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Notes for object PG 1302-102

16 note(s) found in NED.


1. 2009ApJ...705..962C
Re:PKS 1302-102
This sight line contains a strong high-velocity O VI feature (S03, CSG05) with
no associated absorption in any other ions, including Si III. We use the V_LSR_
= 200 to 340 km s^-1^ extent of the O VI feature to establish an upper limit on
the Si III absorption.

2. 2008ApJS..179...37T
Re:PKS 1302-102
3.14. PKS 1302-102 We searched the STIS data for PKS 1302-102 (z_qso_ = 0.2784)
for O VI absorbers in the range 0.1183 absorbers at z_abs_ = 0.22565, 0.22744. This sight line has also been studied by
Cooksey et al. (2008).
z_abs_ = 0.22565(Fig. 26; Table 16).-As with the H1821+643 absorber pair,
these absorbers at z_abs_ = 0.22565 and z_abs_ = 0.22744 along the PKS 1302-102
sight line are separated by only {delta}v = 440 km s^-1^. Also similar to the
previous example, this absorber pair consists of a strong and weak system, with
the weaker system at a slightly higher redshift (although in this case, the
difference is far less dramatic). The system at z_abs_ = 0.22565 consists of two
well-defined O VI components separated by 28 km s^-1^. Both O VI components have
matching H I absorption, detected primarily in Ly{alpha}. The two strong lines
at the expected positions of the N v doublet are obviously unrelated Ly{alpha}
absorbers. The temperature and nonthermal broadening can be determined for only
the v = 0 km s^-1^ component (log T = 4.4; b_nt_ = 12.5 km s^-1^), since the H I
position for the component at v = -28 km s^-1^ has been fixed to that of O VI in
our fitting; see {section} 5.2 for details.
z_abs_ = 0.22744(Fig. 27; Table 16).-The weaker of the two close O VI
absorbers toward PKS 1302-102, this system has only very weak transitions of O
VI {lambda}{lambda}1031, 1037 and Ly{alpha}. The O VI {lambda}1031 line is close
to, but unaffected by, a strong Ly{alpha} absorption line at z = 0.4224. Both
species are well aligned and suitable for temperature analysis in {section} 5.2.
We derive log T = 4.2 and b_nt_ = 10.7 km s^-1^.

3. 2008ApJS..179...37T
Re:PKS 1302-102
4.10. PKS 1302-102 z = 0.19159.-This system is another example that we are
unable to confirm due to lack of O VI {lambda}1037 absorption. A line at the
position of O VI {lambda}1031 is present, as is saturated Ly{alpha}, and
possibly Si III {lambda}1206. Given the strength of the apparent O VI
{lambda}1031 line (~62 mA), we should expect to detect any O VI {lambda}1037
line, but no significant absorption exists, and the O VI {lambda}1031 profile
fit is a poor descriptor of the data in the O VI {lambda}1037 region. The
independent work of Cooksey et al. (2008) confirms this result; those authors
report Ly{alpha} and O VI {lambda}1031 but do not detect O VI {lambda}1037 (see
their Table 3).

4. 2008ApJS..175..314D
Re:VSOP J1305-1033
J1305-1033.-The core is <0.2 mas in size. No additional structure is seen with
VSOP because of lack of short spacings.

5. 2008ApJ...687..767K
Re:PG 1302-102
(Fig. 37).-This object was observed in two different filters (F606W and F702W),
but both images are saturated in the core. The image contains two compact
sources superposed on the main host, which we fit simultaneously. The host can
be fit with a single bulge component, although significant structure on large
scales remain in the residual image. The fits from both filters are in good
agreement to within the uncertainty.

6. 2003ApJS..146....1W
Re:PG 1302-102
PG 1302-102.-This object has a wavy continuum, so that it is necessary
to fit a fifth-order polynomial. This makes the continuum near the
O VI {lambda}1037.617 line too uncertain to confidently compare the
O VI {lambda}1031.926 and O VI {lambda}1037.617 column densities.
The sight line passes through the Virgo Cluster
(v = 1360 +- 720 km s^-1^). The feature at 1030.237 {angstrom}
(-490 km s^-1^ on the O VI velocity scale) is Ly{beta} at
1320 km s^-1^ associated with the Virgo Cluster, as there is a
330 m{angstrom} Ly{alpha} line at 1220.985{angstrom} in the STIS
spectrum. The corresponding Ly{gamma} line is blended with
C III {lambda}977.020, which falls at v = 1375 km s^-1^ on the
Ly{gamma} velocity scale. The C III absorption seems to have a
wing at v(Ly{gamma}) ~1300 km s^-1^, however, which is where the
intergalactic Ly{gamma} would be expected.
The feature at 1032.804 {angstrom} (255 km s^-1^ on the O VI velocity
scale) is most likely high-velocity O VI, as there appears to be a
corresponding feature in the O VI {lambda}1037.617 line, and in many
sight lines in the neighborhood of PG 1302-102 high positive velocity
O VI is also found (e.g., HE 1115-1735, HE 1143-1810, and 3C 273.0).
This feature might be Ly{beta} at v = 2070 km s^-1^, but there is no
Ly{alpha} at that velocity in the STIS spectrum of this target.
The apparent structure in the high-velocity component is caused by noise
peaks in the shorter observations.
This spectrum is particularly rich in Lyman systems. There are systems
at z = 0.09397 and 0.09484 (both in Ly{alpha} to Ly{eta}, both showing
C III), at z = 0. 14537 (Ly{alpha}, Ly{beta}, as well as a weak C II
{lambda}903.9616 at 1035.482{angstrom}, 1033 km s^-1^ on the O VI
velocity scale) and at z = 0.19160 (Ly{alpha} through Ly{zeta}. Another
system near z = 0.097 is less clear in just Ly{alpha} and Ly{beta}. In
none of these systems do H I, C III, or low-ion lines fall near Galactic
O VI.

