  The goal is to compare the intricate details of the magnetic and flow fields
around two solar pores, where one is part of an active region and the other is
an isolated pore, with a secondary goal of demonstrating the scientific
capabilities of the GRIS IFU. Two pores were observed with the HiFI and the
GRIS IFU at the GREGOR solar telescope on 29 May and 6 June 2019. The GRIS IFU
mosaics provide spectropolarimetric data for inversions of the Ca I 1083.9 nm
and Si I 1082.7 nm spectral lines, covering the deep and upper photosphere. The
t-SNE machine learning algorithm is employed to identify different classes of
Si I Stokes-V profiles. The LCT technique derives horizontal proper motions
around the pores. Both pores contain a thin light bridge, are stable during the
observations, and never develop a penumbra. The isolated pore is three times
smaller and significantly darker than the active-region pore, which is not
predicted by simulations. The LCT maps show inflows around both pores, with
lower velocities for the isolated pore. Both pores are embedded in the
photospheric LOS velocity pattern of the granulation but filamentary structures
are only visible in the chromospheric LOS maps of the active-region pore. The
t-SNE identifies five clusters of Si I Stokes-V profiles, revealing an
`onion-peel' magnetic field structure, despite the small size of the pores. The
core with strong vertical magnetic fields is surrounded by concentric layers
with lower and more inclined magnetic fields. The active-region pore shows some
signatures of increased interaction between plasma motions and magnetic fields,
which can be considered as early signs of penumbra formation. However, similar
physical properties prevail for smaller pores. A statistically meaningful
sample of different pore sizes and morphologies is required to distinguish
between active-region and isolated pore formation mechanisms.
