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We aim to interpret future photometric and spectral measurements from theseinstruments, in terms of physical parameters of the planets, with anatmospheric model using a minimal number of assumptions and parameters.  We developed Exoplanet Radiative-convective Equilibrium Model (Exo-REM) toanalyze the photometric and spectro- scopic data of directly imaged planets.The input parameters are a planet's surface gravity (g), effective temperature(Teff ), and elemental composition. The model predicts the equilibriumtemperature profile and mixing ratio profiles of the most important gases.Opacity sources include the H2-He collision-induced absorption and molecularlines from eight compounds (including CH4 updated with the Exomol line list).Absorption by iron and silicate cloud particles is added above the expectedcondensation levels with a fixed scale height and a given optical depth at somereference wavelength. Scattering was not included at this stage.  We applied Exo-REM to photometric and spectral observations of the planetbeta Pictoris b obtained in a series of near-IR filters. We derived Teff = 1550+- 150 K, log(g) = 3.5 +- 1, and radius R = 1.76 +- 0.24 RJup (2-{\sigma} errorbars from photometric measurements). These values are comparable to those foundin the literature, although with more conservative error bars, consistent withthe model accuracy. We were able to reproduce, within error bars, the J- andH-band spectra of beta Pictoris b. We finally investigated the precision towhich the above parameter

Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to beta Pictoris b and SPHERE observations