  The strongest known correspondence between ALMA 3mm emission and other solar
observations is between the H-alpha line width and 3 mm brightness temperature,
while the typical 3-5min p-mode oscillations found in many chromospheric
diagnostics are often lacking from ALMA Band 3 and 6 observations. We study
these issues using a publicly available data set of weak network flux near disk
center at time SOL2017-03-17T15:42-16:45 that includes IBIS H-alpha and ALMA 3
mm data series. We confirm the correlation between the H-alpha line width and
the 3 mm temperature, but find a different slope between the two diagnostics
for hot versus cool regions, both of which are steeper than previous reports.
The origin of the two slopes is unknown, but does hold for the duration of the
observations. Spatially averaged power spectra of the IBIS data do show p-mode
oscillations while the ALMA data do not. However, removing IBIS data at times
corresponding to the ALMA calibration windows makes the averaged power spectra
for the two data series nearly identical. Spatial maps of the power integrated
over p-mode frequency bands agree well between the two data series and show the
typical pattern of magnetic shadows and halos found in many chromospheric
diagnostics. We therefore argue that the lack of observed p-modes in the ALMA
data may be predominantly due to spectral windowing induced by the timing and
duration of the calibration observations.
