EDP Sciences
Free Access
Volume 446, Number 2, February I 2006
Page(s) 561 - 567
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361:20053925
Published online 13 January 2006
A&A 446, 561-567 (2006)
DOI: 10.1051/0004-6361:20053925

Outflows from young objects observed with the ISO-LWS

I. Fine structure lines [O I] 63 $\mu$m, [O I] 145 $\mu$m and [C II] 157 $\mu$m
R. Liseau1, K. Justtanont1 and A. G. G. M. Tielens2

1  Stockholm Observatory, AlbaNova University Center, Roslagstullsbacken 21, 106 91 Stockholm, Sweden
2  Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
    e-mail: [rene.liseau;kay]@astro.su.se;tielens@astro.rug.nl

(Received 26 July 2005 / Accepted 29 September 2005)

Far infrared fine structure line data from the ISO archive have been extracted for several hundred YSOs and their outflows, including molecular (CO) outflows, optical jets and Herbig-Haro (HH) objects. Given the importance of these lines to astrophysics, their excitation and transfer ought to be investigated in detail and, at this stage, the reliability of the diagnostic power of the fine structure transitions of O I and C II has been examined. Several issues, such as the extremely small intensity ratios of the oxygen 63 $\mu$m to 145 $\mu$m lines, are still awaiting an explanation. It is demonstrated that, in interstellar cloud conditions, the 145 $\mu$m line is prone to masing, but that this effect is likely an insufficient cause of the line ratio anomaly observed from cold dark clouds. Very optically thick emission could in principle also account for this, but would need similar, prohibitively high column densities and must therefore be abondoned as a viable explanation. One is left with [O I] 63 $\mu$m self absorption by cold and tenuous foreground gas, as has been advocated for distant luminous sources. Recent observations with the submillimeter observatory Odin support this scenario also in the case of nearby dark molecular clouds. On the basis of this large statistical material we are led to conclude that in star forming regions, the [O I] and [C II] lines generally have only limited diagnostic value.

Key words: ISM: atoms -- ISM: clouds -- ISM: jets and outflows -- stars: formation -- masers -- line: formation

© ESO 2006

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