Table D.1.
Cyclostratigraphic data.
| dataset | Reference | T [ Ga ] | p [ arcsec/yr ] | aM [ RE ] | aM [ km ] | LOD [ hr ] |
|---|---|---|---|---|---|---|
| IC | Laskar et al. (2004) | 0.000 | 50.467718 | 60.142611 | 383598 | 24.00 |
| Walvis Ridge | Meyers & Malinverno (2018) | 0.055 | 51.28± 1.02 | 59.94 ± 0.26 | 382284 ± 1650 | 23.80 ± 0.24 |
| Lucaogou(a) | Huang et al. (2020) | 0.268 | 57.01± 1.37 | 58.57 ± 0.31 | 373538 ± 2000 | 22.56 ± 0.27 |
| Lucaogou(b) | Huang et al. (2020) | 0.270 | 55.36± 0.51 | 58.95 ± 0.12 | 375967 ± 750 | 22.90 ± 0.11 |
| Yangtze Block | Zhong et al. (2020) | 0.445 | 57.19± 0.53 | 58.52 ± 0.12 | 373277 ± 750 | 22.53 ± 0.10 |
| Alum shale | Sørensen et al. (2020) | 0.493 | 60.11± 1.59 | 57.88 ± 0.34 | 369153 ± 2200 | 21.99 ± 0.28 |
| Luoyixi | Fang et al. (2020) | 0.500 | 61.06± 0.94 | 57.67 ± 0.20 | 367854 ± 1300 | 21.82 ± 0.16 |
| Xiamaling | Meyers & Malinverno (2018) | 1.400 | 85.79± 2.72 | 53.27 ± 0.41 | 339777 ± 2600 | 18.70 ± 0.25 |
| Joffre | Lantink et al. (2021) | 2.460 | 108.91± 8.28 | 50.24 ± 0.96 | 320452 ± 6100 | 16.98 ± 0.50 |
Notes. In boldface, we display the direct observables we used: the precession frequency p in arcsec/yr. The time of observation, T, is in the second column. The semi-major axis of the Moon (aM) given in Earth radius (RE) or in km, and the length of the solar day (LOD), in hours, are derived from the observed quantities using the model that is presented in the text. These values may thus differ from the corresponding values published in the referenced publications; IC denotes the initial conditions (Laskar et al. 2004). The two values (a,b) for the Lucaogou data set correspond to different analyses (a): TimeOptMCMC (Meyers & Malinverno 2018; b) obliquity and precession cycle counting (Huang et al. 2020). Whenever it is specified in the original publication, the uncertainty in p is set to 2σ. The uncertainty of the other variables is propagated through the nominal solution of the present study.
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