Architecture of planetary systems with and without outer giant planets - I. Inner planet detections around HD 23079, HD 196067, and HD 86226

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Volume 703 (November 2025)

A&A, 703 (2025) A78

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Table 1

Stellar parameters for HD 23079, HD 196067, and HD 86226.

Star	HD 23079	HD 196067	HD 86226
Spectral Type	59.5 V	G0V	G2V	^{a, b}
π (mas)	29.8633 ± 0.0194	25.0327 ± 0.0205	21.9301 ± 0.0267	^c
V (mag)	7.11	6.44	7.93	^a
B (mag)	7.68	7.05	8.563	^a

d (pc)	${33.50}_{- 0.02}^{+ 0.05}$ $\[33.50_{-0.02}^{+0.05}\]$	${40.0}_{- 0.04}^{+ 0.05}$ $\[40.0_{-0.04}^{+0.05}\]$	${45.68}_{- 0.08}^{+ 0.09}$ $\[45.68_{-0.08}^{+0.09}\]$	^d
T_eff (K)	$5994_{- 64}^{+ 55}$ $\[5994_{-64}^{+55}\]$	$6072_{- 76}^{+ 83}$ $\[6072_{-76}^{+83}\]$	$6007_{- 71}^{+ 75}$ $\[6007_{-71}^{+75}\]$	^d
[Fe/H] (dex)	−0.129 ± 0.041	0.213 ± 0.042	−0.015 ± 0.041	^e
log g (cm s⁻²)	4.37 ± 0.02	4.09 ± 0.02	4.41 ±0.02	^{e, c}
R_*(R_⊙)	${1.08}_{- 0.03}^{+ 0.02}$ $\[1.08_{-0.03}^{+0.02}\]$	${1.71}_{- 0.04}^{+ 0.03}$ $\[1.71_{-0.04}^{+0.03}\]$	${1.03}_{- 0.02}^{+ 0.02}$ $\[1.03_{-0.02}^{+0.02}\]$	^d
M_*(M_⊙)	${1.16}_{- 0.03}^{+ 0.02}$ $\[1.16_{-0.03}^{+0.02}\]$	${1.16}_{- 0.09}^{+ 0.13}$ $\[1.16_{-0.09}^{+0.13}\]$	${1.08}_{- 0.05}^{+ 0.05}$ $\[1.08_{-0.05}^{+0.05}\]$	^d
L_*(L_⊙)	${1.35}_{- 0.08}^{+ 0.08}$ $\[1.35_{-0.08}^{+0.08}\]$	${3.54}_{- 0.20}^{+ 0.27}$ $\[3.54_{-0.20}^{+0.27}\]$	${1.24}_{- 0.07}^{+ 0.09}$ $\[1.24_{-0.07}^{+0.09}\]$	^d
$\log R_{H K}^{'}$ $\[\log~ R_{\mathrm{HK}}^{\prime}\]$	−4.929 ± 0.014	−5.033 ± 0.022	−4.946 ± 0.012	^f
P_rot. (d)	15.0 ± 2.6	22.5 ± 2.9	22.8 ± 3.0	^g
Age (Gyr)	2.6 ± 1.2	4.2 ± 2.0	3.8 ± 1.8	^g

Notes. The uncertainties in this table only reflect the formal error propagation. For some parameters (e.g., the masses), the systematic errors in stellar models dominate these formal uncertainties (e.g., Tayar et al. 2022). ^(a) Gray et al. (2006); ^(b) Houk & Smith-Moore (1988); ^(c) Riello et al. (2021); ^(d) Obtained from ARIADNE (Vines & Jenkins 2022); ^(e) Obtained using the ARES+MOOG method (Sousa et al. 2021); ^(f) Gomes da Silva et al. (2021); Rutten (1984); ^(g) Mamajek & Hillenbrand (2008).

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