Spatial extent of deep moonquake source regions: Are each of them really so confined?

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We have recently cross-correlated waveforms of every possible pair of the more than 10,000 non-impact, non-shallow-moonquake lunar seismic events detected on the long-period seismograms at each of the four stations during our eight-year observation, 1969-1977, on the lunar surface. The new analysis, which was not possible with computing facilities available 30 years ago, now makes us to question some of our earlier findings on the distribution of deep moonquakes. Deep moonquakes were discovered during the Apollo moon-landing missions, 1969-1972, and groups of nearly identical waveforms observed at near-monthly intervals led us to identify more than 100 discrete source regions at depths approximately halfway to the center of the moon. Digitally acquired data, coupled with an excellent inter-station timing accuracy, allowed us to use waveform cross-correlation to estimate relative locations of individual events within a source region decades before the technique became widely used for earthquake signals. At that time, we determined that the hypocenters of the most active group, A1, are distributed in a nearly horizontal planar region of no more than 1 km in diameter. Our new analysis combines waveform cross-correlation with single-link cluster analysis in an effort to identify possible far-side deep moonquakes, which may have escaped our previous visual identification. One of the early findings of the current analysis is that there is a continuous range of values of cross-correlation coefficients among events of any given group, sometimes with an overlap with another group. Thus, we now suspect that the limited spatial extent of the A1 source region may have been an artifact of cross-correlating only those events which were visually matched in their waveforms in our earlier analysis. This also gives us a lesson that we need to be careful how we select events for such analyses.

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