First Detection of Submillimeter [C I] Emission in the Small Magellanic Cloud

Details First Detection of Submillimeter [C I] Emission in the Small Magellanic Cloud First Detection of Submillimeter [C I] Emission in the Small Magellanic Cloud

2000-08-02

arxiv.org/abs/astro-ph/0008055v1

Astronomy and Astrophysics

Astrophysics

12 pages including 1 table and 2 figures, using AASTEX macros v4.0, to appear in The Astrophysical Journal Letters

Scientific paper

10.1086/312893

We report the first detection of [CI] (3P1-3P0) emission at 609 um in a region of the Small Magellanic Cloud (N27). Environments poor in heavy elements and dust such as the SMC are thought to be dominated by photodissociation regions. This is the lowest metallicity source where submillimeter neutral carbon emission has been detected. Studying the [CI]/CO intensity ratio in several sources spanning more than an order of magnitude in metallicity, Z, we find that the [CI]/CO ratio increases for decreasing Z. The existence of such a trend points to a photodissociation origin for most of neutral carbon in molecular clouds, in agreement with standard PDR models. We also report ISO FIR spectroscopic observations of N27, and use them to derive its physical properties. Comparison between the density and radiation field revealed by FIR diagnostics (n~300-1000 cm-3, Xuv~30-100 Xo) and those derived from millimeter and submillimeter data (n~10^5 cm-3, Xuv<30 Xo) suggests that the FIR lines originate in more diffuse gas, and are perhaps dominated by the interclump medium. Regardless of the cause, analysis of the FIR and mm-submm data produces a discrepancy of two orders of magnitude for the density of this source.

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