Table 1: Input catalogue used for the high-level analysis of the FCFOV around the expected position of 3EG J2033+4118. The sources are sorted by decreasing detection significance level in the first energy band. The last three columns provide the significance of the detection of the sources respectively in the three energy bands selected for the data analysis. In the last three columns, "-'' indicates a non detection. References to previous INTEGRAL observations of most of these sources are given below.
Source Nature Ref. $\alpha$ (J2000) $\delta$ (J2000) Status $\sigma_1$ $\sigma_2$ $\sigma_3$
Cyg X-1 HMXRB 2 19h 58m 21.7s +35$^\circ$ 12' 06'' Detected 4204 1492 480
Cyg X-3 Microquasar 5 20h 32m 26.6s +40$^\circ$ 57' 09'' Detected 1252 110 20
EXO 2030+375 Be/X-ray binary 4,6 20h 32m 15.2s +37$^\circ$ 38' 15'' Detected 177 21 -
Cyg X-2 LMXRB 7 21h 44m 41.2s +38$^\circ$ 19' 18'' Detected 65 - -
SAX J2103.5+4545 HMXRB 8 21h 03m 33.0s +45$^\circ$ 45' 00'' Detected 62 7 -
KS 1947+300 Be/X-ray binary 9 19h 49m 35.6s +30$^\circ$ 12' 31'' Detected 47 10 -
QSO B1957+405 Seyfert 1 galaxy 1 19h 59m 28.4s +40$^\circ$ 44' 02'' Detected 30 11 -
IGR J21247+5058 gamma-ray source 10 21h 24m 42.0s +50$^\circ$ 59' 00'' Detected 22 7 -
SS Cyg Dwarf nova 3 21h 42m 48.0s +43$^\circ$ 34' 36'' Detected 12 - -
IGR J21335+5105 gamma-ray source - 21h 33m 50.1s +51$^\circ$ 09' 22'' Not detected - - -
3EG J2033+4118 gamma-ray source - 20h 33m 36.0s +41$^\circ$ 19' 00'' Not detected - - -
TeV J2032+4130 gamma-ray source - 20h 32m 07.0s +41$^\circ$ 30' 30'' Not detected - - -
WR 140 Wolf-Rayet binary - 20h 20m 28.0s +43$^\circ$ 51' 16'' Not detected - - -
WR 146 Wolf-Rayet binary - 20h 35m 45.1s +41$^\circ$ 22' 44'' Not detected - - -
WR 147 Wolf-Rayet binary - 20h 36m 43.7s +40$^\circ$ 21' 07'' Not detected - - -
(1) Bassani et al. (2006); (2) Bazzano et al. (2003); (3) Bird et al. (2004); (4) Camero Arranz et al. (2005); (5) Goldoni et al. (2003); (6) Kuznetsov et al. (2003); (7) Natalucci et al. (2003); (8) Sidoli et al. (2005); (9) Tsygankov & Lutovinov (2005); (10) Walter et al. (2004).

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