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Date and Time of the Query: 2019-06-24 T03:51:53 PDT
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Notes for object PG 0044+030

5 note(s) found in NED.


1. 2002ApJS..140..143B
Re:PKS 0044+030
q0044+0303, z = 0.624.-The FOS spectra are previously discussed in
Bahcall et al. (1993). They describe C IV at z = 0.245 and z = 0.449.
The z = 0.449 system may be identified with an intervening galaxy
at the same redshift (Ellingson, Green, & Yee 1991). The evidence for
the z = 0.245 spectrum is weak, given that only the C IV doublet is seen
in the Ly{alpha} forest part of the spectrum, so the probability of a
chance coincidence is high. G270, G190.

2. 2000ApJS..129..563S
Re:PKS 0044+030
PKS 0044+030 (z_em_ = 0.624). - Sight line is ~ 1^deg^ from
PG 0043+039, but no MS component in Mg II is observed. That is
consistent with the absence of an H I MS detection in the NRAO wide-band
observations.

3. 1996AJ....111..645F
Re:[HB89] 0044+030
0044+030
double, northern object may be slightly elongated on POSS-E.

4. 1995A&A...298..375F
Re:PG 0044+030
This source has a relatively low total flux and appears diffuse elongated
on a recent VLA map at 20 cm while at 6 cm only the core prevails (Price
et al. 1993).

5. 1994AJ....107.1219E
Re:PKS 0044+030
PKS 0044+030. There is no detected associated absorption in the spectrum
of this radio-loud quasar at z = 0.624. However, Bahcall et al. report
intervening C IV absorption at z = 0.4493. They also report that efforts
to detect Mg II at this redshift have been inconclusive.
Our images of this field [Fig. 2(b)] suggest that there may be a
cluster of galaxies associated with this quasar. While the calculated
value of B_gq_ for a radius of 250 kpc is only 86+/-87 Mpc^1.77^,
suggesting at most a poor cluster, there is a dense knot of galaxies
around and to the northeast of the quasar. The value of B_gq_ for a
radius of 125 kpc is 381 Mpc^1.77^, in agreement with the existence of
a very dense concentration of galaxies right around the quasar. Gunn r-i
colors of these galaxies imply that they are probably elliptical galaxies
at a redshift of at least z = 0.5. It may be that in this field, the
foreground /background density is statistically lower than average. If
so, the value of B_gq_, calculated over a large area may be too low and
there may actually be a substantial compact cluster associated with the
quasar.
Assuming that they are at the cluster redshift, three galaxies lie
within 60 kpc of the quasar and all of them have absolute magnitudes of
~-20.8. Ellingson et al (1991) obtained redshifts of a number of galaxies
in this field. However, none of these were of galaxies within 60" of the
quasar and none were found to be at the quasar redshift. This leaves the
possibility of a cluster associated with the quasar as yet inconclusive.
However, one galaxy was found to have a redshift of 0.4486+/-0.0006, at
the same redshift as the intervening C IV absorption. This galaxy is
located 80 arcsec from the quasar, and while it is probably not the
absorber itself, its redshift indicates that it is associated in some
manner with it. It may be that the galaxies close to the quasar are
actually a group or cluster at the intervening redshift and are not
associated after all. If any of the three galaxies closest to the quasar
is at z = 0.449, it would have an absolute magnitude of ~-19.6, or about
0.5M^*^, and the closest of these candidates would be at a distance of
33 kpc.


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