The flux of cosmic ray electrons and positrons (e- and e+) is now measured with unprecedented statistics and precision up to energies of few tens of TeV. Recently, a cut-off in the inclusive (e- + e+) flux has been observed by the DAMPE experiment at 0.9 TeV, while an excess of e+ with respect to standard cosmic ray models has been confirmed in AMS-02 data starting from few hundreds of GeV. The theoretical interpretation of the observed fluxes is still under debate. Different source models have been proposed, including Supernova Remnants, Pulsar Wind Nebulae and most intriguingly the annihilation or decay of dark matter particles in the halo of our Galaxy. Because of intense radiative losses in the interstellar medium, high energy e- and e+ are an incredible window on Earth's local Galactic environment, in particular on the properties of local and discrete sources. In this seminar I will discuss our current understanding of the sources and propagation of Galactic e- and e+ with a special focus on the emission coming from known Galactic sources. In particular, I will show the constraints on local sources such as Supernova Remnants and Pulsar Wind Nebulae obtained from a multi-messenger analysis that combines the most recent cosmic e- and e+ data on the fluxes and dipole anisotropies with the observations of the source candidates from radio to gamma-rays energies.