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E. Dotto, M.A. Barucci (DESPA -- Obs. de Paris, France), T. M\"{u}ller (ISO SOC, Villafranca, Spain), J. Crovisier (ARPEGES -- Obs. de Paris, France), T. Encrenaz (DESPA -- Obs. de Paris, France), M. Fulchignoni (Univ. Paris VII, France), R.F. Knacke (Penn. State Univ., Erie, Penn., USA), E. Lellouch (DESPA -- Obs. de Paris, France), P. Morris (Univ. of Amsterdam, The Netherlands), T. Owen (Univ. of Hawaii, Honolulu, USA), J.R. Brucato, L. Colangeli (Oss. Astron. di Capodimonte, Italy), A. Doressoundiram (JPL, CA, USA)
Observations of asteroids have been performed by Infrared Space Observatory (ISO) with the aim to investigate the physical and compositional properties of these objects.
PHT--S performed observations in the spectral range 2.5--12 micrometres, while SWS investigated the region between 5.3 and 45 micrometres.
The Standard Thermal Model and an advanced thermophysical model have been applied to the infrared spectra. Sub--solar and black--body temperatures have been computed for all observed asteroids. The spectral features above the thermal emission continuum are analyzed and discussed in terms of surface composition of the objects. A strong band centered at about 10 micrometres is visible on the spectra of all the observed asteroids suggesting the presence of silicates on the surface of these bodies.
The obtained results and spectral analysis will be presented and discussed for 6 bright main belt asteroids: 1 Ceres, 2 Pallas, 3 Juno, 4 Vesta, 10 Hygiea, 52 Europa.