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Notes for object [HB89] 1510-089 NED02

14 note(s) found in NED.

1. 2010ApJ...714..605R
Re:PKS 1510-089
PKS 1510-089. The reported magnitude for this quasar is m_V_ = 16.3
(Xie et al. 2001). On 2000 March 20, we measured m_V_ = 16.86 +/-
0.02 at the first data set. A power law with {alpha}_t_0__ = .0.23
+/- 0.03 fits these data (Figures 9(a)). However, the spectral
variation cannot be explained appropriately only with a single
non-thermal component (Figure 9(c)). Thus, a thermal component with
T_t_0__ ~ 26,000 K and b_V_t0__ ~ 40% is added (Figure 9(b)). With
this configuration only thermal variations can reproduce the observed
behavior (Figure 9(d)). Nevertheless, the amplitude of the thermal
component should increase by a rather high factor (n_T_t_5___ > 2.5),
while the temperature should fall 8000 K. In such a case, the rate of
variation has been {DELTA}T ~ 1800 K hr^-1^ and {DELTA}n_T_ ~ 0.57
hr^-1^. The return observed in Figure 9(c) can be caused by a
variation which is dominated first by changes in nT and then by
changes in temperature. This behavior might have been evident if
observations had been prolonged a few hours. With a constant rate of
change (as it seems to have happened; see the V-band light curve in
Figure 2(c) of PII), the simultaneity criterion indicates that
observations were carried out satisfying the simultaneity criterion
(S_B_ = 0.09, S_V_ = 0.22, and S_R_ = 0.86).

2. 2007A&A...464..175B
Re:[HB89] 1510-089 NED02
1510-089 - This is another extreme quasar, highly polarized, and bright at X-ray
and {gamma}-ray energies. It exhibits a highly bent radio jet structure with
fast superluminal speeds of up to 20 c(Hartman et al. 1999; Homan et al. 2001;
Singh et al. 1997). In the radio band, we saw the source fading simultaneously
at all frequencies (Fig. 1). Noticeable variations were seen also in the near-IR
(Fig. 2). Note also that our SEDs (Fig. 3) show a dip between the near-IR and
optical bands, in agreement with the observations by Neugebauer et al. (1979) in
1977 (data reported by NED, grey dots). In that case, however, the optical
spectrum was quite harder and it seems that a much stronger emission component
was present towards smaller wavelength. Such an increase in the spectrum of a
quasar is commonly referred to thermal emission from an accretion disk (e.g.
Bregman 1990), but in that case, although the observations are separated by ~30
years, the component should not be so strongly variable. A similar behaviour was
observed in AO 0235+164, where a variable UV-to-soft-X-ray bump was found
(Raiteri et al. 2006a,2005,2006b). In this case the authors speculate that the
variability could be due to a strong change of e.g. the accretion rate. Another
possibility would be the presence of another emission component, e.g.
synchrotron radiation from an inner jet region with respect to that producing
the radio-near-IR radiation. For 1510-089 the latter explanation would be
favoured by the noticeable optical variability also observed on short time
scales (e.g. Raiteri et al. 1998). Further multi-wavelength monitoring will help
to better characterize the behaviour of this component.

3. 2006AJ....131.1262H
Re:[HB89] 1510-089 NED02
1510-089: We measure m_c_ = +0.20% +- 0.09% in the core at 15 GHz in 2002
November. HW99 did not detect circular polarization in the core at 15 GHz
during 1996: three epochs had limits of 0.1%-0.2%, and for two epochs they
reported peak circular polarization values of +0.2% +- 0.2%. Homan et al.
(2001) find a limit of |m_c_| < 0.24% in the core at 5 GHz in 1996

4. 2005AJ....130.1418J
Re:[HB89] 1510-089 NED02
The radio emission of this quasar is strongly core dominated with
typically weak extended jet structure. Our data indicate that the
quasar possesses an ultrarelativistic jet with apparent speed up to
6c. However, even bimonthly observations are not sufficient to
state that the identification of components shown in Figures 9, 16,
and 42 is unique. On the other hand, this identification is supported
by the total and polarized intensity images along with the total
intensity light curves at 37 GHz (Terasranta et al. 2004) and 14.5
GHz (University of Michigan Radio Astronomy Observatory database). We
detect three moving components: B1 (Fig. 9), B2, and B3 (Fig. 42). In
all three cases we observe a similar polarization behavior in the
core region when the component is emerging from the core: the core
region is strongly polarized with EVPA along the jet direction (see
Fig. 9). In the cases of components B2 and B3, polarized features
with similar EVPA are subsequently observed propagating down the jet
(Fig. 42). For all three components the time of the ejection falls on
the rising branch of an outburst in the total intensity light curves
(an especially prominent flare is connected with the ejection of
component B2). The modeling of the jet structure shows two features,
A1 and A2, that fluctuate near positions 0.14 and 0.54 mas,
respectively (Fig. 16). Component A1 usually cannot be resolved from
a moving component at epochs when the latter is close to A1, while A2
shifts downstream when a moving component is approaching and turns
back when the moving knot has passed by (see Fig. 16). Such a
behavior of jet features formed by stationary shocks is seen in
numerical simulations of jets with variable input flow velocities
(Aloy et al. 2003). At many epochs, a feature, S, with flux
significantly above the noise is seen southeast of the core
(Fig. 17), close to the position angle of the arcsecond-scale jet
(Homan et al. 2002b). On the other hand, this component is located at
a distance from the core si milar to that of A1 but in the opposite
direction. This suggests possible artificial generation of the knot
owing to modeling of an actually slightly extended core using a
pointlike source. However, there is no correlation between the
positions and fluxes of S and A1. The position angle of S varies
within the range 71^deg^-168^deg^, and the flux varies from 0.03 to
0.5 Jy, while the values of {THETA} and the flux of A1 are fairly
stable (parameters of A1 and A2 in Table 5 are computed for epochs
when the features are not confused with moving knots). Differences in
the properties of S and A1 suggest that these features, along with
A0, constitute a complex core region inside the 43 GHz synthesized

