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Notes for object ABELL 2142

8 note(s) found in NED.


1. 2006MNRAS.372.1496S
Re:ABELL 2142
5.19 Abell 2142 - This is the archetypal 'cold-front' cluster, which likely
consists of the largely intact core of a poor cluster enclosed within a halo of
much hotter gas associated with a larger cluster (Markevitch et al. 2000). This
fact accounts for its unusual temperature profile, which is atypical of non-CC
clusters (see Section 6.1).
The two observations of Abell 2142 (ObsIDs 1196 and 1296) were amongst the
very first made by Chandra, and were taken when the CCD temperature was only
-100^deg^C. Since the standard ciao calibration does not cover this CCD
temperature, these data sets were analysed according to the calibration for a
CCD temperature of -110^deg^C. In addition, the corresponding Markevitch period
A blank-sky background data sets are truncated at 10 keV, so the background
renormalization was performed in the range 8-10 keV. The analysis presented here
is based on the 1196 data set, but to verify our results we also analysed the
1296 observation, and found very good agreement between the density and
temperature profiles. As for A401, it was necessary to use the older ciao task
'mkrmf' to generate spectral responses for this data set.

2. 2004ApJ...608..166N
Re:ABELL 2142
A2142. A Seyfert 1 galaxy, IC 1166, is outside the PSPC field, and thus
the flux estimate cannot be given; 4' off-axis from the cluster center
there is a Seyfert 1 galaxy, 1E 1556+27.4, whose photon index is
{alpha}_ph_ = 1.9 as observed with ASCA (Markevitch et al. 1998). The
MECS data consistently give {alpha}_ph_ = 1.8 +- 0.1. Using this and
including the statistical uncertainties of the MECS data, the
extrapolated PDS 20-80 keV count rate is 2.2^+0.7^_-0.5_10^-2^
counts s^-1^, consistent with the PSPC estimate of 2.9 x 10^-2^
counts s^-1^. In A2142 there is another Seyfert 1 galaxy, QSO B1557+272.
At 17' off-axis, the source is quite diffuse in MECS, but the data
extracted from a 4' circle around the source still provide adequate
constraints on the normalization of the power-law model. Including
statistical uncertainties, the PDS prediction is 0.8^+0.3^_-0.2_10^-2^
counts s^-1^. Thus the combined AGN contribution to the PDS 20-80 keV
band is 3.0^+0.8^_-0.6_10^-2^ counts s^-1^, or 30% of the HXR signal.

3. 2002ApJ...576..688B
Re:ABELL 2142
A2142. A2142 shows a clear enhancement of the X-ray emission in the
southeastern quadrant (Briel & Henry 1996).We investigated the
properties of the emission in that region and how it compares with the
emission in the remainder of the azimuthal directions (see Fig. 9 and
Table 6). There is marginal evidence of soft excess emission in the
central 500 kpc of this cluster, detected out to a radius of 1 Mpc. The
southeastern quadrant's X-ray excess (above the azimuthal average) can
be successfully modeled with a power-law model, indicating a possible
nonthermal origin of the X-ray excess brightness.

4. 2000NewA....5..335G
Re:ABELL 2142
A 2142. The presence of a halo in this cluster was suggested by
Harris et al. (1977). We confirm the presence of diffuse emission,
located around the brightest cluster galaxy (Fig. 6), as also detected
in the NVSS (Giovannini et al., 1999). The radio emission could be more
extended in S-SW direction up to 27^deg^10' in declination
(2-{sigma} level), but more sensitive observations are necessary to
confirm the reality of this feature. In the FIRST survey, the diffuse
emission is completely resolved out, and no emission is detected at a
flux level of 0.4 mJy/beam (3-{sigma}) from any of the bright
galaxies present in the region of the extended radio emission. The radio
source could therefore be classified as a cluster halo. We note,
however, that this source is much smaller than radio halos commonly
found in clusters. We cannot rule out the possibility that it is the
remnant of a single galaxy which was active in the past.

5. 1999NewA....4..141G
Re:ABELL 2142
A 2142. The presence of a halo in this cluster was suggested by
Harris et al. (1977). The image here shows that the diffuse radio
emission is ~350kpc in size and is located around a cluster galaxy.
Therefore, we still consider uncertain the classification of this
source as a cluster-wide radio halo.

6. 1999MNRAS.306..857C
Re:ABELL 2142
We have taken the spectrum of each of the two equally bright dominant
galaxies in this binary cluster. They lie along the same slit
position, separated by 104 arcsec (238kpc).

7. 1998MNRAS.301..609B
Re:ABELL 2142
Abell 2142: Fig. 1m. This cooling flow cluster has a clear elongation in
its X-ray emission to the NE/SW, with the NAT oriented in roughly the
same direction. The cooling flow manifests itself in a cool component
fit to the X-ray spectrum, as well as strong evidence for a centrally
enhanced metal abundance (White et al. 1994). A2142 has a cooling time
of 3.0 +/- 0.8 Gyr, and a mass inflow rate ~ 188 M_sun_ yr^-1^
(Edge et al. 1992). X-ray surface brightness and temperature maps imply
A2142 is in the late stages of a merger (Henry & Briel 1996). This
cluster also has a high velocity dispersion of 1280 km s^-1^
(Oegerle et al. 1995). The X-ray point source in the NE is most likely
associated with a Seyfert 1 cluster member galaxy.

8. 1998A&A...330..801P
Re:ABELL 2142
A2142 In the late state of a merger (Henry & Briel 1996). It was already flagged
by Buote & Tsai (1996) as typical "off-center" cluster. Our analysis tends to
confirm their conclusion reached from the PSPC data analysis, as several small
scale structures are conspicuous.


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