We propose to investigate the newly discovered 7.15 micron oxygen-rich
(OR) circumstellar emission feature by observing its profile and
distribution among approximately 50 oxygen-rich stars distributed
throughout the sky.  We expect this study to place constraints on the
abundances, stellar evolution and chemistry of dust formation in these
stars, and the importance of the emitting material as a possible inter-
stellar dust component. The IRAS AutoClass II study of Cheeseman et al.
1989 provides a guide from which we select a set of stars representing
the entire population of OR stars. One star is selected from each of
the 32 OR subclasses expected to have the feature present. Based upon
the work of Goebel et al.(1994 Ap.J. July 15,1994), these objects have
a high probability of displaying the 7.15 um feature. Stars from each
relevant subclass need to be observed with the SWS throughout their
entire spectral range so that all spectral features may be accurately
profiled, defined, and correlated with the 7.15 um feature. High reso-
lution scans are required to determine the influence of molecular
bands on the features at 7.15, 10, 11.3, 13.1, 18, and 19.7 um. Shape
and relative strength of the features should enable identification of
the responsible dust component.  Once high resolution scans of a rep-
resentative sample of OR stars have been obtained, the low resolution
spectra of survey investigators can be used to supplement our statis-
tics, but not to determine the confusing influences of molecular
bands, nor meet the goals of this proposal.  We anticipate reciprocal
sharing of the proposed AOT SWS01-3 high resolution data with other
groups that have AOT SWS01-1 low resolution data of OR objects,
notably Price, Tsuji, de Jong, Heske, Waters, and Barlow. The 7.15
um feature is in a spectral region blocked completely by the earth's
atmospheric water vapor. ISO is the only platform with sufficient
sensitivity, sky coverage, and instrumentation able to address the
goals set forth.