  X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and
an orbital period derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s
s$^{-1}$. The extremely high value of its $\dot{P}_{\rm orb}$ is compatible
with a super-Eddington mass transfer rate from the companion star and,
consequently, an intrinsic luminosity at the Eddington limit. The source is
also an X-ray pulsar, it shows a spin frequency of 1.69 Hz and is in a spin-up
phase with a spin frequency derivative of $7.4 \times 10^{-12}$ Hz s$^{-1}$.
Assuming a luminosity at the Eddington limit, a neutron star magnetic field
strength of $B = 8 \times 10^{10}$ G is estimated. However, a direct measure of
$B$ could be obtained observing a CRSF in the energy spectrum. Analysis of
\textit{XMM-Newton} data suggested the presence of a cyclotron line at 0.73
keV, with an estimated magnetic field strength of $B=(8.8 \pm 0.3) \times
10^{10}$ G. Here we analyze the 0.3-50 keV broadband spectrum of X 1822-371
combining a 0.3-10 keV NICER spectrum and a 4.5-50 keV \textit{NuSTAR} spectrum
to investigate the presence of a cyclotron absorption line and the complex
continuum emission spectrum. The NICER spectrum confirms the presence of a
cyclotron line at 0.66 keV. The continuum emission is modeled with a
Comptonized component, a thermal component associated with the presence of an
accretion disk truncated at the magnetospheric radius of 105 km and a
reflection component from the disk blurred by relativistic effects. We confirm
the presence of a cyclotron line at 0.66 keV inferring a NS magnetic field of
$B = (7.9\pm 0.5) \times 10^{10}$ G and suggesting that the Comptonized
component originates in the accretion columns.
