A study of carbon monoxide and neutral carbon in the S106 molecular core

Details A study of carbon monoxide and neutral carbon in the S106 molecular core A study of carbon monoxide and neutral carbon in the S106 molecular core

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277..307l&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 1, pp. 307-318.

Astronomy and Astrophysics

Astronomy

13

Line: Profiles, Ism: Abundances, Ism: Clouds, Ism: Individual: S106, Ism: Molecules, Radio Lines: Ism

Scientific paper

Maps are presented of J=2-1 and J=3-2 C^18O emission from the molecular environment of the bipolar nebula S106, together with complementary observations of the ^3P_1-^3P_0 CI emission. Line splitting observed extensively over the E molecular cloud suggests that it is best explained as the expanding remnant of a thick toroid surrounding the optical lobes. The poor correlation between the observed molecular line emission and dust continuum emission in the E cloud is probably due to a large temperature gradient. Strong CI emission from the protostellar candidate S106 FIR suggests the nearby presence of a powerful source of far-UV radiation, whose energy supply is unlikely to arise from gravitational contraction of a protostar. It is probable that this source is the star S106 IR, which also heats S106 FIR. There is evidence, in both CI and C^18O, for a predominantly blueshifted outflow from S106 IR, best interpreted as a stellar wind-driven shock into the toroidal remnant. C^18O and ^13CO appear to be depleted, relative to canonical values for their abundances, in S106 FIR, despite its high optical extinction, which should discourage selective photodissociation. Elsewhere in the cloud the CI line profiles show a resemblance to those of C^18O, with intensity equivalent to a few photodissociation regions (PDRs) along the line of sight.

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