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Notes for object SARCS 098

8 note(s) found in NED.


1. 2006MNRAS.370.1893H
Re:3C 295
A15. 3C 295 - The longer observation we use allows us to fit a more
sophisticated model to the data than was possible for Harris et al. (2000): the
two-component best-fitting model explains the inverted spectrum found by Harris
et al. when fitting a single power law with Galactic absorption. The addition of
a narrow Gaussian component with rest-frame energy 6.4^+0.1^_-0.5_ keV gives a
significant improvement to the fits.

2. 2000ApJS..131...95F
Re:VSOP J1411+5212
J1411+5212 (3C 295). - No detection: extended double-lobe radio galaxy,
no core is seen in a MERLIN 1.6 GHz image (Akujor et al. 1994).

3. 2000A&AS..145....1P
Re:3C 295
1409+524 (3C 295): This galaxy (z=0.461) shows no flux variations as
expected. It has been used as a primary flux calibrator;

4. 1999MNRAS.309..969H
Re:3C 295
3.28 3C 295
This radio galaxy is known to lie in an optical cluster (e.g. Yates,
Miller & Peacock 1989) and to have extended X-ray emission (Henry &
Hendriksen 1986). Our best-fitting characterization of the HRI emission
with a {beta}-model and point source is tabulated in Table 2. Acceptable
fits are found with no point-source contribution. Our values for core
radius and {beta} are consistent with the findings of Henry &
Hendriksen. The point-source contribution is much lower than their
adopted value (which would correspond to approximately 115 counts in the
HRI observation, on the assumption of a power-law spectrum and galactic
absorption), but agrees within the errors. Our best-fitting {beta}-model
is also consistent with Neumann (1999). The best-fitting model implies
rapid cooling, with a mass deposition rate of some hundreds of solar
masses per year, consistent with the picture of Henry & Hendriksen
(1986), and the cooling time at the core radius is less than the Hubble
time, so that the isothermal {beta}-model is not physically consistent.
When we fit the data with the most recent versions of the cooling-flow
models used by Hardcastle et al. (1998c), we find that the dependence of
pressure on radius must be weaker than the p is proportional to r^-1^
relation used in our earlier work, because the HRI emission is not
strongly centrally peaked; for example, acceptable fits are obtained for
a model with p is proportional to r^-0.5^, p is proportional to r^-0.75^
and T is proportional to r^0.25^, with the cooling time at the core
radius being ~2 x 10^9^ yr. This fit is not as good as the simple
{beta}-model together with a weak point source, and the cooling time is
rather short, but it fits the data without the need for a central
radio-related contribution. For consistency with our other analyses, we
use the point-source component derived from {beta}-model fitting as our
best estimate of the unresolved contribution to the X-ray emission.

5. 1994A&AS..105..247A
Re:3C 295
1409+524, 3C295, galaxy: This is a very luminous radio source
sometimes classified as a compact steep-spectrum source. Previous maps at
different frequencies have been published (Akujor et al. 1989; Perley &
Taylor 1991). Our map has better sensitivity and higher resolution than
the earlier 1.6 GHz MERLIN map by Akujor et al. The main features of the
source-the northwest lobe with multiple hotspots and the southeast lobe
with its extended arc and a bright hotspot are resolved.

6. 1988ApJ...328..114P
Re:3C 295
1409+524 (3C 295).-This is a Fanaroff-Riley class II source with a weak
central component (< 60 mJy; Laing 1981). It was not detected in the
finding survey.
Where necessary, we have assumed H_0_ = 100h km s^-1^ Mpc^-1^ and
q_0_ = 0.5 to convert angles to projected distances.

7. 1978ApJ...219..803K
Re:3C 295
Positions were measured on a 48-inch plate,
on which the radio galaxy could not be measured directly
because its image is blended with those of its companions.
A transfer was made to a 200-inch plate
by using three galaxies as secondary standards.
The resulting uncertainty is estimated to be 1-2 arcsec.
The position thus obtained places the brightest galaxy
within 1 arcsec of the center of the 5 arcsec double source,
using the very accurate radio positions of
Pooley, G.G., and Henbest, S.N.
(1974) MNRAS, 169, 477.
and unambiguously specifies it as the radio source.
The source is still sometimes referred to as a case of "colliding"
or "interacting" galaxies, dating back to its very early discovery.
Optically, however, it now appears similar to many other
run-of-the-mill radio galaxies in that it is the brightest
member of a cluster and has several close companions
(as also do many nonradio bright cluster galaxies).
Its absolute magnitude and colors are like those of other bright
cluster galaxies at similar redshifts.
Its main distinction is that
it is intrinsically one of the radio-brightest optically
identified sources in the sky at about 10**46 ergs/s,
integrated between 10**7 and 10**11 Hz proper frequency.

8. 1964ApJ...140...35M
Re:3C 295
No. 35.-0utstandingly brightest member of a cluster, richness 4:. There are four
other galaxies in a tight group surrounding the cD galaxy. Redshift by Minkowski
(1960) . .


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