Astronomy & Astrophysics

Table 1: Set of visible and infrared lines considered in this work. $\lambda _{0}$ represents the central wavelength, $\chi$ the excitation potential of the lower level, $\log ~ gf$ the logarithm of the oscillator strength times the multiplicity of the lower level, and $g_{\rm eff}$ the effective Landé factor.
Table A.1: Weak line model parameters and their derivatives for the quiet Sun model. A₀ and A₁ are the residual intensity and the width of Stokes I in the absence of magnetic fields, while A₂ is the continuum intensity. A^V₀ and A^V₁ are the amplitude and width of the Stokes V lobes in the strong field regime. A^*₀ and A^*₁ are the depth and the width of Stokes I in the weak field approximation ( $B=200~{\rm G}$ ).
Table A.2: Same as Table A.1, for the penumbral model.
Table A.3: Same as Table A.1, for the umbral model.