The massive star initial mass function of the Arches cluster

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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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