J. English , A.R. Taylor , J.A. Irwin , S.M. Dougherty , S. Basu , C. Beichman , J. Brown , Y. Cao , C. Carignan , D. Crabtree , P. Dewdney , N. Duric , M. Fich , E. Gagnon , J. Galt , S. Germain , N. Ghazzali , S. J. Gibson , S. Godbout , A. Gray , D.A. Green , C. Heiles , M. Heyer , L. Higgs , S. Jean , D. Johnstone , G. Joncas , T. Landecker , W. Langer , D. Leahy , P. Martin , H. Matthews , W. McCutcheon , G. Moriarity-Scheiven , S. Pineault , C. Purton , R. Roger , D. Routledge , N. St-Louis , K. Tapping , S. Terebey , F. Vaneldik , D. Watson , T. Willis , H. Wendker , X. Zhang, PASA, 15 (1), 56
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Contributions to the project by the Consortium and DRAO
The international collaborative effort of 46 scientists at 20 institutions will make possible a publicly-available database of high resolution, high-dynamic range images of the Galaxy. Table 1 lists each observational contribution and indicates the relevance to multi-phase studies of the interstellar medium (ISM).
408 & 1420 MHz (74 & 21 cm)
Frequency (Wavelength) Telescope Comments 151 MHz (190 cm) MRAO CLFST The Mullard Radio Astronomical Observatory's Cambridge Low-Frequency Synthesis Telescope 232 & 327 MHz (130 & 92 cm) BAO Beijing Astronomical Observatory DRAO ST Dominion Radio Astrophysical Observatory Synthesis Telescope (with zero spacings from previous surveys for the continuum data and the DRAO 26 metre dish for the H I line data) 115 GHz (2.6 mm) FCRAO University of Massachusetts' Five Colleges Radio Astronomy Observatory 3 & 5 THz (100 & 60 m) IRAS Infrared Astronomical Satellite
One of the factors which brought about the leading role of the Canadian scientists in this project was the upgrade of the Dominion Radio Astrophysical Observatory's Synthesis Telescope (DRAO ST) to seven 9-metre antennas. One of the strategies which distinguishes the DRAO observations from those of other interferometers is that the U-V plane is fully sampled. This allows an unambiguous transformation to the plane of the sky. As well, single dish (zero-spacing) data, which contains emission on large angular scales, will be incorporated in order to ensure complete flux density measurements can be made for all modes of DRAO ST observations.
The DRAO ST project is surveying the region , which runs along the Perseus arm in one direction and the Cygnus arm in the other, with an angular resolution of at 1420 MHz. The survey has a width in latitude, about the Galaxy mid-plane, of 9 at 1420 MHz and 15 at 408 MHz.
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