Table B.1
Contamination of the light curves in the HST-WFC3 bandpasses
| Wavelength µm | Bandwidth µm | Dilution(b) (E20) | Dilution(b) (this work) | Contamination(a) (this work) | Correction(c) factor | Corrected Eclipse depth(d) ppm |
|---|---|---|---|---|---|---|
| µm | µm | ppm | ||||
| 1.12625 | 0.0219 | 1.080007 | 1.058201 | 0.055 ± 0.003 | 0.979809 | 595 ± 38 |
| 1.14775 | 0.0211 | 1.081612 | 1.059322 | 0.056 ± 0.003 | 0.979392 | 696 ± 39 |
| 1.16860 | 0.0206 | 1.083408 | 1.061571 | 0.058 ± 0.004 | 0.979844 | 721 ± 42 |
| 1.18880 | 0.0198 | 1.084441 | 1.061571 | 0.058 ± 0.003 | 0.978911 | 584 ± 47 |
| 1.20835 | 0.0193 | 1.085204 | 1.063830 | 0.060 ± 0.004 | 0.980304 | 757 ± 52 |
| 1.22750 | 0.0190 | 1.086487 | 1.064963 | 0.061 ± 0.003 | 0.980189 | 533 ± 40 |
| 1.24645 | 0.0189 | 1.087721 | 1.066098 | 0.062 ± 0.004 | 0.980121 | 620 ± 49 |
| 1.26550 | 0.0192 | 1.089421 | 1.067236 | 0.063 ± 0.003 | 0.979636 | 678 ± 41 |
| 1.28475 | 0.0193 | 1.091716 | 1.069519 | 0.065 ± 0.003 | 0.979668 | 727 ± 46 |
| 1.30380 | 0.0188 | 1.091428 | 1.069519 | 0.065 ± 0.004 | 0.979926 | 755 ± 52 |
| 1.32260 | 0.0188 | 1.092315 | 1.070664 | 0.066 ± 0.003 | 0.980179 | 819 ± 51 |
| 1.34145 | 0.0189 | 1.093736 | 1.071811 | 0.067 ± 0.003 | 0.979954 | 853 ± 49 |
| 1.36050 | 0.0192 | 1.095211 | 1.074114 | 0.069 ± 0.004 | 0.980737 | 957 ± 51 |
| 1.38005 | 0.0199 | 1.096720 | 1.075269 | 0.070 ± 0.003 | 0.980441 | 885 ± 43 |
| 1.40000 | 0.0200 | 1.097740 | 1.076426 | 0.071 ± 0.003 | 0.980584 | 865 ± 47 |
| 1.42015 | 0.0203 | 1.097564 | 1.076426 | 0.071 ± 0.004 | 0.980741 | 937 ± 50 |
| 1.44060 | 0.0206 | 1.099283 | 1.079914 | 0.074 ± 0.004 | 0.982380 | 971 ± 47 |
| 1.46150 | 0.0212 | 1.100529 | 1.081081 | 0.075 ± 0.004 | 0.982329 | 1119 ± 44 |
| 1.48310 | 0.0220 | 1.102016 | 1.082251 | 0.076 ± 0.003 | 0.982065 | 1139 ± 43 |
| 1.50530 | 0.0224 | 1.103614 | 1.083424 | 0.077 ± 0.004 | 0.981705 | 1016 ± 50 |
| 1.52800 | 0.0230 | 1.107372 | 1.088139 | 0.081 ± 0.004 | 0.982632 | 1048 ± 44 |
| 1.55155 | 0.0241 | 1.109843 | 1.090513 | 0.083 ± 0.003 | 0.982583 | 1020 ± 47 |
| 1.57625 | 0.0253 | 1.110741 | 1.091703 | 0.084 ± 0.003 | 0.982860 | 1118 ± 52 |
| 1.60210 | 0.0264 | 1.113385 | 1.096491 | 0.088 ± 0.004 | 0.984827 | 1051 ± 55 |
| 1.62945 | 0.0283 | 1.114973 | 1.097695 | 0.089 ± 0.004 | 0.984504 | 1015 ± 53 |
Notes. (a)The contamination factor is defined as the ratio of the flux due to the contamination sources (in this case WASP-76 B) over the flux due to both the target star and the contamination sources collected in the photometric aperture. (b)The dilution factor (actually called correction factor in Edwards et al. (2020)) is defined as 1/(1 − C) where C is the contamination factor. The depth corrected from the effect of contamination is obtained by multiplying the depth measured on the contaminated light curve by the dilution factor. (c)What we call correction factor here is the factor that we applied to the eclipse depth reported by Edwards et al. (2020) to obtain the new eclipse depth assuming our estimate of the light curve contamination (see Section 3). It is equal to the ratio of our estimate of the dilution factor over the one estimated by Edwards et al. (2020). We warn the reader that Edwards et al. (2020) calls correction factor what we call dilution factor. (d)The corrected eclipse depths are the eclipse depths reported by Edwards et al. (2020) multiplied by the correction factor to adjust them to our estimate of the contamination of the light curves.
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