https://www.ucl.ac.uk/~ucfbpve/papers/VermeeschEPSL2004.pdf

How many grains are needed for a provenance study

https://www.boulder.swri.edu/~bottke/Reprints/Bottke_Icarus_2005_175_111-146_Fossil_Main_Belt.pdf

The fossilized size distribution of the main asteroid belt

https://www.boulder.swri.edu/~bottke/Reprints/Bottke_Icarus_2005_179_63-94_Linking_Collision_Dynamics_MB.pdf

Linking the collisional history of the main asteroid belt to its dynamical excitation and depletion

The Moon is exceptional and important because it is the only planetary body besides the Earth for which we have both a detailed stratigraphic history and datable rock samples that can be related to specific geomorphologic units (Fig. 5.1⇓). The Moon has preserved much of its magmatic and impact record of at least the last 4 billion years. While its endogenic history is of great interest for the fundamentals of planetary interiors and surfaces, the Moon has become a calibration plate for the cratering record of the Earth-Moon system, and by extrapolation, of the entire inner solar system if one assumes a heliocentric origin for impactor populations. These populations range from asteroids through long and short period comets to interplanetary dust, and cover a size range from hundreds of kilometers to micrometers.



 Figure 5.1. 
Telescopic view of the nearside of the Earth’s Moon with landing sites of the Apollo and Luna missions.



This chapter reviews the presently available data sets in support of this paradigmatic assumption, as follows: (1) the phenomenology of lunar impact craters, (2) the terrestrial record of the impact cratering process and the interpretation of terrestrial impactites as far as this “ground truth” is relevant for the interpretation of lunar impact craters and datable lunar impact breccias and melt rocks, (3) the theory and numerical simulation of the cratering process and the characteristics of the Earth-Moon crossing population of impactors (asteroids and comets), (4) the principles of relative age dating of lunar surface units and the general lunar stratigraphy, (5) the stratigraphic significance and ages of lunar samples (impactites and basalts) and, based on this data set, the absolute ages of lunar surface units, (6) the cratering rate of the Moon as a function of time, and (7) the time calibration of this cratering rate based on the …

http://www.planetary.brown.edu/planetary/geo2810/papers/Stoffler_etal_2006.pdf

Cratering History and Lunar Chronology

Lunar meteorites represent a more random sampling of lunar material than the Apollo or Luna collections and, as such, lunar meteorite impact melt ages are the most important data in nearly 30 years with which to reexamine the lunar cataclysm hypothesis. Within the lunar meteorite breccias MAC 88105, QUE 93069, DaG 262, and DaG 400, seven to nine different impact events are represented with 40Ar-39Ar ages between 2.76 and 3.92 billion years ago (Ga). The lack of impact melt older than 3.92 Ga supports the concept of a short, intense period of bombardment in the Earth-moon system at approximately 3.9 Ga. This was an anomalous spike of impact activity on the otherwise declining impact- frequency curve.

https://science.sciencemag.org/content/sci/290/5497/1754.full.pdf

Support for the Lunar Cataclysm Hypothesis from Lunar Meteorite Impact Melt Ages

Lunar spherules are small glass beads that are formed mainly as a result of small impacts on the lunar surface; the ages of these impacts can be determined by the 40 Ar/ 39 Ar isochron technique. Here, 155 spherules separated from 1 gram of Apollo 14 soil were analyzed using this technique. The data show that over the last ∼3.5 billion years, the cratering rate decreased by a factor of 2 to 3 to a low about 500 to 600 million years ago, then increased by a factor of 3.7 ± 1.2 in the last 400 million years. This latter period coincided with rapid biotic evolutionary radiation on Earth.

https://science.sciencemag.org/content/sci/287/5459/1785.full.pdf

Lunar Impact History from 40Ar/39Ar Dating of Glass Spherules

Solar system impact rates back to about 3.5 Ga have been determined by measuring the ages of 155 individual lunar spherules from the Apollo 14 lunar mission. Statistical analysis shows that most (>90%) of these spherules come from different craters. The distribution of spherule ages shows a gradually decreasing rate of impacts from 3.5 Ga, to a low about 0.5 Ga, followed by a sharp increase by a factor of 3.7 ± 1.2 in the last 0.4 Gyr.

Solar System Impact Rates Measured from Lunar Spherule Ages

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Lunar Impact History from 40Ar/39Ar Dating of Glass Spherules

Solar System Impact Rates Measured from Lunar Spherule Ages