From X-ray images in the ROSAT public archives, we determine soft X-ra
y fluxes, or flux upper limits, for 74 A-type stars, which have been o
bserved during deep integrations with the PSPC. Nine supposedly single
, late-A stars (0.20<B-V<0.35) are found to coincide with X-ray source
s. The X-ray luminosities we infer for these stars range from levels c
omparable to the Active Sun, at log L(x) similar to 27.6, to much brig
hter emission levels similar to those observed for active late-type bi
nary systems, near log L(x) similar to 30.1. Another ten sources are i
dentified with early-A stars (0.0<B-V<0.2). Five of these are confirme
d double stars, the rest are ostensibly single. The maximum luminosity
we detect in the early-A stars, log L(x)=30.1, is 3.5 orders of magni
tude brighter than the X-ray upper limits for the nondetected stars. A
dditional study, including radial-velocity monitoring and/or optical i
nterferometry, will be needed to determine whether the putatively sing
le X-ray emitting stars are in fact single, or whether their emission
is produced entirely or in part by unknown or unresolved binary compan
ions. The level of X-ray emission associated with chemically normal, s
ingle A stars thus far appears to be uncorrelated with any obvious ste
llar property, including the rotation rate, which is known to greatly
influence the dynamo activity and the X-ray emission levels of lower m
ass stars.