Table 2: Statistics of the field-star decontamination discriminated by magnitude bins.
$\Delta\mbox{$J$ }$ FSR 1716 ( $R<3\hbox {$^\prime $ }$) Cz 23 ( $R<4\hbox {$^\prime $ }$)
  $N_{\rm obs}$ $N_{\rm cl}$ $N_{1\sigma}$ $\sigma_{\rm FS}$ ${\rm FS}_{\rm unif}$ $N_{\rm obs}$ $N_{\rm cl}$ $N_{1\sigma}$ $\sigma_{\rm FS}$ ${\rm FS}_{\rm unif}$
(mag) (stars) (stars)   (stars)   (stars) (stars)   (stars)  
7-8 $1\pm1.0$ 1 1.0 0.20 0.36 -- -- -- -- --
8-9 $1\pm1.0$ 1 1.0 0.38 0.23 -- -- -- -- --
9-10 $3\pm1.7$ 1 0.6 0.37 0.08 $2\pm1.4$ 1 0.7 0.47 0.63
10-11 $11\pm3.3$ 3 0.9 0.81 0.07 $7\pm2.6$ 6 2.3 0.91 0.38
11-12 $37\pm6.1$ 9 1.5 1.90 0.07 $1\pm1.0$ 0 0.0 1.08 0.22
12-13 $82\pm9.1$ 20 2.2 3.23 0.05 $10\pm3.2$ 2 0.6 1.50 0.15
13-14 $145\pm12.0$ 36 3.0 6.33 0.05 $24\pm4.9$ 5 1.0 2.33 0.11
14-15 $248\pm15.7$ 57 3.6 8.45 0.04 $66\pm8.1$ 22 2.7 3.77 0.08
15-16 -- -- -- -- -- $118\pm10.9$ 30 2.8 5.61 0.07
All $528\pm23.0$ 128 5.0 19.2 0.04 $228\pm15.1$ 66 4.4 15.6 0.07
Notes. The table provides, for each magnitude bin ( $\Delta\mbox{$J$ }$), the number of observed stars ( $N_{\rm obs}$) within the spatial region sampled in the CMDs shown in the top panels of Figs. 3 and 4, the respective number of probable member stars ( $N_{\rm cl}$) computed by the decontamination algorithm, the $N_{1\sigma}$ parameter, the $1\sigma $ Poisson fluctuation ( $\sigma_{\rm FS}$) around the mean, with respect to the star counts measured in the 8 sectors of the comparison field, and the field-star uniformity parameter. The statistical significance of $N_{\rm cl}$ is reflected in its ratio with the $1\sigma $ Poisson fluctuation of $N_{\rm obs}$ ( $N_{1\sigma}$) and with $\sigma_{\rm FS}$. The bottom line corresponds to the full magnitude range.

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