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Fig. 1

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Left: image of the VHE γ-ray excess (in units of γ-rays arcmin-2) from H.E.S.S. J1708−443, smoothed with a 2D Gaussian with a width σ  =  0.10°. The blue-to-red color transition is chosen to reduce the appearance of features which are not statistically significant. The white cross is located at the best-fit position of the center-of-gravity of the emission and its size represents the statistical error of the fit. The small and large dotted white circles, labeled A and C, respectively, denote the regions used for spectral analysis. The a priori defined Region B, from which the detection significance was calculated, is represented by a dotted green circle. The three regions are summarized in Table 2. The position of the pulsar PSR B1706−44, at the center of region A, is marked by a square. The inset (bottom-left corner) shows the point-spread function of the H.E.S.S. telescope array for this particular dataset, smoothed in the same manner as the excess image. Radio contours of constant intensity, as seen at 330 MHz with the Very Large Array (VLA), are shown in green. The radio data were smoothed with a Gaussian of width σ = 0.03°. The local maximum in the radio contours at the center of the image is largely due to PMN J1708−4419, an extragalactic object seen in projection (see Sect. 4.3). Right: gamma-ray excess in quadratic bins of 0.175° width. The upper number in each bin is the excess summed within this bin, and the lower number is the corresponding statistical error. The blue contours correspond to a smoothed excess of 0.14, 0.17, and 0.21 γ-rays arcmin-2, taken from the image on the left. The red-rimmed bin is centered on the pulsar position. Note the different field-of-view used in the two figures.

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