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Date and Time of the Query: 2019-08-19 T07:38:33 PDT
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Notes for object PKS 0118-272

13 note(s) found in NED.


1. 2005A&A...442...97A
Re:PKS 0118-272
0118-272: the linear optical polarization of this object was measured by Impey &
Tapia (1988) with a significantly high value (P_V_~17%). This was one of the
reasons for its classification as a blazar; a similar result was obtained by
Mead et al. (1990). We observed this blazar on two consecutive nights,
presenting variability on the first one, with the degree of polarization rising
from P = 5.77% to P=9.41% in about one hour. On the second night, the degree of
polarization appears as not variable but with a value of about 8%. Meanwhile,
the position angle was variable with similar averages on both nights.

2. 2000ApJS..131...95F
Re:VSOP J0120-2701
J0120-2701. - VLBI image at 5 GHz is published by Shen et al. (1998).
Their centrally symmetric S-shape structure is not confirmed from our
image. It is a prominent radio and X-ray source.

3. 1999ApJS..121..131F
Re:PKS 0118-272
An absorption feature at z=0.559 was found by Falomo (1991). It was
observed in the infrared during the period JD 244,000+4,773-7,753. For
this object, there are no correlations for color-color indices or for
color index and magnitude. It is a highly polarized object (P_opt_ ~17%)
and shows dP/d{nu}>0 (Mead et al. 1990).

4. 1999A&AS..139..601C
Re:PKS 0118-272
0118-272: the radio image from the A array (1.36 GHz in Fig. 3) shows a
halo around the core that contributes significantly to the total
luminosity, while the B configuration image (not shown) displays only a
marginally resolved structure. In the image at 4.88 GHz (Fig. 4) there
is a hint of a jet extending towards SE. Previous observations of this
source are reported by Perley (1982). Our higher dynamic range allows to
image the extended emission to larger distances than in Perley (1982);
the diffuse emission in our image extends to 18 arcseconds.

5. 1998ApJS..118..327K
Re:MRC 0118-272
A known BL Lac object with an absorption-line system at a redshift of
0.557 (Falomo 1991; Stickel, Fried, & Kuhr 1993).

6. 1998AJ....115.1357S
Re:PKS 0118-272
PKS 0118-272 (OC -230.4, Fig. 1a).--This is a BL Lac object with a tentative
emission-line redshift of z=1.62 (Adam 1985 and references therein). A lower
limit of z>0.559 was suggested from several absorption lines (Falomo 1991;
Stickel, Fried, & Kuhr 1993). Strong optical variations of 100% within 3 days
have been reported (Falomo, Scarpa, & Bersanelli 1994). PKS 0118-272 is also
highly optically polarized (Impey & Tapia 1988; Mead et al. 1990).
A 20 cm Very Large Array (VLA) observation revealed a complex structure, while
at 6 cm the source exhibited at least three components within 1" (Perley
1982). A single-baseline 2.3 GHz VLBI observation yielded a correlated flux
density of 0.53+/-0.05, corresponding to a visibility of 0.5+/-0.2 (Preston et
al. 1985). Our observations showed a resolved core with diffuse surrounding
emission. The data were fitted by a single north-south elongated Gaussian
component with a flux density of 0.55 Jy. However, the core accounts for only
half the total flux density of the source, which supports the presence of two or
three additional weak features in the vicinity. The source has a spectral index
of 0.02 at millimeter wavelengths (Steppe et al. 1988), with a total flux
density of 0.60 Jy at 230 GHz.

7. 1998A&A...336..479K
Re:PKS 0118-272
Our H-band magnitude is slightly fainter than that found in the
literature (Table 6). The host galaxy remains unresolved in the
optical (Falomo 1996), however, this is consistent with the presence of
a luminous host (M(R) = -23.5) at the proposed redshift of z>0.559. The
host galaxy remains unresolved in the NIR.

