Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.8410c&link_type=abstract
2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #84.10; Bulletin of the American Astronomical Society, V
Astronomy and Astrophysics
Astronomy
Scientific paper
The 18 cm (1665, 1667, 1612, and 1720 MHz), 6 cm (4765, 4751, and 4660 MHz) and 5 cm (6031, 6035, 6049, and 6017 MHz) OH lines, as well as the 4830 MHz H2CO and the 6668 MHz CH3OH lines, were detected toward the massive star-forming region IRAS 19111+1048. All lines were observed on July 4-5, 2005 using the Arecibo Telescope L-band, C-band and C-high receivers. The analysis was completed using Arecibo routines for reducing correlator data. Maser emission was confirmed in the 1665, 1667, 6031, and 6035 MHz OH lines, and each maser line was accompanied by an absorption feature. By comparison with previous studies, all but the 6031 MHz line appear to be highly variable. The 6 cm OH lines, the 18 cm and 5 cm OH satellite lines, and the absorption features were found to exhibit weak and broad spectral profiles, indicating that their appearance may be due to a form of quasi-thermal excitation rather than the masing process. Currently there is no evidence for either H2O or CH3OH masers, but massive CO outflows have been detected through previous studies. Along with the detection of OH masers, these properties place IRAS 19111+1048 in a late stage of protostellar evolution in which the H II region has expanded and developed enough to allow for conditions that are unable to generate H2O or CH3OH masers.
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