Comparison of the high-energy emission (energy flux versus energy) expected from the MSP binary systems with the sensitivities of Fermi-LAT (10 yrs – extragalactic background, see thin dashed curve, Funk et al. 2013), MAGIC (thin dotted curve, Aleksić et al. 2012) and CTA (thin dot-dashed, Bernlohr et al. 2012), for different ranges of observation angles: 0.9 ≤ cosβ ≤ 1.0 (dot-dashed, away from the companion star), 0.5 ≤ cosβ ≤ 0.6 (dotted), − 0.1 ≤ cosβ ≤ 0. (dashed), − 0.5 ≤ cosβ ≤  − 0.4 (solid), − 1.0 ≤ cosβ ≤  − 0.9 (dot-dot-dashed). The other parameters of the models have been fixed on σ = 10^-4, and v_adv = 10¹⁰ cm s^-1, and E_e is given by Eq. (7). The spectra are normalized to the X-ray fluxes observed from PSR B1957+20 (Huang et al. 2012), PSR J1023+0038 (Bogdanov et al. 2011), PSR J1810+1744 (Gentile et al. 2013). For PSR J1816+4510, the upper limit derived from the Swift data (Kaplan et al. 2012). The spectra have been calculated for the energy conversion efficiencies from pulsars to relativistic electrons estimated on 1.6 × 10^-2 (for PSR J1023+0038), 6.5 × 10^-2 (PSR J1810+1744), 5 × 10^-3 (PSR J1816+4510), and 1.8 × 10^-3 (PSR B1957+20).