7. 2002ApJS..140..143B
Re:PG 1302-102
q1302-1017, z = 0.286.-PKS. J98 present the FOS spectrum. G270, G190,
G130.

8. 2001A&A...371...97M
Re:PKS 1302-102
3.1 PKS 1302-102
The image obtained at CFHT under moderately good seeing conditions is of
similar quality to that obtained with HST by Bahcall et al. (1995) (see
for comparison Hutchings et al. 1994) with FWHM = 0.24 arcsec after
deconvolution (see Fig. 1). The two objects at 1 and 2 arcsec from the
quasar are well-detached, and are more clearly seen when both the PSF and
a model for the host-galaxy (obtained by masking the companions and fitting
ellipses to the isophotes) are subtracted. It is unlikely that these
companions are intervening objects as strong associated metal line
absorption would be expected at such a small impact parameter when no such
absorption is detected in the HST spectrum down to w_obs_ ~ 0.2 A
(Jannuzi et al. 1998). The host-galaxy of this quasar has been detected by
HST and fitted with a r^1/4^ profile (Boyce et al. Disney et al. 1995).
Marquez et al. (1999) derive that the galaxy contributes 40% the total flux
in the J-band when McLeod & Rieke (1994) measure this contribution to be 31%
of the total flux in the H-band after fitting an exponential profile to the
host-galaxy. We have performed a similar fit on the present data and found
that the contribution of the galaxy amounts to 39% in H and 18% in K (see
Table 2). However, Fig. 4 shows that an r^1/4^ profile is a better fit.
In that case, the contribution of the host-galaxy to the total light is
70% (60%) in H (K), in good agreement with the values derived by
subtracting a scaled version of the PSF and directly integrating the
residual flux.

9. 2000ApJS..129..563S
Re:PKS 1302-102
PKS 1302-102 (z_em_ = 0.286). - This QSO was observed with the
G130H, G190H, and G270H gratings (see Table 4). The modest average
velocity equivalent width for Mg II of = 94 km s^-1^ is
consistent with the 21 cm emission full extension width of
{DELTA}v(H I) = 115 km s^-1^ (from Table 2) and the absence of H I HVCs
along this line of sight.

10. 1999A&A...348..653S
Re:[HB89] 1302-102
1302-102 has higher than average errors in the CAMC stars, and the range
of the brightest CAMC star to the QSO is very large (5.6 magnitudes)
which means the signal to noise of the QSO is low. Again, perhaps the
formal error here is an underestimate and the difference found is not
significant.

11. 1998MNRAS.296..721C
Re:PKS 1302-102
3.7 PKS 1302-102
Our spectrum of PKS 1302-102 is similar to that published by EH94. The H{alpha}
profile is comparatively narrow (FWHM=3500+/-200 km s^-1^) and is asymmetric,
with the red wing being more extended than the blue. The only narrow lines which
are clearly seen in the spectrum are H{alpha} at an observed wavelength of
{lambda}=8388+/-2 A and the [S II]{lambda}6717, 31 lines at observed wavelengths
of {lambda}=8586+/-2 and 8604+/-2 A, respectively. These lines have an average
redshift of z=0.2784+/-0.0005, which differs significantly from the value of
0.286 quoted by Boroson & Green (1992). The slight shoulder in the H{alpha}
profile at 940+/-150 km s^-1^ is probably due to the [N II]{lambda}6583 line
which should be present at an observed wavelength of {lambda}=8413+/-2 A.
In comparison with most of the other objects in our ample, the continuum is
relatively weakly polarized, with P~0.40 (Table 2). No significant polarization
was detected in the broad-band observations of Wills et al. (1992) but, as for
Mrk 668, their measurements do not exclude polarization at the level we find
in our data. There are no significant variations in either P or {psi} over the
whole wavelength range covered by our spectra - this is the only object in our
sample in which there are no changes associated with the broad H{alpha}
line. The average emission-line polarization (after continuum subtraction) is
the same, within the errors, as that of the continuum (Table 2).
The compact (<~10 arcsec) radio source has a bright, unresolved core with twin
lobes extending several arcseconds to the NE (PA~20^deg^) and SE (PA~140^deg^)
(Hutchings et al. 1994). The optical continuum polarization angle is roughly
aligned with the NE radio lobe, but this is probably fortuitous. Given the
relatively low value of P and the lack of variation in either P or {psi} over
the spectrum, it seems likely that the measured polarization is largely due to
dichroic absorption along the line of sight either in the Galaxy, or in the host
galaxy of PKS 1302-102. A differential extinction E(B-V)~0.15 mag would
typically be required to produce the observed level of polarization.

