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Table 5 Small bodies for which boulder counts have been made from spacecraft images. The minimum boulder sizes measured are directly related to the best image resolution available for a given object

From: Asteroid Ryugu before the Hayabusa2 encounter

Name Mean diameter (km) Spectral type Min boulder size of global count (m) Min boulder size of regional count (m) Power law found Data source References
Eros 17 S 15 0.05 − 3.2 as low as − 2.3 locally NEAR Rodgers et al. 2016; Thomas et al. 2001
Itokawa 0.35 S 6 0.1 − 3.1
− 3.5
as low as − 1.7 or as high as − 4.1 locally
Hayabusa Mazrouei et al. 2014; Michikami et al. 2008; Noviello et al. 2014; Rodgers et al. 2016
Tancredi et al. 2015
Toutatis 2.9 S n/a 10 − 4.4 locally Chang’e 2 Jiang et al. 2015; Huang et al. 2013
Lutetia 99 M n/a 60 − 5.0 Rosetta Küppers et al. 2012; Sierks et al. 2011
Ida 32 S n/a 45 n/a Galileo Lee et al. 1996
Phobos 22 D n/a 5 − 3.2 Viking MGS
MEX
MRO
Ernst et al. 2015; Rodgers et al. 2016; Thomas et al. 2000
Deimos 12 D n/a ~ 4 − 3.2 Viking Lee et al. 1986; C. Ernst, personal communication
Churyumov-Gerasimenko 4 Comet 7 2 − 3.6 global; local ranges − 2.2 to − 4.0 Rosetta Pajola et al. 2015, 2016