Date and Time of the Query: 2019-08-25 T04:00:30 PDT
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Notes for object ABELL 0068

4 note(s) found in NED.

1. 2007MNRAS.376.1073Z
Re:ABELL 0068
Abell 68. Cooray et al. (1998) have studied this moderate redshift cluster as
part of a 28.5-GHz study of point sources in galaxy clusters.

2. 2005MNRAS.359..417S
Re:ABELL 0068
A 68 - We first constrained the model with just the multiply imaged ERO at
z = 1.6 (CO, Table 2), identifying nine distinct knots of likely star
formation in each image of this galaxy. A model containing just one
cluster-scale mass component (#1), did not fit these data well:
{chi}^2^/dof >= 5. We therefore added a second cluster-scale mass
component (#2) to the north-west of the central galaxy. Despite the strong
evidence for the presence of this mass component in the weak-shear map
(Fig. 1), no single bright cluster galaxy dominates the group of galaxies
found in this region. We therefore adopt the brightest of this group of
galaxies as the centre of clump #2, for which we adopt a circular shape.
CO places strong constraints on the mass required in this second clump
because the spatial configuration of the images is very sensitive to the
details of the bi-modal mass structure of the cluster. We find an
acceptable fit without optimizing the spatial parameters of clump #2. The
south-western comer of CO straddles the z = 1.6 radial caustic in this
best-fitting lens model, causing an additional, radially amplified image
of this portion of the galaxy to be predicted. We search the HST frame in
the vicinity of the predicted radial image, and find a faint radial
feature (C19) 4-arcsec north-west of the central galaxy which is
consistent with the model prediction. Further constraining the model with
C15/C16/C17, at z = 5.4 confirms the validity of the model thus far, mass
component. This model is also able to reproduce the observed morphology of
the other candidate multiple-image systems.

3. 2002ApJS..139..313D
Re:ABELL 0068
5.1. A68 About a dozen strongly gravitationally lensed arcs and arclets
are visible in the central regions of this cluster, surrounding both of
the two brightest cluster galaxies, which are separated by about 1.5'.
The mass distribution is strongly elongated along the axis joining
these two galaxies, indicating a possible ongoing merger of two mass
concentrations. The peak positions of the mass, light, and number
density distributions coincide well, but the mass distribution appears
more elongated than the light and number density distributions. As
indicated by Figure 51 and Table 2, this is one of the most massive
clusters in our observed sample.

4. 1999MNRAS.306..857C
Re:ABELL 0068
Galaxy a is the brighter galaxy, nearer the RASS centroid.

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