The profile of the |υ=1-0 S(1)| line of molecular hydrogen in the proto-planetary nebula CRL 618 has been measured at 35 km s−1 resolution and the resultant spectrum deconvolved. The line is found to have a total velocity width of ∼250 km s−1, the largest yet observed for a galactic source, and to consist of several discrete components. We interpret the high-velocity line emission in terms of discrete molecular clumps embedded in and shocked by a fast stellar wind. The S(1) line profile in CRL 618 constitutes positive evidence for this mechanism in explaining the large H2 linewidths observed in many sources. We suggest that the bulk of the H2 line emission, at low velocities, originates in shocks on the inner edge of a dense gas and dust toroid and has been scattered off dust grains in the optical lobes of the source.
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Burton et al. (1986) studied this question.
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