ISO spectroscopy of Sharpless 171

Details ISO spectroscopy of Sharpless 171 ISO spectroscopy of Sharpless 171

Feb 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003esasp.511..217o&link_type=abstract

Exploiting the ISO Data Archive. Infrared Astronomy in the Internet Age, held in Siguenza, Spain 24-27 June, 2002. Edited by

Astronomy and Astrophysics

Astronomy

Scientific paper

We report the results of far-infrared observations (3-190 μm) of Sharpless 171 (S171) with the spectrometers on board the Infrared Space Observatory (ISO). Based on the observed intensities of forbidden lines and continuum emission, we derive the physical properties of the observed region, such as the temperature, density, and elemental abundance. The observed line and continuum intensities are in agreement with photodissociation region (PDR) models in most observed positions except for the molecular region, where the [O I] 63 μm to 146 μm ratio is too small (˜ 5) compared to the predictions of existing PDR models. We conclude that the absorption by oxygen atoms in foreground cool clouds is the most likely cause. [Si II] 35 μm line emission is quite strong over the observed region and the [Si II] 35 μm to [N II] 122 μm ratio indicates that Si in the gas phase is about 25% of the solar abundance in the diffuse ionized gas. This value is by an order of magnitude larger than that in typical interstellar diffuse clouds, suggesting dust destruction occurring in the ionized region.

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