On detectability of Zeeman broadening in optical spectra of F- and G-dwarfs

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Table 3

Objects investigated sorted by increasing HD number.

Name	HD	Sp.	line		N _DOF	S/N	T _eff	T ₁	T ₂	log g	v _mac	v _mic	v sini	B f _lit	Bf	Bf (3σ)
		Type	set				[K]			[cgs]	[ kms^-1 ]			[G]

Sun	-	G2V	A3	237.6	132	700	5780	6565		4.44	3.29	0.65	1.34	≲130^a	0^+ 90	0−200
TC, cool			A3	169.5	130	700		6571	4876	4.44	2.80	0.61	1.93			150-1400

GJ 297.1	68456	F6V	A3	245.6	227	400	6396	7178		4.14	1.52	3.30	9.48	-		0-1950
			B3	318.6	248	420		7249		4.14	2.33	3.05	9.39	-		750-1300
			B4	384.5	309	420		7209		4.40^*	4.63	1.84	9.35	-		600-1200

59 Vir	115383	G0V	B3	262.5	223	420	6234	7075		4.60	4.89	1.21	6.67			300-600
			B4	401.9	332	420		7077		4.50^*	4.76	1.23	6.70			350-650
TC, equal			B3	262.5	222	420		7075	7075	4.60	4.88	1.21	6.68	190^b		100-550
TC, cool			B3	216.2	221	420		7517	5978	4.60	4.29	1.42	6.72			0-300
TC, warm			B3	226.1	221	420		6047	7440	4.60	4.39	1.33	6.70			0-450

61 Vir	115617	G6V	B3	198.1	175	400	5571	6284		4.47	3.09	< 0.10	0.46	600^c	0⁺⁸⁰	0-150

Notes. Values for T_eff and log g from literature, unless otherwise indicated. Note that T₁ and T₂ are SPINOR best-fit temperatures corresponding to unit optical depth calculated for continuum opacity at 5000 Å. Overall best-fit results as well as 1σ and 3σ ranges determined for Bf, see text. 3σBf range rounded to 50 G.

Trujillo Bueno et al. (2004);

Linsky et al. (1994);

Gray (1984);

log g used as free fit parameter.

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