Our estimates for the abundance of in the hot cores is , while in the warm envelope is . These values have been obtained from the column density, the hydrogen density and assuming that the depth of the cloud along the line of sight is similar to that obtained in the plane of the sky. The fractional abundances of are similar to those found by Cummins et al. (1983) with much lower angular resolution towards Sgr B2. Loren and Mundy (1984) also derived similar values for the hot cores and the ridge in Orion, although they reported that is enhanced a factor 10 in the hot cores. Such a large enhancement of abundances is not seen from our data towards the hot cores in Sgr B2.
© European Southern Observatory (ESO) 1997
Online publication: June 30, 1998