  We investigate the integrated far-ultraviolet (FUV) emission from globular
clusters. We present new FUV photometry of M~87's clusters based on archival
HST WFPC2 F170W observations. We use these data to test the reliability of
published photometry based on HST STIS FUV-MAMA observations, which are now
known to suffer from significant red-leak. We generally confirm these previous
FUV detections, but suggest they may be somewhat fainter. We compare the FUV
emission from bright ($M_{V} < -9.0$) clusters in the Milky Way, M~31, M~81 and
M~87 to each other and to the predictions from stellar populations models.
Metal-rich globular clusters show a large spread in FUV-V, with some clusters
in M~31, M~81 and M~87 being much bluer than standard predictions. This
requires that some metal-rich clusters host a significant population of
blue/extreme horizontal branch (HB) stars. These hot HB stars are not
traditionally expected in metal-rich environments, but are a natural
consequence of multiple populations in clusters - since the enriched population
is observed to be He-enhanced and will therefore produce bluer HB stars, even
at high metallicity. We conclude that the observed FUV emission from metal-rich
clusters in M~31, M~81 and M~87 provides evidence that He-enhanced second
populations, similar to those observed directly in the Milky Way, may be a
ubiquitous feature of globular clusters in the local universe. Future HST FUV
photometry is required to both confirm our interpretation of these archival
data and provide constraints on He-enriched second populations of stars in
extra-galactic globular clusters.
