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Table 1

A list of asteroid families and their physical parameters.

Designation v cutoff N p V Tax. D PB D Durda LR/PB v esc q 1 q 2 Age Notes, references
m/s km km m/s Gyr
3 Juno 50 449 0.250 S 233 ? 0.999 139 −4.9 −3.2 <0.7 cratering, Nesvorný et al. (2005)
4 Vesta 60 11 169 0.351w V 530 425! 0.995 314 −4.5 −2.9 1.0 ± 0.25 cratering, Marchi et al. (2012)
8 Flora 60 5284 0.304w S 150c 160 0.81–0.68 88 −3.4 −2.9 1.0 ± 0.5 cut by ν6 resonance, LL chondrites
10 Hygiea 70 3122 0.055 C,B 410 442 0.976–0.78 243 −4.2 −3.2 2.0 ± 1.0 LHB? cratering
15 Eunomia 50 2867 0.187 S 259 292 0.958–0.66 153 −5.6 −2.3 2.5 ± 0.5 LHB? Michel et al. (2002)
20 Massalia 40 2980 0.215 S 146 144 0.995 86 −5.0 −3.0 0.3 ± 0.1
24 Themis 70 3581 0.066 C 268c 380–430! 0.43–0.09 158 −2.7 −2.4 2.5 ± 1.0 LHB?
44 Nysa (Polana) 60 9957 0.278w S 81c ? 0.65 48 −6.9 −2.6(0.5) <1.5 overlaps with the Polana family
46 Hestia 65 95 0.053 S 124 153 0.992–0.53 74 −3.3 −2.0 <0.2 cratering, close to J3/1 resonance
87 Sylvia 110 71 0.045 C/X 261 272 0.994–0.88 154 −5.2 −2.4 1.0–3.8 LHB? cratering, Vokrouhlický et al. (2010)
128 Nemesis 60 654 0.052 C 189 197 0.987–0.87 112 −3.4 −3.3 0.2 ± 0.1
137 Meliboea 95 199 0.054 C 174c 240–290! 0.59–0.20 102 −1.9 −1.8 <3.0 old?
142 Polana (Nysa) 60 3443 0.055w C 75 ? 0.42 45 −7.0 −3.6 <1.5 overlaps with Nysa
145 Adeona 50 1161 0.065 C 171c 185 0.69–0.54 101 −5.2 −2.8 0.7 ± 0.5 cut by J5/2 resonance
158 Koronis 50 4225 0.147 S 122c 170-180 0.024–0.009 68 −3.6(0.3) −2.3 2.5 ± 1.0 LHB?
163 Erigone 60 1059 0.056 C/X 79 114 0.79–0.26 46 ? −3.6 0.3 ± 0.2
170 Maria 80 3094 0.249w S 107c 120-130 0.070–0.048 63 −2.5(0.3) −2.8 3.0 ± 1.0 LHB?
221 Eos 50 5976 0.130 K 208c 381! 0.13–0.020 123 −3.5 −2.1 1.3 ± 0.2
283 Emma 75 345 0.050 – 152 185 0.92–0.51 90 ? −3.2 <1.0 satellite
293 Brasilia 60 282 0.175w C/X 34 ? 0.020 20 −1.4(0.5) −3.7 0.05 ± 0.04 (293) is interloper
363 Padua (Lydia) 50 596 0.097 C/X 76 106 0.045–0.017 45 −1.8 −3.0 0.3 ± 0.2
396 Aeolia 20 124 0.171 C/X 35 39 0.966–0.70 20 ? −4.3 <0.1 cratering
410 Chloris 90 259 0.057 C 126c 154 0.952–0.52 74 ? −2.1 0.7 ± 0.4
490 Veritas – – – C,P,D – 100–177 – – – – 0.0083 ± 0.0005 (490) is likely interloper (Michel et al. 2011)
