Date and Time of the Query: 2019-06-19 T06:24:36 PDT
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Notes for object ABELL 1758

6 note(s) found in NED.

1. 2005ApJ...624..606J
Re:ABELL 1758
A1758 (z = 0.28): One of the most complicated-looking low-redshift clusters.
A1758 has approximately two main clumps, but these are lumpy and disrupted,
probably because of an ongoing merger in which the two clusters have already
passed through each other. The outer envelope of this cluster is elliptical.

2. 2002ApJS..139..313D
Re:ABELL 1758
5.20. A1758 In our optical images, A1758 appears as a double cluster
which is possibly in the process of merging into a single massive
cluster. Both subclumps appear locally relaxed and strongly
concentrated around a bright early-type galaxy. There is an
apparent blue arc associated with the northwest mass clump. The
mass map shows a highly elongated mass concentration, bridging
the gap between the two subclusters. The total mass of this
cluster is very high, as indicated by the aperture mass plot in
Figure 51 and the {sigma}_WL_ value in Table 2. A third galaxy
concentration is located about 4' south of the edge of the
field. Observations of a 30' field centered on this "triple
cluster" have been obtained with the 3.6 m CFHT, and the results
will be described in a future paper.

3. 2001ApJ...548..639K
Re:ABELL 1758
A1758a. - The brightest source is identified with a narrow-angle tail
galaxy (O'Dea & Owen 1985) with the tail pointing to the southeast. The
bulk of the remaining emission is resolved into two sources in the FIRST
image, but the faint emission to the south of these and between these and
the tailed galaxy may be diffuse emission unrelated to the point sources,
or it may be a blend of fainter point sources. The presence of diffuse
emission is therefore considered uncertain.

4. 1999NewA....4..141G
Re:ABELL 1758
A 1758a. The strongest source to the South is identified with a cluster
galaxy. It shows a Narrow Angle Tailed structure (O'Dea & Owen, 1985)
with the tail oriented to the SE. In the FIRST image, the easternmost
structure is resolved in two compact sources, while the extended
emission in between is not detected. It could be a faint halo or the
blend of individual radio sources.

5. 1999MNRAS.306..857C
Re:ABELL 1758
This double cluster has its two components listed separately in Paper I.
We list here the dominant galaxy associated only with A1758a, which
produces approximately 40 per cent of the combined luminosity; there is
a bright less dominant galaxy also at RA 13 32 51.9, Dec 50 31 36

6. 1998MNRAS.301..328R
Re:ABELL 1758
A1758: This is one of the most intriguing clusters in the sample. There
is very complex structure in the X-ray emission near the Abell cluster
position (northernmost X-ray source in Fig. 1f). This cluster appears to
be bimodal in nature as seen in both the HRI and PSPC data, with the
X-ray peaks coincident with an apparent over-density in the galaxy
distribution. The dominant galaxy in the south-east clump is a
narrow-angle tailed radio source. The position angle of the narrow-angle
tail is aligned with the X-ray emission from the cluster, as is seen in
a number of nearby clusters of similar richness (Bliton et al. 1998).
This Butcher-Oemler cluster has a moderate blue fraction
f_b_ = 0.09 +/- 0.04 (Butcher & Oemler 1984) for its redshift.
Approximately 5 arcmin (~ 1 Mpc) south of the Abell cluster
position is an extended clump of X-ray emission. This clump also
exhibits structure, and seems to be associated with a group of galaxies.
To our knowledge, there is no spectroscopic confirmation of the redshift
of these galaxies, although their magnitude range seems to place them
coincidentally with A1758. If this is true, this is probably a group
falling into the cluster potential, as suggested by Davis & Mushotzky
(1992). Temperatures derived for A1758 using PSPC and ASCA are
inconsistent, perhaps due to the poor resolution and small bandpass of
ROSAT. None the less, both instruments yield similar temperatures for
the cluster itself and the emission from the extreme southern clump.

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