Very high energy γ-ray observations of the binary PSR B1259–63/SS2883 around the 2007 Periastron

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Table 2:

Datasets for the HESS campaigns on PSR B1259-63/SS2883 in 2005, 2006 and 2007.
Period	$\tau$ /[d]	$\theta$	$\phi$	t/[h]	$N_{\rm ON}$	$N_{\rm OFF}$	$\alpha$	$N_{\gamma}$	$S_{\rm Hillas}^{*}$ / $[{\rm\sigma}]$	$S_{\rm Model}^{**}/[\sigma]$
2005	386	0.47	0.31	8.3	347	6909	0.047	22.7	1.2	1.2
2006	-454	-0.48	-0.37	6.9	271	3201	0.079	18.0	1.1	0.5
2007
April	-104	-0.40	-0.084	5.3	205	2571	0.074	15.8	1.1	2.9
May	-74	-0.38	-0.060	14.6	623	7280	0.074	84.4	3.4	5.8
June	-46	-0.35	-0.037	15.5	843	8373	0.073	228.8	8.4	9.3
July	-17	-0.25	-0.014	14.4	575	6238	0.077	96.4	4.1	7.4
August	9	0.17	0.007	3.2	124	1383	0.073	22.9	2.1	0.9
2007 Total	...	...	...	52.5	2353	25633	0.074	448.7	9.5	13.2

Shown are the days relative to periastron $\tau$ , the true anomaly $\theta$ , the orbital phase (mean anomaly) $\phi$ , the livetime t, the number of ON and OFF events $N_{\rm ON}, N_{\rm OFF}$ , the background normalisation $\alpha$ and the number of excess photons $N_{\gamma}$ for the Hillas type analysis for each observation period. The significances S according to Li & Ma (1983) are shown for both analysis techniques, as outlined in the text.
$^{{\rm *}}$ Standard HESS analysis based on Hillas moments.
$^{{\rm **}}$ HESS semi-analytical model analysis used as cross check.

Source LaTeX | All tables | In the text

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