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Astron. Astrophys. 315, L321-L324 (1996)

LWS-spectroscopy of Herbig Haro objects and molecular outflows in the Cha II dark cloud*

B. Nisini1, D. Lorenzetti2, M. Cohen3, C. Ceccarelli1,4, T. Giannini1, R. Liseau1,5, S. Molinari1,6, A. Radicchi1, P. Saraceno1, L. Spinoglio1, E. Tommasi1, P.E. Clegg7, P.A.R. Ade7, C. Armand6, M.J. Barlow8, M. Burgdorf6, E. Caux9, P. Cerulli1, S.E. Church10, A. Di Giorgio6, J. Fischer11, I. Furniss8, W.M. Glencross8, M.J. Griffin7, C. Gry6, K.J. King12, T. Lim 6, D.A. Naylor13, D. Texier6, R. Orfei1, Nguyen-Q-Rieu14, S. Sidher6, H.A. Smith15, B.M. Swinyard12, N. Trams 6, S.J. Unger 12, and G.J. White7

1 CNR-Istituto di Fisica dello Spazio Interplanetario, Casella Postale 27, I-00044 Frascati, Italy
2 Osservatorio Astronomico di Roma, I-00040 Monte Porzio, Italy
3 Radio Astronomy Laboratory, Univ. of California, Berkeley, USA
4 Laboratoire d'Astrophysique de l'Observatoire de Grenoble, rue de la Piscine, BP 53, F-38041 Grenoble, France
5 Stockholm Observatory, S-133 36 Saltsjöbaden, Sweden
6 The LWS Instrument-Dedicated Team, ISO Science Operations Centre, Villafranca, Spain
7 Physics Department, Queen Mary & Westfield College, University of London, Mile End Road, London E1 4NS, UK
8 University College London, Dept. of Physics and Astronomy, Gower Street, London WC1E 6BT, UK
9 CESR/CNRS-UPS, BP 4346, F-31029 Toulouse Cedex, France
10 California Institute of Technology, Pasadena, CA 91125, USA
11 Naval Research Laboratory, Remote Sensing Division, 4555 Overlook Ave., SW Washington D.C., USA
12 Space Science Department, Rutherford Appleton Lab, Chilton, Oxon OX11 OQX, UK
13 Dept. of Physics, University of Lethbridge - Lethbridge, Alberta t1k 3m4, Canada
14 Observatoire de Paris, 61 avenue de l'Observatoire, F-75014 Paris, France
15 Laboratory for Astrophysics, National Air and Space Museum, Smithsonian Institution, Washington D.C., USA

Received 28 June 1996 / Accepted 13 September 1996

Abstract. We present the first far infrared spectra of the Herbig Haro objects HH 52-53-54 and of IRAS 12496-7650, all located in the nearby star forming region known as Chamaleon II dark cloud, obtained with the Long Wavelength Spectrometer (LWS) onboard the Infrared Space Observatory (ISO). The richest spectrum is found in HH54, showing molecular transitions (CO with img1.gif from 19 to 14, water vapour mainly in its ortho form and OH) and low excitation fine structure lines ([OI]63, 145 img2.gifm, [CII]158 img2.gifm). In HH52 and HH53,only the [OI] and [CII] lines are detected. The LWS spectrum of IRAS 12496-7650 shows both fine structure and CO lines. The [CII]158 img2.gifm line is ubiquitous in the region, as proved by its presence in all ISO pointings, including the raster scan maps. The fine structure lines are used to evaluate the physical parameters of the emitting regions. In particular, the mass loss rates of each outflow present in the region, are derived from the [OI]63 img2.gifm line luminosity.

Key words: stars: formation - stars: individual: IRAS 12496-7650 - ISM: jets and outflows - ISM: individual objects: HH52,53,54 - infrared: ISM: lines

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States and with the partecipation of ISAS and NASA

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