Observations of [c I] and Co Absorption in Cold, Low-density Cloud Material toward the Galactic Center Broad-line Emission

We report the detection of a deep (C I) absorption feature at km s~1 with a line 3P1] 3P0 vLSR \ 12 width of 6 km s~1 toward extended line emission at a distance of 11@ from Sgr C. The 492 GHz observations were made with the Antarctic Submillimeter Telescope and Remote Observatory. The absorption feature allows the derivation of lower limits for the C I column density in the cold foreground material. The feature is unlikely to be caused by self-absorption within the [C I]Èemitting cloud because it is observed over a region at least 4@ across and is also seen in emission 22@ north of the Galactic plane in 12CO J \ 2È1. In order to determine the temperature and the abundance ratio of C I to CO in the foreground gas, we compare the observations with 12CO and 13CO J \ 1È0 observations obtained with the Bell Labs 7 m antenna and with 12CO and 13CO J \ 2È1 observations made with the KoŽ lner Observatorium fuŽ r Submillimeter und Millimeter Astronomie 3 m telescope. All these observations have about the same beam size. On the assumption that the background emission is not spatially associated with the absorbing cloud(s), a consistent model for the observed line intensities yields an excitation temperature of 3.5 K for 13CO and 5 K for [C I], which implies low volume densities, cm~3. n(H2) [ 103 The measured abundance ratio of C I to 13CO is D34. This value is consistent with photochemical model calculations that predict an abundance ratio of C I to 12CO of D1 and a 12CO to 13CO ratio of D30 (reduced in comparison to the intrinsic 12C to 13C isotopic ratio of 60 by fractionation). The observed 13CO column density corresponds to an of 4.6 mag, i.e., the hydrogen column density N(H) AV is D9 ] 1021 cm~2. This, together with the observed [C I] line width, indicates that the absorption is likely due to several translucent clouds. We compare our results with line Ñuxes derived from the large-scale, low-resolution COBE FIRAS spectral line survey of [C I] and [C I] emission in the Galactic plane. Taking into 3P1] 3P0 3P2] 3P1 account beam Ðlling, the lower limit for the column density of cold K) C I that is traced by our (Tex1 10 absorption observations is at least a factor of 2 higher than the column density of the warmer C I (Texo 20 K) detected in emission by COBE. Our results suggest that a substantial fraction of atomic carbon in the interstellar medium may be difficult to detect in [C I] emission, owing to its low excitation. Subject headings : Galaxy : abundances È Galaxy : center È ISM: atoms È ISM: general È ISM: molecules È radio lines : ISM