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The determination of extrasolar planet masses with the radial velocity (RV)technique requires spectroscopic Doppler information from the planet's hoststar, which varies with stellar brightness and temperature. We analyze Dopplerinformation in spectra of F--M dwarfs utilizing empirical information fromHARPS and CARMENES, and from model spectra. We come to the conclusions that anoptical setup ($BVR$-bands) is more efficient that a near-infrared one ($YJHK$)in dwarf stars hotter than 3200\,K. We publish a catalogue of 46,480well-studied F--M dwarfs in the solar neighborhood and compare theirdistribution to more than one million stars from Gaia DR2. For all stars, weestimate the RV photon noise achievable in typical observations assuming noactivity jitter and slow rotation. We find that with an ESPRESSO-likeinstrument at an 8m-telescope, a photon noise limit of 10\,cm\,s$^{-1}$ orlower can be reached in more than 280 stars in a 5\,min observation. At4m-telescopes, a photon noise limit of 1\,m\,s$^{-1}$ can be reached in a10\,min exposure in approx.\ 10,000 predominantly sun-like stars with aHARPS-like (optical) instrument. The same applies to $\sim$3000 stars for ared-optical setup covering the $RIz$-bands, and to $\sim$700 stars for anear-infrared instrument. For the latter two, many of the targets are nearby Mdwarfs. Finally, we identify targets in which Earth-mass planets within theliquid water habitable zone can cause RV amplitudes comparable to the RV photonnoise. Assuming the same exposure times, we find that an ESPRESSO-likeinstrument can reach this limit for 1\,M$_\Earth$ planets in more than 1000stars. The optical, red-optical, and near-infrared configurations reach thelimit for 2\,M$_\Earth$ planets in approximately 500, 700, and 200 stars,respectively.

Radial velocity photon limits for the dwarf stars of spectral classes F--M