**Table 3:** List of HMXB candidates
#	RA	Dec	$F_{\rm X}$ (1)	$L_{\rm X}$ (1)	m_R	V-R	$F_{\rm x}$ / $F_{\rm opt}$	Comments
			erg/s/cm^-2	erg s^-1
Likely HMXB candidates⁽³⁾
1	05 38 56.7	-64 05 03	$2.67\times10^{-11}$	$8.0\times10^{36}$	16.7	-0.2⁵	33	LMC X-3
2	05 31 13.1	-66 07 07	$3.01\times10^{-12}$	$9.0\times10^{35}$	14.0	0.23	0.31	Be/X EXO053109-6609
3	05 30 11.4	-65 51 23.4	$6.59\times10^{-13}$	$2.0\times10^{35}$	14.7	0.18	0.13	Be/X ? 272s pulsar⁽²⁾
4	05 31 15.4	-70 53 50	$5.25\times10^{-13}$	$1.6\times10^{35}$	13.6	0.1	0.038
5	05 41 34.7	-68 25 50	$2.04\times10^{-13}$	$6.1\times10^{34}$	14.0	-0.03	0.02
6	05 29 47.7	-65 56 43	$1.51\times10^{-13}$	$4.5\times10^{34}$	14.6	-0.02	0.027	Be/X transient RX J0529.8-6556
7	05 32 32.5	-65 51 41	$5.93\times10^{-14}$	$1.8\times10^{34}$	13.4	-0.36	0.0036	OB RX J0532.5-6551
8	05 20 29.4	-69 31 56	$4.05\times10^{-14}$	$1.2\times10^{34}$	14.1	0.03	0.0046	RX J0520.5-6932
9	05 31 18.2	-66 07 30	$3.42\times10^{-14}$	$1.0 \times10^{34}$	16.0	-1.3⁶	0.023
Sources of uncertain nature⁽⁴⁾
10	05 23 00.0	-70 18 32	$7.93\times10^{-14}$	$2.4\times10^{34}$	17.3	0.45	0.17	M
11	05 37 17.0	-64 12 17	$6.19\times10^{-14}$	$1.9\times10^{34}$	17.2		0.063	GSC, N
12	05 41 23.4	-69 36 34	$5.84\times10^{-14}$	$1.8\times10^{34}$	17.1		0.11	C
13	04 53 11.8	-68 39 47	$5.71\times10^{-14}$	$1.7\times10^{34}$	16.7	0.17	0.071	C
14	05 30 02.3	-71 00 46	$5.3\times10^{-14}$	$1.6\times10^{34}$	14.9		0.013	USNO-B
15	05 44 34.3	-68 28 14	$4.99\times10^{-14}$	$1.5\times10^{34}$	17.4		0.12	USNO-B
16	05 20 13.6	-69 09 42	$4.72\times10^{-14}$	$1.4\times10^{34}$	16.0		0.031	M
17	05 18 03.7	-69 01 14	$3.51\times10^{-14}$	$1.1\times10^{34}$	17.1		0.063	USNO-B
18	05 33 46.9	-70 59 15.4	$3.46\times10^{-14}$	$1.0 \times10^{34}$	14.4	0.93	0.0052	C
19	05 40 43.6	-64 01 45	$3.36\times10^{-14}$	$1.0 \times10^{34}$	17.1		0.062	C
20	05 24 15.3	-70 04 35	$2.80\times10^{-14}$	$8.4\times10^{33}$	17.0		0.024	USNO-B
21	05 27 33.0	-65 34 47	$2.77\times10^{-14}$	$8.3\times10^{33}$	16.2		0.022	M
22	05 27 02.0	-70 05 16	$2.75\times10^{-14}$	$8.3\times10^{33}$	17.4		0.063	USNO-B
23	05 23 15.2	-70 14 38	$2.35\times10^{-14}$	$7.1\times10^{33}$	16.1		0.018	USNO-B
24	05 27 02.6	-67 27 28	$2.11\times10^{-14}$	$6.3\times10^{33}$	14.4		0.0032	USNO-B, N
25	05 21 07.6	-69 03 01	$1.66\times10^{-14}$	$5.0\times10^{33}$	16.4		0.016	USNO-B
26	05 27 31.5	-65 20 34	$1.58\times10^{-14}$	$4.7\times10^{33}$	17.3		0.034	USNO-B
27	05 26 55.5	-65 20 49	$1.41\times10^{-14}$	$4.2\times10^{33}$	17.5		0.037	C
28	05 25 03.6	-70 08 16	$1.37\times10^{-14}$	$4.1\times10^{34}$	17.4		0.033	USNO-B
30 Doradus region ( $r\le4\hbox{$^\prime$ }$ )
29	05 38 44.2	69 06 08	$8.35\times10^{-13}$	$2.5\times10^{35}$				Wolf-Rayet star in R136
30	05 38 41.7	69 05 14	$1.03\times10^{-13}$	$3.1\times10^{34}$				Wolf-Rayet star in R140

(1) - 2-10 keV band; (2) - (Haberl et al. 2003); (3) - optical counterpart is consistent with being an HMXB; (4) - the optical counterpart exists, but the information is insufficient for its reliable classification; (5) - B-V color from Liu et al. (2000); (6) - B-V color.
Comments: USNO-B - counterpart in USNO-B only; GSC - counterpart in GSC only; M - multiple non-overlapping optical and/or infrared counterparts; C - ambiguous color indexes; N - non-HMXB nature is likely.

Source LaTeX | All tables | In the text

	1 Introduction
	2 Observations and data analysis
	3 Nature of X-ray sources in the field of LMC
	4 Identification of HMXB candidates
	5 HMXBs and CXB sources in the field of the LMC
	6 Propeller effect and HMXB XLF
	7 HMXBs and the age of underlying stellar population
	8 Summary
	References