Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...311..282s&link_type=abstract
Astronomy and Astrophysics, v.311, p.282-290
Astronomy and Astrophysics
Astrophysics
22
Ism: Abundances, Atoms, Molecules, Clouds, L 183, Radio Lines: Ism
Scientific paper
Observations of the [C I]^3^P_1_-^3^P_0_492GHz fine structure line and isotopic CO(2-1, 3-2) rotational lines have been made at six positions along an east-west strip through the centre of the high-latitude dark cloud L 183 using the James Clerk Maxwell Telescope. The [C I] spectra have line strengths varying between T_MB_=0.8-3.4K. The lines appear broad due to a blend of two kinematically different components around V=~1km/s and V=~2.3km/s which can be resolved at some positions. If the [C I] emission originates in the warmer, translucent envelopes (A_V_=~1-5mag) of L 183 we derive total column densities in both components in the range 7x10^15^-3x10^17^cm^-2^. In case it would come primarily from the cold dark core (A_V_>5mag) we calculate lower limits of about 10^16^-10^17^cm^-2^. The component around V=~1km/s is most likely entirely translucent. We argue that most of the observed [C I] emission from the V=~2.3km/s component also originates in the translucent regions of L 183 and has an optical depth in the range τ=0.1-6. We find a good correlation between the [C I] and 3CO(3-2, 2-1) measurements but not with C 18O(2-1). The derived C/CO column density ratio along the cut varies between 0.08-0.7 and remains constant within the uncertainty. Chemical model calculations are used to study the [C I] column density as well as the C/CO ratio as a function of density and total hydrogen column density. A close inverse correlation is found between N(C)/N(CO) and A_V_ for N(H_2_)~10^20^-5x10^21^cm^-2^, which is consistent with the generally observed correlation between C and CO from diffuse clouds to dense photon dominated regions.
Laureijs Rene J.
Stark Ronald
van Dishoeck Ewine F.
Wesselius R.. P.
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