The SWS will be used to provide complete spectral scans of the
 unique variable star FG Sge.  This star has always been a true
 puzzle as to its exact nature; however, in 1992, after nearly a
 century of slow brightness and spectral changes, FG Sge began
 undergoing extreme and rapid visual brightness declines follwed
 by a slower return to normal brightness.  These declines are caused
 by mass ejection and dust condensation obscuring the underlying
 stellar photosphere.  This behavior is similar to the R CrB type
 stars (RCB) and leads us to suspect that FG Sge is evolving into
 a new member of the RCB class.  The energy distribution of the SWS
 spectra will be used to infer the distribution of dust with distance.
 Broad spectral features will betray the chemical make-up of the
 dust grains, while broad emission lines from a circumstellar
 envelope may be present.  A comparison of FG Sge's IR dust and gas
 signature with other members of the RCBs will allow us to determine
 whether FG Sge is evolving into a RCB.  The nature and distribution
 of the circumstellar dust and gas will allow us to test certain
 hypothesized formation mechanisms for objects like FG Sge, e.g.
 evolution from a 'born-again' AGB star, where a star on the white
 dwarf cooling track has ignited its He shell and evolved back into
 an object resembling a cooler supergiant star.