Caux E. 1, Ceccarelli C. 2, Castets, A. 2, Loinard, L. 2, Molinari, S. 3, Saraceno, P. 4, Smith, H.A. 5, & White, G.J. 6
1 CESR, BP 4346, F-31028 Toulouse cedex 04, France
2 Observatoire de Grenoble, BP 53, 38041 Grenoble cedex 9, France
3 IPAC, 100-22 Pasadena, CA 91125, USA
4 CNR-IFSI, Area di Rcerca Tor Vergata, via Fosso del Cavaliere, I-00133, Roma, Italy
5 NASA Headquarters, 300 E. Street, S.W., Washington, DC 20546, USA
6 Queen Mary & Westfield College, University of London, Mile end road, London E1 4NS, UK
We present ISO-LWS spectroscopic observations of the nearby long studied region of recent and active star formation, NGC1333. Data were obtained on protostar sources IRAS2, IRAS4 and IRAS6, as well as on some lines of sight of the associated molecular outflows. The molecular line emission (mainly CO and H2O) of the sources will be discussed, and comparison with other observations, particularly in the submillimeter and millimeter range, will be made. The physical parameters of the sources will be deduced and the differences of molecular line emission from the 3 objects, as well as from various positions in the molecular outflows will be emphasised. The ratio of atomic lines emission ([OI], [CII]...) versus molecular line emission for each source will allow us to assess if the major cooling lines are due to PDR emission or shocked gas. The FIR spectra of the sources will be compared to the different shock models (``J'' shocks, e.g. Hollenbach & McKee, 1989, and ``C'' shocks, e.g., Kaufman & Neufeld, 1996).