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Notes for object ABELL 1367

8 note(s) found in NED.


1. 2006MNRAS.372.1496S
Re:ABELL 1367
5.5 Abell 1367 - This is a complex structured cluster, which is clearly
undergoing multiple merging, as seen in both optical (e.g. Cortese et al. 2004)
and X-rays (Sun & Murray 2002). The projected T(r) data were used for the
deprojection, to avoid strong fluctuations in the recovered profile.

2. 2006A&A...450....9F
Re:ABELL 1367
A1367 - At the scale of {alpha} = 129 kpc this cluster has two galaxy groups.

3. 2004ApJ...608..166N
Re:ABELL 1367
A1367. The MECS spectrum of AGN NGC 3862 provides constraints on the
reference model, yielding a PDS estimate of 1.0^+0.4^_0.3_ 10^-2^
counts s^-1^. This value is consistent with HXR emission, and thus the
HXR estimate will be very uncertain. The PSPC count rate of NGC 3884 is
negligible (<1%) of that of NGC 3862 and thus will not change the AGN
contribution estimate.

4. 2002ApJ...576..688B
Re:ABELL 1367
A1367.-A 1367 is an X-ray-faint and very nearby galaxy cluster, near
the brighter Coma Cluster. It has a secondary peak of the X-ray
brightness (Donnelly et al., 1998), which we study here separately. The
secondary peak is located near R.A. = 11h44m21.7s, decl. = +09deg52'132,
approximately 19' offset from the primary brightness peak. While
azimuthally averaged annuli around the primary peak revealed no
evidence of soft excess emission (see, Fig. 1), the secondary peak
(divided into 0'-3' and 3'-6' regions from its center) seems associated
with soft excess emission; see Fig. 9 and Table 5.

5. 1999MNRAS.306..857C
Re:ABELL 1367
The BCG is NGC 3862, which is associated with the strong radio source
3C 264, and detected as an unresolved point source in ROSAT images
contributing approximately 5% to the total X-ray emission from the
cluster (Edge and Rottgering 1995). NGC 3862 is significantly offset
from the centre of the highly extended X-ray emission, and is observed
to have a weak emission line spectrum ([N II]>H{alpha}, weak [O II])
with evidence for a blue continuum. HST observations reveal that
3C 264 contains a nonthermal core and jet (Baum et al. 1998) which
could contribute to this blue continuum. We have observed the galaxy
NGC 3860 at RA 11 44 49.1, DEC 19 47 44 (J2000), which is the brightest
galaxy in the broad cluster core. NGC 3860 has has strong extended line
emission, dominated by H{alpha}.

6. 1998MNRAS.301..609B
Re:ABELL 1367
Abell 1367: Fig. 1i. This cluster contains the strong X-ray and radio
source 3C 264, located in the SW corner of the cluster. A second NAT in
the NW has often been misclassified as a double radio source at low
resolution. Grebenev et al. (1995a) performed a wavelet analysis of the
ROSAT PSPC and Einstein HRI images of this cluster, and found 16
extended X-ray features - nine of which had galaxies coincident. This
elongated NW region also contains several spiral galaxies that appear to
be infalling for the first time. H I maps of these spirals show the
neutral hydrogen emission to be offset from the optical centres and
asymmetric in shape, implying the galaxy discs are interacting with the
ICM (Dickey & Gavazzi 1991). As further evidence for ram
pressure-induced star formation, these spiral galaxies all show giant
H II regions aligned along a peripheral path, suggestive of a bow shock
formation mechanism (Gavazzi et al. 1995a). The luminosity function of
spiral galaxies in this cluster deviates from that of field spirals at
the faint end, with bluer spirals existing in the cluster. This is
another indication of galaxy-ICM interactions causing enhanced star
formation activity (Gavazzi, Randone & Branchini 1995b).

7. 1998A&A...332..395E
Re:ABELL 1367
6.4. Abell 1367: 1140+203
The diffuse radio source found in A1367 is usually called a halo, but it is more
probably a cluster relic because of its noncentral location and asymmetric
shape. The distance to the center of the galaxy distribution is 0.8 Mpc
h_50_^-1^ (Gavazzi 1978), but to that of the X-ray emission it is 1.1 Mpc
h_50_^-1^ (see map in Gavazzi et al. 1995). We use the latter distance, since
the X-ray emission should be a better tracer of the gravitational potential. The
X-ray emission is elongated into the direction of the relic, possibly tracing
the influence of the large-scale structure potential, or the main direction of
the accretion flow onto the cluster, or both. The radio relic could be
contaminated or related to three close irregular galaxies, which have radio
trails behind them (Gavazzi & Jaffe 1987), indicating that they are falling
inwards. Strong on-going star formation, a recent supernova in one of them, and
young and abundant H II regions, which are aligned as if they were formed by bow
shocks (Gavazzi et al. 1995), could be triggered by the sudden change of the
environment of these galaxies during the passage of the accretion shock. A
starburst might increase the accretion within these galaxies onto a possible
central black hole (similar to the argumentation of Wang & Biermann 1998) and
therefore can trigger the ejection of radio plasma.
The measurements of the spectral index and radio flux of the relic differ in the
literature (compare Gavazzi 1987, Hanisch 1980, and Gavazzi & Trinchieri 1983)
and therefore any derived numbers have to be used with care. Especially the
radio power Q_radio_ is an extrapolation of a very steep spectrum ({alpha}=1.9)
down to 10 MHz and probably an overestimate. Due to the low expected viewing
angle only a small polarization of 4% is expected. Gavazzi & Trinchieri (1983)
detected some X-ray emission from the region of the relic. Assuming this to
result from inverse Compton emission they estimate a magnetic field strength of
1.2{mu}G, of the same order as the equipartition value of
B_2,eq_=2{mu}Gh_50_^2/7^ and the predicted strength of
B_2,predicted_=2.4{mu}Gh_50_^1/4^ for pressure equilibrium with the surrounding.

8. 1997ApJ...482...41G
Re:ABELL 1367
This cluster belongs to the Coma supercluster. Irregular in shape and
velocity distribution, this cluster contains a close sextet (S).


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