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B/cgps Log of CGPS exposures (Taylor+, 2003-)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
cgps.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=VI/128
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Beginning of ReadMe :VI/128 Log of CGPS exposures (Taylor+, 2003-)
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Log of the Canadian Galactic Plane Survey (CGPS) images
as provided by the CGPS consortium to the astronomical communitee.
Taylor A.R., Gibson S.J., Peracaula M., Martin P.G., Landecker T.L.,
Brunt C.M., Dewdney P.E., Dougherty S.M., Gray A.D., Higgs L.A.,
Kerton C.R., Knee L.B.G., Kothes R., Purton C.R., Uyaniker B.,
Wallace B.J., Willis A.G., Durand, D.
<Astron. J. 125, 3145 (2003)>
=2003AJ....125.3145T
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ADC_Keywords: Observatory log ; Radio sources
Description:
The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC),
in collaboration with an international Consortium of 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. For each mosaic
(1024x1024 pixels), atomic hydrogen observations are presented as a
data "cube" with 272 spectral channels having a velocity resolution of
1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced,
as well as selected Stokes Q, U and V images at 1420MHz. Complementary
images in the four IRAS infrared bands and data cubes of CO (J=1-0)
emission have also been created as part of the Survey. In addition to
the 5x5deg mosaics, a series of nine 15x15deg mosaics of 408MHz
emission, and possibly other lower radio frequencies, will be created.
Mosaics are archived as they are processed and released to the
Consortium. Archived data are in FITS format, except for the
occasional text file.
Imaging of the molecular phase of the ISM, traced by the CO molecule,
has 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
408MHz are being contributed by the Mullard Radio Astronomy
Observatory of the University of Cambridge and at the Beijing
Astronomical Observatory.
Summary of CGPS Data:
-------------------------------------------------------------------------
| Frequency | Wavelength | Observation | ISM Component | Source |
-------------------------------------------------------------------------
| 151 MHz | 190 cm | | | MRAO |
|-----------|------------| | |---------|
| 232 MHz | 130 cm | | Ionized Gas | |
|-----------|------------| | | BAO |
| 327 MHz | 92 cm | Continuum (I) | and | |
|-----------|------------| | |---------|
| 408 MHz | 74 cm | | Relativistic | |
|-----------|------------| | Plasma | |
| | | | | |
| | |------------------|-----------------| 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 um | | | |
|-----------|------------| | Dust Grains | Caltech |
| 5 THz | 60 um | | | |
|-----------|------------| Continuum (I) |-----------------|---------|
| 12 THz | 25 um | | Very Small | |
|-----------|------------| | Dust Grains | CITA |
| 25 THz | 12 um | | & PAHs | |
-------------------------------------------------------------------------
BAO = Beijing Astronomical Observatory
DRAO = Dominion Radio Astrophysical Observatory at Penticton
FCRAO = Five College Radio Astronomy Observatory
MRAO = Mullard Radio Astronomy Observatory (University of Cambridge)
CITA = Canadian Institute for Theoretical Astrophysics,
Mid-Infrared Galaxy Atlas (MIGA)