* Astronomy

The crater fill is represented by a pebble-diamict to a depth of ~2.9 m.  Below this depth is a sharp transition to a well-sorted medium sand which continues, uninterrupted, to a depth of at least 5.4 m. Rare glassy fragments have been found within the diamict in the crater centre; the amorphous nature of this material has been confirmed by XRD and polarising light microscopy. The glass fragments have an amber colour in transmitted light and range from <0.1 to 0.5 cm diameter. Glass has not been observed at a depth greater than ~3.1 m. We interpret the ~2.9 m transition, represented by a change in sediment from diamict to sand, to be near to the base of the transient crater.  The presence of glass to a depth of 3.1 m is consistent with this interpretation. Two radiocarbon ages of 1130 ± 25 and 1080 ± 25 14C yr BP (UCIAMS 40058 and 40059, respectively) were obtained on charcoal from the A-horizon of a paleosol buried by impact ejecta.  These data provide a concordant maximum age for the overlying ejecta of ca. 880-990 AD, indicating the impact event likely occurred within the last thousand years.

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Title: A GEOLOGIC OVERVIEW OF THE LATE HOLOCENE WHITECOURT METEORITE IMPACT CRATER
Authors: R. S. Kofman, C. D. K. Herd, E. L. Walton, D. G. Froese, E. P. K. Herd

Small impact events resulting in simple impact structures <100 m in diameter are common features recorded on the solid surfaces in our Solar System. Such structures are rare in Earths impact cratering record; most are typically heavily modified by subsequent erosion or are often found in remote locations. The recently discovered Whitecourt Meteorite Impact Crater (WMIC) provides significant contrast in that it is both well preserved and easily accessible. The level of preservation, age (<1.13 ka) and associated meteorite fragments suggest that this site will provide considerable data for the improvement of current models for similar structures.

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