Giannini, T.; Nisini, B.; Lorenzotti, D.; Spinoglio, L.; di Giorgio, A. M.; Benedettini, M.; Saraceno, P.; Smith, H. A. and White, G. J.
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We present the ISO-LWS spectra (45-200 μm) of the molecular cloud NGC2024 and its associated H II region. We observed the two class 0 FIR3 and FIR5 and the infrared source IRS2. All the spectra appear quite similar, all showing, at approximately the same intensity level, the high-J CO rotational lines (from Jup=17 to Jup=14), and several atomic and ionic lines from Oxygen, Carbon and Nitrogen. The molecular emission has been fitted with a Large Velocity Gradient model, and results originating in an extended and clumpy PDR with a temperature ~ 100 K and a density ~ 106 cm-3. Column densities in excess of 1018 cm-2 are derived from this molecular component. an [OI] 63 μm/[OI] 145 μm line ratio of about 5 is found across all the region, indicating that the 63 μm line is strongly absorbed by a cold foreground gas along the line of sight. From the intensity ratios of the ionic lines relevant physical properties of the ionized gas (N/O abundance, electron density) are derived and compared with those of other galactic H II regions.
|Item Type:||Conference Item|
|Copyright Holders:||2000 European Space Agency|
|Extra Information:||Star formation from the small to the large scale.
ESLAB symposium (33 : 1999 : Noordwijk, The Netherlands). Edited by F. Favata, A. Kaas, and A. Wilson.
Proceedings of the 33rd ESLAB symposium on star formation from the small to the large scale, ESTEC, Noordwijk, The Netherlands, 2-5 November 1999 Noordwijk, The Netherlands: European Space Agency (ESA), 2000. ESA SP 445., p.373
|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:||23 Feb 2012 16:15|
|Last Modified:||26 Feb 2016 04:43|
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