Mid-IR Observation and Kinematic Model of A Cometary UC HII Region G29.96 -0.02

Details Mid-IR Observation and Kinematic Model of A Cometary UC HII Region G29.96 -0.02 Mid-IR Observation and Kinematic Model of A Cometary UC HII Region G29.96 -0.02

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20114306z&link_type=abstract

American Astronomical Society Meeting 201, #143.06; Bulletin of the American Astronomical Society, Vol. 35, p.569

Astronomy and Astrophysics

Astronomy

Scientific paper

Mid-Infrared high-resolution spectroscopy allows the possibility of the study of kinematics of Ultracompact HII (UC HII) regions inside dense molecular clouds. Using the TEXAS Echelon Cross Echelle Spectrograph (TEXES) at the IRTF, we mapped a sample of such regions in five ionic emission lines: [Ne II] (12.8μm), [Ar III] (8.99μm), [S III] (18.71μm), [S IV] (10.51μm), Huα (12.3μm). [Ne II] observation in one comet-shaped UC HII - G29.96 -0.02 is displayed here. The comparison between our observations and model predictions shows that the stellar wind compressed bowshock is the major cause of the mass flow in the ionized region.
The TEXES is the prototype of the EXES, an instrument sponsored by NASA SOFIA (the Stratospheric Observatory for Infrared Astronomy) project.

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