  We recall evidence that long gamma-ray bursts (GRBs) have binary progenitors
and give new examples. Binary-driven hypernovae (BdHNe) consist of a
carbon-oxygen core (CO$_{\rm core}$) and a neutron star (NS) companion. For
binary periods $\sim 5$ min, the CO$_{\rm core}$ collapse originates the
subclass BdHN I characterized by: 1) an energetic supernova (the "SN-rise"); 2)
a black hole (BH), born from the NS collapse by SN matter accretion, leading to
a GeV emission with luminosity $L_{\rm GeV} = A_{\rm GeV}\,t^{-\alpha_{\rm
GeV}}$, observed only in some cases; 3) a new NS ($\nu$NS), born from the SN,
originating the X-ray afterglow with $L_X = A_{\rm X}\,t^{-\alpha_{\rm X}}$,
observed in all BdHN I. We record $378$ sources and present for four prototypes
GRBs 130427A, 160509A, 180720B and 190114C: 1) spectra, luminosities, SN-rise
duration; 2) $A_X$, $\alpha_X=1.48\pm 0.32$, and 3) the $\nu$NS spin
time-evolution. We infer a) $A_{\rm GeV}$, $\alpha_{\rm GeV}=1.19 \pm 0.04$; b)
the BdHN I morphology from time-resolved spectral analysis, three-dimensional
simulations, and the GeV emission presence/absence in $54$ sources within the
Fermi-LAT boresight angle. For $25$ sources, we give the integrated and
time-varying GeV emission, $29$ sources have no GeV emission detected and show
X/gamma-ray flares previously inferred as observed along the binary plane. The
$25/54$ ratio implies the GeV radiation is emitted within a cone of
half-opening angle $\approx 60^{\circ}$ from the normal to the orbital plane.
We deduce BH masses $2.3$-$8.9~M_\odot$ and spin $0.27$-$0.87$ by explaining
the GeV emission from the BH energy extraction, while their time evolution
validates the BH mass-energy formula.
