Date and Time of the Query: 2019-06-26 T02:04:25 PDT
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Notes for object ABELL 2199

8 note(s) found in NED.

1. 2006MNRAS.372.1496S
Re:ABELL 2199
5.8 Abell 2199 - This is a known cavity cluster (Johnstone et al. 2002).

2. 2006A&A...453..447E
Re:ABELL 2199
Abell 2199
The parameters of the electron density profile as reported in Mohr et al. (1999)
were used. The temperature of the cool core are taken from Voigt et al. (2002)
and the total luminosity from David et al. (1993).

3. 2006A&A...450....9F
Re:ABELL 2199
A2199 - At the scales of {alpha} = 129 kpc and {alpha} = 94 kpc substructures
occurs in the field of the cluster.

4. 2004ApJ...608..166N
Re:ABELL 2199
A2199. There are no cataloged Seyfert 1 galaxies in A2199, but X-ray
imaging reveals a bright Seyfert 1 galaxy, RXS J16290+4007, of redshift
0.3, located 35' off-axis and thus outside the MECS FOV. Its PSPC
spectrum is not consistent with the reference model. The data can be
modeled with a combination of thermal and a power-law model, yielding a
temperature of 0.1 keV and a photon index of 2.4 +- 0.1, which makes a
negligible contribution to HXR emission. Allowing for spectral hardening
toward higher energies, we fitted the PSPC data with our reference model
plus MEKAL. The fit is bad, but it yields an estimate for the HXR
emission of 0.6^+0.4^_-0.3_10^-2^ counts s^-1^, 8% of the HXR emission,
thereby decreasing the detection confidence slightly. To be consistent
with the treatment of Seyfert 1 galaxies in the rest of the sample, we
assume the harder spectrum in the following.

5. 2002ApJ...576..688B
Re:ABELL 2199
A2199. A2199 has marginal evidence of soft excess emission in this deep
PSPC observation. EUVE data (Lieu et al. 1999a; Bonamente et
al. 2001b) show significant extreme-ultraviolet excess that reaches an
importance of a few times 100% at large distances from the center. The
only possibility to reconcile the two observations is that the soft
excess emission in this source is mainly confined to energies below
~0.2 keV.

6. 2002ApJ...567..202E
Re:ABELL 2199
Abell 2199 contains the diffuse radio source 3C 338. KPTW give fluxes; this
is a steep spectrum source, {alpha} ~ 1.09 at low frequencies. Ge & Owen (1994)
present the radio image. Owen & Eilek (1998) present and deproject ROSAT data
and use Faraday data to infer the magnetic field. We use their X-ray
deprojection and estimate T~2 keV based on Thomas, Fabian, & Nulsen (1987).

7. 1999MNRAS.306..857C
Re:ABELL 2199
The observed galaxy (NGC 6166) is associated with 3C 338.

8. 1997ApJ...482...41G
Re:ABELL 2199
A2197-2199.-This field has no significant structures and is thought to be
elongated in shape. The field we analyzed contains, however, the two
well-known clusters A2197 and A2199, which correspond closely to the
structures we detect at a very low significance level (about 60%). The
background system MS1 in the south (A2199) contains a close foreground
quartet (S1), while the foreground system MS2 at the north (A2197)
contains a background quartet (S2). This peculiar situation is very
difficult to analyze with our method, since the local kinematics cannot
be cleaned from the mutual contamination produced by the four systems.
Therefore, we do not consider these clusters in the final discussion.

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