Date and Time of the Query: 2019-08-19 T08:20:48 PDT
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Notes for object UM 321

4 note(s) found in NED.

1. 2008ApJS..175..314D
Re:VSOP J0125-0005
J0125-0005.-The core is 0.3 mas in size, and there is extended emission to the

2. 2002ApJS..140..143B
Re:UM 321
q0122-0021, z = 1.070.-The FOS spectra were discussed by Bergeron et
al. (1994) and Bahcall et al. (1996). They identify intervening metal
line absorbers at z = 0.398 and z = 0.953. G270, G190.

3. 2000ApJS..129..563S
Re:PKS 0122-00
PG 0122-00 (z_em_ = 1.070). - The average velocity equivalent width
for the Mg II 2796, 2803 A doublet is relatively large
(W_v_ = 142 km s^-1^), suggesting the detection of high-velocity Mg II.
However, the nearest H I HVC is W538, with v = -114 km s^-1^, and lies
1.9^deg^ away. Possibly the strong Mg II is detecting a low column
density envelope to that H I HVC.

4. 1997MNRAS.284..599B
Re:[HB89] 0122-003
3.3 Q0122-0021
This QSO line of sight passes 2^deg^, or 1.8 h^-1^ Mpc, from the centre of
Abell 194 (Chapman, Geller & Huchra 1988). There are three galaxies at the
cluster velocity lying within 500 h^-1^ kpc of the QSO sightline, UGC 0998,
CGCG 385-115 and CGCG 385-141, at separations of 13.9, 20.5 and 22.4 arcmin,
respectively, which correspond to 201, 326 and 353 h^-1^ kpc at the galaxies'
redshifts. The galaxy whose redshift we have measured, labelled G1 in Fig.
2(a), is at a velocity of cz=6386 km s^-1^. The velocity dispersion of
Abell 194 is ~450 km s^-1^, which means that, if G1 is a member of the
cluster, its velocity is 2{sigma} away from the cluster's systemic velocity.
Whether or not G1 is a member of Abell 194, it lies 2.51 arcmin from the QSO
line of sight, which corresponds to only 44.8 h^-1^1 kpc. There are three
other galaxies that lie between Abell 194 and the Milky Way and which are
within 0.5 h^-1^ Mpc of the QSO line of sight: UGC 1011, UM 323 and UGC 0931,
which, with velocities of 1923, 1799 and 1948 km s^-1^, and separations of
26.4, 38.1 and 49.3 arcmin, pass 146, 198 and 277 h^-1^ kpe from the QSO

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