**Table 1:** List of XMM-Newton observations used for analysis.
Obs. ID	Target	RA	Dec	Instrument	Exposure	SFR⁽¹⁾
		J2000	J2000		ks	$M_{\odot}$ /yr
0113000501	0519-69.0	05 19 23	-69 00 52	MOS1+MOS2	25+47	$4.13\times10^{-3}$
0111130201	2E 0509.5-6734	05 09 16	-67 31 41	MOS1+MOS2	34+34	$7.77\times10^{-4}$
0062340101	2E 0453.8-6834	04 53 41	-68 31 07	MOS1+MOS2	16+16	$1.49\times10^{-3}$
0111130301	2E 0525.3-6601	05 25 13	-65 59 38	MOS1+MOS2	9.5+9.5	$1.83\times10^{-3}$
0134520701	AB Dor	05 28 35	-65 28 30	MOS1+MOS2	48+48	$2.92\times10^{-4}$
0123510101	CAL 83	05 43 33	-68 24 07	MOS1+MOS2	10+10	$1.37\times10^{-3}$
0104060101	LMC Deep field	05 31 17	-65 55 58	MOS1+MOS2	38+38	$6.35\times10^{-4}$
0109990201	DEM L71	05 05 49	-67 54 11	MOS1+MOS2	22+23	$1.30\times10^{-3}$
0109990101	LHA 120-N63A	05 35 51	-66 00 32	MOS1+MOS2	9.6+9.6	$1.38\times10^{-3}$
0094410101	LMC-2(f1)	05 42 35	-69 03 20	PN	8.8	$9.74\times10^{-3}$
0094410201	LMC-2(f2)	05 42 58	-69 28 22	PN	8.8	$5.51\times10^{-3}$
0094410401	LMC-2(f4)	05 46 48	-69 33 39	MOS1+MOS2	5.2+5.2	$4.60\times10^{-3}$
0126500101	LMC X-3	05 38 44	-64 06 11	MOS1+MOS2	20+20	$7.82\times10^{-5}$
0113000301	N103B	05 08 41	-68 43 53	MOS2	23ks	$4.52\times10^{-3}$
0089210701	N120	05 18 37	-69 37 56	MOS1+MOS2	36+36	$5.76\times10^{-3}$
0089210901	N206	05 31 51	-70 58 39	MOS1+MOS2	24+24	$3.35\times10^{-3}$
0071940101	N51D	05 26 05	-67 27 21	MOS1+MOS2	32+32	$3.37\times10^{-3}$
0127720201	Nova LMC 2000	05 24 41	-70 14 00	MOS1+MOS2	22+22	$1.34\times10^{-3}$
0113000401	PSR 0540-69.3	05 40 02	-69 21 19	MOS2	35	$2.29\times10^{-2}$
0113020201	PSR J0537-6909	05 37 57	-69 08 52	MOS1	37	$5.08\times10^{-2}$
0008020101	RX J0439.8-6809	04 39 57	-68 07 27	MOS1+MOS2	15+15	$1.83\times10^{-4}$
0089210601	SNR0450-709	04 50 26	-70 48 48	MOS1+MOS2	56+57	$6.19\times10^{-4}$
0137160201	YYMen	04 58 12	-75 15 01	MOS1+MOS2	87+87	$3.50\times10^{-4}$

⁽¹⁾ Star formation rate within the XMM-Newton FOV determined
form the FIR flux as described in Sects. 3.3 and 3.4.

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