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VI/128          Log of CGPS exposures           (Taylor+, 2003-)

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
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 5x5° mosaics, a series of nine 15x15° 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) File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file cgps.dat 81 1925 The Canadian Galactic Plane Survey (2005-Oct)
See also: : CGPS Archive home page Byte-by-byte Description of file: cgps.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [CGPS] Survey name 7- 12 A6 --- --- [MOSAIC] Entry type 14- 17 A4 --- Area Mosaic area name (2) 19- 29 A11 --- Band Bandpass name (1) 32 A1 --- Pol [IQUV] Stokes polarisation vector name 35- 40 A6 --- Mode Image mode (right now, only IMAGE is useful) (3) 42- 47 F6.2 deg GLON Galactic coordinate L of mosaic centre 49- 54 F6.2 deg GLAT Galactic coordinate B of mosaic centre 56- 81 A26 --- file Filename within the CGPS archive
Note (1): the bandpasses are noted as follows: 012um = infra-red, 12µm 025um = infra-red, 25µm 060um = infra-red, 60µm 100um = infra-red, 100µm CO(115GHz) = CO spectral line 1420MHz = Continuum near 21cm HI(1420MHz) = HI spectral line 21cm 408MHz = Continuum See also the "Summary of CGPS Data" section above. Note (2): names and position of the mosaics: ---------------------------------- MV1 142.2<l<147.3, -3.5<b<+1.5 MV2 142.2<l<147.3, +0.5<b<+5.5 MW1 138.2<l<143.3, -3.5<b<+1.5 MW2 138.2<l<143.3, +0.5<b<+5.5 MX1 134.2<l<139.3, -3.5<b<+1.5 MX2 134.2<l<139.3, +0.5<b<+5.5 MY1 130.2<l<135.3, -3.5<b<+1.5 MY2 130.2<l<135.3, +0.5<b<+5.5 MA1 126.2<l<131.3, -3.5<b<+1.5 MA2 126.2<l<131.3, +0.5<b<+5.5 MB1 122.2<l<127.3, -3.5<b<+1.5 MB2 122.2<l<127.3, +0.5<b<+5.5 MC1 118.2<l<123.3, -3.5<b<+1.5 MC2 118.2<l<123.3, +0.5<b<+5.5 MD1 114.2<l<119.3, -3.5<b<+1.5 MD2 114.2<l<119.3, +0.5<b<+5.5 ME1 110.2<l<115.3, -3.5<b<+1.5 ME2 110.2<l<115.3, +0.5<b<+5.5 MF1 106.2<l<111.3, -3.5<b<+1.5 MF2 106.2<l<111.3, +0.5<b<+5.5 MG1 102.2<l<107.3, -3.5<b<+1.5 MG2 102.2<l<107.3, +0.5<b<+5.5 MH1 098.2<l<103.3, -3.5<b<+1.5 MH2 098.2<l<103.3, +0.5<b<+5.5 MIJ1 094.2<l<099.3, -3.5<b<+1.5 MIJ2 094.2<l<099.3, +0.5<b<+5.5 MK1 090.2<l<095.3, -3.5<b<+1.5 MK2 090.2<l<095.3, +0.5<b<+5.5 ML1 086.2<l<091.3, -3.5<b<+1.5 ML2 086.2<l<091.3, +0.5<b<+5.5 MM1 082.2<l<087.3, -3.5<b<+1.5 MM2 082.2<l<087.3, +0.5<b<+5.5 MN1 078.2<l<083.3, -3.5<b<+1.5 MN2 078.2<l<083.3, +0.5<b<+5.5 MO1 074.2<l<079.3, -3.5<b<+1.5 MO2 074.2<l<079.3, +0.5<b<+5.5 ---------------------------------- Note (3): Type of images part of a given Mosaic takes the following values: BEAMS = file containing a grid of selected beam maps illustrating the variation in beam shape across the image. CFV = file showing the correction factor variance (IR only). High values of this quantity can indicate poor noisy data, saturated regions, or unresolved sources. FLAGS = image where non-zero values indicate pixels with caveats (CO data only) IMAGE = file containing the image data. PHN = file giving a measure of the relative noise across an image (IR data only) RESCB = file containing five planes of information illustrating the variation in beam profile across the image. WGHT = file containing a weight map which gives a measure of the relative noise across an image.
Acknowledgement Requirement: Users are requested to include the following acknowledgement in publications making use of CGPS data: "The Canadian Galactic Plane Survey (CGPS) is a Canadian project with international partners. The Dominion Radio Astrophysical Observatory is operated as a national facility by the National Research Council of Canada. The CGPS is supported by a grant from the Natural Sciences and Engineering Research Council of Canada." If you have used CADC facilities for your research, you should refer to the data as obtained "from the CADC" and include the following acknowledgment in any publication: "Guest User, Canadian Astronomy Data Centre, which is operated by the Herzberg Institute of Astrophysics, National Research Council of Canada." History: History: * 05-Jun-2003: Provided by the Canadian Astronomical Data Center (CADC) in its first version (saved as Catalog B/cgps) * 05-Jun-2005: "B/cgps" version 1605 observations * 02-Oct-2005: "B/cgps" version 1925 observations * 13-Dec-2009: Catalog moved to "VI" category (VI/128)
(End) Francois Ochsenbein [CDS] 02-Oct-2005
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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