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We model the atmospheres and spectra of Earth-like planets orbiting theentire grid of M dwarfs for active and inactive stellar models with $T_{eff}$ =2300K to $T_{eff}$ = 3800K and for six observed MUSCLES M dwarfs with UVradiation data. We set the Earth-like planets at the 1AU equivalent distanceand show spectra from the VIS to IR (0.4$\mu$m - 20$\mu$m) to comparedetectability of features in different wavelength ranges with JWST and otherfuture ground- and spaced-based missions to characterize exo-Earths. We focuson the effect of UV activity levels on detectable atmospheric features thatindicate habitability on Earth, namely: H$_2$O, O$_3$, CH$_4$, N$_2$O andCH$_3$Cl.  To observe signatures of life - O$_2$/O$_3$ in combination with reducingspecies like CH$_4$, we find that early and active M dwarfs are the besttargets of the M star grid for future telescopes. The O$_2$ spectral feature at0.76$\mu$m is increasingly difficult to detect in reflected light of later Mdwarfs due to low stellar flux in that wavelength region. N$_2$O, anotherbiosignature detectable in the IR, builds up to observable concentrations inour planetary models around M dwarfs with low UV flux. CH$_3$Cl could becomedetectable, depending on the depth of the overlapping N$_2$O feature.  We present a spectral database of Earth-like planets around cool stars fordirectly imaged planets as a framework for interpreting future lightcurves,direct imaging, and secondary eclipse measurements of the atmospheres ofterrestrial planets in the HZ to design and assess future telescopecapabilities.

Effect of UV Radiation on the Spectral Fingerprints of Earth-like Planets Orbiting M dwarfs