  GRB 190114C is the first gamma-ray burst detected at Very High Energies (VHE,
i.e. >300 GeV) by the MAGIC Cherenkov telescope. The analysis of the emission
detected by the Fermi satellite at lower energies, in the 10 keV -- 100 GeV
energy range, up to ~ 50 seconds (i.e. before the MAGIC detection) can hold
valuable information. We analyze the spectral evolution of the emission of GRB
190114C as detected by the Fermi Gamma-Ray Burst Monitor (GBM) in the 10 keV --
40 MeV energy range up to ~60 sec. The first 4 s of the burst feature a typical
prompt emission spectrum, which can be fit by a smoothly broken power-law
function with typical parameters. Starting on ~4 s post-trigger, we find an
additional nonthermal component, which can be fit by a power law. This
component rises and decays quickly. The 10 keV -- 40 MeV flux of the power-law
component peaks at ~ 6 s; it reaches a value of 1.7e-5 erg cm-2 s-1. The time
of the peak coincides with the emission peak detected by the Large Area
Telescope (LAT) on board Fermi. The power-law spectral slope that we find in
the GBM data is remarkably similar to that of the LAT spectrum, and the GBM+LAT
spectral energy distribution seems to be consistent with a single component.
This suggests that the LAT emission and the power-law component that we find in
the GBM data belong to the same emission component, which we interpret as due
to the afterglow of the burst. The onset time allows us to estimate the initial
jet bulk Lorentz factor Gamma_0 is about 500, depending on the assumed
circum-burst density.
