Dissolution is the solution: on the reduced mass-to-light ratios of Galactic globular clusters

Table 6:

Observed and predicted stellar mass function (MF) slopes $\alpha$ in the range m=0.3- $0.8~\mbox{$M_\odot$ }$ .
MF slopes
NGC	$\alpha _{\rm obs}$	$\alpha _{\rm pred}$
104	$1.2\pm 0.3$	$\rm 1.68_{-0.00}^{+0.00}$
288	$0.0\pm 0.3$	$\rm0.96_{-0.31}^{+0.40}$
1851		$\rm 1.68_{-0.00}^{+0.00}$
1904		$\rm 1.65_{-0.07}^{+0.03}$
4147		$\rm 1.40_{-0.18}^{+0.14}$
4590		$\rm 1.66_{-0.05}^{+0.02}$
5139	$1.2\pm 0.3$	$\rm 1.55_{-0.11}^{+0.12}$
5272	$1.3\pm 0.3$	$\rm 1.68_{-0.00}^{+0.00}$
5466		$\rm 1.57_{-0.12}^{+0.09}$
5904		$\rm 1.64_{-0.08}^{+0.04}$
6093		$\rm 1.52_{-0.20}^{+0.14}$
6121	${\bf 1.0\pm0.2}$	$\rm0.62_{-0.32}^{+0.25}$
6171		$\rm 1.34_{-0.15}^{+0.10}$
6205		$\rm 1.68_{-0.00}^{+0.00}$
6218	$-{\bf0.1\pm0.2}$	$\rm 1.44_{-0.11}^{+0.09}$
6254	$1.1\pm 0.3$	$\rm 1.59_{-0.07}^{+0.05}$
6341	$1.5\pm 0.3$	$\rm 1.35_{-0.15}^{+0.12}$
6362		$\rm0.85_{-0.21}^{+0.15}$
6656	${\bf 1.4\pm0.2}$	$\rm 1.67_{-0.04}^{+0.01}$
6712	$-{\bf0.9\pm0.2}$	$\rm0.87_{-0.24}^{+0.24}$
6779		$\rm0.70_{-0.37}^{+0.63}$
6809	$1.3\pm 0.3$	$\rm 1.44_{-0.06}^{+0.04}$
6934		$\rm 1.68_{-0.02}^{+0.00}$
7089		$\rm 1.68_{-0.00}^{+0.00}$

Listed are the cluster NGC numbers (first column), observed MF slopes from De Marchi et al. (2007) (second column), and predicted MF slopes (third column). The observed low-mass MF slope of clusters representing global MFs from multi-mass Michie-King models are denoted in boldface, while the other values designate local values close to the half-mass radius (see text). The standard errors on $\alpha _{\rm obs}$ is are $\sigma_\alpha=0.2$ for the global MFs and $\sigma_\alpha=0.3$ for the other values (De Marchi, private communication).

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