  The origin of the narrow Fe-K{\alpha} fluorescence line at 6.4 keV from
active galactic nuclei has long been under debate; some of the possible sites
are the outer accretion disk, the broad line region, a molecular torus, or
interstellar/intracluster media. In February-March 2016, we performed the first
X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS)
onboard the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275
at the center of the Perseus cluster of galaxies. With the high energy
resolution of ~5 eV at 6 keV achieved by Hitomi/SXS, we detected the
Fe-K{\alpha} line with ~5.4 {\sigma} significance. The velocity width is
constrained to be 500-1600 km s$^{-1}$ (FWHM for Gaussian models) at 90%
confidence. The SXS also constrains the continuum level from the NGC 1275
nucleus up to ~20 keV, giving an equivalent width ~20 eV of the 6.4 keV line.
Because the velocity width is narrower than that of broad H{\alpha} line of
~2750 km s$^{-1}$, we can exclude a large contribution to the line flux from
the accretion disk and the broad line region. Furthermore, we performed pixel
map analyses on the Hitomi/SXS data and image analyses on the Chandra archival
data, and revealed that the Fe-K{\alpha} line comes from a region within ~1.6
kpc from the NGC 1275 core, where an active galactic nucleus emission
dominates, rather than that from intracluster media. Therefore, we suggest that
the source of the Fe-K{\alpha} line from NGC 1275 is likely a low-covering
fraction molecular torus or a rotating molecular disk which probably extends
from a pc to hundreds pc scale in the active galactic nucleus system.
