ISO Observations of the earliest Evolutionary Stages of Protostars Part 2 of 3

scientific abstract the prime scientific goal is to obtain precise, well spectrally sampled absolute photometry in the 2.5 200 microns wavelength range of a complete sample of a compact dense condensations of cold dust and gas, selected by sensitive, high angular resolution surveys of cloud cores at mm/sub mm wavelengths. the high precision fir/mir spectra, supplemented by mir/nir diffraction limited imaging, will differentiate between various evolutionary stages, allowing true isothermal protostars, disk and cocoon stars to be distinguished from one another. the relative detection rate of these phenomena will reflect the true incidence of these objects within each of the cloud cores surveyed in the submm, and will therby allow statements to be made about the duration of the evolutionary stages of star formation. observation summary for investigation of nearby protostar candidates and their parent clouds: p25 rasters of subfields (3x3 up to 7x7 depending on cloud size) at 200, 100, 60 micron with tint 5s. raster step interval array repeat length (180, 138 arcsec for c200, c100). to be performed concatenated. for each individual protostar candidate within cloud, perform concatenated: p05 1x11,1x10 rasters at 25 micron, using 10 arcsec aperture and minimal raster step of 10 arcsec. the sum of these will provide 5 sampling over a 100 scanlength. to provide information about the background outside the cloud an additional p05 1x7 raster with 50 raster step is proposed. all p05 rasters use tint5s. p32 at 200, 160, 120 micron (4x2)raster, o/s 2, tint 10s per s/c raster point. p32 at 100, 70, 60 micron (4x2)raster, o/s 2/3, tint 10s per s/c raster point. p40 in a 5x1 raster tint 32s. (raster interval chosen to provide 1 point on protostar candidate, 2 points on parent cloud, 2 points trunca [truncated!, Please see actual data for full text]