Date and Time of the Query: 2019-05-25 T02:41:32 PDT
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Notes for object 3C 381

8 note(s) found in NED.

1. 2009MNRAS.396.1929H
Re:3C 381
3C 381 is classed as a BLRG in LRL, but as pointed out by Hardcastle et al.
(1997) the evidence for this classification is very tenuous. Jackson & Rawlings
(1997) classify it as a NLRG, based on the spectroscopy of Saunders et al.
(1989), whose published spectrum shows no evidence for broad H{alpha}. Our X-ray
spectrum gives a well-constrained, high-absorbing column. We infer that the
classification of this source as a BLRG by LRL is likely to have been incorrect.

2. 2008ApJS..175..423P
Re:3C 381
3C 381 (Figs. 53 and 54) does not show alignment between the emission-line
nebula and the radio source.

3. 2006ApJS..164..307M
Re:3C 381
Smooth elliptical with a close projected companion galaxy to the east. Roche &
Eales (2000), with a U-band image taken with the Wide Field Camera on the Isaac
Newton Telescope, find an apparent tidal distortion that confirms that the two
galaxies are interacting. There is an additional faint unresolved source
~2" south.

4. 2000MNRAS.317..120R
Re:3C 381
5.12 3C 381 (z=0.1605)
The V-band image (Fig. 19) shows a round (ellipticity = 0.054) high
surface brightness galaxy, with a fainter (V = 18.80) lower surface
brightness companion (G2), 5.50 arcsec away at PA 650. In the U-band
image, tidal distortion of the two galaxies is more apparent (confirming
that they are interacting), with 3C 381 mildly elongated
(ellipticity = 0.196, PA 1542) perpendicular to the pair orientation.
The [O III] image of McCarthy et al. (1995) shows an elongated
(~ 20-arcsec) region of emission with a similar long axis (PA 135^deg^)
to the galaxy and a fainter filament to the north, close to the radio
axis. Our U-band image also shows a faint extension to the north, but
this curves to the west and may be a tidal interaction feature rather
than a jet ejected from the nucleus (the companion galaxy shows similar
asymmetries), so we find no definite evidence of optical-radio

5. 2000A&A...364..501D
Re:3C 381
3C 381 A compact nucleus and tails appear in the HST image (K96). Grandi
& Osterbrock (1978) claim 'a broad weak component of H{alpha}', but to
our knowledge there is no published spectrum of H to date. We suggest
that its identification as a genuine BLRG may be open to doubt: it has
no detected radio jet, and, unlike all other BLRG observed by Lilly &
Longair (1982) its K band flux density is not higher than the NLRG in
the sample.

6. 1998ApJS..114..177Z
Re:3C 381
3C 381.--This galaxy was mistaken for 3C 327, and no UV measurements exist. The
F702W HST image (also discussed by de Koff et al. 1996) shows an elliptical
galaxy with two tails of emission pointing north and south.

7. 1996ApJS..106..247C
Re:3C 381
3C 381 (z=0.1605; Fig. 29).--Our spectra of 3C 381 sample only the close high
surface brighness [O III] {lambda}5007 emission, rather than the large arc
seen in the [O III] {lambda}5007 image in Paper I. Our spectra reveal only
modest velocities for the material within +/-10".

8. 1995ApJS...99...27M
Re:3C 381
3C 381 (z = 0.16;Fig.5).-This object is quite remarkable in the light of
[O III]. The continuum images reveal a cluster with a close projected
companion galaxy to the east. The [O III] image shows extensive regions
of emission lying in two directions. The inner and highest surface
brightness emission is elongated in position angle 140^deg^. This
emission extends nearly 20". A fainter filament of [O III] emission
stretches ~25" to the north and curves around the outer boundary of the
northern radio lobe. This is one of the largest high-ionization emission-
line regions among the low-redshift 3CR galaxies. The radio source is a
69" double (Riley & Pooley 1975; J. Stocke 1990, private communication).

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