Table A.1
Effect of the different noise types.
| σ α | σ T | σ φ | WVR | S [Jy] | F 0.3 | F 1 | F 3 | F 10 |
|
|
||||||||
| No | No | No | No | 0.1090 | 107 | 208 | 279 | 418 |
| ALMA | No | No | No | 0.1089 | 119 | 200 | 245 | 309 |
| Both | No | No | No | 0.1088 | 114 | 202 | 241 | 312 |
| Both | ALMA | No | No | 0.1046 | 45 | 75 | 114 | 143 |
| Both | Both | No | No | 0.1035 | 44 | 75 | 112 | 141 |
| Both | Both | 30° | No | 0.0908 | 4 | 5 | 5 | 5 |
| Both | Both | 30° | Yes | 0.0987 | 13 | 15 | 16 | 16 |
| Both | Both | 45° | No | 0.0736 | 2 | 3 | 3 | 3 |
| Both | Both | 45° | Yes | 0.0947 | 7 | 7 | 8 | 8 |
Notes. The error-free simulation is that of a combined B = 4 observation of the face-on MU200 model with ALMA in configuration C = 20 and with a single-dish. Pointing errors (σα) and thermal noise (σT) may be applied to neither instrument (“No”), to the interferometer only (“ALMA”), or to both interferometer and single-dish (“Both”). Phase noise is specified via the rms atmospheric phase on a 300-m baseline, which can take the values 30° or 45° and can be corrected via water-vapor radiometers (“WVR”).
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