Study of Hubble Space Telescope counterparts to Chandra X-ray sources in the globular cluster M 71

R. H. H. Huang; W. Becker; P. D. Edmonds; R. F. Elsner; C. O. Heinke; B. C. Hsieh

doi:10.1051/0004-6361/200811245

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Volume 513 (April 2010)

A&A, 513 (2010) A16

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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.	Reference^a
	( $L_\odot ~{\rm pc}^{-3}$ )	( $^{\prime\prime}$ )	(kpc)
NGC 6266	5.14	10.8	6.9	-9.19	37.07	8.24	51	2-3	48-49	2^c	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	2^c	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 288^b	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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