  We present a new grid of presupernova models of massive stars extending in
mass between 13 and 120 Msun, covering four metallicities (i.e. [Fe/H]=0, -1,
-2 and -3) and three initial rotation velocities (i.e. 0, 150 and 300 km/s).
The explosion has been simulated following three different assumptions in order
to show how the yields depend on the remnant mass - initial mass relation. An
extended network from H to Bi is fully coupled to the physical evolution of the
models. The main results can be summarized as follows. a) At solar metallicity
the maximum mass exploding as Red Super Giant (RSG) is of the order of 17 Msun
in the non rotating case, all the more massive stars exploding as WR stars. All
rotating models, vice versa, explode as Wolf-Rayet (WR) stars. b) The interplay
between the core He burning and the H burning shell, triggered by the rotation
induced instabilities, drives the synthesis of a large primary amount of all
the products of the CNO, not just N14. A fraction of them enriches enormously
the radiative part of the He core (and is responsible of the large production
of F) and a fraction enters the convective core leading therefore to an
important primary neutron flux able to synthesize heavy nuclei up to Pb. c) In
our scenario, remnant masses of the order of those inferred by the first
detections of the gravitational waves (GW150914, GW151226, GW170104, GW170814)
are predicted at all metallicities for none or moderate initial rotation
velocities.
