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Table 3:

Scaling parameters of NGC 6266, 47 Tuc, M 28, M 4, M 71, NGC 6366, M 55, and NGC 288.

(1)
(2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12)
Cluster log $\rho_0$ $r_{\rm c}$ d $M_{\rm V}$ $\Gamma $ $M_{\rm h}$ Source Background Member IDs. Referencea
  ( $L_\odot ~{\rm pc}^{-3}$) ( $^{\prime\prime}$) (kpc)                
NGC 6266 5.14 10.8 6.9 -9.19 37.07 8.24 51 2-3 48-49 2c 1, 2, 3
47 Tuc 4.81 24.0 4.5 -9.4 24.91 10.0 79 $\sim $16 $63\pm4$ 53-63 4
M 28 4.75 14.4 5.6 -8.33 11.29 3.73 26 2-3 23-24 2c 1, 5
M 4 4.01 49.8 1.73 -6.9 1.0 1.0 6 1-3 3-5 5 1, 6
M 71 3.05 37.8 4.0 -5.6 0.11 0.30 14 1-7 10 $\pm$ 3 4-9 7
NGC 6366 2.42 109.8 3.6 -5.77 0.08 0.33 5 2-5 1+2-1 $\sim $1 8
M 55 2.15 169.8 5.3 -7.6 0.18 1.82 16 5-12 8+3-4 2-4 8
NGC 288b 1.80 85.0 8.4 -6.7 0.03 0.83 11 4-11 4+3-4 2-5 9

Notes. Columns 2-5 give the values for central density ($\rho_0$), core-radius ($r_{\rm c}$), distance (d), and absolute visual magnitude ($M_{\rm V}$) come from Harris (1996, version of February 2003). For M 4, the values of $\rho_0$ and $M_{\rm V}$ are computed for the distance and reddening of Richer et al. (1997). Columns 6 and 7 are the collision number, which is computed from $\Gamma \equiv \rho_0^{1.5}\
r_{\rm c}^2$ and the half mass from $M_{\rm h} \propto
10^{-0.4M_V}$ (Kong et al. 2006). Values for $\Gamma $ and $M_{\rm h}$ are normalized to the value of M 4. Column 8 shows the total number of sources detected within the half-mass radius. Column 9 is the number of expected fore/background sources. Column 10 gives the number of expected cluster members plus error. Column 11 shows the number of X-ray sources (with $L_{\rm X,0.5{-}6.0~keV} > 4\times10^{30}$ erg s-1) which have optical or/and radio counterparts associated with the cluster, or spectrally confirmed qLMXBs. The last column gives the reference paper. These globular clusters are ordered on the central density.
(a) For each cluster, the basic data for this table were extracted from: 1. Pooley et al. (2003); 2. Cocozza et al. (2008); 3. Trepl (2007); 4. Heinke et al. (2005); 5. Becker et al. (2003); 6. Bassa et al. (2004); 7. this work; 8. Bassa et al. (2008); 9. Kong et al. (2006). (b) NGC 288 was not observed long enough to reach this luminosity limit of $L_{\rm X} \sim 4.0 \times 10^{30}$ erg s-1 in the 0.5-6.0 keV range. Its limiting luminosity is $\sim $ $ 5.7 \times 10^{30}$ erg s-1. However, we keep this cluster's data, as a lower limit, since we have so few constraints on low-density clusters. (c) No information about the optical counterparts to X-ray sources.


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