569 Misa 70 543 0.031 C 88c 117 0.58–0.25 52 −3.9 −2.3 0.5 ± 0.2
606 Brangane 30 81 0.102 S 37 46 0.92–0.48 22 ? −3.8 0.05 ± 0.04
668 Dora 50 837 0.054 C 85 165! 0.031–0.004 50 −4.2 −1.9 0.5 ± 0.2
808 Merxia 50 549 0.227 S 37 121! 0.66–0.018 22 −2.7 −3.4 0.3 ± 0.2
832 Karin – – – S – 40 – – – – 0.0058 ± 0.0002
845 Naema 30 173 0.081 C 77c 81 0.35–0.30 46 −5.2 −2.9 0.1 ± 0.05
847 Agnia 40 1077 0.177 S 39 61 0.38–0.10 23 −2.8 −3.1 0.2 ± 0.1
1128 Astrid 50 265 0.079 C 43c ? 0.52 25 −1.7 −2.6 0.1 ± 0.05
1272 Gefion 60 19 477 0.20 S 74c 100–150! 0.001–0.004 60 −4.3 −2.5 0.48 ± 0.05 Nesvorný et al. (2009), L chondrites
1400 Tirela 80 1001 0.070 S 86 – 0.12 86 −4.2 −3.4 <1.0
1658 Innes 70 621 0.246w S 27 ? 0.14 16 −4.9 −3.5 <0.7 (1644) Rafita is interloper
1726 Hoffmeister 40 822 0.035 C 93c 134 0.022–0.007 55 −4.5 −2.7 0.3 ± 0.2
3556 Lixiaohua 60 439 0.044w C/X 62 220! 0.029–0.001 35 −6.1 −3.3 0.15 ± 0.05 Novaković et al. (2010)
3815 Konig 60 177 0.044 C 33 ? 0.32 20 ? −3.0 <0.1 (1639) Bower is interloper
4652 Iannini – – – S – – – – – – 0.005 ± 0.005
9506 Telramund 40 146 0.217w S 22 – 0.05 13 −3.9 −3.7 <0.5
18 405 1993 FY12 50 44 0.171w C/X 15 – 0.23 15 −2.4 −2.4 <0.2 cut by J5/2 resonance
158 Koronis(2) – – – S 35 – – – – – 0.015 ± 0.005 cratering, Molnar & Haegert (2009)
298 Baptistina 50 1249 0.160w C/X 35c – 0.17 21 −3.6 −2.4 <0.3 overlaps with the Flora family
434 Hungaria 200 4598 0.35 E 25 – 0.15 15 −5.9 −3.1 0.5 ± 0.2 Warner et al. (2010)
627 Charis 80 235 0.081 S >60 – 0.53 35 ? −3.4 <1.0
778 Theobalda 85 154 0.060 C 97c – 0.29 57 ? −2.9 0.007 ± 0.002 cratering, Novaković (2010)
302 Clarissa 30 75 0.054 C 39 – 0.96 23 ? −3.1 <0.1 cratering, Nesvorný (2010)
656 Beagle 24 63 0.089 C 64 – 0.56 38 −1.3 −1.4 <0.2
752 Sulamitis 60 191 0.042 C 65 – 0.83 39 −6.5 −2.3 <0.4
1189 Terentia 50 18 0.070 C 56 – 0.990 33 ? −2.6? <0.2 cratering
1892 Lucienne 100 57 0.223w S 14 – 0.71 8 ? −4.4 <0.3
7353 Kazvia 50 23 0.206w S 16 – 0.57 8 ? −1.8 <0.1
10 811 Lau 100 15 0.273w S 11 – 0.77 5 ? −2.8 <0.1
18 466 1995 SU37 40 71 0.241w S 14 – 0.045 7 ? −5.0 <0.3
1270 Datura – – – S – – – – – – 0.00045–0.00060 identified in osculating-element space,
14 627 Emilkowalski – – – C/X – – – – – – 0.00019–0.00025 Nesvorný & Vokrouhlický (2006)
