  The star ASAS J174600-2321.3 was found to exhibit peculiar photometric
variability (conspicuous brightening of about 4 magnitudes (V), fast luminosity
declines, intrinsic pulsations). It was rejected as an RCB candidate in recent
investigations on spectroscopic grounds. We have collected and present all
available data from public sky surveys, photometric catalogues, and the
literature. From an analysis of these data, we have identified ASAS
J174600-2321.3 as a long-period eclipsing binary (Porb = 1011.5 days). The
primary star, which is probably a white dwarf, is currently in outburst and
exhibits the spectral characteristics of a reddened, early F-type supergiant;
the secondary star is a giant of spectral type late M. We discuss the possible
origin of the observed brightening, which is related to the primary component.
ASAS J174600-2321.3 is most certainly an eclipsing symbiotic binary - probably
a symbiotic nova of GCVS type NC - that is currently in outburst. However,
further photometric and spectroscopic data are needed to confirm this.
