Diagnosing the solar atmosphere through the Mg I b2 5173 Å line - I. Nonlocal thermodynamic equilibrium inversions versus traditional inferences

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Volume 696 (April 2025)

A&A, 696 (2025) A105

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Table 1.

Description of the CRISP/SST observations.

Atom	λ₀	g_eff	N_λ	Δλ	Δλ_i, f	Δλ_C	N_acc
	(Å)			(mÅ)	(mÅ)	(mÅ)
Fe I	6173.33	2.5	18	28	±224	+532	18
Mg I	5172.68	1.75	14	50(*)	±500	−700	27
Ca II	8542.09	1.1	18	100	±800	+2400	4
Hα	6562.81	1.05	21	100	±900	±1000	4

Notes. From left to right, the columns indicate the atomic species of the four observed spectral lines, the central wavelength (λ₀), the effective Landé factor (g_eff), the number of wavelength points within the line (N_λ), the step size (Δλ), the initial and final wavelengths within the spectral line (Δλ_i, f), the continuum wavelength point relative to the line center (Δλ_C), and the number of accumulations per wavelength (N_acc).

^(*)

The spectral window at ±100 mÅ from the line core was sampled with Δλ = 50 mÅ, while Δλ = 100 mÅ was used outside the line core, up to ±500 mÅ.

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