Table 2.
Overview of the star formation modes/bursts as determined from the age distribution of Sco-Cen clusters (Fig. 3).
| Notation | Age (Myr) | Description | Clusters (a) |
|---|---|---|---|
| 20 Myr peak | ∼19–22 | Initial onset of star formation in Sco-Cen | e Lup, Libra-South, US-foreground |
| 15 Myr peak | (14.4, 15.9) | Maximum of star and cluster formation rate | ν Cen, σ Cen, ρ Lup, UPK606, V1062-Sco, μ Sco, ϕ Lup, η Lup, Pipe-N, θ Oph, Sco-Body, Sco-Sting, ρ Sco |
| 10 Myr peak | (8.5, 10.2) | Formation of the major clusters in USco and the chains of LCC and CrA | Antares, σ Sco, δ Sco, β Sco, L134/L183, Acrux, Musca-fg, ϵ Cham, η Cham, Cen-Far, CrA-North, CrA-Main (b) |
| 5 Myr peak | ∼3–5 | Recent star formation, still near or associated with gas | Lupus 1-4, ν Sco, ρ Oph, B59, Cham-1, Cham-2 |
Notes. There are two main modes of star formation, including the second and third peak at 15 Myr and 10 Myr ago, which are confirmed as significant by the excess of mass test. We find two smaller peaks at 20 Myr and 5 Myr ago, for which we give the time-frames approximately.
We tentatively assign each of the 34 SigMA clusters to one of the peaks, as separately displayed in Fig. 4.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.