Table 3
Old families with ages possibly approaching the LHB.
| Designation | D PB | D Durda | Note | ||
| (km) | (km) | ||||
|
|
|||||
| 24 | Themis | 209c | 380–430! | ||
| 10 | Hygiea | 410 | 442 | cratering | |
| 15 | Eunomia | 259 | 292 | cratering | |
| 702 | Alauda | 218c | 290–330! | high-I | |
| 87 | Sylvia | 261 | 272 | cratering | |
| 137 | Meliboea | 174c | 240–290! | ||
| 375 | Ursula | 198 | 240–280 | cratering | |
| 107 | Camilla | >226 | – | non-existent | |
| 121 | Hermione | >209 | – | non-existent | |
| 158 | Koronis | 122c | 170–180 | ||
| 709 | Fringilla | 99c | 130–140 | cratering | |
| 170 | Maria | 100c | 120–130 | ||
Notes. They are sorted according to the parent body size, where DDurda determined by the Durda et al. (2007) method is preferred to the estimate DPB inferred from the observed SFD. An additional “c” letter indicates that we extrapolated the SFD down to D = 0 km to account for small (unobserved) asteroids, an exclamation mark denotes a significant mismatch between DPB and DDurda.
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