We propose to perform broadband spectroscopy of the bulge of M31.
 These observations will allow us to compare the bulge of M31 with
 Guaranteed Time observations of the disk regions as well as to make
 comparisons with the Galactic bulge, as observed by ISO and other
 instruments.  The bulge of M31 is surprisingly different from that of
 our own Galaxy, especially considering the global similarity of the
 two galaxies.  The bulge of M31 contains far less molecular gas or HI
 than the Galaxy, though some emission from ionized (HII) gas is known.
 On the other hand, the bulge of M31 contains far more X-ray emission,
 both point and diffuse sources, than within a similar region of our
 own Galaxy.  The M31 bulge is known to be a strong IR source from IRAS
 observations, particularly in the 60 and 100 micron range.  This long
 wavelength emission is suspected to be due to interstellar dust
 clouds.  Our proposed spectroscopy will allow us to study the thermal
 emission from this dust, to detect the emission from molecular or
 ionized gas, and to determine the elemental abundances in the core of
 M31.