Table 1: Photon energy spectra and luminosity (0.2 to 10 TeV) of the VHE $\gamma $-ray emission of LS 5039 for different orbital phase intervals. The broad phase intervals INFC and SUPC encompass the inferior and superior conjunction epochs. The orbital phase $\phi $ is calculated from the ephemeris of Casares et al. (2005). The best-fit function is indicated for each phase interval. The errors quoted are statistical with systematic errors in the 10 to 15% range.
Orbital phase interval N $\Gamma$ $E_{\rm o}$ Luminosity$^\dagger$
  $\times 10^{-12}$ [ph cm-2 s-1 TeV-1]   [TeV] [erg s-1]
Fit function: \fbox{${\rm d}N/{\rm d}E = N E^{-\Gamma} \exp~(-E/E_{\rm o})$ }
INFC ( $0.45<\phi \leq 0.9$) $2.28 \pm0.10$ $1.85\pm0.06$ $8.7\pm2.0$ $1.1\times 10^{34}$
SUPC ( $\phi \leq 0.45$) and $\phi >0.9$ $0.91 \pm0.07$ $2.53\pm0.07$ - $4.2\times 10^{33}$
All Phases (time averaged) $1.85\pm0.06$ $2.06\pm0.05$ $13.0\pm4.1$ $7.8\times 10^{33}$

Power-Law fit for energies $E\leq 5$ TeV (narrow phase intervals)
0.0-0.1 0.84 $\pm $ 0.17 2.62 $\pm $ 0.23    
0.1-0.2 0.46 $\pm $ 0.21 3.08 $\pm $ 0.47    
0.2-0.3 0.81 $\pm $ 0.13 2.46 $\pm $ 0.20    
0.3-0.4 0.78 $\pm $ 0.18 2.77 $\pm $ 0.60    
0.4-0.5 1.88 $\pm $ 0.27 2.32 $\pm $ 0.17    
0.5-0.6 2.64 $\pm $ 0.20 2.04 $\pm $ 0.10    
0.6-0.7 2.20 $\pm $ 0.23 1.88 $\pm $ 0.13    
0.7-0.8 2.44 $\pm $ 0.20 1.90 $\pm $ 0.10    
0.8-0.9 2.96 $\pm $ 0.17 1.94 $\pm $ 0.08    
0.9-1.0 1.21 $\pm $ 0.25 1.84 $\pm $ 0.25    

$\dagger$ At 2.5 kpc distance.


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