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Table 1:

Results from long-term HESS observations of PKS 2005-489.

Dark
MJD MJD Time On Off $\alpha$ Excess Sig I(>400 GeV)a Crabb $\chi ^2$  (NDFc) P($\chi ^2$)c
period first last [h]         [$\sigma $] [10-12 cm-2 s-1] %    
06/2004 53171 53185 8.1 678 5877 0.0919 138 5.4 $2.64\pm0.50$ 3.0 7.2  (10) 0.71
07/2004 53199 53205 1.5 105 985 0.0909 15 1.5 $1.06\pm1.18$ 1.2 1.4  (1) 0.75
09/2004 53255 53268 5.6 342 3171 0.0916 52 2.8 $1.89\pm0.78$ 2.1 2.1  (5) 0.84
10/2004 53285 53292 9.0 569 5065 0.0916 105 4.5 $2.58\pm0.62$ 2.9 1.5  (4) 0.83
07/2005 53582 53595 9.4 573 4504 0.0908 164 7.3 $3.56\pm0.67$ 4.0 9.2  (9) 0.42
08/2005 53609 53618 5.1 286 2159 0.0989 73 4.5 $2.86\pm0.93$ 3.2 4.6  (4) 0.33
09/2005 53639 53646 18.1 1072 9125 0.0928 225 7.1 $2.93\pm0.46$ 3.3 13.1  (6) 0.041
06/2006 53908 53909 1.3 127 824 0.0938 50 4.9 $4.72\pm1.32$ 5.3 0.0  (1) 0.97
07/2006 53938 53940 4.4 397 2927 0.0901 133 7.3 $4.33\pm0.70$ 4.8 1.3  (2) 0.52
08/2006 53967 53977 8.4 500 4261 0.0913 111 5.1 $2.74\pm0.57$ 3.1 15.1  (7) 0.035
09/2006 53995 54002 7.4 405 4116 0.0920 26 1.3 $1.31\pm0.58$ 1.5 6.0  (5) 0.30
06/2007 54264 54270 5.3 333 3006 0.0924 55 3.1 $1.02\pm0.60$ 1.1 1.9  (6) 0.93
07/2007 54291 54304 4.4 309 2412 0.0964 76 4.5 $2.51\pm0.70$ 2.8 15.2  (8) 0.056
08/2007 54321 54329 1.8 93 849 0.0977 10 1.0 $0.52\pm0.92$ 0.6 2.9  (3) 0.41
09/2007 54345 54345 0.5 11 114 0.1000 0 -0.1 <6.60d <7.4 - -

2004
53171 53292 24.2 1694 15098 0.0917 310 7.7 $2.37\pm0.33$ 2.6 2.0  (3) 0.57
2005 53582 53646 32.6 1931 15785 0.0930 462 11.0 $3.09\pm0.35$ 3.5 0.6  (2) 0.73
2006 53908 54002 21.5 1429 12128 0.0914 320 8.8 $2.84\pm0.34$ 3.2 13.5  (3) 0.0037
2007 54264 54345 12.0 746 6381 0.0947 141 5.3 $1.50\pm0.40$ 1.7 3.8  (3) 0.28

Total
53171 54345 90.3 5800 49392 0.0924 1233 16.7 $2.57\pm0.18$ 2.9 10.2  (3) 0.016

Notes. (a) The integral flux above 400 GeV is calculated using the excess of events above an energy threshold, which differs slightly from the observed excess. The quoted error is statistical only and the 20% systematic error on the observed flux is not shown. (b) The percentage is calculated relative to the HESS Crab Nebula flux above 400 GeV (Aharonian et al. 2006a). (c) The $\chi ^2$, degrees of freedom (NDF), and corresponding $\chi ^2$ probability P($\chi ^2$) are given for fits of a constant to I(>400 GeV) binned nightly within a dark period, or monthly within a year, or yearly within the total. (d) The upper limit is calculated at a 99.9% confidence level (Feldman & Cousins 1998).


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