“TNOs are Cool”: A survey of the trans-Neptunian region - XV. Physical characteristics of 23 resonant trans-Neptunian and scattered disk objects

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Table 5

Clusters identified by Lacerda et al. (2014, Col. 1), using the Lacerda et al. (2014) sample with updates (this work, Col. 2), and usingall targets (this work, Col. 3).

Lacerda et al. (2014)			Original sample			All targets
Mathematica/FindClusters			R/MClust, VVI			R/MClust, VVI

p_V	S′	ID	p_V	S′	ID	p_V	S′	ID
~0.05	~10	DN	0.047 ± 0.008	9.7 ± 4.6	DN	0.046 ± 0.008	10.0 ± 4.5	DN
~0.15	~35	BR	0.125 ± 0.071	29.1 ± 12.3	BR	0.121 ± 0.056	26.7 ± 13.6	BR
>0.30	~0	BN	0.564 ± 0.239	4.6 ± 5.8	BN	0.538 ± 0.221	9.5 ± 13.0	BN

Notes. Clusters are characterized here by their mean geometric albedo (p_V) and spectralslope (S′, %/1000 Å), and the standard deviations using an ellipsoidal varying volume and shape data model. In the second row we also list the tools used to identify the clusters.

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