Date and Time of the Query: 2019-08-26 T01:21:58 PDT
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Notes for object LBQS 0106+0119

3 note(s) found in NED.

1. 2008ApJS..175..314D
Re:VSOP J0108+0135
J0108+0135.-The core is 0.2 mas in size and the location of the extended
component is in agreement with other VLBA images.

2. 2000ApJS..131...95F
Re:VSOP J0108+0135
J0108+0135. - The weak feature 6 mas southwest of the core is outside
the field of view of Shen et al. (1997).

3. 1995AJ....109.1555P
Re:4C +01.02
0106+013: (Figs. A3 and A4) This is an important object for the rest
of the study since a variety of maps and resolutions exist. The map in
Fig. A4 is from the study of core dominated objects in Kollgaard et al.
(1990). It has the strongest extended emission in that study by a large
margin and it is the only object where it is concentrated in the jet (no
halo emission). Kollgaard et al. (1994) have produced a variety of
superior maps since then which will be described in the following. The
strong jet points due south and radiates 4.55 x 10^45^ ergs/s. On the
counter-jet side there is 2.5 x 10^44^ ergs/s of luminosity. At 8.5 GHz,
eight knots can be seen in the jet in polarized light. In unpolarized
light at 5 and 8.5 GHz the final three knots appear as one due to
insufficient resolution and the very intense luminosity of the first knot
in this cluster (4.45" from the core). This bright knot is the only one
visible in Fig, A4 which is not as deep as the more recent maps. The
existence of the second knot (4.8" from the core) is clear in polarized
light at both 5 and 8.5 GHz but it is undetectable in the total intensity
images. The third knot (5" from the core) is more detectable because it
is defined by only the two lowest contours at 8.5 GHz in the polarized
image. Consistently, a similar feature exits in the 5 GHz polarized image
and even the 5 GHz total intensity map. In this scenario, the jet appears
to veer due east in the last 0.5". This structure reveals a classical jet
magnetic field configuration. At 8.5 GHz, the magnetic field is parallel
to the jet direction through the first two knots in the cluster, then
becomes perpendicular to the jet in the third knot after the jet has
turned eastward. Thus, the knot 5" from the core could be considered a
hot spot. A similar curved structure is seen near the end of other jets
in Table 3 in such objects as 0836+710 and 1954+513. It should be noted
that if the cluster of knots were viewed near the sky plane then the
knots would most likely have an angular separation on the order of 2".
Another interpretation has been suggested by Bridle (1993) that the
second knot is probably a hot spot and the third knot is actually just
part of the lobe emission, but one would need higher resolution to be
sure. In either interpretation, the first knot in the cluster is much
more luminous than the hot spot.
Another interpretation would be to call the whole structure a hot
spot. In support of decomposing the structure, the asymmetry in hot spot
luminosities, between the jet and counter jet sides, would be
inconsistent with the relatively slow advance speeds (0.2c-0.3c) commonly
associated with hot spots (Browne & Perley 1986). If a faster flow
through the hot spot is responsible for the emission, than this is
equivalent to considering the emission at the hot spot as part of the jet
for our beaming analysis.
The 1.6 GHz map of Murphy et al (1993) in Fig. 8 is of lower
resolution and is a good example of what one would expect to see in the
under-resolved images prevalent in the rest of the sample when a jet is

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