Date and Time of the Query: 2022-01-23 T05:20:05 PST
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Notes for object [HB89] 1739+522

9 note(s) found in NED.

1. 2004ApJS..155...33S
Re:VSOP J1740+5211
A GOT image can be found in VSOPPR.

2. 2003A&A...401..161K
Re:[HB89] 1739+522
8. 1739+522: This quasar was observed in May 1991. In addition to
variations on a few percent level, a rapid flux density dip has been
seen at {lambda} = 11,6 cm (see, e.g. Fig. 7, upper panel) which - as in
0954+658 (see before) - could be interpreted as an extreme scattering

3. 2002AJ....124..662Z
Re:IERS B1739+522
1739+522: A MERLIN image of this highly polarized QSO shows
a secondary component 3" away from the core (Reid et al. 1995). A
high-resolution 43 GHz image of the core region by Lister (2001)
shows a jet that starts out in an easterly direction and curves
over 90^deg^ to the north. Our image shows only an unresolved

4. 2001ApJS..134..181J
Re:[HB89] 1739+522
1739+522. - The 1.7 GHz VLBI map of this quasar by Polatidis et al.
(1995) contains very weak extended structure to the east up to 10 mas and,
perhaps, a faint secondary component to the northwest 20 mas from the core.
A 2.3 GHz VLBI image reveals a weak, thin structure out to 15 mas along
P.A. ~ 28^deg^ (Fey et al. 1996). The 8.55 GHz map of these authors at the
same epoch shows a jetlike structure curved from P.A. ~ 36^deg^ near the
bright core to P.A. ~ -10^deg^ beyond 1 mas. The 5 GHz image by
Pearson & Readhead (1988) contains a dominant core plus a weak component
at P.A. ~ 3^deg^ 1.7 mas from the core.
Our images at 22 GHz (Fig. 33) during the last two epochs of our program
are also dominated by the unresolved core. The lower dynamic range 1993.86
image contains a short jet along P.A. ~ 77^deg^ plus the suggestion (near
the noise level) of a sharply curved extension to the north. Our images
indicate strong variability of the intensity of the jet, but the absence of
features that can be followed negates any possibility of estimating the jet
velocity. However, a comparison of the results of model fitting of our
1993.86 observations with the Gaussian model of the 8.55 GHz image at epoch
1994 July presented by Fey et al. (1996) suggests that our component B1 in
1993.86 might correspond to their component 2 at 8.55 GHz. If we make this
identification and assume no frequency-dependent gradients in separation
from the core, we can make a very tentative estimate of the proper motion
of ~0.56 mas yr^-1^, which corresponds to a high apparent speed,
~24 h^-1^ c (not included in Table 5 or in our subsequent analysis).

5. 2000A&AS..145....1P
Re:[HB89] 1739+522
1739+522: In this quasar (z=1.379), two (adjacent) continuous outbursts
appear at 6 and 2.8 cm. Its modulation index varies with wavelength;

6. 1997A&AS..121..119V
Re:4C +51.37
3.16. 4C 51.37(1739+522)
Apart from the identification of the radio source 4C 51.37 with a quasar of
photographic magnitude 18.5 (Kuhr 1977), the optical information about this
source is very poor in the literature (Cohen et al. (1977) give R=18.5 and
B=18.7). Impey & Tapia (1990) found an optical polarization of 3.7%. This
object was detected in the {gamma} band by EGRET, with a maximum flux of
3.6 10^-7^ cm^2^ s^-1^ (von Montigny et al. 1995).
Without calibration of the reference stars, our data are presented in Tables 36
and 37 and in Fig. 36 as magnitude differences with respect to the minimum
value. The maximum variation in the monitoring period was {DELTA}R=1.19. Some
intranight variation can be distinguished on JD^bar^=889 and JD^bar^=969.

7. 1996ApJ...459..100N
Re:[HB89] 1739+522
J1738+51 = 1739+522 = 4C+51.37.--This is a flat-spectrum QSO.

8. 1995A&AS..110..213R
Re:[HB89] 1739+522
1739+522: Though only made from 2 minutes of data the 1465 MHz map
confirms the presence of the faint secondary component ~3 arcsec to the
west of the core.

9. 1988ApJ...328..114P
Re:[HB89] 1739+522
1739+522.-In 1.7 GHz observations on the VLA Perley (1982) and Shone
(1986) found that this core-dominated object has a weak secondary
component situated 3.5" from the core in P.A. 260deg. There is no other
evidence for extended structure above a level of 0.3 mJy within 6" of
the core. The fractional polarization at 5 GHz is 1% (Perley 1982), and
the source is strongly variable (Seielstad, Pearson, and Readhead 1983).
We found that a single component gave a fair fit to our data, but there
were systematic deviations in the closure phases of up to 10deg,
indicating that a more complex, asymmetric model was required. We
obtained an excellent fit with the two-component model given in Table 4,
which shows that the object is extended in the north-south direction,
i.e., roughly orthogonal to the large-scale structure. Observations at
22 GHz by Lawrence et al. (1985) give a mean visibility on the
OVRO-Effelsberg baseline of 0.65.
Where necessary, we have assumed H_0_ = 100h km s^-1^ Mpc^-1^ and
q_0_ = 0.5 to convert angles to projected distances.

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