent
global VLBI and VLA images of this source can be found in Lara et al.
(1997), while MERLIN images appear in Baum et al. (1997).

9. 1999MNRAS.309..969H
Re:3C 264
3.18 3C 264
This narrow-angle-tail radio galaxy lies ~7 arcmin away from the
X-ray centroid of the cluster Abell 1367, and 8.4 arcmin off-axis in the
PSPC observation. We use the parameterized off-axis PSPC PSF
(Hasinger et al. 1995) to perform a radial-profile fit in a standard
2-arcmin source region, which excludes most of the emission from the
cluster. The results (Table 2) suggest that there is some extended
emission associated with the radio source, in addition to a strong,
point-like component. Our result is consistent with the count rate
quoted by Edge & Rottgering (1995).

10. 1999ApJS..122...81M
Re:3C 264
3C 264 (NGC 3862). - Our WFPC2 image distinctly shows the optical
synchrotron jet and dust disk discovered by Crane et al. (1993) with FOC
images. Baum et al. (1997) discuss and model these observations in
greater detail with the addition of MERLIN radio maps. The disk is
optically thick, nearly face-on, and "puffed up." The jet is resolved
and disrupted at the outer boundary of the disk. According to their
models, it is inclined at ~ 50^deg^ from our line of sight. The nucleus
is unresolved, and the host galaxy is very circular and smooth.

11. 1999AJ....118.2592V
Re:NGC 3862
NGC 3862 is part of the cluster Abell 1367 and has a nearby
lenticular companion (IC 2955) at a distance of 54" (22 kpc). There is
an apparent faint face-on circular dust disk (Crane et al. 1993) 610 pc
(1.5") in diameter, which is studied in detail by Baum et al. (1997).
The apparent disk is edge-darkened, especially the southern half. This
might be a projection effect or could indicate that the inner parts of
the dust disk are swept clear by either the jet or some other nuclear
process (Hutchings et al. 1998). The H{alpha} + [N II] emission is
strongly peaked at the nucleus, and diffuse low-level emission is seen
throughout the disk. There is a strong blue nuclear point source. 3C 264
is a head-tail radio source displaying S-shaped wiggles extending to a
long bifurcated tail of diffuse radio emission (e.g., Baum et al. 1988;
Parma et al. 1991; Lara et al. 1999). The optical jet, discovered by
Crane et al. (1993), seems to interact with the surrounding ISM (Baum
et al. 1997).

12. 1998ApJS..114..177Z
Re:3C 264
3C 264.--This galaxy is classified as an S0 galaxy (Schombert 1986) in a rich
Abell cluster and has a bright core and an amorphous radio structure (Baum et
al. 1988). It contains an unresolved and possibly variable X-ray source (Elvis
et al. 1981) and has a prominent optical jet to the northeast of the nucleus
(Crane et al. 1993; Baum et al. 1997). In the radio this jet extends tens of
arcseconds to the north and a faint counterjet to the south. This jet is
discussed extensively by Baum et al. (1997). There seems to be an enhanced ring
of optical emission just at the location at which the jet decollimates and
decreases in surface brightness, which suggests an interaction between the jet
and ambient medium. Apparently this ring is likely to be the manifestation of
absorption by a nearly face-on circumnuclear dust disk. Crane et al. note that
3C 264 has a pointlike nucleus with a blue color. The pointlike nucleus is
consisted with our modeling where we show that the PSF contribution in the
F220W and F320W filters is 47%+/-13% and 19%+/-9%. The UV (F220W and F320W) and
optical (F702W) images clearly show the jet, which is ~1" in length.

13. 1976RC2...C...0000d
Re:NGC 3862
= 3C 264
= 4C 19.40
In Abell 1367
Ap. J., 140, 35, 1964.
P.A.S.P., 80, 129, 1968.
Photometry (UBVR):
Ap. J., 178, 25, 1972.
Ap. J., 183, 731, 1973.
Radio Observations:
Ap. J., 142, 106, 1965.
A.J., 72, 230, 1967.
A.J., 73, 1, 1968.
Astr. Ap., 34, 341, 1974.
X-RAYS (in Abell 1367)
Ap. J. (Letters), 185, L13, 1973.
Ap. J. (Letters), 193, L57, 1974.

14. 1973UGC...C...0000N
Re:UGC 06723
In a dense part of the cluster (Abell 1367)
11 42.5 +19 54 = IC 2955 at 0.9, 343, 0.25 x 0.20, red envelope 0.6 x 0.6,

15. 1964ApJ...140...35M
Re:3C 264
No. 24.-Probably outlying member of cluster A1367, richness 2. The radio source
has a diameter of about 3' and is displaced by 1.2' to the northeast from the

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