**Table 2:** List of detected sources with 2-10 keV flux $F_{\rm X}\geq 10^{-13}$ erg/s/cm².
Source ID	$F_{\rm X}$ [2-10 keV]	$L_{\rm X}$ [2-10 keV]⁽¹⁾	Rmag⁽²⁾	F $_{\rm x}$ /F $_{\rm opt}$	Comments
	erg/s/cm²	erg/s
XMMUJ053856.7-640503	$2.67\times10^{-11}$	$8.0\times10^{36}$	16.7	33	HMXB LMC X-3
XMMUJ054011.5-691953	$2.45\times10^{-11}$	$7.4\times10^{36}$			Crab-like pulsar PSR B0540-69
XMMUJ052844.9-652656	$1.30\times10^{-11}$		6.4^*	0.0012	foreground star ABDor
XMMUJ045818.0-751637	$6.06\times10^{-12}$		7.5^*	0.0016	foreground star YYMen
XMMUJ053747.4-691020	$5.39\times10^{-12}$	$1.6\times10^{36}$			Crab-like pulsar PSRJ0537-6910
XMMUJ053113.1-660707	$3.01\times10^{-12}$	$9.0\times10^{35}$	14.0	0.31	HMXB Be EXO053109-6609
XMMUJ052402.1-701108	$2.08\times10^{-12}$				AGN RX J0524.0-7011
XMMUJ043831.4-681203	$8.88\times10^{-13}$	$2.7\times10^{35}$
XMMUJ053844.2-690608	$8.35\times10^{-13}$	$2.5\times10^{35}$			W-R stars (?) in R136
XMMUJ053011.3-655123	$6.59\times10^{-13}$	$2.0\times10^{35}$	14.7	0.13	HMXB Be (?) 272s pulsar⁽³⁾
XMMUJ050550.2-675018	$5.80\times10^{-13}$	$1.7\times10^{35}$	17.6	1.5
XMMUJ053115.4-705350	$5.25\times10^{-13}$	$1.6\times10^{35}$	13.8	0.043
XMMUJ053218.6-710746	$4.28\times10^{-13}$	$1.3\times10^{35}$	17.9	1.6
XMMUJ053833.9-691157	$3.65\times10^{-13}$	$1.1\times10^{35}$	17.8	1.3
XMMUJ050026.6-750449	$3.50\times10^{-13}$	$1.1\times10^{35}$	18.2	1.7
XMMUJ052847.3-653956	$2.70\times10^{-13}$	$8.1\times10^{34}$
XMMUJ045208.7-705652	$2.33\times10^{-13}$	$7.0\times10^{34}$
XMMUJ045637.9-751015	$2.06\times10^{-13}$	$6.2\times10^{34}$	18.3	1.1
XMMUJ054134.7-682550	$2.04\times10^{-13}$	$6.1\times10^{34}$	14.0	0.020
XMMUJ052312.9-701531	$1.94\times10^{-13}$	$5.8\times10^{34}$
XMMUJ050526.6-674313	$1.91\times10^{-13}$		10.8⁽⁴⁾	0.0011	foreground star GSC 9161.1103
XMMUJ053528.5-691614	$1.89\times10^{-13}$	$5.7\times10^{34}$			SNR SN1987A
XMMUJ054151.2-682609	$1.75\times10^{-13}$	$5.3\times10^{34}$
XMMUJ045244.2-704821	$1.71\times10^{-13}$	$5.1\times10^{34}$
XMMUJ050833.2-685427	$1.70\times10^{-13}$	$5.1\times10^{34}$
XMMUJ052403.1-673606	$1.67\times10^{-13}$	$5.0\times10^{34}$	18.3	0.91
XMMUJ053041.1-660535	$1.66\times10^{-13}$	$5.0\times10^{34}$	18.2	0.83
XMMUJ053810.0-685658	$1.58\times10^{-13}$	$4.7\times10^{34}$
XMMUJ052947.7-655643	$1.51\times10^{-13}$	$4.5\times10^{34}$	14.8	0.033	HMXB Be/X transient RX J0529.8-6556
XMMUJ045219.8-684151	$1.49\times10^{-13}$	$4.5\times10^{34}$
XMMUJ053734.9-641012	$1.46\times10^{-13}$	$4.4\times10^{34}$
XMMUJ053909.8-640310	$1.33\times10^{-13}$	$4.0\times10^{34}$
XMMUJ051832.5-693521	$1.32\times10^{-13}$	$4.0\times10^{34}$
XMMUJ051747.0-685458	$1.32\times10^{-13}$	$4.0\times10^{34}$
XMMUJ051003.9-671858	$1.31\times10^{-13}$	$3.9\times10^{34}$
XMMUJ054237.8-683205	$1.29\times10^{-13}$	$3.9\times10^{34}$
XMMUJ050736.6-684752	$1.23\times10^{-13}$	$3.7\times10^{34}$
XMMUJ053257.7-705113	$1.23\times10^{-13}$	$3.7\times10^{34}$	19.0^*	1.3
XMMUJ052422.4-672020	$1.22\times10^{-13}$	$3.7\times10^{34}$
XMMUJ052353.7-672824	$1.21\times10^{-13}$	$3.6\times10^{34}$
XMMUJ054212.6-692442	$1.19\times10^{-13}$	$3.6\times10^{34}$	19.3^*	1.6
XMMUJ054543.2-682528	$1.17\times10^{-13}$	$3.5\times10^{34}$
XMMUJ050048.6-750653	$1.15\times10^{-13}$	$3.5\times10^{34}$
XMMUJ053632.6-655644	$1.14\times10^{-13}$	$3.4\times10^{34}$
XMMUJ045137.0-710210	$1.14\times10^{-13}$	$3.4\times10^{34}$
XMMUJ053841.7-690514	$1.03\times10^{-13}$	$3.1\times10^{34}$			W-R stars (?) in R140
XMMUJ052558.0-701107	$1.03\times10^{-13}$		11.0	0.00068	foreground star, K2IV-Vp, RS CVn
XMMUJ052952.9-705850	$1.02\times10^{-13}$	$3.1\times10^{34}$

⁽¹⁾ Calculated assuming distance to LMC 50 kpc.
⁽²⁾ Apparent magnitude in the R-band of the optical counterpart from GSC2.2.1 catalogue (Morrison & McLean 2001), located within 3.6 arcsec from the X-ray source.
⁽³⁾ Haberl et al. (2003).
⁽⁴⁾ Apparent R-band magnitude from the USNO-B catalogue (Monet et al. 2003).

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