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.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|Google Scholar:||Look up in Google Scholar|
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.
|Item Type:||Journal Article|
|Copyright Holders:||1996 European Southern Observatory|
|Keywords:||stellar formation; IRAS 12496-7650; jets and outflows; HH 52; HH 53; HH 54; infrared; lines|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||22 Mar 2012 11:36|
|Last Modified:||24 Feb 2016 06:26|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.