  We use the first publically available data from the Daniel K. Inouye Solar
Telescope (DKIST) to track magnetic connections from the solar photosphere into
the corona. We scrutinize relationships between chromospheric magnetism and
bright chromospheric, transition region and coronal plasmas. In June 2022, the
Visible Spectro-Polarimeter (ViSP) instrument targeted unipolar network within
a decaying active region. ViSP acquired rastered scans with longitudinal Zeeman
sensitivities of 0.25 Mx/cm2 (Fe I 630.2 nm) and 0.5 Mx/cm2 (Ca II 854.2 nm).
ViSP was operated in a "low" resolution mode (0.214" slit width, spectral
resolution R ~ 70,000) to produce polarization maps over a common area of 105"
x 50". Data from SDO and IRIS are combined to ask: Why is only a fraction of
emerging flux filled with heated plasma? What is the elemental nature of the
plasmas? No correlations were found between heated plasma and properties of
chromospheric magnetic fields derived from the WFA, on scales below
supergranules. Processes hidden from our observations control plasma heating.
While improved magnetic measurements are needed, these data indicate that "the
corona is a self-regulating forced system" (Einaudi et al. 2021). Heating
depends on the state of the corona, not simply on boundary conditions. Heating
models based upon identifiable bipolar fields, including cool loops, tectonics
and observable magnetic reconnection, are refuted for these regions with
unipolar chromospheric magnetic fields.
