Spectropolarimetric characterisation of exoplanet host stars in preparation of the Ariel mission - II. The magnetised wind environment of TOI-1860, DS Tuc A, and HD 63433

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Volume 705 (January 2026)

A&A, 705 (2026) A40

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Table 1

Properties of the selected stars.

Star	RA	Dec	SpT	Mass (M_⊙)	H	V	P_rot (d)	v_eq sin(i) (km s⁻¹)	S-index	$\log R_{H K}^{'}$ $\[\log~ \mathrm{R}_{\mathrm{HK}}^{\prime}\]$	N_pl
HD 63433	07 49 55.06	+27 21 47.46	G5	0.99	5.36	6.92	6.5^a	7.3^a	. . .	−4.36^b	3
HD 63935	07 51 41.99	+09 23 09.79	G5	0.97	6.96	8.58	. . .	0.3^c	. . .	. . .	2
HD 89345	10 18 41.06	+10 07 44.50	G5	1.18	7.77	9.38	. . .	0.1^c	...	. . .	1
HD 152843	16 55 08.36	+20 29 28.79	G0	1.06	7.66	8.86	. . .	7.5^c	. . .	. . .	2
HD 158259	17 25 24.10	+52 47 26.47	G0	1.03	5.03	6.48	20.0^d	1.6^c	0.19^e	−4.75^e	5
HD 260655	06 37 10.80	+17 33 53.33	M0	0.44	6.03	9.59	37.5^f	<2.0^f	0.92^e	−4.84^e	2
HAT-P-22	10 22 43.59	+50 07 42.06	G5	1.13	7.94	9.76	28.7^g	1.65^g	0.15^e	−5.09^e	1
DS Tuc A	23 39 39.48	−69 11 44.71	G5	1.01	6.76	8.23	2.85^h	17.8^h	0.88^e	−4.06^e	1
Kepler-444	19 19 00.55	+41 38 04.58	K0	0.67	6.77	8.87	17.2ⁱ	. . .	...	. . .	5
K2-116	22 24 36.38	−11 34 43.30	K7	0.69	8.02	10.80	29.8^j	. . .	. . .	. . .	1
TOI-836	15 00 19.40	−24 27 14.69	K4	0.68	6.98	9.92	21.99^k	1.9^k	1.31^e	−4.44^e	2
TOI-1136	12 48 44.37	+64 51 19.15	G5	1.02	8.09	9.53	8.19^l	6.7^m	0.32^m	−4.49^m	6
TOI-1860	15 05 49.90	+64 02 49.94	G5	0.99	6.88	8.40	4.43ⁿ	10.4ⁿ	. . .	−4.25ⁿ	1
TOI-2076	14 29 34.24	+39 47 25.54	K1	0.82	7.19	9.14	6.84^o	5.7^p	. . .	−4.37°	3
Wolf 503	13 47 23.44	−06 08 12.73	K3.5	0.63	7.77	10.30	. . .	2.8^c	. . .	. . .	1

Notes. The columns are: identifier, right ascension and declination (J2000), spectral type, stellar mass, H band magnitude, V band magnitude, rotation period, projected equatorial velocity, S-index, chromospheric activity index, and number of exoplanets. The information is primarily extracted from the Ariel stellar catalogue (Danielski et al. 2022) available at https://sites.google.com/inaf.it/arielstellarcatalogue/. References: a. Mann et al. (2020) b. Marsden et al. (2014), c. Tsantaki et al. (2025), d. Hara et al. (2020), e. Boro Saikia et al. (2018), f. Luque et al. (2022), g. Mancini et al. (2018), h. Newton et al. (2019), i. Angus et al. (2018), but Mazeh et al. (2015) reported a rotation period of 49.4 d instead, j. Reinhold & Hekker (2020), k. Hawthorn et al. (2023), l. Canto Martins et al. (2020), m. Dai et al. (2023), n. Giacalone et al. (2022), o. Osborn et al. (2022) and Frazier et al. (2023) reported a rotation period of 7.12 d, and p. Frazier et al. (2023).

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