The Dominion Radio Astrophysical Observatory, in collaboration with a consortium of university astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. Within this region the observations will yield an atomic hydrogen ``cube'' with 256 channels and velocity resolution 1.2 km/s, Stokes I, Q, U and V continuum polarization images at 1420 MHz, and a Stokes I continuum image at 408 MHz.
These observations form the centerpiece of the CGPS, an international collaboration to map all of the major interstellar components of the Milky Way at a common resolution: neutral atomic gas, molecular gas, ionized gas, dust grains, and relativistic plasma. For many of these constituents, angular resolution will be improved over previous studies by more than a factor of 10. The principal goal of the project is the creation and scientific analysis of a database of panoramic, high resolution images of all the major components of the ISM.
This effort is possible only now because of the convergence of new technical developments. A Pilot Survey Project was carried out prior to the full survey to evaluate mosaicing issues at DRAO. Imaging of the molecular phase of the ISM, traced by the CO molecule, has recently been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408 MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.
|151 MHz||190 cm||Continuum (I)||Ionized Gas
|232 MHz||130 cm||BAO|
|327 MHz||92 cm|
|408 MHz||74 cm||DRAO|
|1420 MHz||21 cm|
|Continuum (QUV)||Magnetic Fields|
|H Spectral Line||Atomic Gas|
|115 GHz||2.6 mm||CO Spectral Line||Molecular Gas||FCRAO|
|3 THz||100 µm||Continuum (I)||Dust Grains||Caltech|
|5 THz||60 µm|
|12 THz||25 µm||Very Small
|25 THz||12 µm|