We present the first reconstruction of the star formation history for two of the most luminous M31 dwarf satellite galaxies: NGC 147 and NGC 185, using the Long Period Variable stars over 6.'4 × 6.'4 field of view of each galaxy. Long period variable stars were chosen from Lorenz et al. (2011). Theoretically, evolved stars, in Asymptotic Giant Branch (AGB) phase achieve their maximum luminosity in K-band with the wavelength of 2.2 micrometer. Maximum luminosity of a star is related to its birth ma therefore, it is possible to construct birth mass function and drive the star formation history. For NGC 185 we found a 9.5 Gyr old single star formation epoch at a rate of 0.14 M ? y followed by a relatively continuous star formation. In the case of NGC 147, one peak as old as 7 Gyr with the rate of 0.019 M ? y can be seen, which descend to lower amount with less steep in respect to NGC 185. AGB stars are also important dust factories; we fit a Spectral Energy Distribution model on observed near and mid infrared data in Lorenz et al. (2011) and Wide-Field Infrared Survey Explorer respectively, with ”Dusty” code. Therefore we are able to estimate AGB stars’ dust production rates. Carbon stars’ total rate of mass loss is 1.06 M ? y for NGC 147 and 2.89 M ? y for NGC 185.
