  We present an extended suite of the Auriga cosmological
gravo-magnetohydrodynamical "zoom-in" simulations of 40 Milky Way-mass halos
and 26 dwarf galaxy-mass halos run with the moving-mesh code Arepo. Auriga
adopts the $\Lambda$ Cold Dark Matter ($\Lambda$CDM) cosmogony and includes a
comprehensive galaxy formation physics model following the coupled cosmic
evolution of dark matter, gas, stars, and supermassive black holes which has
been shown to produce numerically well-converged galaxy properties for Milky
Way-mass systems. We describe the first public data release of this augmented
suite of Auriga simulations, which includes raw snapshots, group catalogues,
merger trees, initial conditions, and supplementary data, as well as public
analysis tools with worked examples of how to use the data. To demonstrate the
value and robustness of the simulation predictions, we analyse a series of
low-redshift global properties that compare well with many observed scaling
relations, such as the Tully-Fisher relation, the star-forming main sequence,
and HI gas fraction/disc thickness. Finally, we show that star-forming gas
discs appear to build rotation and velocity dispersion rapidly for $z\gtrsim 3$
before they "settle" into ever-increasing rotation-dispersion ratios
($V/\sigma$). This evolution appears to be in rough agreement with some
kinematic measurements from H$\alpha$ observations, and demonstrates an
application of how to utilise the released data.
