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We report the analysis of simultaneous multi-wavelength data of the highenergy peaked blazar RGB J0710+591 from the LAXPC, SXT and UVIT instrumentson-board AstroSat. The wide band X-ray spectrum (0.35 -- 30 keV) is modelled assynchrotron emission from a non-thermal distribution of high energy electrons.The spectrum is unusually curved, with a curvature parameter $\beta_p \sim 6.4$for a log parabola particle distribution, or a high energy spectral index $p_2> 4.5$ for a broken power-law distribution. The spectrum shows more curvaturethan an earlier quasi-simultaneous analysis of Swift-XRT/NuSTAR data where theparameters were $\beta_p \sim 2.2$ or $p_2 \sim 4$. It has long been known thata power-law electron distribution can be produced from a region where particlesare accelerated under Fermi process and the radiative losses in accelerationsite decide the maximum attainable Lorentz factor, $\gamma_{max}$.Consequently, this quantity decides the energy at which the spectrum curvessteeply. We show that such a distribution provides a more natural explanationfor the AstroSat data as well as the earlier XRT/NuSTAR observation, makingthis as the first well constrained determination of the photon energycorresponding to $\gamma_{max}$. This in turn provides an estimate of theacceleration time-scale as a function of magnetic field and Doppler factor. TheUVIT observations are consistent with earlier optical/UV measurements andreconfirm that they plausibly correspond to a different radiative componentthan the one responsible for the X-ray emission.

Unravelling the unusually curved X-ray spectrum of RGB J0710+591 using AstroSat observations