Table 3: Parameters resulting from the best fits of stellar population models to the photometric data for Sal, MS and Kro IMFs. The $\tilde\chi^2$ represent the reduced $\chi ^2$. The model which formally provides the best fit (the lowest $\tilde\chi^2$) is marked with "*''. The V-band absolute magnitude has been derived by the Ks-band apparent magnitude. The absolute magnitudes in the Ks and in the V bands are corrected for the extinction.
ID SFH $\tilde\chi^2$ P( $\tilde\chi^2$) $z_{\rm phot}$ Age AV Z MV MK aM/LK $\mathcal{M}_{\rm stars}$
          [Gyr] [mag] [$Z_\odot$] [mag] [mag] [M/L]$_\odot$ [1011$M_\odot $]
  Sal IMF                    
HDFS_1269* $\tau=0.3$ 0.33 0.92 $\rm 2.4^{+0.3}_{-0.2}$ 2.0 0.3 0.4 -22.9 -25.1 0.50 1.2
HDFS_822 $\tau=0.3$ 0.06 0.99 $\rm 3.0^{+0.3}_{-0.2}$ 1.7 1.0 0.2 -24.1 -26.1 0.45 3.3
HDFS_850 $\tau=0.1$ 0.16 0.98 $\rm 2.9^{+0.2}_{-0.3}$ 0.5 1.9 1.0 -24.1 -25.8 0.30 1.4
  MS IMF                    
HDFS_1269 $\tau=0.3$ 0.34 0.92 $\rm 2.5^{+0.3}_{-0.2}$ 2.0 0.2 0.4 -22.9 -25.1 0.26 0.6
HDFS_822* $\tau=0.3$ 0.04 0.99 $\rm 3.0^{+0.3}_{-0.2}$ 1.7 0.9 0.2 -24.1 -26.1 0.23 1.4
HDFS_850 $\tau=0.1$ 0.17 0.98 $\rm 2.9^{+0.2}_{-0.3}$ 0.5 1.8 1.0 -24.0 -25.8 0.14 0.6
  Kro IMF                    
HDFS_1269 $\tau=0.3$ 0.38 0.89 $\rm 2.4^{+0.3}_{-0.2}$ 2.0 0.4 0.4 -22.9 -25.1 0.38 0.9
HDFS_822 $\tau=0.3$ 0.04 0.99 $\rm 3.0^{+0.3}_{-0.2}$ 1.7 1.0 0.2 -24.1 -26.0 0.35 2.1
HDFS_850* $\tau=0.1$ 0.16 0.98 $\rm 2.9^{+0.2}_{-0.3}$ 0.5 1.9 1.0 -24.0 -25.8 0.22 1.0
a We used $M_{\odot,K}=3.4$ (Allen 1973).


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