The late Miocene 10Be anomaly and the possibility of a supernova

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Table B.2.

Properties for the 19 clusters of interest.

Name	Other name	N_*	N_*, RV	N_{*, ≥8 M_⊙}	Age	M^cls	$M_{corr}^{cls}$ $M^{\mathrm{cls}}_{\mathrm{corr}}$	$D_{\min}^{Sun - cls}$ $D^{\mathrm{Sun-cls}}_{\mathrm{min}}$	t_{D_min}^{Sun − cls}	$t_{\leq 100 pc}^{Sun - cls}$ $t^{\mathrm{Sun-cls}}_{\le100\,\mathrm{pc}}$	$P_{\leq 100 pc}^{Sun - cls}$ $\mathrm{P}^{\mathrm{Sun-cls}}_{\le100\,\mathrm{pc}}$
					[Myr]	[M_⊙]	[M_⊙]	[pc]	[Myr]	[Myr]	%
ASCC 20	-	525	110	$5_{- 2}^{+ 2}$ $5_{-2}^{+2}$	$21 . 7_{- 0.4}^{+ 0.5}$ $21.7_{-0.4}^{+0.5}$	306	$513_{- 61}^{+ 103}$ $513_{-61}^{+103}$	34.2 ± 2.0	−11.9 ± 0.1	[−15.0 ± 0.1, −8.7 ± 0.1]	100
ASCC 24	-	18	4	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$23 . 4_{- 2.8}^{+ 4.7}$ $23.4_{-2.8}^{+4.7}$	24	$24_{- 9}^{+ 25}$ $24_{-9}^{+25}$	82.9 ± 3.2	−9.9 ± 0.2	[−13.1 ± 0.3, −6.9 ± 0.4]	100
CWNU 1057	-	54	14	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$19 . 8_{- 3.0}^{+ 3.3}$ $19.8_{-3.0}^{+3.3}$	25	$46_{- 15}^{+ 34}$ $46_{-15}^{+34}$	20.5 ± 6.4	−7.5 ± 0.3	[−12.7 ± 0.6, −2.3 ± 0.1]	100
CWNU 1111	-	40	8	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$33 . 4_{- 6.8}^{+ 2.9}$ $33.4_{-6.8}^{+2.9}$	25	$59_{- 16}^{+ 37}$ $59_{-16}^{+37}$	95.7 ± 11.2	−10.7 ± 0.5	[−12.3 ± 0.5, −8.7 ± 0.9]	68
HSC 1340	-	194	65	$2_{- 1}^{+ 1}$ $2_{-1}^{+1}$	$24 . 0_{- 1.8}^{+ 3.3}$ $24.0_{-1.8}^{+3.3}$	94	$205_{- 38}^{+ 61}$ $205_{-38}^{+61}$	56.5 ± 2.1	−5.6 ± 0.1	[−10.2 ± 0.1, −1.2 ± 0.1]	100
HSC 1373	-	46	10	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$20 . 4_{- 3.2}^{+ 2.8}$ $20.4_{-3.2}^{+2.8}$	19	$39_{- 11}^{+ 32}$ $39_{-11}^{+32}$	76.4 ± 4.2	−7.6 ± 0.4	[−11.7 ± 0.6, −3.5 ± 0.3]	100
HSC 1469	-	41	15	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$23 . 0_{- 1.3}^{+ 3.5}$ $23.0_{-1.3}^{+3.5}$	23	$56_{- 15}^{+ 34}$ $56_{-15}^{+34}$	91.2 ± 8.5	−11.7 ± 0.6	[−14.9 ± 1.3, −8.7 ± 1.1]	85
HSC 1523	-	17	4	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$20 . 9_{- 1.2}^{+ 3.3}$ $20.9_{-1.2}^{+3.3}$	13	$40_{- 13}^{+ 30}$ $40_{-13}^{+30}$	89.2 ± 17.7	−13.1 ± 0.9	[−15.5 ± 0.7, −10.1 ± 1.3]	74
HSC 1640	Eridanus-North	128	24	$1_{- 1}^{+ 1}$ $1_{-1}^{+1}$	$15 . 7_{- 1.9}^{+ 0.1}$ $15.7_{-1.9}^{+0.1}$	63	$138_{- 27}^{+ 53}$ $138_{-27}^{+53}$	93.5 ± 12.5	−14.7 ± 0.5	[−17.8 ± 1.2, −11.8 ± 1.1]	69
