Mid-infrared High Resolution Spectroscopy of UCHII Region G29.96 -0.02

Details Mid-infrared High Resolution Spectroscopy of UCHII Region G29.96 -0.02 Mid-infrared High Resolution Spectroscopy of UCHII Region G29.96 -0.02

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...207.8118z&link_type=abstract

American Astronomical Society Meeting 207, #81.18; Bulletin of the American Astronomical Society, Vol. 37, p.1303

Astronomy and Astrophysics

Astronomy

Scientific paper

We present our high resolution mid-infrared fine-structure line observations of an UCHII region - G29.96 -0.02. By stepping the telescope across the object, we mapped the region in [Ne II] 12.8{μ } m, [Ar III] 8.99{μ } m, [S III] 18.7{μ } m, [S IV] 10.51{μ } m, Hua 12.3{μ } m with Texas Echelon Cross Echelle Spectrograph (TEXES) on the NASA IRTF 3m infrared telescope at Mauna Kea, Hawaii. Our 4km/s resolution observations enable us to measure the wavenumber of the [Ar III], [S III] and [S IV] lines accurately with an uncertainty less than 0.001 cm-1. Using the ionization code Cloudy, we fit the line fluxes and estimate the physical properties of the region and the ionizing source. The model shows that the emitting gas forms dense clumps with density ne 6*104cm-3. The filling factor of the emitting region is below 0.1. The ionized region is slightly over-abundant in neon, sulfur and argon. We also find that the spectral type (O7.5) predicted by Cloudy is two subtypes later than the value estimated from radio free-free continuum emission.
Acknowledgement: This work was supported by NSF grant AST-0205518.

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