The GAPS programme at TNG - LX. Atmospheric characterisation of KELT-9 b via single-line analysis: Detection of six H I Balmer lines, Na I, Ca I, Ca II, Fe I, Fe II, Mg I, Ti II, Sc II, and Cr II

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Volume 690 (October 2024)

A&A, 690 (2024) A237

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Table 3

Summary of the results obtained from the Gaussian fits to the detected H I Balmer lines.

	Gaussian fit					NLTE model

Line ⁽^a⁾	Depth (%)	Rp	FWHM (km/s)	v (km/s)	$χ_{red}^{2}$ $\[\chi_{\text {red }}^2\]$	v_mic (km/s)	v_mac (km/s)	$χ_{red}^{2}$ $\[\chi_{\text {red }}^2\]$
Hα	0.97 ± 0.02	1.56 ± 0.01	49.25 ± 0.95	−3.34 ± 0.36	1.37	2.0 ± 1.5	21 ± 3	0.66
Hβ	0.64 ± 0.02	1.39 ± 0.01	45.0 ± 1.58	−5.67 ± 0.61	1.08	1.0 ± 0.8	24 ± 1	0.71
Hγ	0.51 ± 0.03	1.33 ± 0.01	36.63 ± 2.17	−5.74 ± 0.86	0.66	3.0 ± 0.5	24 ± 2	0.6
Hδ	0.62 ± 0.05	1.38 ± 0.03	28.97 ± 2.79	−8.24 ± 1.13	1.03	1.0 ± 1.2	10 ± 12	0.9
Hϵ	0.39 ± 0.06	1.25 ± 0.03	30.65 ± 5.35	−5.36 ± 2.11	0.7	1.0 ± 1.7	19 ± 16	0.83
Hζ	0.92 ± 0.16	1.53 ± 0.08	26.1 ± 5.4	−7.56 ± 2.16	3.6	14.0 ± 4.8	1 ± 14	3.75

Notes. We report the Depth, FWHM, and v columns representing the Gaussian best-fit parameters, while R_p is the transit depth translated into planetary radii. v_mic and v_mac are the micro- and macro-turbulence velocity, respectively, for the best-fitting NLTE model. For both analyses, we also report the reduced chi-squared, $χ_{red}^{2}$ $\[\chi_{\text {red }}^2\]$ ^(a)For each line, we show the wavelength in Å.

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