Date and Time of the Query: 2019-05-20 T15:36:47 PDT
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Notes for object NGC 0708

10 note(s) found in NED.

1. 2010A&A...516A...1L
Re:NGC 0708
NGC 708 (B2 0149+35) in Abell 262. This cluster is one of the most conspicuous
condensations in the Pisces-Perseus supercluster. Its redshift is 0.0161. It is
a spiral-rich cluster, characterized by the presence of a central X-ray source
centered on a D/cD galaxy. Braine & Dupraz (1994) detect molecular gas and
suggest that it contains a cooling flow that may contribute to the central X-ray
emission. Observations show a double gaseous component.
The BCG has a dust lane almost perpendicular to the direction of its radio
emission (Ebneter & Balick 1985), which extends along the direction PA =
70[IMAGE] (Parma et al. 1986). Blanton et al. (2004) discuss the interaction
between the cooling gas and the radio source, which shows at arcsecond
resolution a core with a symmetric structure. The total 1.4 GHz flux density is
78 mJy (Blanton et al. 2004). This gives a power at 1.4 GHz of P_1.4 GHz_ = 4.7
x 10^22^ W/Hz, classifying the source as a fairly weak, double-lobed FR I galaxy
(Fanaroff & Riley 1974).
On parsec-scale, we observed an unresolved structure with a total flux
density of 3.2 mJy - about 64% of the arcsecond core flux density. The lack of
visible jets and the low core radio power are in agreement with the suggestion
that the core is in a low activity phase and that the offset of the radiative
cooling is due to several outburst episodes (Clarke et al. 2009).

2. 2001ApJ...550..503J
Re:NGC 0708
Abell 262 (NGC 708). - The central galaxy in A262 is littered with dust.
We used the high-resolution I-band WFPC-2 images (Lauer et al. 1998) to
identify dusty regions and create a mask for our NICMOS image. In addition
to the copious dust, we had to exclude exposures because of worminess in
the background. The uncertainty in fluctuation magnitude is relatively
large because of the dustiness and wormy background corrections, even
though A262 is among the closest of the clusters we observed.

3. 2000A&A...362..871C
Re:NGC 0708
0149+35 (NGC 708): A low brightness galaxy whose nuclear regions are
crossed by an irregular dust lane and dust patches. It is the brightest
galaxy of the cluster Abell 262.

4. 1999MNRAS.310...30C
Re:B2 0149+35
B2 0149+35 is identified with NGC 708 and is associated with the
brightest galaxy in the cluster Abell 262. Braine & Dupraz (1994)
suggest that it contains a cooling flow which may contribute excess
central X-rays, and this may explain why B2 0149+35 has a higher
point-like X-ray luminosity and flux than expected based on other sample
members. It is not possible to separate spatially a cooling-flow
contribution from unresolved X-ray emission using the PSPC observation,
and the asymmetry of the source makes the extraction of a radial profile
The HRI observation is split into two OBIs (observation intervals),
one of which shows a barred N-S structure. Each OBI was individually
analysed by taking close-in source regions, and this gives results that
are consistent with the PSPC data from the inner region of B2 0149+35.
In the longer, and more reliable, of the two OBIs (12.7 ks), 207 counts
were detected. The point-like contribution to the net emission from this
source, however, is not significant at the 95 per cent level when an
F-test is performed. The detected counts are therefore taken as an upper
limit on the point-model emission. The shorter OBI was not used.

5. 1998A&AS..128...75P
Re:NGC 0708
4.3.2. NGC 708
This E2 galaxy belongs to the Abell 262 cluster and it is usually qualified as
a Cooling Flow. Baars et al. 1976 have discovered HI in emission but no gas
mass has been derived. Molecular gas was also detected by Braine et al. (1994)
He gives a superior limit for the mass but this limit is very low for an object
who has to accrete 300 M_sun_/year in the hypothesis of a cooling flow (Heckman
et al. 1989). Observations show a double gaseous component. A monochromatic
image and a velocity field have been derived for each of them. Both components
are not counter rotating with respect to one another but Position Angles (PA)
of the MA of both components are strongly different. The first one has a PA of
the MA equal to 137^deg^ and the second component has a PA of 42^deg^. So the
second component is almost aligned with the stellar component and the first is
decoupled with it. The {phi} viewing angle is quite well defined for the first
component but for the second one there is no constraint at all.

6. 1994ApJS...91..507D
Re:NGC 0708
NGC 708 - This galaxy, located in the Abell cluster A262, has a dust
lane almost perpendicular to the direction of its radio emission (Ebtener
& Balick 1985), which extends along direction P.A. 70^deg^ (Parma et al.
Smith & Heckman (1989b) presented R-magnitude, ellipticity, and
position angle profiles of this object. Their results agree with ours.
The resulting parameters show distortions in the inner ~2" due to the
presence of the dust lane. Ellipticity shows large gradients, varying
form 0.03 at r~8" to 0.4 at r~40". Isophotes centers tends to move to the
northwest, being the outer isophotes (at r~40") displaced 1.4" from the

7. 1986A&AS...64..135P
Re:B2 0149+35
Brightest galaxy in the cluster Abell 262; it has a dust lane in
position angle ~ - 4{deg}. (Battistini et al 1980), roughly
perpendicular to the radio axis.

8. 1977A&AS...29..279F
Re:B2 0149+35
0149+35 See Wilson et al. (1977) for a 610 MHz map of this source. The
central source coincides with the galaxy NGC 708, the brightest of the
Abell cluster A262. The southern source is associated to the spiral
galaxy NGC 710. The northern source is not associated to any optical
object and may not be connected to NGC 703. At 4995 MHz only the
northern source is detected. The southern one was out of the observed
field. A new source is detected at 4995 MHz and coincides with the
nucleus of the galaxy NGC 703. Its flux is 9 mJy and the radio spectrum
is flat.

9. 1976RC2...C...0000d
Re:NGC 0708
In Abell 0262.
There is a superimposed star.
A.J., 75, 695, 1970.

10. 1973UGC...C...0000N
Re:UGC 01348
See UGC 01343, UGC 01345, UGC 01346
The group appears to be surrounded by an extremely diffuse halo

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