5. 2004ApJS..155...33S
Re:VSOP J1512-0905
The redshift for this source is from Thompson et al. (1990). Optical
ID is from Hewitt & Burbidge (1993).

6. 2004ApJ...608..698S
Re:[HB89] 1510-089 NED02
1510-089. The VLA contours in Figure 1 were restored with beam size
0.4". The lowest contour is 0.45 mJy beam^-1^. Three X-ray knots are
detected (Table 2), with no optical counterparts. This jet has an
interesting morphology. The inner part up to knot B follows the radio
closely, with an almost one-to-one correspondence. After knot B, the jet
widens at both X-ray and radio, and there is no clear correspondence
between the two wavelengths. The X-ray jet is shorter than at radio:
X-ray emission ends at ~5"; from the core, while the radio continues
up to ~10", bending slightly to the west.

7. 2001ApJS..134..181J
Re:TXS 1510-089
1510-089. - This is a highly polarized quasar at optical wavelengths,
with rather bright and flat-spectrum X-ray emission (e.g., Singh, Shrader,
& George 1997). VLA images at 20 and 6 cm (Price et al. 1993) reveal an
unresolved core and a secondary component about 8" to the southeast. The
15 GHz image of Kellermann et al. (1998) reveals a short jet extended to
the north and then bending to the northwest within 2 mas of the core. In
the VLBI image at 1.67 GHz presented by Bondi et al. (1996) the dominant
component lies to the north, which suggests that the core is faint at this
frequency. That map also contains faint secondary components to the
north-northwest and south-southeast that are probably artifacts caused by
small calibration errors.
At 43 GHz (Fig. 26a) the jet has complex diffuse structure out to
1.5 mas. This seems to be in the form of a broad jet that appears to bend
from P.A. ~ -40^deg^ near the core to P.A. ~ -10^deg^ beyond 1 mas,
consistent with the lower resolution 15 GHz image of Kellermann et al.
(1998). Component C at a distance ~0.6 mas from the core is probably a
stationary feature; its model-fit parameters are similar to those of
component 2 in the 8.55 GHz map of Fey & Charlot (1997) obtained in 1995
April. In 1996.90, moving component B1 appears to merge with component C.
The model fit for epoch 1997.58 indicates the presence of a new component
(B2) near the core. Our model fitting suggests a double structure for the
farthest component, D1 and D2, with different proper motions and therefore
different times of zero separation. However, this region is heavily
resolved, leading us to consider these to belong to the same, complex

8. 2001ApJ...548..200X
Re:PKS 1510-08
3.2. PKS 1510-089
This quasar presents a pronounced UV excess, a very flat X-ray spectrum,
and a steep {gamma}-ray spectrum. The maximum brightness variation of
5.4 mag in the B band has been obtained by Liller & Liller (1975). In 1948,
this quasar underwent a period of intense activity, during which two maxima
separated by 57 days were observed: in one of these the source magnitude
reaches B = 11.8. In 1952, the brightness decreased down to B = 15.0
(Villata et al. 1997). The small-amplitude oscillations on short timescales
have been obtained by Villata et al. (1997), the total maximum variation
being 0.63 mag in the R and B bands. Our new observations on 1999 March 14
and 15 and June 14 and 15 show it to be very active each night during the
monitoring period. On 1999 March 14 it brightens from B = 17.21 to
B = 16.65 mag within 40 minutes (see Table 1 and Fig. 3). On 1999 June 14
it faded slowly from R = 16.20 to R = 16.76 mag within 28 minutes, then it
brightened rapidly to R = 16.11 mag in 13 minutes. After that it faded
again to R = 16.76 mag within 23 minutes (see Fig. 4). We also examined the
CCD brightness measurements of the field standard star 3. The maximal
deviation of the field standard star 3 for one night is 0.08 mag. That is,
the time evolution of the standard stars should not cause more than 8%
error. A rapid decline of 0.55 mag/22 minutes and a flare of 0.51 mag/26
minutes were observed, respectively, on 1999 May 15 and June 15 in the
R band (see Table 2). But it became quite stable with a variability range
smaller than 0.24 mag in the R band and 0.35 mag in the V band on 1999
March 13. Its minimum and maximum GeV {gamma}-ray fluxes registered are
1.26 +/- 0.53 x 10^-7^ and 4.94 +/- 1.83 x 10^-7^ photons cm^-2^ s^-1^
(Hartman et al. 1999).

