Detection of [CI] 492 GHz emission from a high-latitude translucent cloud

Details Detection of [CI] 492 GHz emission from a high-latitude translucent cloud Detection of [CI] 492 GHz emission from a high-latitude translucent cloud

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286l..43s&link_type=abstract

Astronomy and Astrophysics 286L, L43-L46 (1994)

Astronomy and Astrophysics

Astrophysics

27

Ism: Abundances, Atoms, Clouds: Hd 210121, Radio Lines: Ism

Scientific paper

The [CI]^3^P_1_-^3^P_0_ 492 GHz fine structure line has been detected in the high-latitude cloud toward HD 210121 using the James Clerk Maxwell Telescope. The measured [CI] line strengths vary between T_MB_=0.6-1.6K and appear correlated with the CO J=1-0 emission. The inferred [CI] column densities can be well explained by models with densities n_H_~500-5000cm^-3^ and a low incident radiation field, which causes the C^+^, C -> CO transition zone to be shifted to lower A_V_ values. The derived N(C)/N(CO) ratio is about 3 6, significantly larger than found in dense PDRs. Cooling by [CI] is larger than that by CO in this cloud and may be compatable to that by [CII] within a factor of a few.

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