  This work aims to characterize precisely and systematically the non-thermal
characteristics of the electron Velocity Distribution Function (eVDF) in the
solar wind at 1 au using data from the Wind spacecraft. We present a
comprehensive statistical analysis of solar wind electrons at 1 au using the
electron analyzers of the 3D-Plasma instrument on board Wind. This work uses a
sophisticated algorithm developed to analyze and characterize separately the
three populations - core, halo and strahl - of the eVDF up to 2 keV. The eVDF
data are calibrated using independent electron parameters obtained from the
quasi-thermal noise around the electron plasma frequency measured by the
Thermal Noise Receiver. The code determines the respective set of total
electron, core, halo and strahl parameters through non-linear least-square fits
to the measured eVDF, taking properly into account spacecraft charging and
other instrumental effects. We use four years, ~ 280000 independent
measurements of core, halo and strahl parameters to investigate the statistical
properties of these different populations in the solar wind. We discuss the
distributions of their respective densities, drift velocities, temperature, and
temperature anisotropies as functions of solar wind speed. We also show
distributions with solar wind speed of the total density, temperature,
temperature anisotropy and heat flux, as well as those of the proton
temperature, proton-to-electron temperature ratio, proton and electron beta.
Intercorrelations between some of these parameters are also discussed. The
present dataset represents the largest, high-precision, collection of electron
measurements in the pristine solar wind at 1~AU. It provides a new wealth of
information on electron microphysics. Its large volume will enable future
statistical studies of parameter combinations and their dependencies under
different plasma conditions.
