Table 1
Sco–Cen subgroups and their properties.
| Sub-group | Initial stellar mass | Age | Distance | Diameter | B starsa | Past SNb |
|---|---|---|---|---|---|---|
| name |  |
 |
(pc) | (pc) | (number) | (number) |
| USco | 2060 | ≈5–10c | 145 | 35 | 49 | 1 |
| LCC | ≈2000d | ≈15 | 118 | 50 | 42 | ≈4e |
| UCL | ≈3000d | ≈17 | 140 | 100 | 66 | ≈7 |
Notes. Data are taken from Preibisch & Mamajek (2008) unless indicated otherwise. (a)Current number of B stars according to de Bruijne (1999). (b)Estimated number of past supernovae. (c)Stars with M < 1 M⊙ have age determinations towards the lower end of the range; more massive ones are found to be older (Herczeg & Hillenbrand 2015; Pecaut & Mamajek 2016). The range is likely related to measurement and model uncertainties and not necessarily a real age spread (Preibisch 2012; Donaldson et al. 2017). (d)Estimated from the number of B stars with Salpeter initial mass function and scaled to the well determined mass of USco. For the initial mass function used in Preibisch & Mamajek (2008) for USco, USco would have lost only one B-star from the main sequence while ageing from 5 to 16 Myr. (e)Scaled to the estimate in UCL using a Salpeter initial mass function.
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