ISO Spectroscopy of H2 in Star Forming Regions
| dc.creator | Ancker, M. E. van den | |
| dc.creator | Wesselius, P. R. | |
| dc.creator | Tielens, A. G. G. M. | |
| dc.date | 2000-01-19 | |
| dc.date.accessioned | 2026-07-07T01:51:48Z | |
| dc.date.available | 2026-07-07T01:51:48Z | |
| dc.description | We have studied molecular hydrogen emission in a sample of 21 YSOs using spectra obtained with the Infrared Space Observatory (ISO). H2 emission was detected in 12 sources and can be explained as arising in either a shock, caused by the interaction of an outflow from an embedded YSO with the surrounding molecular cloud, or in a PDR surrounding an exposed young early-type star. The distinction between these two mechanisms can not always be made from the pure rotational H2 lines alone. Other tracers, such as PAH emission or [S I] 25.25 micron emission, are needed to identify the H2 heating mechanism. No deviations from a 3:1 ortho/para ratio of H2 were found. Both shocks and PDRs show a warm and a hot component in H2, which we explain as thermal emission from warm molecular gas (warm component), or UV-pumped infrared fluorescence in the case of PDRs and the re-formation of H2 for shocks (hot component). | |
| dc.description | 4 pages, 2 figures, to appear in proc. "H2 in Space", eds. F. Combes & G. Pineau des Forets | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0001336 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0001336 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/417 | |
| dc.subject | Astrophysics | |
| dc.title | ISO Spectroscopy of H2 in Star Forming Regions | |
| dc.type | text |