Table 4: Atomic data for the Ca I and Ca II lines, solar $\log gf\varepsilon_{\rm Ca}^\odot$ values determined from NLTE analysis of the Ca line profiles in the Kitt Peak Solar Atlas (Kurucz et al. 1984) neglecting hydrogenic collisions ($S_{\rm H}$ = 0), and abundance corrections $\Delta_{\rm X} = \log\varepsilon_{\rm X} - \log\varepsilon_{\rm S_H = 0}$ where X takes the meaning 0.1, 1, and LTE for $S_{\rm H}$ = 0.1, $S_{\rm H}$ = 1 and the LTE assumption, respectively.

$\lambda$		 mult $E_{\rm low}$ $\log gf$ log C6 $\log gf\varepsilon_{\rm Ca}^\odot$ $\Delta_{0.1}$ $\Delta_1$ $\Delta_{\rm LTE}$ $W_\lambda $
(Å)   (eV) LAB NIST VALD OP           (mÅ)
1 2 3 4 5 6 7 8 9 10 11 12 13
Ca I                      
4226.73 2 0.00  0.244a  0.244  0.265  0.276 -31.23g -5.47 -0.03 -0.06 -0.08 1500
4425.44 4 1.87 -0.358b -0.358 -0.286 -0.566 -30.90* -5.95 0.00 -0.03 -0.03 174
4578.56 23 2.51 -0.697c -0.558 -0.697 -0.804 -30.30i -6.33 0.00 -0.04 -0.06 87
5261.71 22 2.51 -0.579c -0.73 -0.579 -0.836 -30.86i -6.14 0.00 -0.03 -0.05 102
5349.47 33 2.70 -0.310c   - -0.310 -0.730 -31.45i -5.92 0.02 0.02 0.00 97
5512.981   2.92 -0.464d -0.30 -0.447 -0.396 -30.61i -6.05 0.00 0.02 0.00 89
5588.76 21 2.51  0.358c  0.21  0.358  0.339 -31.39i -5.36 0.00 0.00 0.00 171
5590.12 21 2.51 -0.571c -0.71 -0.571 -0.590 -31.39i -6.18 0.00 -0.03 -0.03 97
5857.45 47 2.92  0.240c  0.23  0.240  0.025 -30.61i -5.40 0.00 -0.02 -0.02 160
5867.572   2.92 -1.570d   - -0.801 -2.402 -30.97h -7.12 -0.02 -0.06 -0.09 26
6122.22 3 1.88 -0.315b -0.315 -0.386 -0.356 -30.30g -6.06 0.01 -0.01 -0.02 228
6162.17 3 1.89 -0.089b -0.089 -0.167 -0.137 -30.30g -5.83 0.02 0.00 -0.02 289
6161.29 20 2.51 -1.266c -1.03 -1.266 -1.290 -30.48i -6.85 -0.01 -0.06 -0.07 67
6166.44 20 2.51 -1.142c -0.90 -1.142 -1.166 -30.48i -6.70 -0.02 -0.06 -0.07 77
6169.06 20 2.51 -0.797c -0.54 -0.797 -0.821 -30.48i -6.40 -0.02 -0.03 -0.03 100
6169.56 20 2.51 -0.478c -0.27 -0.478 -0.502 -30.48i -6.09 -0.02 -0.03 -0.03 129
6439.07 18 2.51  0.390c  0.47  0.390  0.301 -31.58i -5.32 -0.02 -0.01 -0.01 188
6471.66 18 2.51 -0.686c -0.59 -0.686 -0.775 -31.58i -6.33 -0.02 0.01 0.01 97
6493.78 18 2.51 -0.109c  0.14 -0.109 -0.198 -31.58i -5.77 -0.03 -0.01 0.00 139
6499.65 18 2.51 -0.818c -0.59 -0.818 -0.907 -31.58i -6.41 -0.03 -0.06 0.00 89
6449.81 19 2.51 -0.502c -0.55 -0.502   - -31.45i -6.14 -0.02 0.00 0.00 106
6455.60 19 2.51 -1.34d -1.36 -1.29   - -31.45i -6.95 -0.02 -0.04 -0.05 59
6572.78 1 0.00 -4.24e -4.30 -4.104   - -31.54g -9.90 -0.03 -0.08 -0.10 31
7326.15 44 2.92 -0.208d   -  0.073  0.021 -31.42h -5.74 0.02 0.00 0.02 116
Ca II                      
5339.19 20 8.40   -   - -1.099 -0.079 -30.31h -5.77 0.00 0.00 0.00 6
5001.48 15 7.47   - -0.52 -0.755 -0.505 -30.66h -6.18 0.00 0.01 0.03 11
6456.91 19 8.40   -   - -0.171  0.412 -30.77h -5.20 0.01 0.02 0.02 16
8248.80 13 7.48   -  0.57  0.621  0.556 -30.85* -4.97 0.02 0.08 0.14 65
8254.70 13 7.48   - -0.39 -0.333 -0.398 -30.85* -5.92 0.00 0.01 0.02 18
8498.02 2 1.69 -1.416f -1.318 -1.416 -1.465 -31.51g -7.14 0.00 0.00 0.00 1132
8912.073   7.05   -   -  0.575  0.636 -31.10* -4.98 0.03 0.10 0.17 111
8927.364   7.05   -   -  0.750  0.811 -31.10* -4.81 0.03 0.09 0.12 121
9890.705   8.40   -   -  1.200  1.270 -31.34h -4.42 0.06 0.12 0.16 70

Column 2 contains the multiplet numbers accordingly to Moore (1972).
Column 13 contains solar equivalent widths.
1 $\rm 4p~^1{\rm P}^{\circ}_{\rm }$ - $\rm 4p^2~^1{\rm S}^{}_{\rm }$. a Smith & Gallagher (1966). g $A\&O'M$.
2 $\rm 4p~^1{\rm P}^{\circ}_{\rm }$ - $\rm 6s~^1{\rm S}^{}_{\rm }$. b Smith & O'Neil (1975). h Kurucz's calculations.
3 $\rm 4d~^2{\rm D}^{}_{\rm 3/2}$ - $\rm 4f~^2{\rm F}^{\circ}_{\rm 5/2}$. c Smith & Raggett (1981). i Smith (1981).
4 $\rm 4d~^2{\rm D}^{}_{\rm 5/2}$ - $\rm 4f~^2{\rm F}^{\circ}_{\rm 5/2,7/2}$. d Smith (1988). * from solar line profile fitting.
5 $\rm 4f~^2{\rm F}^{\circ}_{\rm }$ - $\rm 5g~^2{\rm G}^{}_{\rm }$. e Drozdowski et al. (1997).
  f Theodosiou (1989).

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