Table 4.
Fraction of accreting stars, median accretion luminosity, and median mass accretion rate for 34 Sco-Cen clusters.
| Sco-Cen clusters from Ratzenböck et al. (2023b) | Median values per cluster | |||||
|---|---|---|---|---|---|---|
| SigMA | Group | Age B-BpRp [Myr] | N. sources with pEW | Accretors [%] | Lacc [L⊙] | Ṁacc [M⊙ yr−1] |
| 1 | ρ Oph/L1688 | 3.2 (3.1, 3.4) | 406 | 15.0 ± 1.9 | 1.51E−3 (4.81E−4, 7.97E−4) | 1.86E−10 (8.50E−11, 5.70E−10) |
| 2 | ν Sco | 3.9 (3.4, 4.1) | 127 | 11.0 ± 2.9 | 6.89E−4 (2.02E−4, 8.07E−3) | 6.50E−11 (4.25E−11, 4.84E−10) |
| 3 | δ Sco | 6.4 (5.8, 7.5) | 594 | 8.6 ± 1.2 | 2.75E−4 (1.00E−4, 2.17E−3) | 3.88E−11 (1.47E−11, 1.86E−10) |
| 4 | β Sco | 4.8 (4.6, 5.3) | 241 | 7.5 ± 1.8 | 2.43E−4 (1.07E−4, 4.46E−4) | 2.93E−11 (1.86E−11, 5.86E−11) |
| 5 | σ Sco | 6.0 (5.8, 6.3) | 411 | 3.1 ± 0.9 | 1.08E−4 (5.40E−5, 1.86E−4) | 1.42E−11 (8.88E−12, 4.16E−11) |
| 6 | Antares | 6.0 (5.8, 6.5) | 429 | 5.9 ± 1.1 | 2.61E−4 (1.26E−4, 1.26E−3) | 3.84E−11 (2.12E−11, 1.59E−10) |
| 7 | ρ Sco | 7.9 (7.4, 8.3) | 197 | 2.0 ± 1.0 | 1.12E−4 (9.90E−5, 1.42E−4) | 2.01E−11 (9.39E−12, 3.07E−11) |
| 8 | Scorpio-Body | 9.1 (8.8, 9.5) | 315 | 3.5 ± 1.1 | 5.50E−5 (4.30E−5, 9.10E−5) | 1.10E−11 (6.20E−12, 1.41E−11) |
| 9 | US-foreground | 12.5 (12.1, 13.1) | 233 | 3.9 ± 1.3 | 6.20E−5 (2.20E−5, 8.80E−5) | 9.27E−12 (4.52E−12, 1.19E−11) |
| 10 | V1062-Sco | 10.0 (9.8, 10.5) | 808 | 2.4 ± 0.5 | 9.00E−5 (6.00E−5, 1.40E−4) | 1.11E−11 (8.92E−12, 2.41E−11) |
| 11 | μ Sco | 9.6 (9.0, 10.5) | 40 | 2.5 ± 2.5 | ||
| 12 | Libra-South | 12.4 (10.8, 13.3) | 61 | 0 | ||
| 13 | Lupus 1-4 | 4.3 (4.1, 5.2) | 188 | 25.5 ± 3.7 | 1.99E−3 (4.55E−4, 1.21E−2) | 2.32E−10 (5.21E−11, 9.12E−10) |
| 14 | η Lup | 9.8 (9.1, 10.1) | 657 | 3.7 ± 0.7 | 5.90E−5 (4.70E−5, 1.93E−4) | 1.01E−11 (6.90E−12, 5.57E−11) |
| 15 | ϕ Lup | 9.9 (9.4, 10.3) | 947 | 3.9 ± 0.6 | 8.30E−5 (4.90E−5, 2.42E−4) | 1.12E−11 (7.97E−12, 2.51E−11) |
| 17 | e Lup | 11.0 (10.7 11.5) | 431 | 2.3 ± 0.7 | 4.40E−5 (3.90E−5, 6.70E−5) | 9.10E−12 (5.71E−12, 1.16E−11) |
| 18 | UPK606 | 8.5 (8.0, 8.9) | 110 | 6.4 ± 2.4 | 1.03E−4 (8.30E−5, 2.74E−4) | 2.64E−11 (1.59E−11, 4.06E−11) |
| 19 | ρ Lup | 9.4 (8.9, 10.2) | 211 | 7.1 ± 1.8 | 3.40E−5 (2.20E−5, 5.40E−5) | 6.84E−12 (5.08E−12, 1.35E−11) |
