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Microflares have been considered to be among the major energy input sourcesto form active solar corona. To investigate the response of the low atmosphereto events, we conducted an ALMA observation at 3 mm coordinated with IRIS andHinode observations, on March 19, 2017. During the observations, a soft X-rayloop-type microflare (active-region transient brightening) was captured usingHinode X-ray telescope in high temporal cadence. A brightening loop footpointis located within narrow field of views ALMA, IRIS slit-jaw imager, and Hinodespectro-polarimeter. Counterparts of the microflare at the footpoint weredetected in Si IV and ALMA images, while the counterparts were less apparent inC II and Mg II k images. Their impulsive time profiles exhibit the Neuperteffect pertaining to soft X-ray intensity evolution. The magnitude of thermalenergy measured using ALMA was approximately 100 times smaller than thatmeasured in the corona. These results suggest that impulsive counterparts canbe detected in the transition region and upper chromosphere where the plasma isthermally heated via impinging non-thermal particles. Our energy evaluationindicates a deficit of accelerated particles that impinge the footpoints for asmall class of soft X-ray microflares. The footpoint counterparts consist ofseveral brightening kernels, all of which are located in weak (void) magneticareas formed in patchy distribution of strong magnetic flux at the photosphericlevel. The kernels provide a conceptual image in which the transient energyrelease occurs at multiple locations on the sheaths of magnetic flux bundles inthe corona.

Simultaneous ALMA-Hinode-IRIS observations on footpoint signatures of a soft X-ray loop-like microflare