Date and Time of the Query: 2019-08-17 T05:41:24 PDT
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Notes for object [HB89] 0215+015

6 note(s) found in NED.

1. 2008ApJS..175..314D
Re:VSOP J0217+0144
J0217+0144.-The core is unresolved, <0.1 mas in size. The faint extended
structure from lower resolution VLBA images is not detected.

2. 2005A&A...435..839T
4.2 Previously identified inverted-spectrum sources
B0215+015: this source is a BL Lac object at redshift 1.72
(Falomo et al. 1994). It is observed to be a violently variable AGN
(Schramm et al. 1994). Its optical polarization is high: 17.4%
(Wills et al. 1992). Using simultaneous data (epoch 14 Jun., 1999) from
the Very Large Array (VLA), which showed a convex spectral shape,
Dallacasa et al. (2000) classified this source as a high frequency
peaker (HFP) having a peak at a frequency of more than 22 GHz. Our plot
in Fig. 3 confirms the convex shape of the upper envelope but the lower
envelope is quite steep. Our data show that the source was having a
flare at the time of Dallacasa et al. were observing it with the VLA in
July, 1999. This source is indeed very variable (Var_{DELTA}S_(37) =
10.25) and during the outbursts the spectrum is inverted.

3. 2002A&A...386...97J
Re:PKS B0215+015
Extremely variable BL Lac object (Bolton & Wall, 1969AstL....3..177B;
Gaskell, 1982ApJ...252..447G).

4. 1994ApJS...93..125F
Re:[HB89] 0215+015
0215+015:-This radio-selected source is one of the most distant (z = 1.72
Boisse & Bergeron 1988) BL Lac objects known. Some intervening narrow
absorption lines are present in our spectra but no emission lines are
detected, probably because we observed the source in a brighter state
compared to the one observed by Boisse & Bergeron (1988), who found weak
C IV emission lines. The energy distribution is compatible with a single
power-law model.

5. 1994A&AS..106..349S
Re:PKS 0215+015
PKS 0215+015 is a BL Lac object with a very high redshift. WSLF have
monitored this object since 1981 and detected variations over a 3.5 mag
range. Our data indicate violent variability, too; however, both observed
time-span and amplitude are smaller.

6. 1992ApJ...400..435K
Re:[HB89] 0215+015
0215+015 (z_em_ = 1.715)
The well-observed complex absorption features seen between the
Ly{alpha} emission line and the Lyman edge at 912A have been
investigated by Blades et al. (1983, 1985). We have not taken into
account the absorption features in the fit presented in Figure 2.
Nevertheless, the fit correctly shows a partial discontinuity at
z_abs_ = 1.715 associated with some known absorption lines and a
complete discontinuity at z_abs_ = 1.346.

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