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Small-scale brightenings in solar atmospheric observations are amanifestation of heating and/or energy transport events. We present statisticalcharacteristics of brightenings from a new detection method applied to 1330,1400, and 2796 \AA\ IRIS slitjaw image time series. 2377 events are recordedwhich coexist in all three channels, giving high confidence that they are real.$\approx$1800 of these are spatially coherent, equating to event densities of$\sim9.7\times10^{-5}$arcsec$^{-2}$s$^{-1}$ within a$90\arcsec\times100\arcsec$ FOV over 34.5 minutes. Power Law indices estimatesare determined for total brightness ($2.78<\alpha<3.71$), maximum brightness($3.84<\alpha<4.70$), and average area ($4.31<\alpha<5.70$) distributions.Duration and speed distributions do not obey a power law. A correlation isfound between the events' spatial fragmentation, area, and duration, and a weakrelationship with total brightness, showing that larger/longer-lasting eventsare more likely to fragment during their lifetime. Speed distributions showthat all events are in motion, with an average speed of $\sim7$\kms. Theevents' spatial trajectories suggest that cooler 2796 \AA\ events tend toappear slightly later, and occupy a different position/trajectory to the hotterchannel results. This suggests that either many of these are impulsive eventscaused by reconnection, with subsequent rapid cooling, or that the triggeringevent occurs near the TR, with a subsequent propagating disturbance to cooleratmospheric layers. The spatial distribution of events is not uniform, withbroad regions devoid of events. A comparison of spatial distribution withproperties of other atmospheric layers shows a tentative connection betweenhigh magnetic field strength, the corona's multithermality, and high IRISbrightening activity.

A multi-wavelength analysis of small-scale brightenings observed by IRIS