  The Virgo and A1795 clusters of galaxies were re-observed by EUVE with {\it
in situ} background measurements by pointing at small offsets. Earlier, a
similar re-observational strategy applied to the cluster A2199 revealed that
the background radial profile was consistent with a flat distribution, and
therefore the original method of extracting cluster EUV signals by the
subtraction of an aymptotically determined background was valid. It is shown
here that the same conclusions hold for the current sample. A model of the
background was obtained from its known properties and the {\it in situ}
measurements, and the subtracted cluster fluxes remain in agreement with those
reported in our discovery papers. They are also consistent with results from
the most conservative procedure of direct point-to-point subtraction of the
{\it in situ} background and proper error propagation, which still preserves
the existence of the EUV excess and its rising radial trend. We present
evidence which argues against the soft excess as due to peculiarities in the
line-of-sight Galactic absorption. The data appear to favor a thermal origin of
the emission.
