  The (sub)millimeter radiation of solar flares is poorly understood. Without
spatial resolution, it cannot be compared easily to flare emissions in other
wavelengths. The Atacama Large Millimeter-submillimeter Array (ALMA) offers
sufficient resolution for the first time. However, used as an interferometer,
its field of view is smaller than an active region and ALMA cannot observe on
demand when a flare occurs. We use readily available large scale single-dish
ALMA observations of solar millimeter flares and compare them to well-known
features observed in other wavelengths. The properties of these other flare
emissions, correlating in space and time, may then be used to interpret the
millimeter brightenings and vice versa. The aim is to obtain reliable
associations, limited by the time and space resolution of single-dish
observations. We collected ALMA observations at 3 mm and 1 mm and searched for
millimeter brightenings during times given in a flare catalog. We found five
events with 9 or more images that can be used for comparison in time and space.
The millimeter brightenings are associated with a variety of flare features in
cool (H$\alpha$, 30.4 nm), intermediate (17.1 nm), and hot (9.4 nm) lines. In
several cases, the millimeter brightening peaked at the footpoint of a hot
flare loop. In other cases the peak coincided with the top or footpoint of an
active H{\alpha} filament. We found correlations also with post-flare loops and
tops of a hot loop, and in some cases to no features at all. The wide field of
view provided by the single-dish observations allowed for completely
overviewing the flare activity in millimeter waves for the first time. The
associated phenomena often changed during the flare in type and location, and
may explain the sometimes bewildering behavior of millimeter flare emissions
observed previously without spatial resolution.
