Flares detected in ALMA single-dish images of the Sun

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$α$, 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 Hα 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.