The massive star initial mass function of the Arches cluster

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Table 7:

Slopes of the Arches cluster IMF derived from average dereddening are shown in the two first rows.
	r < 0.2 pc	0.2 < r < 0.4 pc	r < 0.4 pc
$\Gamma^{a}$	$-0.60\pm0.17$	$-1.15\pm0.20$	$-0.81\pm0.19$
$\Gamma^{b}$	$-0.60\pm0.17$	$-1.23\pm0.23$	$-0.96\pm0.24$
$\Gamma^{c}$	$-0.88\pm0.20$	$-1.28\pm0.20$	$-1.1\pm0.2$

^a IMF slope derived without radial correction; ^b IMF slope derived with a radial correction for r > 0.2 pc to take into account the differential extinction (as proposed in SGB02, SBG05); ^c this work. Individual derredening results described in Sect. 4.1.
A 2.5 Myr theoretical isochrone with solar metallicity (Lejeune & Shaerer 2001) was used to derive these results.

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