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Date and Time of the Query: 2019-04-22 T21:27:01 PDT
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Notes for object ABELL 0133

7 note(s) found in NED.


1. 2006ApJ...643..730D
Re:Abell 0133
The center of Abell 133 hosts an impressive radio relic source spanning 55 kpc.
Slee et al. (2001) conclude from 4&arcsec; resolution VLA observations that the
central galaxy is not the current source of the relic but may have been where
the radio source began. ROSAT X-ray observations show that the radio source is
clearly interacting with the ICM (Rizza et al. 2000). The central galaxy also
has a compact, low-ionization emission-line source (Hu et al. 1985).
Fujita et al. (2002) report Chandra observations of Abell 133. We find
statistical agreement with their projected temperature, metallicity, and N_H_
profiles for the fits in which Fujita et al. (2002) restrict the spectral
fitting to photons with energies greater than 0.9 keV. However, their fits for
data that include the less energetic photons disagree with ours. This finding is
in accord with the general trend that early Chandra spectral fitting results
involving soft X-ray data are probably not reliable because the low-energy
calibration for Chandra was not well characterized until at least 2004. Hence,
the energy range chosen for any given fit can have a significant impact on the
best-fit temperatures, absorption column NH, and metallicity values. The fact
that the fits of Fujita et al. (2002) that were restricted to higher energies
agree with ours supports our suspicion that the Chandra calibration of the soft
X-ray bandpass has improved with time.

2. 2006A&A...450....9F
Re:ABELL 0133
A133 - In this bimodal cluster, small subclusters occur at the scale of
{alpha} = 188 kpc.

3. 2005MNRAS.364.1387P
Re:ABELL 0133
Abell 133: Our adopted position is taken from Jones & Forman (1999), and is
offset by {DELTA}RA =+3" and {DELTA}Dec. =-4'51" from the original Abell
position. Edge & Stewart (1991) note the presence of a bright cD galaxy with
multiple nuclei at the centre of a cooling flow X-Ray cluster. Slee et al.(2001)
point out the cluster has a radio relic, which is a diffuse steep-spectrum
source with no optical identification. Fujita et al. (2002) found a tongue of
X-ray emission extending the the northwest of the cD galaxy with no optical
counterpart. The X-ray spectrum showed the emission to be thermal and at a lower
temperature than the ambient gas. Fujita et al. (2004) find evidence of a weak
merger shock, and suggest it to be the origin of the tongue-like X-ray
structure.

4. 2002ApJ...576..688B
Re:ABELL 0133
A133-There is clear evidence of soft excess emission in this cluster,
from the central regions to ~500 kpc, the limiting radius of the PSPC
detection.

5. 2001MNRAS.320...49K
Re:ABELL 0133
A133: Probably a confirmed unimodal cluster by all substructure measures
(Mohr et al. 1995; BT96) showing small values of ellipticities and values of
sc. Optical and X-ray {theta}s differ by more than 64^deg^. One projected
X-ray source at z ~ 0.235 has been subtracted (EXO 0059.82218).

6. 1999NewA....4..141G
Re:ABELL 0133
A 133. Komissarov & Gubanov (1994) reported the existence of a very
steep spectrum radio source ({alpha} > 2) coincident with the first
ranked galaxy of this cluster. The high resolution image published by
Slee et al. (1994) shows a northern diffuse component of ~100kpc,
probably not related to the radio galaxy. The emission detected in the
NVSS extends to the South where another discrete radio source is present
(see also the image by Owen et al., 1993). The existence of a
cluster-wide diffuse emission is uncertain, as well as its connection to
the steep spectrum northern diffuse component.

7. 1994A&AS..106....1G
Re:ABELL 0133
A 133: Bright cD galaxy with companion or multiple nuclei at the center
of a cooling flow X-Ray cluster (Edge & Stewart 1991). Data at 1.5 GHz
are presented by Slee et al. (1989) and by Owen et al. (1993).


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