CONDOR observations of high mass star formation in Orion
-
Published:2006-08
Issue:S237
Volume:2
Page:492-492
-
ISSN:1743-9213
-
Container-title:Proceedings of the International Astronomical Union
-
language:en
-
Short-container-title:Proc. IAU
Author:
Volgenau N. H.,Wiedner M. C.,Wieching G.,Emprechtinger M.,Bielau F.,Graf U. U.,Honingh C. E.,Jacobs K.,Vowinkel B.,Güsten R.,Rabanus D.,Stutzki J.,Wyrowski F.
Abstract
CONDOR, the CO, N+, Deuterium Observations Receiver, is designed to make velocity-resolved observations of the CO, [NII], and p-H2D+ lines in the 1.4 THz (200-240μm) atmospheric windows. CONDOR's first light observations were made with the APEX telescope in November 2005. The CONDOR beam on APEX (at ν = 1.5 THz) was expected to consist of a 4.3″ main beam and a 73″ error beam; this beam structure was verified from scans of Mars. The pointing accuracy, also determined from Mars scans, was better than 7″. The average atmospheric transmission during our Orion observations (elev~57°) was 19 ± 4% along the line-of-sight. A forward efficiency of Feff = 0.8 was determined from sky dips, and observations of the Moon and Mars were used to couple the CONDOR beam to sources of different sizes (ηc = 0.40 and ~0.10, respectively). For more information, see Wiedner et al. 2006.
Publisher
Cambridge University Press (CUP)
Subject
Astronomy and Astrophysics,Space and Planetary Science