Table 5
Adopted stellar parameters for HAT-P-42 and HAT-P-43 assuming circular orbits.
| HAT-P-42 | HAT-P-43 | ||
| Parameter | Value | Value | Source |
|
|
|||
| Astrometric properties | |||
| GSC ID | GSC 0232-01451 | GSC 0801-00608 | |
| 2MASS-ID | 2MASS 09012265+0605500 | 2MASS 08354217+1012239 | |
| RA (J2000) | 09h01m22.66s | 08h35m42.18s | 2MASS |
| Dec (J2000) | 2MASS | ||
| μRA (mas yr-1) | −6.2 ± 1.9 | −10.3 ± 2.6 | UCAC4 |
| μDec (mas yr-1) | −29.3 ± 2.0 | −16.0 ± 3.2 | UCAC4 |
| Spectroscopic properties | |||
| Teff ⋆ (K) | 5743 ± 50 | 5645 ± 74 | SPCa |
| [Fe/H] | 0.27 ± 0.08 | 0.23 ± 0.08 | SPC |
| vsini (km s-1) | 3.5 ± 0.5 | 2.4 ± 0.5 | SPC |
| γRV (km s-1) | 20.26 ± 0.15b | -4.86 ± 0.15b | TRES |
| Photometric properties | |||
| B (mag) | 12.827 ± 0.020 | 14.120 ± 0.060 | APASS |
| V (mag) | 12.168 ± 0.030 | 13.356 ± 0.030 | APASS |
| J (mag) | 10.960 ± 0.023 | 12.146 ± 0.021 | 2MASS |
| H (mag) | 10.677 ± 0.024 | 11.809 ± 0.029 | 2MASS |
| Ks (mag) | 10.626 ± 0.026 | 11.764 ± 0.023 | 2MASS |
| Derived properties | |||
| M⋆ (M⊙) | 1.178 ± 0.068 |
|
YY+a/R⋆+SPCc |
| R⋆ (R⊙) | 1.530 ± 0.140 |
|
YY+a/R⋆+SPC |
| log g⋆ (cgs) | 4.14 ± 0.07 | 4.37 ± 0.02 | YY+a/R⋆+SPC |
| L⋆ (L⊙) | 2.27 ± 0.43 | 1.11 ± 0.10 | YY+a/R⋆+SPC |
| MV (mag) | 3.94 ± 0.21 | 4.73 ± 0.11 | YY+a/R⋆+SPC |
| MK (mag,ESO) | 2.38 ± 0.20 | 3.11 ± 0.07 | YY+a/R⋆+SPC |
| Age (Gyr) |
|
|
YY+a/R⋆+SPC |
| AV (mag)d | 0.000 ± 0.020 | 0.000 ± 0.019 | YY+a/R⋆+SPC |
| Distance (pc) | 447 ± 41 |
|
YY+a/R⋆+SPC |
Notes.
SPC = “stellar parameter classification” method, described by Buchhave et al. (2012), which derives stellar atmospheric parameters from high-resolution spectra. These parameters rely primarily on SPC, but have a small dependence also on the iterative analysis incorporating the isochrone search and global modeling of the data, as described in the text.
These velocities corresponds to an absolute scale references thanks to nightly observations of HD 182488 and correction of the gravitational redshift of the Sun.
YY+a/R⋆+SPC = Based on the YY isochrones (Yi et al. 2001), a/R⋆ as a luminosity indicator, and the SPC results.
V band extinction determined by comparing the measured 2MASS and APASS photometry for the star to the expected magnitudes from the YY+a/R⋆+SPC model for the star. We use the Cardelli et al. (1989) extinction law.
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