9. 1998A&AS..131..451R
Re:[HB89] 1510-089 NED02
VLBI observations at {lambda}18cm (Bondi et al. 1996) of this low
frequency variable show a core-jet structure, with the jet extending
5mas in PA ~ 180^deg^. We found fringes to the source in 1990 for two
scans, not enough to make a hybrid map, but sufficient to make a fit to
the uv data. The result of the fit is presented in Table 14.
The resulting model fit has a Gaussian component elongated in NS, this
elongation may very well be the result of poor uv-coverage and should
not be interpreted as actual source structure.

10. 1997A&AS..121..119V
Re:PKS 1510-08
3.12. PKS 1510-089
This quasar presents strong spectral analogies with 3C 273: in both sources a
pronounced UV excess, a very flat spectrum, and a steep {gamma} spectrum are
found. From the analysis of observational data from 1933 to 1952 Liller &
Liller (1975) report a maximum brightness variation of 5.4 mag in the B band.
Between 1935 and 1945 the mean magnitude is B~15.5; during 1946 the brightness
increases and stabilizes around B=14.8 during 1947. In 1948 the quasar
undertakes a period of intense activity, during which two maxima separated by
57 days are bserved: in one of these the source magnitude reaches B=11.8. Later
on the brightness decreases down to B=15 in 1952. Between 1968 and 1977 a
further slow decrease is seen. After a maximum in 1987.3, the quasar lminosity
rapidly falls again (Pica et al. 1988).
The data we collected during our monitoring campaign are presented in Tables 5,
28, and 29, and in Figs. 24 and 25. The comparison stars adopted are shown in
Fig. 26; their magnitudes are given in Table 4. Small amplitude oscillations
are visible on short time scales, the total maximum variation being 0.63 mag in
both the R and B bands. A peculiarity of this source is the evidence of a
sensitively different trend of the R light curve with respect to the B one.

11. 1996A&A...308..415B
Re:[HB89] 1510-089 NED02
1510-089: core-jet structure. This source was a candidate for superluminal
motion after the first two epochs. Epoch 3 does not confirm such an expansion.
The observed variation is produced by a decrease of the core flux density.

12. 1995ApJS..100...37G
Re:PKS 1510-08
PKS 1510-089 was confirmed as a blazar by Moore & Stockman (1984) and
Smith et al.(1987). It is one of the most violently variable ({DELTA}V ~
5.4 during the flare states) and highly polarized quasar (Moore &
Stockman 1981; Ledden & O'Dell 1985; Mead et al. 1990; Burbidge & Hewitt
1992). This blazar has been classified as an RBL (Hewitt & Burbidge
1993). Two spectra of this source, obtained with EXOSAT have signal
significances above 4{sigma}, and these two spectra can be best fitted
with the power-law plus absorption model; the parameters are listed in
Table 3. Variations of the LE and ME fluxes, on time-scales of hours, are
absent in this source. There is no detection of any significant low-
energy absorption within this flat spectrum. Results of our spectral
analysis are consistent with the results of Singh, Rao, & Vahia (1990).
Radio through X-ray continuum fluxes of this object are shown in Figure
3j, and the spectrum can be well represented by two parabolic components.

13. 1994A&A...289..673T
Re:OR -017
1510-089 (OR 017)
This source has gone through several flares which have been
simultaneously visible both at optical and all of our radio frequencies.
The most prominent flaring events were observed in 1987.2 and 1988.4,
and a smaller one in 1990.2. The time delays from optical to all the
four radio frequencies are small. The two strongest optical outbursts
with 90 GHz counterparts are not very well sampled and the best that can
be said is that the time delays between the frequencies are smaller than
our bin size of 50-100 days. Optical and radio events after 1990 have
been studied also in Borgeest et al. (1993) and similar results of strong
correlations with no time lags between optical and the radio frequencies
22 and 37 GHz were found in several events. Typical for this source seem
to be relatively fast outbursts also in the radio regime; even at the
lower frequencies the faster flares rise and fall within less than 100

14. 1992AJ....104.1311H
Re:[HB89] 1510-089 NED02
1510-089 (z = 0.36). Neither the R nor narrowband profiles can be seen to
be extended, and no faint structure is seen in them. See comments below on
the continuum subtracted image.

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