Submillimetre molecular line observations of M17: The interaction of an ionisation front and molecular clouds

Details Submillimetre molecular line observations of M17: The interaction of an ionisation front and molecular clouds Submillimetre molecular line observations of M17: The interaction of an ionisation front and molecular clouds

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf...33r&link_type=abstract

In NASA. Ames Research Center Summer School on Interstellar Processes: Abstracts of Contributed Papers p 33-34 (SEE N87-15043 0

Astronomy and Astrophysics

Astronomy

Astronomical Maps, Interstellar Chemistry, Ionization, Ionized Gases, Line Spectra, Molecular Clouds, Molecular Gases, Radio Emission, Space Observations (From Earth), Submillimeter Waves, Carbon Monoxide, H Ii Regions, Interstellar Masers, Star Formation

Scientific paper

An area of about 9 by 10 arc minutes in the M17 molecular cloud has been mapped in the J=3-2 transition of CO. The strongest CO emission is observed to come from the two bars to the north and southwest, which lie just outside the area of ionized gas seen in the radio continuum studies. We are viewing the boundary between the ionized and molecular gas almost edge on. The most intense CO emission is from the area around the dense molecular cloud core M17SW in the southwest bar. To the east of M17SW there are signs of recent or continuing star formation including H2O masers and an ultra-compact HII region. The CO J=3-2 spectra observed are complex with considerable variation in line shapes occuring over distances of less than one arc minute. We interpret the velocity structure of this region as arising from an ensemble of molecular cloud fragments in addition to extended emission. We have identified several cloud components at different velocities within both the northern and southwest bars of CO emission. A simple kinematic model of the cloud components in the southwest bar in which they are considered to be clumps of post-shock gas lying close to the edge of the expanding HII region, with the shock being driven by Kleinmann's star, gives a velocity of approx. 10.8 km s(-1) for the expansion velocity of the HII region, which is currently at a distance of approx. 2.4 pc from Kleinmann's star. The resulting shock is thought to be preceding the ionisation front and appears to have led to the fragmentation of the original cloud.

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