Abell 2034 (Figure 13). This diffuse feature was tentatively identified as a
relic by Kempner & Sarazin (2001). Using Chandra observations, Kempner et al.
(2003) found multiple signatures of an ongoing merger including a cold front,
and possible indications of inverse Compton radiation from the radio source.
Here, we designate the diffuse source as a halo, because it is centered on the
overall X-ray surface brightness, not at the cold front. We also show in Figure
13 the overlay between the original WENSS image and the Faint Images of the
Radio Sky at Twenty-Centimeters (FIRST) image at 5" resolution. Just SW of the
X-ray peak there is a pair of tailed radio sources. The southern one is a WAT,
and the northern is a NAT that undergoes an extremely rapid expansion and drop
in brightness as it extends toward the cluster center, where it can still be
seen in WENSS, but not in FIRST. It blends in to the more extended emission that
we classify as a halo. The WENSS source to the NW of center is completely resolv
ed out in FIRST.
A2034 (z = 0.11): A2034 is fairly round but has some small-scale core
structure, including a curved structure extending away from the peak. It also
shows both a northern cold front and a southern excess (Kempner et al. 2003).
It is currently unclear if the southern excess is associated with A2034, and
Kempner et al. (2003) suggest that it may be a background cluster. Most of the
southern excess is not in the 0.5 Mpc aperture, but our aperture does overlap
the top of this feature. Comparing to the 0.3 and 0.4 Mpc apertures that do not
contain the excess, P_3_/P_0_ and P_4_/P_0_ do shift somewhat. However, this
shift is toward smaller values of the power ratios, which would only strengthen
our conclusions. This cluster has the lowest redshift in our sample, and the
0.5 Mpc aperture overlapped all four ACIS-I CCDs.
A2034. - The extended emission is located north of the cluster center.
It is coincident with a discontinuity in the X-ray surface brightness,
which may indicate the presence of a merger shock. Forthcoming observations
of the cluster with XMM-Newton and Chandra will be able to confirm the
existence of a merger shock at this location.
RXC J1510.1+3330, RXC J1556.1+6621, and RXC J1700.7+6412. - These
objects show a contamination by a point source in the available HRI
image by no more than 10%-15%.
Galaxy b is the more likely central dominant galaxy.