If you have used CADC facilities for your research, please include the following acknowledgment:
This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency.
The CGPS survey
The Dominion Radio Astrophysical Observatory, in collaboration with an international Consortium of astronomers, has carried out a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. The observations of 373 fields with the DRAO Synthesis Telescope are presented in sixty-eight 5 deg x 5 deg mosaics, covering Galactic longitudes from L = 63 to 175 degrees and latitudes from B = -3.5 to +5.5 degrees and a latitude extension to B = +17.5 degrees between L = 100 to 116.5 degrees, with a resolution as small as 1 arcminute. For each mosaic (1024 x 1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3 km/s. Stokes I continuum images at 1420 MHz and 408 MHz are produced, as well as selected Stokes Q, U and V images at 1420 MHz. 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 5 deg x 5 deg mosaics, a series of nine 15 deg x 15 deg mosaics of 408-MHz 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.
These observations comprise the Canadian Galactic Plane Survey (CGPS), the product of an international Consortium, which maps all the major interstellar components of the Milky Way at 1 - 3 arcmin resolution: neutral atomic gas, molecular gas, ionized gas, dust grains and relativistic plasma. For many of these constituents, angular resolution is improved over previous studies by more than a factor of ten. 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.
The locations of the mosaics can be determined from the menu to the left. Note that not all mosaics have been archived to date.
In order to start browsing through the CGPS archive, select "Search for CGPS data" in the Queries menu above.
The VGPS survey
The 21-cm line emission from neutral atomic hydrogen (HI) in the Milky Way disk is being mapped with 1' resolution and brightness sensitivity of a few K rms by three groups using telescopes at the ATNF (the Southern Galactic Plane Survey, SGPS, McClure-Griffiths et al. 2001), the DRAO (the Canadian Galactic Plane Survey, CGPS, Taylor et al. 1999), and the VLA (Stil, J. M., Taylor, A. R., Dickey, J. M., Kavars, D. W., Martin, P. G., Rothwell, T. A., Boothroyd, A. I., Lockman, Felix J., & McClure-Griffiths, N. M. 2006, AJ 132, 1158). These projects are charting the disk between longitudes 255° and 357°, between 50° and 147° and between 18° and 50° respectively. Working together as an international community, we are now in a position to obtain a complete image of the HI emission from the plane of the Galaxy at 1' resolution. The longitude range 18° and 67° can only be explored with the VLA, because at these longitudes the Galactic plane passes through the celestial equator. The VLA survey will provide a link between the northern and southern surveys and cover the first quadrant of the Galaxy, where the effects of star formation and the interaction between the disk and halo are expected to be dominant shapers of the ISM (e.g. Heiles 1984). The VGPS will also overlap the FCRAO survey of CO emission in the molecular ring from 18° to 52°, providing, together with high resolution infrared images, complete imaging of the major components of the interstellar medium in this region down to scales of a few pc.
The VLA survey, in combination with the CGPS and SGPS, will provide a 3D image of this detail and quality for over 90% of the stellar disk of the Galaxy. The global image of the Galaxy will be a unique resource for the astronomical community. The observing parameters for the VLA Galactic Plane Survey are summarized in Table 1. The VGPS sky coverage is shown in the following figure.
If you are using the VGPS for your research, please cite the following VGPS paper: Stil, J. M., Taylor, A. R., Dickey, J. M., Kavars, D. W., Martin, P. G., Rothwell, T. A., Boothroyd, A. I., Lockman, Felix J., & McClure-Griffiths, N. M. 2006, AJ 132, 1158
The documentation for the VGPS survey is available here.