Nisini, B.; Lorenzetti, D.; Cohen, M.; Ceccarelli, C.; Giannini, T.; Liseau, R.; Molinari, S.; Radicchi, A.; Saraceno, P.; Spinoglio, L.; Tommasi, E.; Clegg, P. E.; Ade, P. A. R.; Armand, C.; Barlow, M. J.; Burgdorf, M.; Caux, E.; Cerulli, P.; Church, S. E.; di Giorgio, A.; Fischer, J.; Furniss, I.; Glencross, W. M.; Griffin, M. J.; Gry, C.; King, K. J.; Lim, T.; Naylor, D. A.; Texier, D.; Orfei, R.; Nguyen-Q-Rieu, N; Sidher, S.; Smith, H. A.; Swinyard, B. M.; Trams, N.; Unger, S. J. and White, G. J.
LWS-spectroscopy of Herbig Haro objects and molecular outflows in the Cha II dark cloud∗.
Astronomy and Astrophysics, 315 L321-L324.
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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 HH 54, showing molecular transitions (CO with Ju from 19 to 14, water vapour mainly in its ortho form and OH) and low excitation fine structure lines ([OI]63, 145μm, [CII]158μm). In HH 52 and HH 53, only the [OI] and [CII] lines are detected. The LWS spectrum of IRAS 12496-7650 shows both fine structure and CO lines. The [CII]158μm 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]63μm line luminosity.
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