Chemistry in infrared dark clouds (Vasyunina+, 2011)

Details Chemistry in infrared dark clouds (Vasyunina+, 2011) Chemistry in infrared dark clouds (Vasyunina+, 2011)

Feb 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ycat..35279088v&link_type=abstract

VizieR On-line Data Catalog: J/A+A/527/A88. Originally published in: 2011A&A...527A..88V

Physics

Molecular Clouds, Infrared Sources, Spectroscopy, Interstellar Medium

Scientific paper

The observations were made with the 22-m Mopra radio telescope, operated by the Australia Telescope National Facility (ATNF) in position switching mode. In total we spent 7 minutes on source and 7 minutes on the OFF position. Our targets are dense molecular condensations within larger molecular clouds with often widespread molecular emission. Therefore, we refrained from using one standard OFF position throw. Instead, OFF positions were chosen individually for every target region and were approximately 8-10' away from the source.
The Mopra spectrometer (MOPS) offers zoom-mode configurations with the possibility to observe up to 16 sub-bands of 138MHz each within a total frequency range of 8.3GHz. This set-up delivers a velocity resolution of ~0.11km/s.
The observations were carried out on 9-11 May 2008 with the 3mm band receiver. We put the central frequency for the 8.3GHz block to 89270MHz and thus covered the range from 85 to 93 GHz. In this range we distributed 13 zoom windows, which covered N2H+, 13CS, CH3CN, HC3N, HNC, HCO+, HCN, HNCO, C2H, SiO, H13CO+^, H13^CN, and CH3C2H.
System temperature measurements were performed every 30 minutes and a pointing scan every hour. Typical system temperatures (measured with the common chopper-wheel technique) during the observations were 170-210K. At Mopra observatory, SiO masers are used to correct the telescope pointing, giving a pointing accuracy better than 10". The main beam of the telescope varies between 36" at 86 GHz and 33" at 115GHz and the main beam efficiency varies between 0.49 at 86GHz and 0.44 at 100GHz (Ladd et al., 2005PASA...22...62L).
Mopra data are originally stored in RPFITS format. Using the ATNF Spectral line Analysis package (ASAP), we transformed these raw data into ascii files, which were then fed into GILDAS for further analysis. Data files were written in CLASS77 format.
(3 data files).

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