R. F. Shipman 1, A. M. Heras 2, S.D. Price 1, Th. de Graauw 3, H. J. Walker 4, M. Jourdain de Muizon 5, M. F. Kessler 2, & T. Prusti 2
1 Air Force Research Laboratory, 29 Randolph Rd., AFRL/VSBC, Hanscom AFB, MA 01731-3010, USA
2 ISO Science Operations Centre, Astrophysics Division of ESA, P. O. Box 50727, E-28080 Villafranca, Spain
3 Space Research Organization of The Netherlands, Postbus 800, NL-9700 AV, Groningen, The Netherlands
4 CLRC, Rutherford Appleton Laboratory, Chilton, Didcot, Oxon, OX11 0QX, UK
5 DESPA, Observatoire de Paris, F-92190 Meudon, France
We present the preliminary results from our effort to classify silicate sources observed by the STARTYP1/2 and ZZSTARTY programs. To characterize our silicate sources, we calculate the silicate emission index, SE, developed by Sloan and Price (1995). This index is a valuable description of the 10 5m silicate emission feature as seen in the IRAS Low Resolution Spectrometer (LRS) data of ABG stars. The wide wavelength coverage and high spectral resolution of SWS are extremely useful in providing added details to the SE classification. Although our sources do not span a wide range in SE types, the approach adopted here will be of great utility for analyzing the final ISO database. The objective of the STARTYP1/2 and ZZSTARTY programs is to construct an ISO database for spectral classification of the brightest representative sources. The final database will be made up of all sources with full SWS grating scans or PHOT-S observations (roughly 700 sources).