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Date and Time of the Query: 2019-08-24 T20:31:51 PDT
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Notes for object [HB89] 0637-752

8 note(s) found in NED.


1. 2008MNRAS.384..775M
Re:PKS 0637-752
Table 2 source 92 (PKS 0637-752) is a quasar with an asymmetric jet seen in
radio and X-ray images (Schwartz et al. 2000). The tabulated flux density is
dominated by the core with about 10 per cent in the 15-arcsec jet. It is one of
the largest (100 kpc) and most luminous jets known with properties similar to
3C273.

2. 2006ApJ...638..642B
Re:PKS 0637-75
PKS 0637-75 - Several sources may have been marginally suspected in the
INTEGRAL data. They either were targets of dedicated observations or were
detected in some single science windows. We performed the same analysis as
for the other sources presented here, but found only spurious source
candidates that result from image reconstruction problems such as ghosts
and mask patterns. Among those sources are Mrk 231, ESO 33-2, PKS 0637-75,
MCG -05-23-16, QSO 1028+313, NGC 4736, NGC 4418, 3C 353, and QSO
1730-130.8

3. 2004ApJS..155...33S
Re:VSOP J0635-7516
An image made from all the GOT data is found in VSOPsth. The core is
complex and extended. We have used the easternmost component in our
determination of core brightness temperature.

4. 2003AJ....126.2237D
Re:[HB89] 0637-752
.
4.7. Quasars
.
There are a number of known radio-loud quasars in the radio-excess
sample: PKS 0104-408 (F01044-4050), Q0521-365 (F05212-3630), Q0558-504
(F05585-5026), Q0637-752 (F06374-7513), Q1244-255 (F12440-2531),
3C 345 (F16413+3954), PKS 2313-477 (F23135-4745), and Q2349-014
(F23493-0126). These objects all have high radio powers [L_{nu}_(4.8
GHz) > 10^25^ W Hz^-1^] and FIR luminosities {nu}L_{nu}_(60 micron) >
10^10.7^L_solar_. All but one of these quasars have large radio
excesses with u < -0.2; Q0558-504 is the exception.

5. 2002ApJS..140..143B
Re:[HB89] 0637-752
q0637-7513, z = 0.656.-We identify metal absorption at z = 0.152 and
0.416. The spectrum is also discussed in J98. G270, G190.

6. 2000ApJS..129..563S
Re:PKS 0637-75
PKS 0637-75 (z_em_ = 0.654). - The direction to PKS 0637-75 passes
through the MS where the H I has been detected in 21 cm emission with
v = 245 km s^-1^ and T = 0.18 K (Bajaja et al. 1985). The broad strong
Mg II profiles have each been fitted with two Mg II absorbing
components. The wavelength zero point for the PKS 0637-75 G270H spectrum
appears to be off by ~ 1.5 A, or ~ 160 km s^-1^. With that adjustment we
identify the shorter wavelength Mg II absorption components with
W_{lambda}_ = 0.98 +/- 0.17 and 1.33 +/- 0.27 A as the Galactic
absorption and the longer wavelength Mg II absorption components with
W_{lambda}_ = 1.62 +/- 0.24 and 1.10 +/- 0.20 A as the Magellanic Stream
absorption. The Fe II lines at 2344, 2382, 2586 and 2600 A are very wide
and imply the detection of absorption by gas in the Milky Way and in the
MS.

7. 1993MNRAS.263..999T
Re:PKS 0637-75
0637-75. Quasar spectrum: broad Balmer lines, blue continuum, and
[O III] {lambda}{lambda}5007, 4959 lines of moderate equivalent width.

8. 1978MNRAS.185..149H
Re:[HB89] 0637-752
0637-75
An independent IDS spectrum has been obtained by Savage, Browne & Bolton(1976)
using slightly higher resolution but similar wavelength coverage. We confirm
their redshift but find an additional six lines. On the other hand, we do not
see [Ne III] {lambda}3968 claimed by Savage et al. although its detection
would be unlikely in our spectrum considering the low signal/noise ratio found
for [Ne III] {lambda}3869.


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