Contents of: VI/111/./abstract/JCERNICH_HH_JETS.abs

The following document lists the file abstract/JCERNICH_HH_JETS.abs from catalogue VI/111.
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==> 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.



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