Herschel spectroscopy for very young star-forming cores: excitation comma outflows comma and dust emissivity

The properties of very young starforming cores are difficult to trace. Many of their physical parameters still need to be refined observationally, before a meaningful modelling can advance. The Herschel satellite provides access to the wavelength regime where the bulk of emission arises for such objects. We plan to employ the two versatile spectrographs SPIREFTS and PACSSpec in order to scrutinise ^en very young protostars comprising a larger range of masses and luminosities. The selected objects have been revealed as promisinging targets within our Herschel GT project EPoS. Our goals are threefold: (1) We want to recover emission from molecular species like CO and HCO+ with SPIREFTS, which in combination with groundbased data enables an excitation analysis and constraints for line transfer and structure modelling. (2) We want to reveal the slope of the submm continuum emission with FTS lowres spectra, which gives us a handle on the related dust emissivities. This is crucial to lift the degeneracy between column density, temperature, and dust emissivity, which usually renders an interpretation of submm continuum maps ambiguous. (3) With the PACS spectroscopy for a subsample of two objects we want to trace the most important cooling lines of oxygen, carbon, and water to assess the thermal budget for these object stages. Of special importance is the measurement of the OI 63.2 micron line strength. This line gives a more direct access to the true outflow rate than common CO observations and is thus an important tool to characterise our targets which all are known to drive outflows. truncated!, Please see actual data for full text [truncated!, Please see actual data for full text]