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Notes for object 3C 275.1

9 note(s) found in NED.


1. 2006MNRAS.366..339B
Re:3C 275.1
3C 275.1. There is no evidence for X-ray emission from a resolved jet, but the
source shows extended emission which has been interpreted as arising from a
cluster-like atmosphere (Hardcastle & Worrall 2000; Crawford & Fabian 2003) or
from lobe IC emission (Croston et al. 2005).

2. 2005A&A...443...61O
Re:3C 275.1
B.4 3C 275.1 This well-known source at z = 0.555 has been studied in many
aspects. It is at the centre of the galaxy group it is associated with
(Krempec-Krygier et al. 1998). The close companion to the south-east is at the
same redshift as the quasar (Ellingson & Yee 1994) and thus separated from the
host by 28 kpc, but the object in close projection to the north-west is a
foreground object. The magnitude of the companion is R = 21.0, in good agreement
with the value obtained by Ellingson & Yee of R = 21.22.
Marquez et al. (1999) have performed imaging in J band and derive a host
magnitude of M_J_ = -24.8. Combined with our R magnitude, this leads to the
quite blue R-J colour of 0.9. In comparison, an elliptical galaxy at this
redshift has a colour of R-J=1.5 while an Sc spiral galaxy has R-J=1.1 (Fioc &
Rocca-Volmerange 1997).

3. 1999MNRAS.309..969H
Re:3C 275.1
3.23 3C 275.1
Both HRI and PSPC data are available for this quasar. The PSPC data
are confused by weak extended emission from the nearby spiral galaxy
NGC 4651; when this is removed, the data show a point-like source. The
longer HRI observation shows a profile slightly broader than the nominal
PRF, characteristic of a source affected by aspect smearing. When the
profile is fitted with a broadened PRF, there is some indication of
additional extension on scales of 20-60 arcsec. Using the broadened PSF,
we fit an additional {beta}-model component, with results tabulated in
Table 2. As for 3C 215, the galaxy counts of Ellingson et al. (1991)
imply a rich cluster environment for this source, so it is likely that
the extended emission we detect is real and due to hot intracluster gas.
Hintzen & Romanishin (1986) suggest that the extended emission-line
region around the source is due to a cooling flow, but the best-fitting
{beta}-model does not require cooling.

4. 1999MNRAS.308.1159C
Re:3C 275.1
3.5 3C275.1
3C275.1 was the first quasar discovered from optical galaxy counts to be
located at the centre of a rich cluster of galaxies (Hintzen, Boeshaar
& Scott 1981; Hintzen 1984; Ellingson et al. 1991). The radio source is
only slightly bent, but the two sides display an asymmetry in the
Faraday depolarization (Garrington et al. 1991). The quasar is embedded
in a host galaxy with a continuum spatial profile and absolute magnitude
typical of a bright cluster cD; this is in turn surrounded by a large
(100 kpc) optical emission-line nebula (Hintzen & Romanishin 1986;
Hintzen & Stocke 1986). Crawford & Fabian (1989) deduce a pressure
within this gas of > 3 x 10^5^ cm^-3^ K at radii of < 20 kpc and thus
also the presence of an intracluster medium (Crawford & Fabian 1989).
The fit to the X-ray radial profile improves slightly with the addition
of an extended component to the HRI PSF. The models all imply a
surprisingly broad core, so much so that fitting a second component to
data only within a 50 arcsec radius is not robust. The King and broken
power-law models yield very similar results, with R ~ 36 arcsec (where
1 arcsec corresponds to 7.4 kpc at the redshift of the quasar), and
24 per cent of the total X-ray luminosity of the source at
L_X_ ~ 3 x 10^44^ erg s^-1^.

5. 1996A&A...313..423H
Re:3C 275.1
3C 275.1 The line image of this quasar (Fig. 10) shows a large emission line
nebula with a remarkable conical shape directed towards the north-east. A
further bar-shaped extension lies south of the nucleus. The nebula measures
~10" across, corresponding to 75 kiloparsecs.
This large nebulosity was already reported by Hintzen et al. (1981), who also
presented an inventory of the numerous field sources. Spectroscopy confirmed
that the surrounding cluster is located at the redshift of the quasar, z=0.555
(Hintzen 1984). A continuum subtracted [O II]3727 image of the quasar (Hintzen
& Romanishin 1986) shows a morphology comparable to our result, although with
less detail. A depression of the emission lines south-east of the nucleus is
less pronounced in our data. Solid-body type rotation was measured along
position angle PA=32^deg^ with a total velocity amplitude of 700 km s^-1^
(Hintzen & Stocke 1986). Further spectroscopic observations along PA=45^deg^
(Crawford & Fabian 1989) show the extent of the nebula, and the run of
[O III]/[O II] with radius is interpreted as indication for a pressure gradient
in a cooling flow cluster.
Although 3C 275.1 lies in the heart of an X-ray cluster and was also
interpreted by Hintzen & Stocke (1986) in terms of a cooling flow, the large
size and orderly rotation are indicative of a merger origin for the gas.

6. 1995AJ....110.1492R
Re:3C 275.1
1241+166: The curvature of this source (3C 275.1) is suggestive of a
collision with a neighboring galaxy because the southern lobe is larger
and closer to the central core (Stocke et al. 1985). An object on the
southern side of 1241+166, which has the same redshift and is collinear
with the northern lobe, is the most likely deflector.

7. 1994A&AS..105..247A
Re:3C 275.1
1241+164, 3C275.1, quasar: This is another `dog-leg' quasar.
Previously published maps include those of Stocke et al. (1985),
Garrington et al. (1991) and Liu & Pooley (1990). The distortion of the
northern component is thought to be related to an interaction between the
quasar and a companion galaxy close to the Northern lobe (Hintzen et al.
1981). As for 3C270.1, 40% of the flux is missing in our high-resolution
map.

8. 1994A&AS..105...91B
Re:3C 275.1
1241+166 (3C 275.1, Fig. 35) Radio maps of this quasar can be found in
Stocke et al. (1985; 8.4 GHz VLA A array). Their image clearly shows the
jet towards the north-western lobe.

9. 1992MNRAS.257..545L
Re:3C 275.1
This source is associated with a quasar. High-resolution observations by
SBc and Laing (1988) show a jet pointing towards the north-west hotspot.
On the spectral index map presented by Liu & Pooley (1991a) it can be
seen that the spectrum is almost unchanged along the jet path between the
core and the Np hotspot. The integrated strip spectra still steepen,
however, although not as significantly as those in the southern lobe,
from the hotspot back towards the nucleus. This indicates that the bright
jet does not contribute a significant amount of flux to the total. The
integrated spectrum of the whole source is straight from 80 MHz to 5 GHz
with a spectral index of 0.9 (data from LP), agreeing with our current
observation that there is not much steepening in the spectrum between 1.4
and 5 GHz across this source. A companion galaxy next to the southern
hotspot and lying along the Nf hotspot-core axis was observed by Hintzen
(1984). Liu & Pooley (1990) found strong depolarization associated with
the region where the companion galaxy lies, in agreement with the
suggestion by SBC that the distortions in the southern component are the
result of an interaction between the quasar itself and the companion
galaxy.


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