Table 3
Photometry and error budget.
| Target | Filter | MCMC contrast (a) | Bias offset (a) | Calib. error (b) | ND filter error | Final contrast (c) | Star magnitude | Apparent magnitude | Absolute magnitude | Flux |
|---|---|---|---|---|---|---|---|---|---|---|
| (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (W m−2 μm−1) | ||
| β Pic b | NB3.74 | 8.13 ± 0.11 | − 0.33 ± 0.24 | - | - | 7.80 ± 0.26 | 3.45 ± 0.01(d) | 11.25 ± 0.26 | 9.77 ± 0.26 | 1.70 ± 0.42 ×10−15 |
| β Pic b | NB4.05 | 7.54 ± 0.02 | − 0.01 ± 0.04 | - | - | 7.53 ± 0.04 | 3.45 ± 0.01(d) | 10.98 ± 0.04 | 9.50 ± 0.05 | 1.61 ± 0.07 ×10−15 |
| HIP 65426 b | L′ | 8.56 ± 0.06 | 0.01 ± 0.08 | 0.07 | - | 8.56 ± 0.12 | 6.76 ± 0.04(e) | 15.32 ± 0.13 | 10.13 ± 0.13 | 3.90 ± 0.46 ×10−17 |
| HIP 65426 b | NB4.05 | 8.39 ± 0.15 | 0.07 ± 0.21 | 0.03 | - | 8.46 ± 0.26 | 6.77 ± 0.04(f) | 15.23 ± 0.26 | 10.04 ± 0.26 | 3.22 ± 0.78 ×10−17 |
| HIP 65426 b | M′ | 7.83 ± 0.16 | 0.06 ± 0.24 | - | - | 7.89 ± 0.29 | 6.76 ± 0.04(g) | 14.65 ± 0.29 | 9.46 ± 0.29 | 2.99 ± 0.82 ×10−17 |
| PZ Tel B | L′ | 4.94 ± 0.13 | − 0.16 ± 0.12 | 0.11 | 0.03 | 4.78 ± 0.21 | 6.26 ± 0.05(e) | 11.04 ± 0.22 | 7.68 ± 0.22 | 2.01 ± 0.41 ×10−15 |
| PZ Tel B | NB4.05 | 4.69 ± 0.01 | − 0.00 ± 0.02 | 0.04 | - | 4.69 ± 0.05 | 6.25 ± 0.05(f) | 10.94 ± 0.07 | 7.57 ± 0.07 | 1.67 ± 0.11 ×10−15 |
| PZ Tel B | M′ | 4.63 ± 0.01 | − 0.00 ± 0.02 | - | - | 4.63 ± 0.03 | 6.30 ± 0.02(g) | 10.93 ± 0.03 | 7.56 ± 0.03 | 9.18 ± 0.28 ×10−16 |
| HD 206893 B | L′ | 8.28 ± 0.12 | − 0.02 ± 0.28 | 0.02 | - | 8.27 ± 0.30 | 5.53 ± 0.07(e) | 13.80 ± 0.31 | 10.74 ± 0.31 | 1.59 ± 0.46 ×10−16 |
| HD 206893 B | NB4.05 | 7.62 ± 0.21 | 0.01 ± 0.32 | 0.08 | - | 7.63 ± 0.39 | 5.53 ± 0.07(f) | 13.16 ± 0.40 | 10.11 ± 0.40 | 2.16 ± 0.81 ×10−16 |
| HD 206893 B | M′ | 7.22 ± 0.15 | 0.01 ± 0.27 | - | - | 7.23 ± 0.31 | 5.54 ± 0.07(g) | 12.77 ± 0.32 | 9.72 ± 0.32 | 1.68 ± 0.50 ×10−16 |
Notes. (a) For asymmetric uncertainties, we conservatively use the largest of the two values that were derived from the MCMC and bias analysis (see Figs. 4, 5, and A.1). (b) The uncertainty related to the variable observing conditions which may bias the relative flux calibration in cases where the unsaturated PSF was only sampled at the start and/or end of the observations. (c) The final contrast is calculated by adding the bias offset and combining the error components in quadrature. (d) The L′ and M′ photometry (3.454 ± 0.003 and 3.458 ±0.009 mag, respectively) in the ESO photometric system have been adopted from Bouchet et al. (1991). The errors have been inflated to 0.01 mag to account for a minor color offset with the VLT/NACO filters. (e) The L′ magnitude has been adopted from the WISE W1 photometry (see top left panel of Fig. C.1). (f) The NB4.05 magnitude has been adopted from the WISE W1 photometry with a minor color correction of 0.01 mag for HIP 65426 and − 0.01 mag for PZ Tel (see top right panel of Fig. C.1). (g)The M′ magnitude has been adopted from the WISE W1 magnitude with a minor color correction of 0.04 mag for PZ Tel and 0.01 mag for HD 206893 (see bottom left panel of Fig. C.1).
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.