Date and Time of the Query: 2019-06-18 T09:20:04 PDT
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Notes for object ABELL 0400

4 note(s) found in NED.

1. 2002ApJ...567..202E
Re:ABELL 0400
2.1. Abell 400
Abell 400 is a richness class 1, Rood-Sastry I cluster. Its
dynamics have been analyzed by Beers et al. (1992). They find
a mean redshift z = 0.0235, which corresponds to 26.5 kpc arcmin^-1^,
using H_0_ = 75 km s^-1^ Mpc. After separating out a background
group of galaxies to the northeast, they find that the cluster
itself has substructure. The central, elliptical-rich population
is composed of two subgroups separated by 700 km s^-1^. These groups
are not apparent in the galaxy distribution projected on the sky.
From this, they conclude that a merger is taking place, close to the
line of sight. The cluster centers on a dominant galaxy with two
nuclei separated by 435 km s^-1^ (e.g., Balcells et al. 1995). The
double nuclei have been interpreted as due to projection (Tonry 1985),
as closely interacting (Lauer 1988), and as merging clump centers
(Beers et al. 1992; see also Balcells et al. 1995).
The X-ray image is fairly smooth, with some elongation of the
inner isophotes (see also Beers et al. 1992, who present ellipse fits
to the inner isophotes). Figure 1 shows the image from the ROSAT PSPC,
together with the central radio galaxy. Abell 400 does not have a
strong cooling core. White, Jones, & Forman (1997) agree with earlier
authors in finding that any spherical mass inflow is small,
M^dot^<~10M_sun_ yr^-1^.
The central galaxy is host to an unusual radio source: each
nucleus gives rise to a radio jet, and the jets merge into the striking
tailed radio source, 3C 75 (Owen et al. 1985). Figure 1 shows that the
tails can be detected to ~7' ~185 kpc at 327 MHz. They bend to the
northeast, away from the X-ray centroid and axis of elongation. Note
that our RM data (based on higher frequencies than the image in Fig. 1)
extend only to ~200" ~90 kpc.

2. 2002ApJ...567..202E
Re:ABELL 0400
Abell 400 contains 3C 75, a wide-angle tail radio source. KPTW give fluxes
and spectral indices; the source can be fitted by a single power law,
{alpha}= -d ln S_{nu}_/d ln{nu} ~ 0.8 from 10 MHz to 10 GHz. Owen et al. (1985)
present the radio image; the Faraday data and cluster magnetic fields are
discussed in the present paper. Beers et al. (1992) present Einstein data;
the ROSAT data is presented in this paper. In section 4 we take the typical
T ~ 1.5 keV. This cluster has a broad gas core, making it a noncooling
cluster, but also has a weak central X-ray excess, which may be a small
cooling core.

3. 1999MNRAS.306..857C
Re:ABELL 0400
The dominant galaxies are a dumbell system separated by 16.2 arcsec
(~11 kpc) in projection, and are associated with the twin radio source
3C 75.

4. 1999MNRAS.306..857C
Re:ABELL 0400
A400 The dominant galaxies are a dumbbell system separated by
16.2 arcsec (~ 11 kpc) in projection, and are associated with the twin
radio source 3C75.

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