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Fig. 6

image

Expected γ-ray luminosities Lγ,1−10 GeV of SLSNe powered by neutron stars with dipole magnetic field B and rotation period P, assuming a pair luminosity fraction ηe = 1 and an attenuation factor ξ = 0.1 (see Eq. (3)). Overlaid are the γ-ray luminosity limits derived in this work for selected individual SLSNe in black lines, and for the total joint likelihood analysis sample as a white line (Table 2), for time windows of tSN to tSN + 2 years or tSN + 1 year for CSS140222. The white dotted line indicates the limit derived for standard core-collapse SNe (Ackermann et al. 2015). The parameter-space above the line is allowed for a given source or population, modulo the scaling factor ηe ξ−1 , with ξ < 1 in any case. The high magnetic field end (B ≳ 5 × 1013 G) should be viewed with care as in the magnetar regime, ξ ≪ 1, implying less stringent constraints on the parameter space.

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