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Date and Time of the Query: 2019-08-20 T05:26:32 PDT
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Notes for object PKS 1519-273

14 note(s) found in NED.


1. 2008ApJS..175..314D
Re:VSOP J1522-2730
J1522-2730.-The core is 0.25 mas in size. There is extended structure to the
west.

2. 2006A&A...456..131P
Re:PKS 1519-273
Another source of comparable flux ~ 7.5 pixels away in the LW7 image; we then
estimated the background in a two (instead of four) pixel wide annulus. No
significant detection in the LW3 filter.

3. 2005AJ....129..559S
Re:PKS 1519-273
Our VLT spectra yield z = 1.297 and confirm the results obtained by
Heidt et al. (2004), who detect an emission line identified as Mg II
{lambda}2798, giving z = 1.294. Several absorption features from the
ISM of our Galaxy are observed in this spectrum: DIBs at 4428, 4726,
4882, and 5772 A, along with the Ca II {lambda}{lambda}3934, 3968 and
Na I {lambda}5892 atomic lines. Although the redshift of this source
is based only on a single line, the value z = 0.07, proposed by
Zensus et al. (2002, no spectrum published), appears inconsistent
with our data.

4. 2004A&A...424...91E
Re:PKS J1522-2730
J1522-2730 is classified as a BL Lac object, and, as noted in Sect. 2,
shows the highest variability index of this group. The redshift for this
object was recently reported by Heidt et al. (2004). Intra-Day
Variability at radio wavelengths has been observed in this source
(Jauncey et al. 2003; Kedziora-Chudczer et al. 2001) and VLBI imaging
confirms the core is very compact (e.g., Fomalont et al. 2000).
Tornikoski et al. (2001) present a composite spectrum derived from a
large number of observations, and note that the source appears to
have a relatively flat quiescent spectrum that is inverted during
flares. The high variability and apparent lack of a persistent GHz
peaked spectrum suggest this is less likely to be a bona fide GPS
source.

5. 2002AJ....124..662Z
Re:IERS B1519-273
1519-273: This BL Lac object has a featureless spectrum and a
high degree (5%-12%) of variable optical linear polarization
(Impey & Tapia 1988). It displays IDV at radio frequencies and also
in circular polarization (Macquart et al. 2000). It is unresolved at
kiloparsec scales (Cassaro et al. 1999). Our image shows a very
compact structure with slight extension to the west.

6. 2002A&A...386...97J
Re:PKS B1519-273
A BL Lac object, the featureless spectrum seen by White et al.
(1988ApJ...327..561W), Veron-Cetty & Veron (1993ESOSR..13....1V) and
ourselves (Paper II). PKSCAT90 gives a redshift of 0.510, but no such
redshift measurement is present in the literature.

7. 2001AJ....122..565R
Re:PKS 1519-273
PKS 1519-273. - No spectral features are present, in agreement with
SFK93 and White et al. (1988). However, because of its low declination, we
were unable to obtain a high-quality spectrum. Further observations are
needed. It is optically unresolved (SFK93), suggesting z > 0.2.

8. 2001AJ....121.1306T
Re:PKS 1519-273
B1519-273. - A BLO with unknown redshift and high optical polarization
(p_max_ = 11.4%; Impey & Tapia 1988, 1990). This source is listed as a
bona fide GPS source in de Vries et al. (1995), with {nu}_T_ = 5 GHz. Our
plot shows a relatively flat quiescent spectrum that is inverted during
flares.

9. 1999ApJS..121..131F
Re:PKS 1519-273
This polarized (P_opt_ =11.4%, Impey & Tapia 1988) object has been
observed only twice, by Gear (1993) and Glass (1981). The observations
indicate color indices of (J-H)=0.45+/-0.21, (J-K)=1.35+/-0.17, and
(H-K)=0.90+/-0.24. The optical variation is {DELTA}m=2.43 (Fan 1997).

10. 1999A&AS..139..601C
Re:PKS 1519-273
1519-273: this is a very compact source, unresolved in our images at the
resolution of 1". The source is still unresolved at the mas scale
(O'Dea et al. 1991; Shen et al. 1997). Perley (1982) gives an upper
limit of about 5 mJy for any extended emission. We did not detect
significant extended emission above 0.5 mJy/beam, and we do not show any
image for this source.

11. 1994ApJS...93..125F
Re:PKS 1519-273
1519-273.-We obtained one spectrum of this faint (m_V_ ~ 19) radio-
selected object with unknown redshift. We found that the energy
distribution is structureless (in agreement with White et al. 1988) and
well represented by a simple power-law model.

12. 1994A&AS..105..211S
Re:[KWP81] 1519-273
The classification as a BL Lac Object as well as the optical spectrum is
given by Stickel et al. (1993b) and Veron-Cetty & Veron (1993).

13. 1993A&AS..100..521V
Re:PKS 1519-273
PKS 1519-273 (Bolton et al. 1975) has been identified with an 18.5 mag
starlike object (Peterson et al. 1973) with a featureless spectrum (White
et al. 1988) and a high degree of optical polarization (Impey & Tapia
1988; 1990). The radio (Perley 1982) and optical (Argue & Sullivan 1980)
positions are in good agreement. The radiosource is flat, shows signs of
variability (Bolton et al. 1975; Condon et al. 1977; Steppe et al. 1988)
and has a VLBI core (Preston et al. 1985; Wehrle et al. 1984; Morabito et
al. 1986).
An image obtained on May 6, 1989 with the ESO/MPI 2.2 m telescope
through a Gunn i filter with a 1.4" seeing shows an elongation toward
East. Our spectrum is featureless confirming that this object is most
probably a BL Lac.

14. 1993A&AS...98..393S
Re:PKS 1519-273
1519-273
Neither emission nor absorption features have been detected in the
optical spectrum, in agreement with the observations of White et al.
(1988). The unresolved appearance on the direct image gives a lower
redshift limit of z >~ 0.2.


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