Date and Time of the Query: 2019-06-20 T05:04:21 PDT
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Notes for object ABELL 2111

5 note(s) found in NED.

1. 2008ApJS..174..117M
Re:ABELL 2111
A2111.-An extended source at {al[pha}[2000.0] =
15^h^39^m^32.70^s^,{delta}[2000.0] = +34^h^28^m^07.37^s^, 210" (0.8 Mpc) from
the cluster core, was manually excluded.

2. 2008A&A...487..453A
Re:ABELL 2111
A2111. This cluster has the largest amount of information available in the
literature of all the clusters in our sample. The redshift was established from
spectroscopic observations by Lavery & Henry (1986). The center given by NED
comes from the ACO catalogue given by Abell et al. (1989), namely,
{alpha}(J2000) = 15h39m38.3s, {delta}(J2000) = +34d24m21s. However, the
subsequent analysis of the X-ray data by Henriksen et al. (1999); Wang et al.
(1997); Miller et al. (2006), led them to conclude that the cluster center
position is at {alpha}(J2000) = 15h39m40.9s , {delta}(J2000) = +34d25m04s, only
5.04 kpc away from the Brightest Cluster Galaxy. Miller et al. (2006) also
provide a large number of spectra. Interestingly, the X-ray works showed that
this cluster is undergoing a merger and presents a rather large blue fraction.

3. 2005ApJ...624..606J
Re:ABELL 2111
A2111 (z = 0.23): This cluster is very elongated and extended toward the
northwest. It also has a double-peaked core.

4. 2002ApJS..139..313D
Re:ABELL 2111
5.26. A2111 Henriksen, Wang, & Ulmer (1999) use ASCA and ROSAT PSPC data
to detect a highly significant temperature gradient in A2111,
with a higher temperature cluster core (kT = 6.46 +/- 0.87 keV at
R < 3') surrounded by a cooler region (kT = 3.10 +/- 1.19 keV at
3' < R < 6'). The non-isothermality of the 1CM may indicate a
system which has undergone a recent merger which heated the ICM
in the cluster center, or it may be due to the gravitational
potential of the cluster. In optical images, the cluster core is
dominated by two bright early-type galaxies separated by about
1'. The mass map shows a peak situated between the two brightest
cluster galaxies, but closer to the brightest galaxy of the
pair. The light and number density distributions both have a
much more elongated morphology than the mass distribution. By
itself, the cluster mass distribution does not provide any
strong evidence for significant dynamical activity within this
cluster. There are several very red arc candidates around the
mass center. A secondary mass peak in the northeast corner of
our image is most likely an artifact, given its proximity to the
corner and the absence of any corresponding peaks in the light
and number density distributions.

5. 1999MNRAS.306..857C
Re:ABELL 2111
This cluster has two equally dominant central galaxies, separated by 47
arcsec (220kpc) in projection. The X-rays from this cluster are
elongated (Wang, Ulmer and Lavery 1997).

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