Spatial morphology and emission measure distribution of the selected EUV bursts. The top segment of each panel shows maps covering the burst in five of the six AIA EUV filters (in inverted color), and the lower right tile presents the cotemporal HMI line-of-sight magnetic field map, saturated at ±30 G. The field of view is about 11.4″ × 11.4″. The AIA 171 Å and 193 Å time series from the green box regions are plotted in the respective panels in Figs. 4a–d. The spatial coordinates of the green box are listed at the left side of the top segment. The bottom segment in each panel is a plot of the DEM as a function of temperature derived using a regularized inversion technique (solid black; method-I; Hannah & Kontar 2012) and a sparse inversion technique (solid blue; method-II; Cheung et al. 2015) by combining the AIA EUV emission in the green box regions from the six filters. The vertical black bars are the 1σ errors in DEMs, and the horizontal black bars are associated with the energy resolution of the regularized inversion technique. The dashed curve is the quiet-Sun DEM profile based on Hinode observations (Brooks et al. 2009), available in the CHIANTI atomic database (Dere et al. 1997, 2019). The emission-weighted temperature of the plasma (in MK) and thermal energy content of the burst (in erg) are quoted. The time stamp corresponds to the snapshots in the top segment (same as the peak time identified with the vertical line in Fig. 4). These bursts are detected in the 2011 dataset. See Sect. 3.3 for details.