Observations of [Ci] and CO Absorption in Cold, Low‐Density Cloud Material toward the Galactic Center Broad‐Line Emission

We report the detection of a deep P-3(1) --> P-3(0) (C I) absorption feature at upsilon(LSR) = 12 km s(-1) with a line 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]-emitting 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 (CO)-C-12 J = 2-1. In order to determine the temperature and the abundance ratio of C I to CO in the foreground gas, we compare the observations with (CO)-C-12 and (CO)-C-13 J = 1-0 observations obtained with the Bell Labs 7 m antenna and with (CO)-C-12 and (CO)-C-13 J = 2-1 observations made with the Kolner Observatorium fur 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 (CO)-C-13 and 5 K for [C I], which implies low volume densities, n(H-2) less than or similar to 10(3) cm(-3). The measured abundance ratio of C I to (CO)-C-13 is similar to 34. This value is consistent with photochemical model calculations that predict an abundance ratio of C I to (CO)-C-12 of similar to 1 and a (CO)-C-12 to (CO)-C-13 ratio of similar to 30 (reduced in comparison to the intrinsic C-12 to C-13 isotopic ratio of 60 by fractionation). The observed (CO)-C-13 column density corresponds to an A(v) of 4.6 mag, i.e., the hydrogen column density N(H) is similar to 9 x 10(21) 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 fluxes derived from the large-scale, low-resolution COBE FIRAS spectral line survey of [C I] P-3(1) --> P-3(0) and [C I] P-3(2) --> P-3(1) emission in the Galactic plane. Taking into account beam filling, the lower limit for the column density of cold (T-ex less than or equal to 10 K) C I that is traced by our absorption observations is at least a factor of 2 higher than the column density of the warmer C I(T-ex greater than or equal to 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.