The following document lists the file abstract/JCERNICH_HH_JETS.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
==> In this proposal, we would like to observe HH jets and HH objects in Orion ==> that are now visible as a consequence of the extra ISO flying time HH jets and molecular outflows represent probably different aspects of the same physical phenomena : the formation of stars and their first stages of evolution. This conexion between HH jets and molecular outflows has been strongly confirmed recently by Cernicharo and Reipurth (1996) in HH111 where they have found, for the first time, extremely high velocity CO bullets just and the end of the optical jet, i.e. the jet appears to coexist with previous ejections of matter from the newly formed star similar to that found in class 0 sources. As HH111 becomes now visible for ISO we would like to observe this keystone HH jet with ISOCAM and the SWS and LWS spectrometers. Molecular outflows have been studied in detail through the observation of the molecular emission of CO and other molecular species. In the regions of shocks between the HH/molecular jets and the ambient gas the density is high enough to couple gas and dust. Hence, the emission of dust will be playing a key role in the global cooling and in the evolution of the shock/post-shock regions. Unfortunately little is known about the dust in these regions. In the central program a few class 0 objects have been observed with ISOCAM but nothing has been done concerning HH jets and HH objetcs with this instrument. In order to reveal the dust properties in these regions we propose a systematic study of the dust emission with ISOCAM (filters and CVFs), and the SWS and LWS spectrometers in HH111 and towards the remarkables HH jets and HH objects HH1-2 and HH7-11. The main goal of this proposal is to analyze the interaction of the energetic HH jets with the ambient clouds. We ask for high priority time in view that is the last chance for ISO to take deep images of low mass star forming regions. The proposed observations will constitute for long the only available data on prominent HH jets and objets. It will be sad to let it go.