Contraints on albedo and eccentricity from the secondary eclipse depth, in the case of an airless planets. The light green shaded areas are in agreement with the 131 ± 28 ppm depth measured with Spitzer/IRAC2 by D12. The right hand side plot is for an Earth-like dissipation constant σ_p; the left and middle plots are for 10^-3 × σ_p and 10^-2 × σ_p, respectively. The dotted (resp. dashed) lines indicate where reflection (resp. tidal dissipation) accounts for 10 and 50% of the planetary flux (reflection + thermal re-emission + tides = 100%). The long dashed pink vertical line represents the observational constraint on the eccentricity given by D12. Horizontal grey bars below the graphs indicate the range of eccentricities found with the dynamical simulations described in Sect. 3.2. The upper and lower bars correspond to initial orbital elements from Endl et al. (2012) and Dawson & Fabrycky (2010), respectively. The maximum and mean values of the eccentricity are indicated, as well as the minimum when larger than 5 × 10^-4. The blue areas are in agreement with the transit depth, the condition that tides accounts for more than 10% of the planetary flux and compatible with an eccentricity within the range found with the dynamical simulations. For 10^-3 × σ_p and 10^-2 × σ_p the agreement is met for simulations of Dawson & Fabrycky (2010) while for 1 × σ_p the agreement is met for Endl et al. (2012).