ISO-LWS observations of IRAS16293-2422

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Title:		ISO-LWS observations of IRAS16293-2422
Authors:		Ceccarelli, C.; Caux, E.; Liseau, R.; Molinari, S.; Nisini, B.; White, G. J.; Wolfire, M.; Furniss, I.; Saraceno, P.
Affiliation:		AA(Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, F-38041 Grenoble cedex, France and CNR-Istituto di Fisica dello Spazio Interplanetario, CP 27, I-00044 - Frascati, Italy ), AB(CESR/CNRS-UPS, BP 4346, 31029 Toulouse cedex, France), AC(Stockholm Observatory, S-133 36 Saltsjobaden, Sweden), AD(CNR-Istituto di Fisica dello Spazio Interplanetario, CP 27, I-00044 - Frascati, Italy and LIDT, ISO Science Operations Centre Villafranca, Spain), AE(CNR-Istituto di Fisica dello Spazio Interplanetario, CP 27, I-00044 - Frascati, Italy), AF(Queen Mary & Westfield College - Un. of London, Mile End Road - London E1 4NS, UK), AG(University of Maryland, College Park, MD, 20742, USA), AH(University College, Gower St., London WC1E6BT, UK), AI(CNR-Istituto di Fisica dello Spazio Interplanetario, CP 27, I-00044 - Frascati, Italy)
Publication:		Low Mass Star Formation - from Infall to Outflow, Poster proceedings of IAU Symposium No. 182 on Herbig-Haro Objects and the Birth of Low Mass Stars. 20-24 January 1997, Chamonix, France, Edited by F. Malbet and A. Castets, p. 66.
Publication Date:		00/1997
Origin:		AUTHOR
Bibliographic Code:		1997IAUS..182P..66C

Abstract

We obtained LWS grating spectra toward IRAS 16293-2422 and the surrounding region, which covers the entire extent of the molecular outflow. The LWS spectra show that the region is relatively uncontaminated by PhotoDissociationRegion (PDR)-like emission, showing only a weak diffuse CII emission. The on-source spectrum revealed the presence of the OI(63 microns) line and several lines from CO, H_2O and OH molecules. In this work we derive the macroscopic quantities associated with the UV-illuminated emitting gas which surrounds IRAS16293-2422 and compare it with previous studies. We show that the molecular lines originate in a hot (~1600 K), dense (~ 3 \cdot 10^4cm^ -3) and extended (~ 8 \cdot 10¹⁶cm) region, that we interprete as the shock of the wind impacting obliquely with the walls of the cavity created by the wind itself. The OI(63 microns) line observed by the Kuiper Airborne Observatory (KAO: Ceccarelli et al. 1997a) at ~ 1.2 \cdot 10¹⁷cm west from the central source is hence interpreted as the head of the shock where the wind strikes the ambient gas. Finally we speculate that the OI(63 microns) line emission seen on-source originates in the collapsing envelope that surrounds the central object(s).

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