  We present new optical, near infrared, and archival ultraviolet observations
of XX Ophiuchi and AS 325, two proposed iron stars. These unusual stars have
optical spectra dominated by emission lines arising from hydrogen as well as
ionized metals such as iron, chromium, and titanium. Both stars have been
classified as iron stars and a number of exotic models have been presented for
their origin. Using two years of moderately high resolution optical
spectroscopy, the first high signal-to-noise K-band spectroscopy of these
sources (which reveals stellar photospheric absorption lines), and new
near-infrared interferometric observations, we confirm that both systems are
composed of two stars, likely binaries, containing a hot Be star with an
evolved late-type secondary. The hydrogen emission features arise in the hot
wind from the Be star while the corresponding P-Cygni absorption lines are
produced from dense material in the expanding, radiation driven, wind around
each system. The optical FeII emission lines are pumped by ultraviolet FeII
absorption lines through fluorescence. Contrary to some claims in the
literature, the spectral features of XX Oph and AS 325 are quite similar,
evidence that they are comparable systems. We examine the variability of the
spectral morphology and radial velocity motions of both sources. We also study
the variability of XX Oph during a major photometric event and find that the
spectral nature of the system varies during the event. A comparison of the
velocity of the absorption line components in our new spectra with those in the
literature show that the structure of the stellar wind from XX Oph has changed
since the system was observed in 1951.
