  The impact flux over the last 3 Ga in the inner Solar System is commonly
assumed to be constant through time. However, asteroid break-up events in the
main belt may have been responsible for cratering spikes over the last ~2 Ga on
the Earth-Moon system. We investigate here the possible variations of the size
frequency distributions of impactors from the record of small craters of 521
martian impact craters larger than 20 km in diameter. We show that 49 craters
(out of the 521) correspond to the complete crater population of this size
formed over the last 600 Ma. Our results on Mars show that the flux of both
small (> 5 m) and large asteroids (> 1 km) are coupled, does not vary between
each other over the last 600 Ma. Existing data sets for large craters on the
Earth and the Moon are analyzed and compared to our results on Mars. On Earth,
we infer the formation location of a set of impact craters thanks to plate
tectonic reconstruction and show that a cluster of craters formed during the
Ordovician period, about 470 Ma ago, appears to be a preservation bias. On the
Moon, the late increase seen in the crater age signal can be due to the
uncertain calibration method used to date those impacts (i.e. rock abundance in
lunar impact ejecta), and other calibrations are consistent with a constant
crater production rate. We conclude to a coupling of the crater production rate
between kilometer-size craters and down to ~100 m in diameter in the inner
Solar System. This is consistent with the traditional model for delivering
asteroids to planet-crossing orbits: the Yarkovsky effect slowly pushes the
large debris from asteroid break-ups towards orbital resonances while smaller
debris are grinded through collisional cascades. This suggests that the
influence of past asteroid break-ups in the cratering rate for D > 100 m is
limited or inexistent.
