Table 1
Comparison of basic parameters of recent H i surveys of the Milky Way.
| LAB | GASS | GALFA∗ | EBHIS | ||
|
|
|||||
| δ | Full | ≤1° | − 1°...38° | ≥–5° | |
| ϑfwhm | 36′ |
|
|
|
|
| | vlsr | | ≤460† | ≤470 | ≤750 | ≤600 | km s-1 |
| Δv | 1.03 | 0.82 | 0.18 | 1.29 | km s-1 |
| δv | 1.25 | 1.00 | 0.18 | 1.44 | km s-1 |
| σ rms | 80 | 57 | 325 | 90 | mK |
|
89 | 57 | 140 | 108 | mK |
| Γmb | 0.132 | 0.649 | 10.52 | 1.434 | K Jy-1 |
|
|
|||||
|
3.9 | 2.5 | 6.1 | 4.7 | 1018 cm-2 |
|
16.1 | 2.1 | 0.3 | 1.8 | Jy km s-1 |
Notes. The table quotes the declination range, δ, angular resolution ϑfwhm, velocity interval, vlsr, channel separation, Δv, spectral resolution, δv, brightness temperature noise level, σrms, as well as the normalized noise level, , the data would have at a common spectral resolution of 1 km s-1. The main beam sensitivity, Γmb, is the conversion factor between brightness temperature and flux density, i.e., TB = ΓmbS. The two bottom rows quote theoretical 5σ detection limits (velocity-integrated intensity) of an object with a Gaussian profile of 20 km s-1 line width (FWHM).
Numbers given are for the shallowest mode. Effective integration time varies across the survey area. Fields observed in commensal mode with AGES (Minchin et al. 2007, 
) and ALFALFA (Giovanelli et al. 2005; Haynes et al. 2011, 
) are much deeper (J. Peek, priv. comm.).
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