  We present the results of a spectral-imaging analysis of X-ray data obtained
with the Position Sensitive Proportional Counter aboard the ROSAT Observatory
in a 32 ks pointed observation of Hickson's Compact Group (HCG) #94. Besides
HCG94, A2572, a richness class 0 Abell cluster, is also contained in the
central region of the field of view.
  Both systems are at a redshift of z~0.04 and are falling toward each other at
a velocity of about 1000 km/s. Their three-dimensional spatial separation is
probably of the order of an Abell radius; however, as yet, no clear signs of
dynamical interaction are discernible in the X-ray.
  We find HCG94's gas temperature and unabsorbed X-ray luminosity to be far too
high for a galaxy group thereby confirming the claim of Ebeling, Voges &
B"ohringer (1994) that HCG94 should be classified as a galaxy cluster. The
opposite is true for the Abell cluster A2572, the optical richness of which has
been overestimated due to the inclusion of HCG94. In the X-ray, A2572 appears
at first sight like the prototypical binary cluster with two equally massive
and X-ray bright subclusters in the process of merging. However, the available
X-ray, optical, and radio data strongly suggest that A2572 proper is in fact
merely a loose group of galaxies, while the second component is a much richer
and more distant cluster seen in superposition.
  A deprojection analysis shows HCG94 to host a moderate cooling flow; this
picture is supported by a radial increase in the column density of absorbing
material and a decrease in the gas temperature toward the cluster centre.
HCG94's total gravitating mass is much higher than what could be anticipated
from its appearance in the optical. Our findings hence underline the need for
