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Table 6:

IMF slopes plotted in Fig. 13.
$\tau^{{a}}$ $\Gamma_{r \leq 0.2~{\rm pc}}$ $\Gamma_{0.2 < r \leq 0.4~{\rm pc}}$ $\Gamma_{r < 0.4~{\rm pc}}$ $\Gamma_{\rm NACO~field}$
2 -0.96 (-0.90) -1.24 (-1.37) -1.17 (-1.19) -1.34 (-1.35)
2.2 -0.88 (-0.94) -1.30 (-1.34) -1.11 (-1.18) -1.27 (-1.34)
2.5 -0.88 (-0.92) -1.28 (-1.31) -1.10 (-1.10) -1.26 (-1.29)
2.8 -0.92 (-0.86) -1.36 (-1.26) -1.14 (-1.06) -1.31 (-1.24)
3.2 -0.82 (-0.83) -1.31 (-1.28) -1.05 (-1.04) -1.24 (-1.23)
a Age of the isochrone in Myr.
For each annular region the IMF is obtained from the comparison of our observations with a set of isochrones (Lejeune & Schaerer 2001) with solar metallicity ranging from 2 to 3.2 Myr. The values between parenthesis correspond to slopes derived using double solar metallicity models.

Source LaTeX | All tables | In the text

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