Table 3
Summary of the main observational parameters of the Galactic Plane surveys used to obtain emission spectra.
| Survey | Observatory | θmaj,min | δν [km s-1] | σ [K] | SD | θSD | Reference | |
|
|
||||||||
| VGPS | VLA | 1′ × 1′ | 1.56 | 2 | GBT | 9′ | Stil et al. (2006) | |
| CGPS | DRAO | 1′ × 1′cscδ | 1.32 | 3 | DRAO 26-m | 36′ | Taylor et al. (2003) | |
| SGPS | ATCA | 2′ × 2′ | 1.00 | 1.6 | Parkes | 15′ | McClure-Griffiths et al. (2005) | |
| Galactic Center | ATCA | 145″ × 145″ | 1.00 | 0.7 | Parkes | 15′ | McClure-Griffiths et al. (2012) | |
Notes. Column 1: survey name, Col. 2: name of the interferometer used, Col. 3: angular resolution of the interferometric data (FWHM), Col. 4: spectral resolution, Col. 5: typical RMS noise level per spectral channel, Col. 6: single-dish telescope used to add-in the short-spacings information, Col. 7: angular resolution of the single-dish instrument, and Col. 8: the survey reference paper. Note that for the Galactic Center survey, σRMS increases to about 2 K close to (l,b) = (0°,0°). No meaningful H i column density could be determined toward the strong far-infrared source DR 21 (OH). This was possible for the neighboring compact H ii region DR 21 (see text), however.
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