Table 2
IFS and IRDIS astrometry of HD 284149 B from the non-coronagraphic data obtained in November 2015.
| Filter | Separation | PA | Δ mag | Mass | |||||||
| (mas) | (au) | (°) | (M⊙) | ||||||||
|
|
|||||||||||
| Y | 90.02 ± 1.32 | 10.58 ± 0.15 | 195.19 ± 1.86 | 4.54 ± 0.13 | 0.23 ± 0.02 | ||||||
| J | 90.73 ± 1.22 | 10.66 ± 0.15 | 194.99 ± 1.66 | 4.57 ± 0.11 | 0.17 ± 0.02 | ||||||
| H | 94.18 ± 1.16 | 11.07 ± 0.16 | 195.03 ± 1.47 | 4.87 ± 0.23 | 0.12 ± 0.01 | ||||||
| K1 | 80.16 ± 18.57 | 9.42 ± 0.66 | 187.53 ± 67.03 | 4.07 ± 0.24 | 0.19 ± 0.02 | ||||||
| K2 | 81.72 ± 18.27 | 9.60 ± 0.66 | 193.22 ± 34.00 | 3.79 ± 0.21 | 0.20 ± 0.02 | ||||||
|
|
|||||||||||
| Adopted values | |||||||||||
| 91.78 ± 2.16 | 10.71 ± 0.34 | 195.06 ± 0.16 | – | 0.16 ± 0.04 | |||||||
Notes. A true north position of −1.7470 ± 0.0048° and pixel scale of 7.46 ± 0.02 mas/pixel and 12.255 ± 0.009 mas/pixel, for IFS and IRDIS respectively (see Maire et al. 2016b, for details) were used. The value of the separation in AU was obtained using the value of the parallax of the star provided by the Gaia satellite (Gaia Collaboration 2016). The values of the masses are derived using the COND Models by Baraffe et al. (2003) and taking into account both the uncertainties on the photometry and on the age value. The uncertainties listed take into account all the possible sources of errors. In the case of the astrometry, the dominant source of error is the uncertainty on the centering of the star, whether the error on the mass is dominated by the uncertainty on the age estimate.
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