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Date and Time of the Query: 2019-06-25 T10:31:41 PDT
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Notes for object ABELL 0520

11 note(s) found in NED.


1. 2008ApJ...687..899R
Re:ABELL 0520
A520.-The cluster appears to have no well-defined optical core (Dahle et al.
2002) and instead has several concentrations of galaxies, none of which coincide
with the X-ray core. Crawford et al. (1999) note that there are three dominant
galaxies and chose the southwestern one as the CDG, as did we.

2. 2007MNRAS.376.1073Z
Re:ABELL 0520
Abell 520. Chapman et al. (2002) provide a previous analysis of the submm data
for this cluster. The SZ effect has been measured at 30 GHz by Reese et al.
(2002), with SuZIE II (Benson et al. 2004), and Cooray et al. (1998) provide a
list of point sources at 28.5 GHz in this field.

3. 2005ApJ...624..606J
Re:ABELL 0520
A520 (z = 0.20): This cluster has clear substructure in the form of a bright
arm of emission leading to a bright knot to the southwest. This clump is cooler
than the surrounding gas, and it appears to be a group of galaxies that has
recently passed through the main cluster (Govoni et al. 2004).

4. 2002ApJS..139..313D
Re:ABELL 0520
5.6. A520 This cluster, also known as MS 0451+02, appears complex,
with no well-defined center judging from the optical images. A giant
arc discovered by Le Fevre et al. (1994) is visible around a
giant elliptical galaxy at = 04h54m20s, {delta} = 2deg57.7'. This
galaxy is offset toward the northeast from the peaks in the mass,
light, and galaxy distributions. The mass distribution derived
from UH8K data has three main peaks, two of which coincide
closely with peaks in the light and number density distributions.
According to Le Fevre et al. (1994), this cluster has a complex
X-ray structure, and it may still be forming, with subcluster
concentrations in the process of merging. However, our estimated
velocity dispersion of 1050 +/- 100 km s^-1^ is consistent with the
spectroscopically measured value of 988 -/+ 76 km s^-1^
(Carlberg et al. 1996). The field of this cluster is rich in stars
and is well suited to study the PSF anisotropy and distortion at the
Cassegrain focus of the UH 2.24 m (see Figs. 2 and 5).

5. 1999NewA....4..141G
Re:ABELL 0520
A 520. The diffuse emission is centrally located, but of irregular shape
with the present sensitivity.

6. 1999MNRAS.306..857C
Re:ABELL 0520
This is a bimodal cluster, and we have observed the brightest (to the
SW of the cluster) of three dominant galaxies. This cluster was
detected in the Einstein Medium Sensitivity Survey (EMSS; Stocke et al.
1991).

7. 1999MNRAS.306..857C
Re:ABELL 0520
A520 This is a bimodal cluster, and we have observed the brightest (to
the SW of the cluster) of three dominant galaxies. This cluster was
detected in the Einstein Medium Sensitivity Survey (EMSS) (Stocke et al.
1991).

8. 1999ApJ...517..587L
Re:MS 0451.5+0250
MS 0451.5+0250 (also Abell 520) at z = 0.20 exhibits extremely
disturbed, clumpy morphology in a relatively short ROSAT HRI exposure,
resulting in a surface brightness profile that is not well fit by a
{beta} model. We have therefore chosen to use the PSPC data for our
fits, but we constrain r_core_ to be 100 +/- 50 kpc in order to avoid
overestimating this parameter because of the large PSF of the
instrument. It is also noted in C96 that it contains two dominant
galaxies and two peaks in its galaxy velocity distribution. We suggest
this as a strong candidate for a core merger. We also identify it as a
non-cooling flow cluster based on the lack of a bright peak in the X-ray
surface brightness profile and a nondetection of H{alpha} by D92. Our
X-ray centroid (from the PSPC data) lies at
R.A. (1950) = 04^h^51^m^32.4", decl. (1950) = 02^deg^50'18.2", which is
within ~30" of the optical center given by G94. They note, "There is not
a well defined optical center in this cluster but several galaxy
condensations are visible."
Interestingly, the PSPC exposure yields a reasonably smooth surface
brightness profile, which is well fit by a {beta} model. We anticipate
that future imaging of this cluster with higher resolution
instrumentation (e.g., AXAF, XMM) may reveal new insight into merging
cluster structure.

9. 1999A&A...351..413M
Re:MS 0451.5+0250
MS 0451.5+0250 (Abel 520)
One observation was performed for this cluster. No correlation was found
between the sources higher than 3{sigma} in the HRI field of view and
objects cataloged in HRASSCAT or ROSID. This cluster does not show a
significant X-ray peak, i.e. the X-ray center, we therefore define the
X-ray center as source count rate weighted mean position of sources
around pointing center. The source count rates were calculated by the
EXSAS command "DETECT/SOURCES".

10. 1994ApJS...94..583G
Re:MS 0451.5+0250
Abell 520. There is not a well defined optical center in this cluster but
several galaxy condensations are visible. The X-ray source was detected
near the edge of the IPC frame with the observed X-ray emission
associated with a tight clump of galaxies at z = 0.202. A more detailed
analysis of the X-ray emission indicates that it may extend an additional
2 arcmin to the NE. If so, a portion of this source may be due to a poor
cluster in that vicinity at a slightly higher redshift (z = 0.22).

11. 1991ApJS...76..813S
Re:MS 0451.5+0250
This cluster source was detected near the edge of the
IPC frame with the observed x-ray emission associated with a tight
clump of galaxies at z=0.202. A more detailed analysis of the x-ray
emission indicates that it may extend an additional 2 arcmin to the NE.
If so, a portion of this source may be due to a poor cluster in that
vicinity at a slightly higher redshift (z=0.220).


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