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Table 3

A few sources of the X-ray sample detected towards the Fornax dSph correlate with the 2MASS catalog.

Src FX FJ J  K
(×10-14 cgs) (×10-13 cgs)

6 0.14  ±  0.12 1.82  ±  0.20 16.12  ±  0.11 15.18  ±  0.20
10 0.18  ±  0.16 10.90  ±  0.32 14.17  ±  0.03 13.35  ±  0.04
19 0.34  ±  0.16 17.11  ±  0.43 13.68  ±  0.03 13.14  ±  0.04
40 0.57  ±  0.28 1.77  ±  0.16 16.15  ±  0.10 15.32  ±  0.19
41 0.59  ±  0.45 102.71  ±  2.30 11.74  ±  0.02 11.30  ±  0.02
46 0.69  ±  0.28 8.86  ±  0.43 14.40  ±  0.05 13.42  ±  0.10
48 0.74  ±  0.28 1.53  ±  0.20 16.30  ±  0.15 14.10  ±  0.15
75 1.42  ±  0.47 1.50  ±  0.21 16.33  ±  0.15 15.14  ±  0.18
82 1.75  ±  0.26 76.42  ±  1.70 12.06  ±  0.02 11.47  ±  0.02
84 1.87  ±  0.25 54.25  ±  1.10 12.43  ±  0.02 11.58  ±  0.02
86 2.03  ±  0.38 1.32  ±  0.22 16.46  ±  0.17 14.95  ±  0.20
102 4.25  ±  0.93 2.10  ±  0.19 15.97  ±  0.10 15.32  ±  0.20
107 9.84  ±  1.22 6.97  ±  0.48 14.66  ±  0.10 13.43  ±  0.10

Notes. Following Haakonsen & Rutledge (2009), we can try to constrain the nature of the sources by using the X-ray (in the 0.2–2.4 keV band) and NIR (J and K bands) fluxes (see text and Fig. 3 for details).

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