Table C.1.
Comparison of the properties of the protoplanets inferred from the NIRCam F187N and F480M observations using NEGFC combined with either roll subtraction or IPCA, and the predictions made in either Wang et al. (2021b) for b and c and M19 for candidate d.
| Parameter | Roll subtraction | IPCA | Final | Prediction(a) |
|---|---|---|---|---|
| F187N | ||||
| PDS 70 b | ||||
| Separation(b) | 164.5 ± 12.0 | 151.9 ± 12.1 | 158.2 ± 12.1 | 155.5 ± 1.4 |
| PA(c) | 129.0 ± 4.1 | 129.4 ± 2.6 | 129.2 ± 4.1 | 132.6 ± 0.3 |
| Contrast(d) | (3.28 ± 0.78)×10−4 | (2.50 ± 0.56)×10−4 | (2.89 ± 0.78)×10−4 | (2.4 ± 0.1)×10−4 |
| Flux(e) | (8.69 ± 2.07)×10−17 | (6.62 ± 1.48)×10−17 | (7.65 ± 2.07)×10−17 | (6.3 ± 0.3)×10−17 |
| PDS 70 c | ||||
| Separation(b) | – | 203.3 ± 23.3 | 203.3 ± 23.3 | 210.1 ± 1.0 |
| PA(c) | – | 269.7 ± 6.8 | 269.7 ± 6.8 | 270.1 ± 0.3 |
| Contrast(d) | – | (1.37 ± 0.42)×10−4 | (1.37 ± 0.42)×10−4 | (4.5 ± 0.4)×10−5 |
| Flux(e) | – | (3.63 ± 1.11)×10−17 | (3.63 ± 1.11)×10−17 | (1.2 ± 0.1)×10−17 |
| PDS 70 d? | ||||
| Separation(b) | – | 110.2 ± 23.3 | 110.2 ± 23.3 | 90.4 ± 5.9 |
| PA(c) | – | 294.6 ± 11.4 | 294.6 ± 11.4 | 284.6 ± 1.3 |
| Contrast(d) | – | (1.63 ± 0.69)×10−4 | (1.63 ± 0.69)×10−4 | (1.2 ± 0.2)×10−4 |
| Flux(e) | – | (4.31 ± 1.83)×10−17 | (4.31 ± 1.83)×10−17 | (3.2 ± 0.5)×10−17 |
| F480M | ||||
| PDS 70 b | ||||
| Separation(b) | 145.6 ± 20.4 | 141.6 ± 10.9 | 143.6 ± 20.4 | 155.5 ± 1.4 |
| PA(c) | 130.4 ± 6.7 | 127.1 ± 6.7 | 128.7 ± 6.7 | 132.6 ± 0.3 |
| Contrast(d) | (3.93 ± 1.50)×10−3 | (2.96 ± 1.02)×10−3 | (3.44 ± 1.50)×10−3 | (2.8 ± 0.6)×10−3 |
| Flux(e) | (8.13 ± 3.11)×10−17 | (6.12 ± 1.08)×10−17 | (7.11 ± 3.11)×10−17 | (5.8 ± 1.1)×10−17 |
| PDS 70 c | ||||
| Separation(b) | 216.7 ± 20.6 | 219.2 ± 12.7 | 217.9 ± 20.6 | 210.1 ± 1.0 |
| PA(b) | 272.8 ± 3.6 | 276.8 ± 3.7 | 274.8 ± 3.7 | 270.1 ± 0.3 |
| Contrast(c) | (1.55 ± 0.30)×10−3 | (1.39 ± 0.15)×10−3 | (1.47 ± 0.30)×10−3 | (1.0 ± 0.3)×10−3 |
| Flux(e) | (3.21 ± 0.62)×10−17 | (2.87 ± 0.62)×10−17 | (3.04 ± 0.62)×10−17 | (2.1 ± 0.6)×10−17 |
Notes: (a)Astrometric and contrast or flux predictions based on orbital fits and best-fit atmospheric models presented in Wang et al. (2021b) and M19. The contrast value reported for d in M19 is corrected for the expected change in total intensity-scattering efficiency based on the difference in PA with respect to the 2019 epoch. (b)Radial separation in mas. (c)Position angle measured east of north in °. (d)Contrast ratio with respect to the star and unresolved inner disk. (e)Spectral flux density in Wm−2μm−1.
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