16 598 1992 YC2 – – – S – – – – – – 0.00005–0.00025
21 509 Lucascavin – – – S – – – – – – 0.0003–0.0008
2384 Schulhof – – – S – – – – – – 0.0007–0.0009 Vokrouhlický & Nesvorný (2011)
27 Euterpe 70 268 0.260w S 118c – 0.998 70 −2.9 −2.2 <1.0 cratering, Parker et al. (2008)
375 Ursula 80 777 0.057w C 203c 240–280 0.71–0.43 120 −4.1 −2.3 <3.5 old?
1044 Teutonia 50 1950 0.343 S 27–120 – 0.17–0.98 16–71 −3.5 −3.9 <0.5 depends on (5) Astraea membership
1296 Andree 60 401 0.290w S 17–74 – 0.010–0.95 10–43 ? −2.9(0.5) <1.0 depends on (79) Eurynome membership
2007 McCuskey 34 236 0.06 C 29 – 0.41 17 ? −5.6 <0.5 overlaps with Nysa/Polana
2085 Henan 54 946 0.200w S 27 – 0.13 16 −4.2 −3.2 <1.0
2262 Mitidika 83 410 0.064w C 49-79c – 0.037–0.81 26–46 −4.5 −2.2 <1.0 depends on (785) Zwetana membership, (2262) is interloper, overlaps with Juno
2 Pallas 200 64 0.163 B 498c – 0.9996 295 ? −2.2 <0.5 high-I, Carruba (2010)
25 Phocaea 160 1370 0.22 S 92 – 0.54 55 −3.1 −2.4 <2.2 old? high-I/e, cut by ν6 resonance, Carruba (2009)
148 Gallia 150 57 0.169 S 98 – 0.058 58 ? −3.6 <0.45 high-I
480 Hansa 150 651 0.256 S 60 – 0.83 35 −4.9 −3.2 <1.6 high-I
686 Gersuind 130 178 0.146 S 52c – 0.48 40 ? −2.7 <0.8 high-I, Gil-Hutton (2006)
945 Barcelona 110 129 0.248 S 28 – 0.77 16 ? −3.5 <0.35 high-I, Foglia & Masi (2004)
1222 Tina 110 37 0.338 S 21 – 0.94 12 ? −4.1 <0.15 high-I
4203 Brucato – – – – – – – – – – <1.3 in frequency space
31 Euphrosyne 100 851 0.056 C 259 – 0.97 153 −4.9 −3.9 <1.5 cratering, high-I, Foglia & Massi (2004)
702 Alauda 120 791 0.070 B 218c 290-330! 0.025 129 −3.9 −2.4 <3.5 old? high-I, cut by J2/1 resonance, satellite (Margot & Rojo 2007)
107 Camilla ? ? 0.054 – >226 ? ? ? ? ? 3.8? LHB? Cybele region, non-existent today,
121 Hermione ? ? 0.058 – >209 ? ? ? ? ? 3.8? LHB? Vokrouhlický et al. (2010)
1303 Luthera 100 142 0.043 X 92 – 0.81 54 −3.9 −2.7 <0.5 above (375) Ursula
1547 Nele 20 57 0.311w X 19 – 0.85 11 ? −2.8(0.3) <0.04 close to (3) Juno
2732 Witt 60 985 0.260w S 25 – 0.082 15 −4.0(0.3) −3.8 <1.0 only part with sinI > 0.099, above (363) Padua
81 Terpsichore 120 70 0.052 C 119 – 0.993 71 ? −4.4 <0.5 cratering, less-certain families in the “pristine zone”
709 Fringilla 140 60 0.047 X 99c 130-140 0.93–0.41 59 −6.2 −1.7 <2.5 old?
918 Itha 140 63 0.23 S 38 – 0.16 22 −2.7 −1.5 <1.5 shallow SFD
5567 Durisen 100 18 0.044w X 42 – 0.89 25 ? −1.7 <0.5 shallow SFD
5614 Yakovlev 100 34 0.05 C 22 – 0.28 13 ? −3.2 <0.2
12 573 1999 NJ53 40 13 0.190w C 15 – 0.13 9 ? −2.0(0.5) <0.6 incomplete SFD
15 454 1998 YB3 50 14 0.054w C 21 – 0.41 13 ? −1.6(0.3) <0.5 shallow SFD
15 477 1999 CG1 110 144 0.098w S 25 – 0.065 14 ? −4.6(0.5) <1.5
36 256 1999 XT17 60 30 0.210w S 17 – 0.037 10 ? −1.4(0.5) <0.3 shallow SFD

Notes. There are the following columns: vcutoff is the selected cut–off velocity for the hierarchical clustering, N the corresponding number of family members, pV the adopted value of the geometric albedo for family members which do not have measured diameters (from Tedesco et al. 2002 or Masiero et al. 2011, a letter “w” indicates it was necessary to use the WISE data to obtain median/mean albedo), taxonomic classification (according to the Sloan DSS MOC 4 colours, Parker et al. 2008), DPB parent body size, an additional “c” letter indicates that we prolonged the SFD slope down to zero D (a typical uncertainty is 10%), DDurda PB size inferred from SPH simulations (Durda et al. 2007), an exclamation mark denotes a significant mismatch with DPB, LR/PB the ratio of the volumes of the largest remnant to the parent body (an uncertainty corresponds to the last figure, a range is given if both DPB and DDurda are known), vesc the escape velocity, q1 the slope of the SFD for larger D, q2 the slope for smaller D (a typical uncertainty of the slopes is 0.2, if not indicated otherwise), dynamical age including its uncertainty.

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