8. 1996MNRAS.283..241F
Re:PKS 0118-272
0118-272 This is a relatively bright BL Lac source that shows a power-law
spectrum in the UV to near-IR region(see e.g. Pian et al. 1994). The optical
spectrum is featureless apart from a narrow absorption doublet identified as
Mg II 2800 and yielding a lower limit to the redshift of z=0.559 (Falomo 1991).
We secured images of this target at two epochs (see Table 1). In one case,
several short (2 min) exposure frames were obtained from the 'service
operation' mode available on the NTT. These images were then co-added to
obtain one single average frame. Our images show that this source is not
resolved even at sub-arcsec resolution. The radial brightness profile is
well-matched by the estimated PSF down to the faintest surface brightness
(see Fig. 2). The observation is still consistent with the presence of a
luminous host (M_R_=23.5) at z>~0.6.
There are several faint galaxies in the neighbourhood of the BL Lac object.
Within a circle of 30 arcsec radius (corresponding to ~250 kpc at z=0.56), we
find ~15 galaxies with magnitudes in the range of 20.5 to 21.5. The closest
galaxy (m_R_=21.1) lies at 8 arcsec (PA~40). These galaxies are likely to form
a foreground small cluster at z=0.56.

9. 1994ApJS...93..125F
Re:PKS 0118-272
0118-273.-Ten spectra were secured for this radio-selected BL Lac object.
The optical emission is smooth and well represented by a power law. Only
a weak absorption line is present, which was identified as
Mg II(2798 A) at z = 0.557 (Falomo 199 1b). Flux variability was detected
on short time scales, with a variation of 100% in 3 days. The spectral
index has shown some variation with a maximum {DELTA}{alpha} = 0.55.

10. 1994A&AS..105..211S
Re:[KWP81] 0118-272
The optical spectrum and the absorption line redshift are given in
Falomo (1991) and Stickel et al. (1993b). An incorrect absorption line
redshift is listed in Veron-Cetty & Veron (1991).

11. 1993AJ....106...11F
Re:PKS 0118-272
0118-272
A high redshift blazar exhibiting an absorption feature at z = 0.559
(Falomo 1991). The image of the object is unresolved. The source was
observed at three epochs; brightness variations of ~15% are found. Its
spectral flux distribution is always well represented by a single power
law of {alpha} ~ 1.1. The same power law is found to extend in the UV up
to 1.2 X 10^15^ Hz (Falomo et al. 1993).

12. 1993A&AS...98..393S
Re:MRC 0118-272
0118-272
The unresolved image of this object is consistent with the lower redshift
limit of z_abs_ = 0.557, derived from a single absorption line in the
spectrum, which was identified with Mg II {lambda}2798. This absorption
feature has also been detected by Falomo (1989). With subsequent medium
resolution spectroscopy, Falomo (1991) was able to resolve the Mg II
{lambda} 2796,2803 doublet. The stellar appearance of this object was
already noted by Falomo et al. (1990). There appears to be a cluster of
faint (m >= 21 mag) galaxies surrounding 0118-272, also noticed by Falomo
(1991). It would be very important to measure the redshifts of a few of
these surrounding galaxies in order to check if some of these cluster
galaxies have the same redshift as the absorption line system found in
the BL Lac spectrum. Very weak broad emission features have been
observed by Wills & Wills (1976), from which Adam (1985) suggested a
tentative redshift of z = 1.62. Although highly uncertain, this value is
consistent with the lower redshift limit derived from the observed
absorption feature. It should be noted that an incorrect absorption line
redshift for 0118-272 is listed in the catalogue of Veron-Cetty &
Veron(1991).

13. 1976ApJS...31..143W
Re:PKS 0118-272
0118-272: The ultraviolet continuum is not as strong as in typical QSOs,
although the large zenith distance of the object may be partly responsible for
this. There is no obvious break near Ca H and K, and the object is probably
not a star. One spectrogram showed a possible emission line at 4061 A and
possible absorption at 5006 A; it is probably not significant that the
wavelength ratio is close to that of C III] and C IV {lambda}{lambda}1549,
1909.


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