| 20 | ν Cen | 9.5 (8.8, 12.1) | 1401 | 3.9 ± 0.5 | 6.40E−5 (3.80E−5, 1.00E−4) | 9.23E−12 (6.28E−12, 1.92E−11) |
| 21 | σ Cen | 9.5 (8.8, 9.9) | 1550 | 3.5 ± 0.5 | 5.50E−5 (3.00E−5, 1.89E−4) | 8.98E−12 (5.12E−12, 2.23E−11) |
| 22 | Acrux | 7.3 (6.9, 7.4) | 349 | 4.6 ± 1.1 | 6.30E−5 (4.40E−5, 2.37E−4) | 1.14E−11 (6.02E−12, 2.96E−11) |
| 23 | Musca-foreground | 6.9 (6.7, 7.4) | 87 | 3.4 ± 2.0 | ||
| 24 | ϵ Cham | 5.4 (5.0, 6.0) | 35 | 8.6 ± 4.9 | ||
| 25 | η Cham | 6.1 (5.5, 6.9) | 28 | 7.1 ± 5.0 | ||
| 26 | B59 | 3.0 (2.1, 3.1) | 22 | 40.9 ± 13.6 | 2.91E−2 (6.69E−3, 4.81E−2) | 2.52E−09 (4.30E−10, 2.60E−09) |
| 27 | Pipe-North | 10.1 (8.4, 10.8) | 38 | 7.9 ± 4.6 | ||
| 28 | θ Oph | 9.5 (8.9, 10.5) | 85 | 1.2 ± 1.2 | ||
| 29 | CrA-Main | 6.1 ( 5.5, 8.5) | 77 | 11.7 ± 3.9 | 3.06E−4 (1.66E−4, 6.64E−3) | 4.40E−11 (2.72E−11, 8.23E−10) |
| 30 | CrA-North | 6.6 (5.8, 6.9) | 278 | 7.2 ± 1.6 | 1.27E−4 (6.50E−5, 2.25E−3) | 2.54E−11 (1.13E−11, 1.81E−10) |
| 31 | Scorpio-Sting | 8.5 (8.1, 9.0) | 101 | 5.9 ± 2.4 | 4.10E−5 (2.40E−5, 5.30E−5) | 6.24E−12 (5.25E−12, 6.91E−12) |
| 32 | Centaurus-Far | 5.9 (5.6, 7.1) | 69 | 1.4 ± 1.4 | ||
| 33 | Chamaeleon-1 | 3.0 (2.6, 3.8) | 142 | 26.1 ± 4.3 | 9.54E−3 (1.73E−3, 2.91E−2) | 1.12E−09 (1.16E−10, 3.07E−09) |
| 34 | Chamaeleon-2 | 2.8 (2.4, 3.1) | 43 | 44.2 ± 10.1 | 4.70E−3 (1.64E−3, 2.75E−2) | 4.55E−10 (2.03E−10, 1.57E−09) |
| 35 | L134/L183 | 5.7 (5.1, 6.6) | 22 | 0 | ||
Notes. The Sco-Cen clusters are the ones identified in Ratzenböck et al. (2023a). Ages are the Baraffe et al. (2015) Bp-Rp ages calculated in Ratzenböck et al. (2023b). The median values reported here are calculated using the med-GSP-Phot extinction correction and considering all sources in each cluster that are in Table 2 and have pEW < − 1.0 nm. The median values reported here do not correspond to the ones presented in Fig. 13, which were corrected for stellar mass by only considering sources in the mass range 0.08–0.25 M⊙. The 16th and 84th percentiles are reported in brackets. Clusters have no median values if they have fewer than four members that can be used to calculate the median. The full table, including the mass-corrected medians, and the value of the Ṁacc-M⋆ and Lacc-L⋆ correlations for each cluster (Fig. 15), is available at the CDS.
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