Table 6
Summary of planet and star parameters for the Qatar-1 system.
| Parameter [Units] | Symbol | Value | Method |
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| Transit epoch (BJD_TCB−2 450 000.0) [days] | T 0 | 5518.41094 ± 0.00016 | (1) |
| Orbital period [days] | P | 1.42002504 ± 0.00000071 | (1) |
| Transit duration [days] | T 14 | 0.0678 ± 0.0010 | (2) |
| Planet/star area ratio | (Rp/R⋆)2 | 0.02280 ± 0.00011 | (2) |
| Planet/star radii ratio | Rp/R⋆ | 0.1513 ± 0.0008 | (2) |
| Orbital inclination [degrees] | i p | 83.82 ± 0.25 | (2) |
| Impact parameter | b | 0.675 ± 0.016 | (2) |
| Scaled stellar radius | R⋆/a | 0.1601 ± 0.0025 | (2) |
| Scaled planet radius | Rp/a | 0.0241 ± 0.0005 | (2) |
| Star reflex velocity [km s-1] | K ⋆ | 0.2657 ± 0.0035 | (3) |
| Orbital eccentricity | e | 0 | (3) |
| Systemic velocity [km s-1] | γ | − 38.0558 ± 0.0002 | (3) |
| Star density [ρ⊙] | ρ ⋆ | 1.62 ± 0.08 | (4) |
| Planet surface gravity [cgs] | log gp | 3.372 ± 0.024 | (4) |
| Star mass [M⊙] | M ⋆ | 0.85 ± 0.03 | (5) |
| Planet mass [MJ] | M p | 1.33 ± 0.05 | (6) |
| Orbital semi-major axis [AU] | a | 0.02343 ± 0.0012 | (7) |
| Star radius [R⊙] | R ⋆ | 0.80 ± 0.05 | (7) |
| Star surface gravity | log g⋆ | 4.55 ± 0.10 | (7) |
| Planet radius [RJ] | R p | 1.18 ± 0.09 | (7) |
| Planet density [ρJ] | ρ p | 0.80 ± 0.20 | (7) |
| Spin-orbit misalignment [degrees] | λ | − 8.4 ± 7.1 | (8) |
| Star projected rotational velocity [km s-1] | vsinI | 1.7 ± 0.3 | (8) |
| Star effective temperature [K] | T eff | 4910 ± 100 | (9) |
| Stellar metallicity | [Fe/H] | 0.20 ± 0.10 | (9) |
| Star age [Gyr] | Ag e ⋆ | ≈4.5 | (10) |
| Planet equilibrium temperature [K] | T P | 1389 ± 39 | (11) |
Notes.(1) Derived by combining the determinations of the mid-transit times from our photometric data sets with those derived from Alsubai et al. (2011). Kept fixed in the orbital and Rossiter RV fitting. (2) Derived as weighted mean of the best-fit determinations from our five transit light curves. (3) Derived by fitting the orbital RV curve to out-of-transit RV measurements. (4) Derived following Sozzetti et al. (2007). (5) Derived from evolutionary models. (6) Derived by using the expression of the mass function. (7) Derived from parameters above. (8) Derived by fitting our RM effect model to in-transit RV measurements. (9) Derived from spectroscopic analysis. (10) Derived from gyrochronology. (11) Derived following Cowan & Agol (2011).
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