Star Formation in Molecular Cloud Cores

scientific abstract the new detector saturation limits given by the isophot team have it made necessary to replace the three brightest targets in m17sw by a fainter protostellar condensation. the two condensations in m17sw will be observed with the same aot.s as originally proposed. it was only necessary to replace some of the filters and to make minor changes of the map parameters. the molecular cloud cores m17sw and mon r2 play central roles in the discussion of starformation processes. in both cases previous high spatial resolution observations show the existence of gas clumps and cool dust condensations. sometimes these are related to compact ir sources. dependent on the launch date, we propose to measure the spectral flux distributions of deeply embedded premain sequence stars and presumably protostellar condensations either in m17sw or in mon r2. because the energy distributions of our targets peak at or beyond 100 microns iso is especially suited to supplement available submm/mm fluxes and derive broadband flux distributions for these examples of very early stellar evolutionary phases. observation summary m17sw: from ipac maps and submm/mm observations by the bonn mpifr bolometer group, we selected two protostellar condensations. we propose to make oversampled maps of the protostellar condensations with phtc200 (filters: 135 and 200 microns, aot p32: oversampling factor 1) as well as singlepointed raster maps with phtp at 60 microns. furthermore, the condensations should be observed in the singlepointing multi filter mode with phtp and filters 3.6, 4.85, 7.7, 11.5, and 25 microns (aot p03). mon r2: we propose make oversampled maps at the position of mon r2irs1 with phtc100 and filters 60 and 100 microns, and with phtc200 and filters 135 and 200 microns (aot p32). furthermore, we want to get singlepointing multifilter observations with phtp at wavelengths 3.6, 4.85, 7.7 truncated!, Ple [truncated!, Please see actual data for full text]