Date and Time of the Query: 2019-05-19 T09:43:18 PDT
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Notes for object 3C 266

11 note(s) found in NED.

1. 2003ApJ...585...90Z
Re:3C 266
3CR 266 (z = 1.275). One of the most elongated of all 3CR galaxies in
the rest-frame UV, the alignment of 3CR 266 persists into the NIR,
although the isophotes are generally rounder. The NIR morphology is
striking; cleanly separating into a relaxed, elliptical host and a
thin, aligned component nearly identical to the WFPC2 image.

2. 2000ARep...44..286T
Re:3C 266
3C 266
This is a radio galaxy with redshift z = 1.275. Observations at 8.4,
5, and 1.6 GHz show that it has a double structure with separation 4". The
northern and southern components have sizes 0.5" x 0.1" and 0.7" x 0.3",
respectively. The flux densities of the components are roughly equal at all
frequencies. We therefore expect both components to scintillate at 102 MHz.
We observed 3C 266 over six days. Scintillations were recorded
reliably. Given the source elongation (44^deg^), the component separation
(4"), and the direction of solar-wind propagation, we estimated the flux
density in the compact features and the integrated flux density to be
S_scin_ = 4.2 Jy and S_int_ = 19 Jy, respectively. There is no
low-frequency turnover in the spectra of the two compact features.

3. 1999ApJ...526...27D
Re:3C 266
3C 266.-[O II], z = 1.275. This high-redshift galaxy is only
marginally detected in [O II]. The faintness of the source, coupled with
the decrease in detector sensitivity toward 1 micron, makes deeper
exposures a necessity.

4. 1997MNRAS.286..241J
Re:3C 266
3.3.8 3C 266
We used the Laing et al. (1983) optical position to centre the slit. Hammer &
Le Fevre (1990) observed this object in an [O II] filter and detect extended
emission lying roughly north-south (and also claimed gravitational
amplification of the object by the nearby cluster A1374). We detect extended
[O III] in both pixels on either side of the nucleus.

5. 1997ApJS..112..415M
Re:3C 266
3C 266 (z=1.275; Fig. 12).--This object is very extended with a spectacular
morphology. The emission can be traced over more than 2.5" and is aligned with
the radio source axis. The radio source is a 4" double, and the best VLA maps
available to us do not reveal a core. The northern lobe lies just beyond the
termination of the visible structure in our HST image. The F702W filter does
not contain significant [O II] {lambda}3727 emission at this redshift. HST
images taken with other filters can be found in Best et al. (1996a).

6. 1997ApJS..110..191d
Re:3C 266
3C 266 (galaxy, z = 1.275, m_F702W_ = 21.25).- Determining the nucleus in
this image of highly filamentary structure is difficult. It is not clear
if the bright spot to the east of the long filament is associated with
the source. We therefore aligned the radio source with the elongated
emission to the west of the bright spot. The position of the radio axis
differs by 13^deg^ from that of the optical.

7. 1996ApJS..106..247C
Re:3C 266
3C 266 (z=1.275; Fig. 9).--An [O II] {lambda}3727 image is given in Rigler et
al. (1992). Our spectra were obtained with the Cryocam and show a spatial
extent to [O II] {lambda}3727 consistent with that seen by Rigler et al.
(1992). Our Gaussian fits required a second component, blueshifted with
respect to the nucleus by 1400 km s^-1^. This is seen in more than one spatial
pixel, and we believe it to be real.

8. 1995A&AS..112..235A
Re:3C 266
3C266 (1143+50)
This source is fairly symmetric in polarization at 8.4 GHz

9. 1993MNRAS.263..936D
Re:3C 266
3C266 (Fig. A1l). The V and [O II] images presented by Hammer & Le Fevre
(1990) show this object to be a classic example of a galaxy with
elongated optical continuum and line emission closely aligned with the
radio axis. The optical position angle given by McCarthy et al. (1987b)
is 7^deg^, while the radio source is a 4-arcsec double in position angle
179^deg^ (Spencer et al. 1989). Although the galaxy definitely appears
more nucleated at K than at V, our K-band image yields a position angle of
1^deg^. Such alignment is not apparent in the K-band image of Rigler
et al. (1992), although the low-level extension to the west is.

10. 1992MNRAS.257..545L
Re:3C 266
There is a possible 0.4-mJy core at the centre of the source on the 5-GHz
map, but it could not be confirmed by the rather noisy 15-GHz map. Both
hotspots in this source lie on the axis some way behind the leading edges
of the lobes. The spectra are flatter at these embedded hotspots,
steepening both outwards and inwards with about the same gradient.

11. 1978ApJ...219..803K
Re:3C 266
New Identification?
Possible object at limit of shallow 200-inch B plate,
at position of Adgie, R.L., Crowther, J.H., and Gent, H.
(1972) MNRAS, 159, 233.
Needs confirmation.
The Wyndham, J.D. (1966) Ap. J., 144, 459
candidate (D on our chart) is 21 arcsec away.
Single radio source.

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