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Table 6:

Table of elements and spectral lines used for mapping of HD 50773.
Species $\lambda$ (Å) $\log gf$ $E_{\rm low}$ (eV) min, max Blended with $\odot$
        $\log(N/N_{{\rm tot}})$   $\log(N/N_{{\rm tot}})$
Mg   I 5401.5210 -0.340 11.6300   Fe, Y -4.51
Si   II 5055.9840 0.593 10.0740 -4.8, -2.6   -4.53
Si   I 5421.1680 -2.250 5.6190   Cr, Mn  
Si   I 5421.3830 -1.480 5.6190   Cr, Mn  
Ca   I 6102.7230 -0.862 1.8790 -6.5, -2.7 Fe -5.73
Ca   II 6456.8750 -0.539 8.4380   Fe  
Ti   II 5154.0680 -1.750 1.5660 -8.3, -6.1 Cr, Fe -7.14
Cr   II 5237.3290 -1.350 4.0730 -7.1, -3.6   -6.40
  5280.0540 -2.316 4.0740      
  5510.7020 -2.614 3.8270   Fe, Y, Ni  
Fe   I 5383.3692 0.645 4.3120 5.4, -3.6   -4.59
  5400.5022 -0.160 4.3710      
  5400.6560 -2.482 3.6350      
  5401.2689 -1.920 4.3200      
Ni   I 5510.0030 -0.900 3.8470 -6.1, -5.6 Cr, Fe, Y -5.81
Y   II 5509.8950 -1.010 0.9920 -9.9, -7.5 Cr, Fe, Ni -9.83
  5662.9250 0.160 1.9440   Fe  
Cu   II 5153.2300 0.217 3.7860 -8.0, -6.9 Cr, Ti, Fe -7.83

Notes. Element, spectral lines used, the $\log gf$ values of these lines, abundance interval in dex, for comparison the solar values (Asplund et al. 2005) are presented. Atomic parameters used in our study were extracted from VALD.


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