Table 1
SMGPS parameters compared to previous radio continuum surveys covering the Galactic plane in the frequency range 0.8–6.0 GHz.
| Survey | Instr. | l Coverage (deg) | b Coverage (deg) | Quadrant | Freq. (GHz) | Bandwidth (MHz) | FWHM (arcsec) | rms (µJy/beam) | LAS (arcmin) | Ref. |
|---|---|---|---|---|---|---|---|---|---|---|
| 2 < l < 60 | |b| < 1.5 | I | ||||||||
| SMGPS | MeerKAT | 252< l <358 | |b| < 1.5 | III, IV | 1.284 | 792 | 8 | 30 | 27 | 1 |
| 18 < l < 46 | |b| < 1.3 | |||||||||
| VGPS | VLA+GBT | 46 < l < 59 | |b| < 1.9 | I | 1.4 | 1.866 | 60 | –(a) | –(b) | 2 |
| 59 < l < 67 | |b| < 2.3 | |||||||||
| 0 < l < 49.5 | |b| < 1.0 | I | ||||||||
| MAGPIS (6 cm) | VLA | 350<l<360 | |b| < 0.4 | IV | 5.0 | 50 | 6 | 179 | – | 3 |
| VLA+Effelsberg | 5 < l < 48.5 | |b| < 0.8 | I | 1.4 | 95 | 6 | 897 | –(c) | 4 | |
| MAGPIS (21 cm) | −20< l < 120 | |b| < 0.8 | I, IV | |||||||
| VLA | −10< l <40 | |b| < 1.7 | I, IV | 1.4 | -(d) | 6 | 897 | – | 3 | |
| 100< l < 105 | |b| < 2.2° | I | ||||||||
| CORNISH | VLA | 10< l <65 | |b| < 1.1 | I | 5.0 | 25 | 1.5 | 400 | 2 | 5 |
| CORNISH-South | ATCA | 295 < l < 350 | |b| <1 | IV | 5.5 | 2000 | 2.5 | 110 | – | 6 |
| −2° < 1 < 60°, −1° < b < 1° | ||||||||||
| GLOSTAR | VLA+Effelsberg | 76° < 1 <83°, −1° < b < 2° | I | 5.8 | 18 | 150 | 4 | 7 | ||
| MGPS | MOST | 245 < l < 365 | |b| < 10 | III, IV | 0.843 | 3 | 45×45 csc|δ| | 1000 | 25 | 8 |
| SGPS | ATCA + Parkes | 253 < l < 358 | |b| < 1.5 | III, IV | 14 | 128 | 132 | <1000 | –(f) | 9 |
| 5< l <20 | |b| < 1.5 | I | 198 | |||||||
| CGPS | DRAO Synth. Tel. | 74.2 < l < 147.3 | −3.6 < b < 5.6 | I, II | 1.42 | 35 | 60×60 csc|δ| | 300 | 40 | 10 |
| 18.1×11.1 to | ||||||||||
| THOR | VLA | 14 < l < 67.4 | |b| < 1.25 | I | 1.42 | 128 | 12.0×11.6 | 300–1000 | 2 | 11 |
Notes. (a)Noise level ~0.3 K.(b)Without Green Bank Telescope data, the quoted LAS of VLA D-configuration is ~16 arcmin. (c)Without Effelsberg data, the quoted LAS of VLA D-configuration is ~16 arcmin. (d) Bandwidth variable across different observations, from 40 to 200 MHz. (e)Final mosaic obtained by integrating 8 sub-band images formed from two 1-GHz wide bands centred at 4.7 and 6.9 GHz. (f)Without Parkes data, the theoretical LAS of ATCA smallest baseline configuration is ~23 arcmin. References: (1) Goedhart et al. (2024); (2) Stil et al. (2006); (3) White et al. (2005); (4) Helfand et al. (2006); (5) Hoare et al. (2012); (6) Irabor et al. (2023); (7) Brunthaler et al. (2021); (8) Murphy et al. (2007); (9) McClure-Griffiths et al. (2005); (10) Taylor et al. (2003); (11) Beuther et al. (2016).
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