Table 1
Summary of the WASP-43b observations with the GROND instrument.
| Date | Start/end time | Type | Airmass | Moon | Filter | N obs | t exp | Aperture | N ref | β | σ 120 s | |
| (UT) | (UT) | illum. (d) | (s) | (′′) | β χ | β r | (ppm) | |||||
| 2012-01-08 | 05:24 → 08:21 | Tran. | 1.29 → 1.06 → 1.07 | 99% (65°) | g ′ | 81 | 90 | 3.6, 4.9, 6.0 | 1 | 1.26 | 1.21 | 678 |
| r ′ | 81 | 90 | 5.5, 8.4, 9.0 | 1 | 1.40 | 1.00 | 504 | |||||
| i ′ | 81 | 90 | 6.2, 9.0, 9.6 | 1 | 1.23 | 1.00 | 645 | |||||
| z ′ | 81 | 90 | 4.7, 7.6, 8.4 | 1 | 1.57 | 1.00 | 798 | |||||
| J | 244 | 3 × 8 | 6.3, 11.1, 15.6 | 3 | 0.59 | 1.97 | 1241 | |||||
| H | 244 | 3 × 8 | 6.3, 11.7, 15.6 | 1 | 1.01 | 2.83 | 1269 | |||||
| K | 244 | 3 × 8 | 5.1, 9.9, 14.4 | 2 | 0.64 | 1.50 | 1269 | |||||
| 2012-03-03 | 02:52 → 05:59 | Occ. | 1.12 → 1.06 → 1.18 | 69% (63°) | g ′ | 98 | 90 | 5.4, 7.3, 8.1 | 2 | 1.57 | 1.00 | 673 |
| r ′ | 98 | 90 | 6.5, 9.0, 9.6 | 1 | 2.31 | 1.52 | 475 | |||||
| i ′ | 98 | 90 | 5.5, 7.7, 8.5 | 2 | 2.58 | 1.00 | 604 | |||||
| z ′ | 98 | 90 | 5.5, 7.7, 8.5 | 1 | 2.50 | 1.49 | 575 | |||||
| J | 389 | 4.5 × 4 | 8.4, 11.4, 15.6 | 3 | 1.30 | 2.53 | 953 | |||||
| H | 389 | 4.5 × 4 | 6.9, 11.1, 15.6 | 3 | 0.95 | 3.38 | 885 | |||||
| K | 389 | 4.5 × 4 | 6.0, 9.6, 14.4 | 2 | 0.47 | 1.09 | 1425 | |||||
Notes. Type “Tran.”/“Occ.” corresponds to transit/occultation, respectively. “Moon illum.” is the fraction of the Moon that is illuminated, while the d in parenthesis is the minimum distance to the Moon. Nobs is the number of retrieved images, while Nref is the number of reference stars to create a composite reference light curve. texp refers to integration time for g′r′i′z′, and detector integration time (DIT) times the number of DIT (NDIT) for JHK. Aperture sizes refer to the optimal aperture, inner/outer annuli radii adopted in the photometry. βχ and βr are the χν-rescaling and red noise rescaling factors as described in Sect. 3.1. σ120 s refers to the standard deviation of light-curve O–C residuals binned every 2 min. The last three columns are calculated from the global joint analysis with wavelength-dependent radius (or flux ratios), i.e. Method 3 as described in Sect. 3.2.
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