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Date and Time of the Query: 2019-05-19 T10:50:26 PDT
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Notes for object 3C 138

9 note(s) found in NED.


1. 2005A&A...443...61O
Re:3C 138
B.2 3C 138 This object at z = 0.759 was observed and marginally resolved by
Kotilainen & Falomo (2000) in H band, resulting in a magnitude of the nucleus of
M_H_ = -24.9 and a host magnitude of M_H_=-24.2. Imaging by Hutchings & Neff
(1990) in R band yields a nuclear magnitude of M_R_ = -23.9 and a host magnitude
of M_R_=-24.0. This is similar to the values found in this paper of M_R_ = -24.4
for the nucleus and M_R_ = -24.1 for the host.

2. 2000AJ....120.2284A
Re:3C 138
3C 138 appears unresolved at the resolution and sensitivity of the
snapshot images which are presented. However, the central continuum
source accounts for only 15% of the on-band emission, indicating that
line emission is associated with its nuclear regions and it originates
in a very compact region, <~0.1" (1.5 kpc). The radio source has a
triple structure, with a bright radio core and a bright jet embedded in
the northeast lobe. Around the radio core position Cotton et al. (1997)
found a large Faraday rotation measure which is likely to occur in the
compact line-emitting region. In contrast, in the northern jet/lobe, the
rotation measure is virtually zero, consistent with the lack of line
emission indicating the presence of little warm gas.

3. 2000A&AS..145....1P
Re:3C 138
0518+165 (3C 138): This quasar (z=0.759) shows no flux variations as
expected. It has been used as a primary flux calibrator;

4. 2000A&A...364...70K
Re:3C 138
3C 138 = PKS 0518+16. The host galaxy is marginally resolved, with
M_H_ = -25.4 and R_e_ = 8 kpc. This quasar was imaged with HST in the
optical by De Vries et al. (1997), who claim it to be slightly extended
(although they did not attempt any modeling).

5. 1998MNRAS.299..467L
Re:3C 138
3C 138. The structure of the quasar, which consists of a core with a
bright jet and hotspot to the east and a fainter, more diffuse lobe to
the west, has been discussed by Akujor et al. (1993). Polarization
images at 8.4, 15 and 22 GHz have been presented by Akujor & Garrington
(1995), van Breugel et al. (1992) and Akujor et al. (1993), and a VLBI
polarization image at 5 GHz has been made by Dallacasa et al. (1995).
The average polarization of the jet and hotspot increases slightly from
12 per cent at 5 GHz to 14 per cent at 15 GHz. Locally, the polarization
of the jet increases to 25 per cent near the core at 15 and 22 GHz, but
at 5 GHz with similar resolution the polarization is only 15-20 per cent
in the MERLIN image. This may indicate some depolarization of the jet
near the core.

6. 1997ApJS..110..191d
Re:3C 138
3C 138 (quasar, z = 0.759, m_F702W_ = 18.48).-This object is one of the
CSS quasars where some extended emission is present. The optical axis
position angle is 90^deg^. We placed the radio core, as identified by van
Breugel et al. (1992) and corroborated by Dallacasa et al. (1995), on top
of the optical peak, resulting in an alignment angle of 23^deg^.

7. 1995A&AS..112..235A
Re:3C 138
3C 138 (0518+16)
This source has been discussed in detail by Akujor et al. (1993). It
shows a striking asymmetry in the degree of polarization at 8.4 and 15
GHz.

8. 1994ApJS...91..491G
Re:3C 138
0518+165 (3C 138) - The emission falls amid strong, closely spaced sky
emission, affecting the [O III] {lambda}5007 wing measurements. The
H{beta} profile is also affected by sky emission and absorption lines,
but we suspect the sharp blue edge is real.

9. 1992A&A...256...56v
Re:3C 138
3C 138: Two faint sources are found in this field, at 1.5 GHz, at
distances of 155" in pa. = -108^deg^ (Fig. 1) and 243" in p.a. = 120^deg^
from 3C 138 (see also De Waard 1984). There is no evidence in our map for
any physical association of these sources with 3C 138. The 22.5 GHz map
(Fig. 11) confirms earlier findings (e.g. Fanti et al. 1989) that
component A has a flat spectrum and, therefore, contains the radio core.


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