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Date and Time of the Query: 2019-08-21 T11:50:49 PDT
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Notes for object [HB89] 0605-085

7 note(s) found in NED.


1. 2004ApJ...608..698S
Re:[HB89] 0605-085
0605-085. The VLA contours in Figure 1 were restored with beam size
0.45". The lowest contour is 0.75 mJy beam^-1^. Two X-ray knots were
detected, with no optical counterpart in the HST image, as well as faint
intraknot emission. The X-ray emission peaks at 4.0" (B), before the
radio knot, which peaks at 4.5". This radio knot is centered with a
difference of position angle, {DELTA}P.A. = 18deg, farther south. The
nearby bright source in the southwest is a foreground star, with a
bright optical counterpart on the HST map.

2. 1998AJ....115.1295K
Re:[HB89] 0605-085
0605-085.--Structure to the west of the brightest component (the core?) could be
part of an initial tight loop of a strongly bent jet that continues to the east.

3. 1996A&A...308..415B
Re:[HB89] 0605-085
0605-085: core-jet structure. The large scale structure (> 10 mas) detected in
epoch 3 is clearly produced by the better sensitivity of these observations
compared to the previous epochs. An estimate of the variations on a small
scale structure (< l0 mas) was performed by analysing the fringe amplitudes
along p.a. 90^deg^ (Fig. 8). The epoch 2 data are compatible with a single
component. The epoch 3 amplitudes show a minimum at 31 M{lambda} implying two
components separated by 3.3 mas at this p.a. If we assume that this component
was not resolved during epoch 2 because it was too close to the core, the
separation would be < 2.3 mas (corresponding to the maximum observed baseline)
during epoch 2. We therefore derive a lower limit to the proper motion of the
component as {mu} >= 0.2 mas/year. This proper motion is in good agreement
with that derived from the broadening of the nuclear component between epochs
1 and 2. The parameters in Table 3 indicate this proper motion with an
expansion of about 1.4 mas in p.a. 120^deg^ of component C.
The structure of this source is confirmed by 5 GHz VLBI observations
(Cerchiara, private communication).

4. 1994MNRAS.269..998d
Re:[HB89] 0605-085
0605-08
The accurate VLA position (Paper II) coincides with that of the blue
stellar object identified by Wills (1976). Its spectrum shows broad
Mg II 2800, already detected by Wills & Wills (1976) and [NeV] 3426 at
z = 0.871 (Fig.3 and Table 3).

5. 1994A&AS..105..211S
Re:[KWP81] 0605-08
The redshift has also been listed by Allington-Smith et al. (1991) and
Stickel et al. (1993a).

6. 1993A&AS...97..483S
Re:[HB89] 0605-085
0605-085
The optical spectrum shows only a single broad emission line which was
first noted by Wills & Wills (1976). It is most likely identified with
Mg II {lambda}2798 at a redshift of z = 0.872. This agrees with the value
given by Allington-Smith et al. (1991).

7. 1976ApJS...31..143W
Re:[HB89] 0605-085
0605-085: The ~16 mag RSO(Table 4) showed H{alpha} and H{beta} emission lines
at rest on the first three spectrograms obtained in 1973.25. Three further
spectrograms obtained in 1973.9 fail to show the emission, but exhibit an
M-type absorption spectrum. The final spectrogram(1974.15) showed the H{alpha}
and H{beta} emission again. Presumably the RSO is simply a variable M star; it
is unlikely to be a Mira variable, since we did not note any large (>1 mag)
changes in the visual magnitude between any of the observations, and its
apparent magnitude is too faint. The fainter(>~19 mag) BSO (Table 5) is about
3" from the RSO. Two spectrograms obtained in <~1" seeing show a broad
emission line whose central wavelength was measured as 5238 and 5244 A,
respectively. The continuum, while blue, is less ultraviolet than for typical
QSOs, and the nature of the object remains in doubt.


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