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Canadian Galactic Plane Survey
The Canadian Galactic Plane Survey (CGPS) is a project aimed at improving
our understanding of the constituents and processes of the interstellar
medium (ISM) in our Galaxy. To this end, wide-field images of
unprecedented detail are being assembled at many wavelengths by a
consortium of astronomers from Canadian and international institutions.
These will allow us to study dust grains, molecular gas, atomic gas,
ionized gas, and relativistic plasmas, with spatial resolutions that are up
to a factor of 10 better than in previous surveys, made possible by
advances in technlogy and computing in recent years.
NRC-HIA's Dominion Radio Astrophysical Observatory (DRAO) is contributing data on the distribution and kinematics of atomic gas,
as well as the distribution of ionized gas and relativistic plasmas. These
observations are the centerpiece of the CGPS, and will cover Galactic
longitudes from l=74.2 to 147.3 degrees and latitudes from b=-3.5 to +5.5
degrees, resolving features as small as 1 arcminute. The DRAO data
products consist of a "data-cube" of the spatial distribution of atomic
hydrogen over 256 velocity channels, with a spatial resolution of 1
arcminute and a velocity resolution of 1.2 km/s, together with 1420MHz
continuum images of Stokes I, Q, U and V (i.e., full polarimetry) having 1
arcminute resolution, and 408 MHz continuum images of Stokes I at 3.5
arcminute resolution.
About 85% of the time available for observing at DRAO is being devoted
to this project (the remainder is assigned to external proposals
selected through a peer review process; proposal forms
are available electronically). A total of 190 CGPS fields are
being observed with the Synthesis
Telescope during the 5-year observing phase, which ends in March
2000, with the data being reduced on-site from raw form to final
images by a team of 6 people. Some data processing is also being
carried out at the University of Calgary, notably the registration of
source positions and flux densities relative to established scales,
and reduction of the 1420MHz Stokes Q, U, and V data.
Other data products being contributed to the CGPS by consortium members
include:
These are summarized in the table below:
Frequency | Wavelength |
Observation | ISM Component | Source |
151 MHz | 190 cm |
Continuum (I) |
Ionized Gas and Relativistic Plasma |
MRAO |
232 MHz | 130 cm |
BAO |
327 MHz | 92 cm |
408 MHz |
74 cm |
NRC-HIA |
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 Dust Grains & PAHs |
CITA |
25 THz | 12 µm |
Further information on the survey
CGPS page at the University
of Calgary.
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