Date and Time of the Query: 2019-01-17 T15:04:48 PST
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Notes for object 3C 268.3

12 note(s) found in NED.

1. 2008ApJS..175..423P
Re:3C 268.3
3C 268.3 (Figs. 33 and 34) is an aligned CSS source (de Vries et al. 1999). The
emission extends beyond the radio source. Registration of the radio core and the
emission-line image was problematic due to the lower resolution of the optical
image. 3C 268.3 shows broad lines, indicating this source may not be in the
plane of the sky.

2. 2000MNRAS.317..120R
Re:3C 268.3
5.1 3C 268.3 (z=0.371)
The radio size is by far the smallest in our sample. In the R band it
appears round and featureless, and it is only just visible in our U-band
image (Fig. 3). Two slightly fainter galaxies, both ~ 11 arcsec from
3C 268.3, are probably physical neighbours (3C 268.3 lies in a cluster),
but we are not able to ascertain whether they are interacting. Deeper
R-band WFPC2 (de Koff et al. 1996) and [O III] (McCarthy et al. 1995)
images show a faint radio-axis-aligned structure, but we fail to see
this; evidently our exposure times were inadequate for this galaxy,
optically the faintest of the sample.

3. 2000AJ....120.2284A
Re:3C 268.3
The line emission has a jetlike morphology which extends 0.7"
northeast and 2.0" toward the southwest from the center of the host
galaxy. In the brightest regions it is oriented along P.A. -45^deg^
while it bends toward smaller position angles in the fainter extensions
on both sides. The central component is also dominated by line emission.
Another galaxy, possibly a companion, is seen 2" southwest of 3C 268.3.
The radio emission has an asymmetric double lobed morphology (Fanti
et al. 1985), extended ~1.4" along P.A. -20^deg^, clearly misaligned
with respect to the line-emitting gas. A weak core is detected, closer
to the southern component (Ludke et al. 1998). Registering the radio
core on top of the peak of line emission, shows that the northern lobe
is at the edge of the line emission, while the southern, due to the
difference in optical and radio P.A., is outside the line emission

4. 1999ApJ...526...27D
Re:3C 268.3
3C 268.3.-[O III], z = 0.371. A clear aligned component can be seen in
the I_line_ image. The decomposition into line and continuum images makes
it clear in this case that the aligned component is dominated by line
emission, since the continuum emission is confined to the nuclear region.

5. 1998MNRAS.299..467L
Re:3C 268.3
3C 268.3. This radio galaxy is quite asymmetric in both radio structure
and polarization. As in 3C 67. only the fainter, more diffuse component
is strongly polarized at 5 GHz. At higher frequencies, this lobe shows
steadily higher polarization (Akujor & Garrington 1995), whereas the
northern lobe remains unpolarized. A weak, unresolved component at
12^h^03^m^54.096^s^, 64^deg^30'18.68", which may be the core, is
detected 0.3 arcsec south of the northern hotspot, but further
observations are required to confirm this.

6. 1997ApJS..110..191d
Re:3C 268.3
3C 268.3 (galaxy, z = 0.371, m_F702W_ = 20.19).-This galaxy displays a
large tail to the southeast, approximately 5.5 h^-1^ kpc long. The
detection of a probable core by Ludke et al. (1997) close to the northern
lobe causes the rather asymmetric positioning relative to the optical
center. The inferred alignment angle is 8^deg^.

7. 1995ApJS...99...27M
Re:3C 268.3
3C 268.3 (z = 0.37; Fig. 19).-This object is small and unremarkable in
the continuum. The [O III] image shows extended emission on a scale of
4" with fairly high surface brightness. The radio source is a small 1.3"
double, oriented in position angle 161^deg^. This object is one of
several sources that show extended emission along the radio source axis,
but on scales larger than the radio source.

8. 1995A&AS..112..235A
Re:3C 268.3
3C 268.3 (1203+64)
This source shows very asymmetric polarization at both 8.4 and 5 GHz (see
van Breugel et al. 1984). The weak core seen in the MERLIN map by
Sanghera et al. (1994) is present as an extension of the northern
component of our 8.4 GHz map.

9. 1994ApJS...91..491G
Re:3C 268.3
1203+645 (3C 268.3) - The [O III] {lambda}{lambda}4959,5007 profiles are
difficult to assess. Correction for B-band absorption did not remove the
double nature of the [O III] {lambda}5007 profile. Although the major
peaks of the [O III] {lambda}5007 line correspond in redshift to peaks in
[O III] {lambda}4959, the relative flux in the components is very
different. Additional observations are needed to resolve these

10. 1994A&AS..105..211S
Re:[KWP81] 1203+64
The redshift listed by Herbig & Readhead (1992) is incorrect.

11. 1994A&AS..103..349S
Re:S4 1203+64
1203+645: An incorrect redshift is listed by Herbig & Readhead (1992).

12. 1974ApJ...191...43K
Re:3C 268.3
New identification with faint galaxy
based on 1 arcsec position agreement.
200-inch red image-tube plate shows many other faint galaxies
in a very distant cluster, as suggested earlier by
Parker, E.A., Elsmaore, B., and Shakeshaft, J.R.
(1966) Nature, 210, 22.
from red Sky Survey print.

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