Table D.1
Peak flux and map rms from the science target images processed with and without WVR scaling.
| UID | Separation | Peak flux | Image rms | S/N | Peak flux | Image rms | S/N | Improvement | |
| to BP cal. | standard | standard | scaled | scaled | ratio | ||||
| (°) | (mJy/bm) | (μJy/bm) | (mJy/bm) | (μJy/bm) | |||||
|
|
|||||||||
| Juno − Band 6 | |||||||||
|
|
|||||||||
| Xbc7 − a | 8.6 | 7.045 | 84.92 | 83.0 | 7.049 | 84.64 | 83.3 | 1.004 | |
| Xbc7 − b | 8.6 | 6.945 | 81.60 | 85.1 | 6.962 | 81.54 | 85.4 | 1.003 | |
| Xdae − a | 8.6 | 6.512 | 87.96 | 74.0 | 6.516 | 87.99 | 74.0 | 1.000 | |
| Xdae − b | 8.6 | 6.865 | 88.95 | 77.2 | 6.852 | 88.90 | 77.1 | 0.998 | |
| X1363 − a ∗ | 8.6 | 3.434 | 182.18 | 18.8 | 3.470 | 182.24 | 19.0 | 1.010 | |
| X1363 − b ∗ | 8.6 | 3.251 | 156.62 | 20.8 | 3.189 | 157.71 | 20.2 | 0.974 | |
|
|
|||||||||
| Mira − Band 6 | |||||||||
|
|
|||||||||
| X423 | 7.6 | 44.30 | 395.5 | 112.0 | 48.94 | 290.1 | 168.7 | 1.506 | |
|
|
|||||||||
| X137 | 20.2 | 65.13 | 163.1 | 399.2 | 65.23 | 143.9 | 453.1 | 1.135 | |
|
|
|||||||||
| HL Tau − Band 3 | |||||||||
|
|
|||||||||
| Xc7f | 9.1 | 2.887 | 26.72 | 108.0 | 2.843 | 26.76 | 106.2 | 0.983 | |
|
|
|||||||||
| HL Tau − Band 6 | |||||||||
|
|
|||||||||
| Xb2 | 9.1 | 7.485 | 51.05 | 146.6 | 7.693 | 49.73 | 154.7 | 1.055 | |
|
|
|||||||||
| Xc8c | 9.1 | 5.171 | 46.39 | 111.4 | 5.307 | 46.28 | 114.6 | 1.028 | |
|
|
|||||||||
| Xdc | 19.7 | 8.250 | 61.60 | 133.9 | 8.259 | 62.78 | 131.5 | 0.982 | |
|
|
|||||||||
| X760 | 27.0 | 5.519 | 38.16 | 144.6 | 5.877 | 38.07 | 154.3 | 1.067 | |
| X9dd | 19.7 | 5.661 | 37.11 | 152.5 | 5.933 | 36.16 | 164.0 | 1.076 | |
| Xc3c | 9.1 | 6.261 | 35.72 | 175.2 | 6.366 | 35.92 | 177.1 | 1.011 | |
|
|
|||||||||
| X387 | 9.1 | 6.738 | 38.34 | 175.7 | 6.789 | 38.32 | 177.1 | 1.008 | |
|
|
|||||||||
| HL Tau − Band 7 | |||||||||
|
|
|||||||||
| X20a | 19.7 | 8.203 | 80.65 | 101.7 | 8.399 | 81.00 | 103.7 | 1.018 | |
| X6d8 | 19.7 | 8.057 | 83.93 | 96.0 | 8.250 | 83.85 | 98.4 | 1.024 | |
| Xa16 | 9.1 | 8.469 | 82.30 | 102.9 | 8.682 | 83.23 | 104.3 | 1.013 | |
|
|
|||||||||
| X585 | 19.7 | 8.369 | 82.44 | 101.5 | 8.516 | 82.42 | 103.3 | 1.017 | |
| X826 | 9.1 | 8.083 | 80.82 | 100.0 | 8.245 | 80.65 | 102.2 | 1.022 | |
|
|
|||||||||
| X5ab | 19.7 | 7.062 | 91.87 | 76.9 | 7.294 | 91.83 | 79.4 | 1.033 | |
|
|
|||||||||
| X446 | 9.1 | 8.548 | 91.83 | 93.1 | 8.622 | 92.08 | 93.6 | 1.005 | |
|
|
|||||||||
| SDP.81 − Band 6 | |||||||||
|
|
|||||||||
| X1716 | 9.7 | 0.199 | 28.52 | 7.0 | 0.210 | 28.58 | 7.3 | 1.050 | |
|
|
|||||||||
| X65f | 9.7 | 0.295 | 31.07 | 9.5 | 0.293 | 31.09 | 9.4 | 0.998 | |
|
|
|||||||||
| X1f23 | 1.7 | 0.386 | 60.54 | 6.4 | 0.389 | 60.41 | 6.5 | 1.009 | |
|
|
|||||||||
| SDP.81 − Band 7 | |||||||||
|
|
|||||||||
| Xb6 | 9.7 | 0.261 | 35.81 | 7.3 | 0.262 | 35.83 | 7.3 | 1.005 | |
| X517 | 1.7 | 0.293 | 45.85 | 6.4 | 0.321 | 45.47 | 7.1 | 1.104 | |
|
|
|||||||||
| X5e6 | 9.7 | 0.248 | 32.23 | 7.7 | 0.244 | 32.21 | 7.6 | 0.984 | |
|
|
|||||||||
| X1059 | 9.7 | 0.271 | 37.37 | 7.3 | 0.271 | 37.38 | 7.3 | 1.000 | |
| X1336 | 9.7 | 0.271 | 38.04 | 7.1 | 0.275 | 38.05 | 7.2 | 1.011 | |
| X1562 | 9.7 | 0.323 | 37.97 | 8.5 | 0.324 | 37.92 | 8.6 | 1.003 | |
|
|
|||||||||
| Xa99 | 16.1 | 0.270 | 48.23 | 5.6 | 0.275 | 48.21 | 5.7 | 1.016 | |
| Xcc5 | 16.1 | 0.281 | 46.06 | 6.1 | 0.274 | 46.01 | 6.0 | 0.983 | |
Notes. Separation column indicates the angular separation between the bandpass target and the source using the casa analysis utilities “aU.angularSeparationOfFields”. The improvement ratio is with respect to the change in S/N. For Juno there are two science target images made, (a) and (b), per EB to account for the rotation of the asteroid. Although both (a) and (b) images are presented separately the average from each EB is used in the main analysis. The (∗) indicates that this Juno EB the calibration is worse with or without WVR scaling. The EBs suffix X12c and Xa47 (SDP.81 B4) have very weak emission such that blends with the noise and image parameters cannot be reported. The noise is measured within the same area for both images with and without WVR scaling applied. The horizontal lines separate the different SBs as noted in Table A.1.
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