Table B.2
Spectral and physical characteristics of primitive asteroid families and the largest members.
| Family | Tax. | Albedo | Qhyd (%) | DPB (km) | Largest member | |||
|---|---|---|---|---|---|---|---|---|
| Asteroid | Taxono | 3 μm | ||||||
| This study | prev. | |||||||
| Blue-dominant families | ||||||||
| Pallas Type | ||||||||
| Pallas (h) | B | 13.0 ± 4.3 | 0 | 498 | (2) Pallas | B | B | Sharp(3) |
| Themis Type | ||||||||
| Themis | B,C | 7.5 ± 2.2 | 11–13 | 268–430 | (24) Themis | C | C | Ceres/Europa(6,7) |
| Beagle | B | 8.1 ± 3.4 | 64 | (656) Beagle | B | − | ||
| Hygiea | F,B | 7.4 ± 2.1 | 0–15 | 410 | (10) Hygiea | C | C | Ceres(6,8,9) |
| Adeona (h) | B,G | 6.2 ± 1.6 | 69 | 171–185 | (145) Adeona | C | C(h) | Sharp(14) |
| Dora (h) | B,F | 5.6 ± 1.6 | 83 | 85–165 | (668) Dora | G | C(h) | |
| Alauda | F,P | 6.8 ± 2.2 | 218–330 | (702) Alauda | C | C | Ceres/Europa(5) | |
| Brucato (h) | C,B,F | 6.5 ± 1.4 | 45(1) | (4203) Brucato | G | − | ||
| Polana–Eulalia Type | ||||||||
| Polana–Eulalia | F | 6.0 ± 1.7 | 7 | >76* | (142) Polana | F | F | No abs.(4) |
| (100–160)** | (495) Eulalia | − | − | |||||
| Mitidika | F | 7.1 ± 1.8 | 49–79 | (404) Arsinoe | C | C | ||
| Hoffmeister | F | 5.0 ± 1.4 | 0 | 93–134 | (1726) Hoffmeister | P | CbBB | |
| Theobalda | F | 7.4 ± 2.3 | 97 | (778) Theobalda | F | F | No abs.(5) | |
| Clarissa | F | 5.6 ± 1.5 | 9 | 39 | (302) Clarissa | F | F | |
| High NUV absorption families | ||||||||
| Veritas Type | ||||||||
| Veritas (h) | G | 6.7 ± 1.7 | 75–77 | 100–177 | (490) Veritas | G | C(h) | |
| Inarradas (h) | G | 7.2 ± 1.5 | 37(1) | (3438) Inarradas | C | − | ||
| Padua Type | ||||||||
| Padua | C,G | 7.2 ± 1.4 | 0 | 76 | (363) Padua | − | P | Sharp(5) |
| Chloris (h) | G,C | 6.8 ± 2.0 | 126–154 | (410) Chloris | G | C(h) | ||
| Misa (h) | G,C | 6.1 ± 1.7 | 88–117 | (569) Misa | − | C(h) | ||
| Chaldaea | G,C | 6.6 ± 1.7 | 79 | >95(2) | (313) Chaldaea | C | C(h) | Sharp(5) |
| Astrid (h) | G,C | 5.6 ± 1.9 | 20 | 43 | (1128) Astrid | − | C | |
| Erigone Type | ||||||||
| Erigone (h) | C,G | 5.4 ± 1.3 | 58 | 79 | (163) Erigone | G | C(h) | Sharp(10) |
| Nemesis | C,G | 7.5 ± 1.5 | 0 | 189–197 | (128) Nemesis | C | C | Sharp(6) |
| Meliboea (h) | C,P | 6.2 ± 1.9 | 78 | 174–290 | (137) Meliboea | C | C(h) | Sharp(10) |
| Klio (h) | C,P | 6.6 ± 1.8 | 23 | 80(1) | (84) Klio | − | G(h) | |
| Naema (h) | C,F,B | 6.6 ± 1.8 | 77 | (845) Naema | − | C(h) | ||
| Sulamitis (h) | C,P | 5.3 ± 1.4 | 60 | 65 | (752) Sulamitis | − | C(h) | |
| Vibilia(h) | C,B | 6.6 ± 1.3 | >142(2) | (144) Vibilia | − | C(h) | Sharp(10) | |
| Konig (h) | C | 5.0 ± 1.6 | 33 | (3815) Konig | − | − | ||
| Red-dominant families | ||||||||
| Lixiaohua Type | ||||||||
| Lixiaohua | P | 4.5 ± 1.1 | 0 | 62–220 | (3556) Lixiaohua | − | P | |
| Emma (h) | F,P | 4.7 ± 1.6 | 152 | (238) Emma | − | P | ||
| Fringilla | P | 4.9 ± 1.5 | 99–140 | (709) Fringilla | C | P | ||
| Luthera | P | 5.1 ± 1.0 | 92 | (1303) Luthera | D | − | ||
| Euphrosyne Type | ||||||||
| Euphrosyne | P,F | 5.7 ± 1.6 | 259 | (31) Euphrosyne | − | C | Europa(8) | |
| Ursula | P,F,C | 6.3 ± 1.7 | 0 | 203–280 | (375) Ursula | − | C | Europa(8,9) |
| Phaeo | P,G | 5.7 ± 1.5 | 75(1) | (322) Phaeo | P | P | ||
| Sylvia | P,F | 6.0 ± 1.9 | 261 | (87) Sylvia | P | P | Europa(5)/below detection limit(6) | |
| Karma | P | 5.3 ± 1.6 | 32(1) | (3811) Karma | − | − | ||
| Postrema | P | 5.2 ± 2.3 | >47(2) | (1484) Postrema | − | BBB | ||
Notes. Albedo and Qhyd are the same as Table B.1 and Tax. indicates the main consituents of family members. DPB is estimated parent body size by Brož et al. (2013). Taxonomy of largest member in the asteroid families is from Tholen (1984) without notation and from Bus & Binzel (2002a) with the superscript “BB”. The notation of “(h)” indicates presence of the 0.7-μm absorption.
References. *Estimated value for Polana family by Milani et al. (2014) **Estimated value for Eulalia family by Walsh et al. (2013). (1) Nesvorný et al. (2015); (2) Lower limit is given by the largest body in the family from Usui et al. (2013); (3) Rivkin (2012); (4) Takir et al. (2024); (5) Rivkin et al. (2022); (6) Usui et al. (2019); (7) Rivkin & Emery (2010); (8) Rivkin et al. (2019); (9) Takir & Emery (2012); (10) Rivkin et al. (2015).
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