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Stars stripped of their envelope through interaction in a binary aregenerally not considered when accounting for ionizing radiation from stellarpopulations, despite the expectation that stripped stars emit hard ionizingradiation, form frequently and live 10-100 times longer than single massivestars. We compute the first grid of spectral models specially made for starsstripped in binaries for a range of progenitor masses (2-20$M_{\odot}$) andmetallicities covering a wide range.  For stripped stars with masses between 0.3-7$M_{\odot}$, we find higheffective temperatures (20-100 kK, increasing with mass), small radii(0.2-1$R_{\odot}$) and high bolometric luminosities, comparable to that oftheir progenitor before stripping. The spectra show a continuous sequence thatnaturally bridges subdwarf-type stars and Wolf-Rayet like spectra. Forintermediate masses we find hybrid spectral classes showing a mixture ofabsorption and emission lines. These appear for stars with mass loss rates of$10^{-8}-10^{-6}M_{\odot}$/yr, which have semi-transparent atmospheres. At lowmetallicity, substantial H-rich layers are left at the surface and we predictspectra that resemble O-type stars instead. We obtain spectra undistinguishablefrom subdwarfs for stripped stars with masses up to 1.7$M_{\odot}$, whichquestions whether the widely adopted canonical value of 0.47$M_{\odot}$ isuniformly valid.  Increasing the observed sample of stripped stars will provide necessary testsfor the physics of interaction, internal mixing and stellar winds. Weinvestigate the feasibility to detect stripped stars next to an opticallybright companion and recommend searches for their UV excess and possibleemission lines, most notably HeII4686 in the optical and HeII1640 in the UV.Our models are publicly available for further investigations or inclusion inspectral synthesis simulations.

Spectral models for binary products: Unifying Subdwarfs and Wolf-Rayet stars as a sequence of stripped-envelope stars