Diurnal and annual temperature variations in some Atypical Pit Craters (APCs) on Mars may be affected by the presence of interior cave entrances (Cushing et al., 2007; Cushing et al., 2015). The purpose of this document is to publish the data collected for a Mars-analog study where topography, temperature and climate variations were recorded in 7 pit craters. The pits in this study were specifically chosen because they are morphologically comparable to martian APCs (i.e., having vertical walls, high depth-to-diameter ratios and relatively flat floors). In THEMIS thermal-infrared spacecraft observations of Mars (Christensen et al., 2004), APC floors exhibit strongly damped diurnal temperature variations when compared with those of common (bowl-shaped) pit craters, and are warmer in pre-dawn thermal-infrared spacecraft observations (Lopez et al., 2012) by up to 53 K (Cushing et al., 2015). Our primary purpose for recording temperatures in the Kīlauea pits was to determine whether terrestrial analogs exhibit similarly damped temperature variations, and if so, to determine whether atmospherically connected cave systems can influence this effect. When atmospherically connected to pit craters, we suspect that subsurface microclimates (i.e., caves) will have a stabilizing influence and behave as thermal capacitors—effectively damping the pit’s diurnal temperature amplitude and causing a slight temporal phase delay (e.g., Wynne et al., 2008). Comparing these specific, time-dependent thermal signatures in pits with and without cave entrances may reveal characteristic thermal distinctions between the two cases. Results from such an analysis will aid in developing tools to evaluate extraterrestrial pit craters for the presence of cave entrances.