Applicability of Milne-Eddington inversions to high spatial resolution observations of the quiet Sun

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Table 1:

Atomic parameters of the spectral lines.
I ON	$\lambda$ (nm)	$\chi_{{\rm low}}$	$\log (gf)$	T RANSITION	$\alpha$	$\sigma/a_0^2$	$g_{\rm eff}$
Fe I	630.1501	3.654	-0.75	$\rm 5P_2{-}5D_2$	0.243	840.5	1.67
Fe I	630.2494	3.686	-1.236	$\rm 5P_1{-}5D_0$	0.240	856.8	2.5

Notes. $\lambda$ stands for the central wavelength of the transition, $\chi_{{\rm low}}$ is the excitation potential of the lower atomic level in eV, $\log gf$ represents for the multiplicity of the lower level times the oscillator strength, $\alpha$ and $\sigma$ are the collisional broadening parameters in the quantum theory of Anstee et al. (in units of Bohr's radius, a₀), and $g_{\rm eff}$ is the effective Landé factor of the transition.

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