  I use a sample of more than 120,000 stars in the solar neighbourhood with
parallaxes, magnitudes and colours estimated with unprecedented accuracy by the
second data release of the Gaia mission to derive the initial mass function of
the Galactic disc. A full-forward technique is used to take into account for
the population of unresolved binaries, the metallicity distribution, the star
formation history and their variation across the Galactic disk as well as all
the observational effects. The shape of the initial mass function is well
represented by a segmented power-law with two breaks at characteristic masses.
It has a maximum at M~0.15 Ms with significant flattening (possibly a
depletion) at lower masses and a slope of alpha=-1.34 +/- 0.07 in the range
0.25<M/Ms<1. Above 1 Ms the IMF shows an abrupt decline with a slope ranging
from alpha=-2.68 +/- 0.09 to alpha=-2.41 +/- 0.11 depending on the adopted
resolution of the star formation history.
