**Table 1:** Properties of the OGLE-fields and the number of detected eclipsing binaries.
BUL_SC	l	b	Total^a	Variable^b	$A_{\rm V}$ ^c	EBs^d
1	1.08	-3.62	730	4597	1.68 / 1.49	77
2	2.23	-3.46	803	5279	1.55 / 1.65	70
3	0.11	-1.93	806	8393	2.89	130
4	0.43	-2.01	774	9096	2.59 / 2.94	146
5	-0.23	-1.33	434	7257	5.73 / - / 4.13	39
6	-0.25	-5.70	514	3211	1.37	41
7	-0.14	-5.91	463	1618	1.33 / 1.28	21
8	10.48	-3.78	402	2331	2.14	29
9	10.59	-3.98	330	1847	2.08	18
10	9.64	-3.44	458	2499	2.23	36
11	9.74	-3.64	426	2256	2.27	25
12	7.80	-3.37	535	3476	2.29 / 2.20	36
13	7.91	-3.58	570	3084	2.06 / 1.82	41
14	5.23	2.81	619	4051	2.49	83
15	5.38	2.63	601	3853	2.77	41
16	5.10	-3.29	700	4802	2.15 / 2.23	48
17	5.28	-3.45	687	4690	1.94 / 2.29	46
18	3.97	-3.14	749	5805	1.83	78
19	4.08	-3.35	732	5255	2.74	61
20	1.68	-2.47	785	5910	1.94 / 2.02	119
21	1.80	-2.66	883	7449	1.83 / 1.78	116
22	-0.26	-2.95	715	5589	2.74	91
23	-0.50	-3.36	723	4815	2.70	68
24	-2.44	-3.36	612	4304	2.52	68
25	-2.32	-3.56	622	3046	2.34	77
26	-4.90	-3.37	728	4713	1.86	76
27	-4.92	-3.65	691	3691	1.69	66
28	-6.76	-4.43	406	1472	1.64	26
29	-6.64	-4.62	492	2398	1.53	44
30	1.94	-2.84	762	6893	1.91 / 1.78	137
31	2.23	-2.94	790	4789	1.81 / 1.74	87
32	2.34	-3.14	797	5007	1.61 / 1.82	99
33	2.35	-3.66	739	4590	1.70 / 1.82	44
34	1.35	-2.40	961	7953	2.52 / 2.32	127
35	3.05	-3.00	771	5169	1.84 / 2.20	64
36	3.16	-3.20	873	8805	1.62 / 1.52	85
37	0.00	-1.74	664	8367	3.77	119
38	0.97	-3.42	710	5072	1.83 / 1.94	119
39	0.53	-2.21	784	7338	2.63 / 2.70	144
40	-2.99	-3.14	631	4079	2.94	48
41	-2.78	-3.27	603	4035	2.65	55
42	4.48	-3.38	601	4360	2.29	67
43	0.37	2.95	474	3351	3.67	34
44	-0.43	-1.19	319	7836	6.0 / - / 6.00	32
45	0.98	-3.94	627	2262	1.64 / 1.53	4
46	1.09	-4.14	552	2057	1.71 / 1.65	3
47	-11.19	-2.60	301	1152	2.60	7
48	-11.07	-2.78	287	973	2.35	9
49	-11.36	-3.25	251	826	2.09	6
Total			30 490	221 701		3053

^a Total number of objects detected in the field. From Udalski et al. (2002), in units of 10³ objects.
^b Total number of candidate variable stars. From Wozniak et al. (2002).
^c Visual extinction. From Sumi (2004), except for SC44, where $A_{\rm V}$ = 6.0 has been adopted based on the proximity to C5. The second value - when listed - comes from Popowski et al. (2003). The third value - when listed - comes from Schultheis et al. (1999).
^d Total number of EBs.

Source LaTeX | All tables | In the text

	1 Introduction
	2 The data sets
	3 Analysis of the lightcurve shape and selecting eclipsing binaries
	4 Results
	5 Summary
	References
	Online Material
	Appendix A: The model
	Appendix B: Newly discovered eclipsing binaries in the Magellanic Clouds