12. 1998ApJ...495..152L
Re:PKS 1302-102
PKS 1302-102.--BKS95 found two companions within 25 kpc. The limit set by BKS95
was just 0.4 mag fainter than L*. This quasar was also observed by Disney et
al. (1995), who detected a host galaxy using a different filter and detector
(the Faint Object Camera, rather than the Wide Field/Planetary Camera). When
they apply a standard color correction for the elliptical galaxy that they
detected, they find that their detected galaxy is 0.2 mag fainter than the
BKS95 limit. This galaxy has been included in several studies of the
environments of quasars. Green & Yee (1984) find 10 galaxies on their 140"
field frames. Its cross-correlation with galaxy counts is typical of an Abell
richness class 0 cluster, but the significance of the cross-correlation is
marginal (Yates et al. 1989; Yee & Ellingson 1993).

13. 1997ApJ...479..642B
Re:PKS 1302-102
The HST images show there are two small compact galaxies at 1" and 2"
from the quasar, which are expected to spiral into the quasar in a time
short compared to the Hubble time (Bahcall et al. 1995a). The presence of
these very close companions can be seen most clearly in the expanded
image, Figure 8, of Bahcall et al. (1995a). Hutchings & Neff (1992)
performed optical imaging with 0.5" resolution and reported structures at
the positions of those galaxies; they suggest the host is a mildly
disturbed elliptical galaxy. The PSF-subtracted residual image (see Fig.
2) appears to the eye to be similar to an elliptical galaxy, but an
exponential disk fits the data slightly better. The absolute V magnitude
estimated for the host galaxy is 0.4 mag fainter than the value
determined from the McLeod & Rieke (1994b) H-band observations and is 0.9
mag fainter than the value estimated from i-band images (Veron-Cetty &
Woltjer 1990). Wyckoff et al. (1981) obtained R = 19.0 for the host;
using the Fukugita et al. (1995) transformations of galaxy colors, this
corresponds to M_V_ ~ -20.0.

14. 1995AJ....110.1492R
Re:PKS 1302-102
1302-102: This source is not fully resolved. The value of the FR ratio is
a lower limit because the outer edge of the jets are not resolved and it
is probable that the source is more edge brightened than calculated.

15. 1995AJ....110.1492R
Re:PKS 1302-102
1302-102: The low surface brightness gives evidence for jet-like
structure which is used to measure the bending angle. However, it is only
suggestive of outer lobes so that the FR ratio is merely a lower limit.

16. 1992AJ....104....1H
Re:[HB89] 1302-102
1302-102. This z=0.29 QSO had no resolved structure
in our previous work, although the profile was more ex-
tended than that of a star. Veron-Cetty & Woltjer (1990)
show an extension to the north. Our new optical data shows
this feature (Fig. 2) 2 arcsec to the north, some 0.5 arcsec
wide, and also a bright feature only 0.8 arcsec from the
nucleus, to the west. These two features are elongated along
the same line, and thus may be related, or even be parts of
a single feature which is obscured or fainter in the middle.
Figure 2 shows this in the model-subtracted image (besides
the telescope diffraction spikes). In this object, the outer
knot is redder than the main galaxy, and the inner feature
is too close to the edge of the guiding hole to measure its
color. The host galaxy has no other structure, being a
smooth ellipse with a small eccentricity. The luminosity
profiles are close to an R^1/4^ law for the inner 3 arcsec
radius, and there is an exponential halo outside this, which
we can measure to a radius of 7 arcsec.
Gower & Hutchings (1984) found small (15 arcsec)
two-sided radio structure to the northeast and southeast, with a 570
mJy core at 20 cm. The compact radio core is unresolved
at 21 cm (this work) on a scale of 100 X 40 milliarcsec at
10^deg^ P.A., and contained 640 mJy flux in that size at the
time of the observations. Thus, essentially all of the radio
emission arises from a size of <=300 pc. The optical and
radio structures have no features in common: rather, the
radio lobes are swept back from the inner optical knot. The
bent morphology and extent (45 kpc) of the extended ra-
dio emission suggest that the radio source is moderately
old and/or poorly confined.
The hybrid luminosity profile is consistent with a mildly
disturbed elliptical galaxy. The linear nature of the object
nearest the nucleus suggests the trajectory of a small merg-
ing companion. We suggest that the companion may have
been spiralling into the main galaxy for some time. The
smoothness of the profile and presence of the small com-
panion(s) suggest this rather than an old merger where a
new elliptical has formed after merging with a massive
companion. This is in agreement with the relatively undis-
turbed extended radio source.


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