The GAPS Programme at TNG - XXV. Stellar atmospheric parameters and chemical composition through GIARPS optical and near-infrared spectra

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Volume 640 (August 2020)

A&A, 640 (2020) A123

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Table 3

Input values of the atmospheric parameters and results of the spectroscopic analysis derived for the stars in our sample from the optical analysis.

ID	T_eff,phot	log g_trig	ξ	T_eff,spec	log g_spec	ξ_spec	[Fe/H]_I	[Fe/H]_II	[Ti/H]_I	[Ti/H]_II
	(K)	(dex)	(km s⁻¹)	(K)	(dex)	(km s⁻¹)	(dex)	(dex)	(dex)	(dex)
Standard stars
HD3765	5111 ± 92	4.56 ± 0.02	0.79 ± 0.04	5001 ± 75	4.56 ± 0.10	0.59 ± 0.20	0.02 ± 0.01 ± 0.08	0.13 ± 0.03 ± 0.09	0.14 ± 0.01 ± 0.11	0.13 ± 0.02 ± 0.06
HD159222	5863 ± 111	4.41 ± 0.05	1.03 ± 0.04	5900 ± 75	4.43 ± 0.05	1.03 ± 0.10	0.14 ± 0.01 ± 0.06	0.12 ± 0.02 ± 0.04	0.09 ± 0.01 ± 0.07	0.08 ± 0.01 ± 0.03

Coma Berenices
TYC 1991-1235-1	5040 ± 108	4.62 ± 0.04	0.77 ± 0.04	5070 ± 70	4.53 ± 0.05	0.87 ± 0.12	−0.05 ± 0.01 ± 0.04	−0.03 ± 0.03 ± 0.07	−0.03 ± 0.01 ± 0.09	−0.02 ± 0.02 ± 0.04
HIP 61205	5972 ± 114	4.58 ± 0.02	1.05 ± 0.04	5825 ± 50	4.52 ± 0.05	1.05 ± 0.10	−0.04 ± 0.01 ± 0.04	−0.03 ± 0.02 ± 0.03	−0.06 ± 0.01 ± 0.05	−0.05 ± 0.01 ± 0.03
TYC 1989-0049-1	4718 ± 76	4.73 ± 0.02	0.67 ± 0.04	4718 ± 50	4.61 ± 0.05	0.63 ± 0.07	−0.06 ± 0.02 ± 0.03	0.01 ± 0.04 ± 0.07	0.00 ± 0.02 ± 0.07	0.02 ± 0.03 ± 0.03
TYC 1989-147-1	5333 ± 100	4.66 ± 0.03	0.85 ± 0.04	5313 ± 50	4.51 ± 0.05	0.80 ± 0.10	−0.05 ± 0.01 ± 0.04	−0.01 ± 0.03 ± 0.05	−0.04 ± 0.01 ± 0.06	−0.02 ± 0.02 ± 0.04
Ursa Major
HD 167389	6038 ± 140	4.51 ± 0.02	1.07 ± 0.04	6000 ± 75	4.55 ± 0.05	1.07 ± 0.15	0.01 ± 0.01 ± 0.06	0.00 ± 0.02 ± 0.04	0.03 ± 0.01 ± 0.07	0.02 ± 0.02 ± 0.04
HD 59747	5206 ± 110	4.71 ± 0.02	0.81 ± 0.04	5106 ± 50	4.58 ± 0.05	0.73 ± 0.10	−0.02 ± 0.01 ± 0.03	−0.01 ± 0.03 ± 0.05	0.01 ± 0.01 ± 0.06	0.02 ± 0.02 ± 0.03
Hercules Lyra
HD 70573	5755 ± 129	4.43 ± 0.03	1.00 ± 0.04	5800 ± 75	4.40 ± 0.07	1.10 ± 0.10	−0.03 ± 0.02 ± 0.09	0.02 ± 0.02 ± 0.07	−0.02 ± 0.02 ± 0.10	0.00 ± 0.02 ± 0.06

Notes. The derived abundances of Fe and Ti are also reported. The uncertainties on the abundances are σ₁ and σ₂, which are due to the EW measurements and related to the atmospheric parameters, respectively.

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