Table 7: Results of our revised abundance analyses of Praesepe stars. In the upper part of the table, theoretical parameters are used (temperature from the photometry, gravity from the models and the temperature and microturbulence from the fit). In the lower part of the table, we adopted the most reliable measurements of parameters found by ignoring constraints from photometry or models. Also these analyses confirm the high metallicity of Praesepe is evident.
Star [Fe/H] $\xi$ T G Ion. Eq. corr.(chi vs. ab) corr.( EW vs. ab)
$T=T_{\rm phot},\ G=G_{\rm phot}, \ \xi=\xi_{\rm fit}$
KW 49 0.220 1.15 6028 4.44 -0.11 0.35 0.62
KW 100 0.354 1.09 5977 4.45 -0.30 0.10 0.76
KW 208 0.202 1.11 5993 4.45 -0.22 0.44 0.54
KW 326 0.447 0.98 5873 4.47 0.07 -0.10 0.54
KW 368 0.409 0.91 5811 4.48 0.12 -0.36 0.59
KW 392 0.246 1.01 5902 4.46 -0.27 0.39 0.47
KW 418 0.187 1.19 6062 4.44 -0.16 0.48 0.40
Minimising parameters with very loose photometric constraints

KW 49

 0.268 1.58 6290 4.66 0.01 0.01 0.01
KW 100 0.409 1.76 6370 4.64 -0.01 -0.22 0.05
KW 208 0.322 1.52 6340 4.64 0.00 -0.01 -0.02
KW 326 0.366 1.14 5860 4.62 -0.01 -0.06 0.10
KW 368 0.166 1.34 5700 4.52 0.00 -0.03 0.04
KW 392 0.354 1.44 6250 4.60 0.00 0.01 0.02
KW 418 0.359 1.44 6450 4.76 0.00 0.00 0.03


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