1.2mm maps of southern Infrared Dark Clouds (Vasyunina+, 2009)

Details 1.2mm maps of southern Infrared Dark Clouds (Vasyunina+, 2009) 1.2mm maps of southern Infrared Dark Clouds (Vasyunina+, 2009)

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009ycat..34990149v&link_type=abstract

VizieR On-line Data Catalog: J/A+A/499/149. Originally published in: 2009A&A...499..149V

Physics

Molecular Clouds, Infrared Sources, Millimetric/Submm Sources

Scientific paper

The 1.2mm continuum observations were carried out with the 37-channel bolometer array SIMBA (Nyman et al., 2001Msngr.106...40N) at the SEST on La Silla, Chile between July 16-18, 2003. SIMBA is a hexagonal array in which the HPBW of a single element is about 24" and the separation between elements on the sky is 44". The observations were made using a fast mapping technique without a wobbling secondary (Weferling et al., 2002A&A...383.1088W).
Maps of Uranus were taken to check the flux calibration of the resulting data. To correct for the atmospheric opacity, skydips were performed every 2-3 hours. Despite the occurrence of some thin clouds, the observing conditions were good which is reflected in zenith opacity values of 0.16-0.18. The pointing was checked roughly every two hours and proved to be better than 6". The combination of typically three maps with sizes of 560"x900" resulted in a residual noise of about 22-28mJy/beam (rms) in the center of the mapped region. The 1.2mm data for the IRDC regions from SIMBA at the SEST telescope were reduced using the MOPSI package (developed by R. Zylka, IRAM). All maps were reduced by applying the atmospheric opacity corrections, fitting and subtracting a baseline, and removing the correlated sky noise. Thereby, we followed a three-stage approach as suggested in the SIMBA manual. After a first iteration using all data for the sky noise removal, the map regions showing source emission are neglected for sky noise removal in the second iteration. From this second interim map a source model is derived which is being included in the third iteration. The resulting maps were flux-calibrated using the conversion factor obtained from observations of Uranus. For our July 2003 observations, this factor was around 60mJy/beam per count.
(2 data files).

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