Table 4: Stellar parameters and Fe abundances for stars in NGC 6253. Numbers in parenthesis in Col. 6 are [Fe/H] estimated by spectral synthesis.
Star $T_{\rm eff}$ $_{\rm {phot}}$ $\log g_{\rm {phot}}$ $T_{\rm eff}$ $_{\rm {spec}}$ $\xi$ [Fe/H] $\sigma _1$ $\sigma_{\rm {tot}}$ Membership
  (K)   (K) (km s-1)        
069885 6032 3.84 6200 1.27 +0.45(+0.35) 0.09 0.11 M
023501 5842 3.75 6050 0.90 +0.29 0.09 0.11 M?
023498 5509 3.44 5630 1.30 +0.32 0.09 0.11 M
024707 4972 3.05 4940 1.16 +0.39 0.09 0.11 M
105495* 4520 2.46 4450 1.23 +0.49(+0.35) 0.10 0.13 M
Average Fe         +0.39(+0.34)   0.08(0.04) (rms)  
Likely non-members                
069360 4741 2.81 4680 1.20 +0.48 0.10 0.12 NM
022182 4865 3.13 4770 1.20 +0.12 0.07 0.09 NM
* Note: the initial parameters of the clump star have been computed from EIS magnitudes calibrated to Bragaglia et al. (1997, see Table 2). We also performed a test using the Strömgren photometry by Twarog et al. (2003) reported to the UBV system. In this case we found $T_{\rm eff}$ $_{\rm {phot}}$ = 4666 K and $\log g=2.58$, and, from the spectroscopic analysis, $T_{\rm eff}$ $_{\rm {spec}}=4500$ K, $\xi=1.23$ km s-1, [Fe/H]=+0.51 ( $\log g=2.58$), which agree within the errors with the values reported in Table 4.


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