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Figure 1:
Main figure: distribution of background-subtracted ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 2:
Significance sky-map centred on the position of PSR B1259-63 for
the HESS February data. The excess ![]() ![]() ![]() ![]() |
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Figure 3:
Differential energy spectrum ![]() ![]() ![]() |
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Figure 4:
Differential energy spectra of ![]() ![]() |
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Figure 5:
VHE ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 6:
Sketch of the orbit of PSR B1259-63 with respect to the line of
sight (adapted from Johnston et al. 1999). The pulsar approaches the
equatorial disk prior to periastron while it is "behind'' the
companion star and turns towards the observer before it crosses the
disk after periastron for the second time. Note that the orientation
of the disk with respect to the orbital plane is not precisely known.
The colour gradient bars along the orbit indicate the periods of
HESS observations and show the integral VHE ![]() |
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Figure 7:
Spectral energy distribution from Kirk et al. (1999) assuming the electron
cooling to be dominated by radiative (dashed lines) or adiabatic
losses (solid lines) for a magnetic field strength of 0.32 G at an
orbital phase 12 days prior to periastron. The spectra were calculated
by Kirk et al. (1999) for different electron injection spectra with the
power law indices
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Figure 8:
Comparison of the light curves predicted by different models of VHE
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