Abstract
The Cepheus A East high-mass star-forming region has been mapped at 1.4 mm using the OCS(17–16) and (18–17) lines observed with the IRAM 30 m antenna. Contour maps and high-resolution line profiles reveal the association of OCS with both (i) the hot-core region, and (ii) with the NE, SE, and S outflows driven by the young stellar objects. This confirms that OCS is among the main S-molecules observed in the gas-phase after thermal evaporation due to protostellar heating or shocks due to propagation of protostellar jets. Adopting Local Thermodynamic Equilibrium conditions, optically thin emission, and a temperature of 100 K, the total OCS column density (after correction for beam dilution) of the hot-core component is ∼1016 cm−2. For the outflow component, assuming a temperature range of 20–100 K, and extended emission, the OCS column density is ≤ 5 ×1014 cm−2 for a temperature ≥ 20 K.
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