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M-dwarf stars are prime targets for exoplanet searches because of their closeproximity and favorable properties for both planet detection andcharacterization. However, the potential habitability and atmosphericcharacterization of these exoplanetary systems depends critically on thehistory of high-energy stellar radiation from X-rays to NUV, which driveatmospheric mass loss and photochemistry in the planetary atmospheres. With theFar Ultraviolet M-dwarf Evolution Survey (FUMES) we have assessed the evolutionof the FUV radiation, specifically 8 prominent emission lines, includingLy$\alpha$, of M-dwarf stars with stellar rotation period and age. Wedemonstrate tight power-law correlations between the spectroscopic FUVfeatures, and measure the intrinsic scatter of the quiescent FUV emissions. Theluminosity evolution with rotation of these spectroscopic features is welldescribed by a broken power-law, saturated for fast rotators, and decaying withincreasing Rossby number, with a typical power-law slope of $-2$, althoughlikely shallower for Ly$\alpha$. Our regression fits enable FUV emission lineluminosity estimates relative to bolometric from known rotation periods towithin $\sim$0.3 dex, across 8 distinct UV emission lines, with possible trendsin the fit parameters as a function of source layer in the stellar atmosphere.Our detailed analysis of the UV luminosity evolution with age further showsthat habitable zone planets orbiting lower-mass stars experience much greaterhigh-energy radiative exposure relative the same planets orbiting more massivehosts. Around early-to-mid M-dwarfs these exoplanets, at field ages, accumulateup to 10-20$\times$ more EUV energy relative to modern Earth. Moreover, thebulk of this UV exposure likely takes place within the first Gyr of the stellarlifetime.

The Far Ultraviolet M-dwarf Evolution Survey. I. The Rotational Evolution of High-Energy Emissions