Spatial distribution of exoplanet candidates based on Kepler and Gaia data

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Table C.3

Characteristics of our exoplanet host star candidates near NGC 6811 and NGC 6866.

Name	P_μ	P_ρ	P_d	P_tot	ΔG	g − r	P_rot ± ΔP	P_orb	R_p∕R_s	P_f
NGC 6811

KIC 9655005	0.65	0.72	1.00	0.47	0.38	0.06	1.537 ± 0.008	1.399	0.006	1.0
KIC 9533489⁽¹⁾	0.97	0.36	0.80	0.28	0.49	0.35	2.70	197.146	0.342	1.0
Kepler − 67⁽²⁾	0.64	0.47	0.99	0.30	1.15	0.76	10.487 ± 0.199	15.726	0.033	1.7 × 10⁻⁴
Kepler − 66⁽²⁾	0.92	0.30	0.82	0.23	0.90	0.53	10.462 ± 0.053	17.816	0.031	5.7 × 10⁻³
KIC 9776794	2.5 × 10⁻⁴	0.68	0.71	1.2 × 10⁻⁴	1.38	0.98	11.770 ± 0.031	18.222	0.071	0.85

NGC 6866

KIC 8396288	0.85	0.42	0.99	0.36	1.16	0.76	8.795 ± 0.037	8.585	0.034	2.6 × 10⁻²
KIC 8331612(a)	0.32	0.28	0.90	0.082	1.03	0.61	8.159 ± 0.039	13.835	0.033	2.7 × 10⁻³
KIC 8331612(b)	0.32	0.28	0.90	0.082	1.03	0.61	8.159 ± 0.039	25.697	0.033	1.2 × 10⁻¹

NGC 6819

Kepler − 1625	3.0 × 10⁻¹⁵	0.10	0.77	2.3 × 10⁻¹⁶	−	−	−	287.377	0.060	7.5 × 10⁻³

Notes. P_μ, P_ρ and P_d are membership probabilities (see Sect. 6), ΔG = G_bp − G_rp is the colour based on Gaia filters (Gaia Collaboration 2016, 2018), g and r are stellar magnitudes in SDSS filters (Brown et al. 2011). P_rot (days) is the rotational period of the star, ΔP is its error estimated with the Monte-Carlo method, P_orb is the planet orbital period in days, R_p∕R_s is the planet to star radius ratio, and P_f is a false positive probability (Morton et al. 2016).⁽¹⁾Is a γ Doradus/δ Scuti star studied in Bognár et al. (2015),⁽²⁾Are the exoplanet host stars studied in Meibom et al. (2013).

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