HSC 1687	-	19	6	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$33 . 5_{- 2.2}^{+ 3.8}$ $33.5_{-2.2}^{+3.8}$	14	$35_{- 12}^{+ 28}$ $35_{-12}^{+28}$	95.8 ± 2.6	−10.5 ± 0.1	[−11.4 ± 0.3, −9.7 ± 0.2]	94
HSC 1692	-	24	4	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$29 . 9_{- 2.0}^{+ 2.1}$ $29.9_{-2.0}^{+2.1}$	13	$34_{- 11}^{+ 26}$ $34_{-11}^{+26}$	82.0 ± 4.6	−9.9 ± 0.3	[−12.1 ± 0.5, −7.6 ± 0.3]	100
NGC 2232	-	286	101	$3_{- 2}^{+ 1}$ $3_{-2}^{+1}$	$26 . 8_{- 0.9}^{+ 1.0}$ $26.8_{-0.9}^{+1.0}$	171	$293_{- 47}^{+ 80}$ $293_{-47}^{+80}$	92.2 ± 2.2	−11.7 ± 0.2	[−13.2 ± 0.1, −10.1 ± 0.4]	100
OCSN 50	-	24	9	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$16 . 3_{- 2.2}^{+ 3.5}$ $16.3_{-2.2}^{+3.5}$	14	$34_{- 12}^{+ 30}$ $34_{-12}^{+30}$	84.0 ± 4.2	−10.0 ± 0.4	[−13.1 ± 0.4, −6.9 ± 0.6]	100
OCSN 56	omega-Ori	52	5	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$13 . 2_{- 0.4}^{+ 2.2}$ $13.2_{-0.4}^{+2.2}$	23	$45_{- 13}^{+ 32}$ $45_{-13}^{+32}$	44.9 ± 8.6	−13.0 ± 0.6	[−16.1 ± 0.7, −9.9 ± 0.6]	100
OCSN 61	OBP-b	530	102	$5_{- 2}^{+ 2}$ $5_{-2}^{+2}$	$15 . 7_{- 0.1}^{+ 0.7}$ $15.7_{-0.1}^{+0.7}$	312	$540_{- 71}^{+ 99}$ $540_{-71}^{+99}$	59.2 ± 3.3	−12.8 ± 0.1	[−15.5 ± 0.1, −10.1 ± 0.2]	100
OCSN 64	OBP-e	67	11	$1_{- 1}^{+ 0}$ $1_{-1}^{+0}$	$22 . 6_{- 1.8}^{+ 2.1}$ $22.6_{-1.8}^{+2.1}$	48	$81_{- 22}^{+ 43}$ $81_{-22}^{+43}$	77.2 ± 12.0	−11.4 ± 0.7	[−13.7 ± 1.1, −9.2 ± 0.6]	97
Theia 69	-	31	8	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$24 . 7_{- 0.9}^{+ 2.3}$ $24.7_{-0.9}^{+2.3}$	17	$37_{- 12}^{+ 30}$ $37_{-12}^{+30}$	33.7 ± 5.4	−6.9 ± 0.2	[−10.9 ± 0.4, −3.0 ± 0.1]	100
Theia 71	-	13	3	$0_{- 0}^{+ 1}$ $0_{-0}^{+1}$	$14 . 4_{- 3.6}^{+ 8.5}$ $14.4_{-3.6}^{+8.5}$	6	$20_{- 8}^{+ 25}$ $20_{-8}^{+25}$	76.4 ± 8.3	−9.7 ± 0.7	[−13.4 ± 0.5, −6.1 ± 1.0]	99
Theia 72	-	140	14	$1_{- 1}^{+ 1}$ $1_{-1}^{+1}$	$30 . 7_{- 1.7}^{+ 1.8}$ $30.7_{-1.7}^{+1.8}$	70	$129_{- 27}^{+ 47}$ $129_{-27}^{+47}$	64.1 ± 9.2	−9.2 ± 0.3	[−11.8 ± 0.4, −6.7 ± 0.4]	100

Notes. For each cluster, the following information is provided: name as given in its source catalog, along with an alternative commonly used name if available; number of stellar members (N_*); number of stars with RV (N_*, RV); expected number of massive stars (N_{*, ≥8 M_⊙}); estimated isochronal age; cluster mass derived from the stellar members (M^cls); initial cluster mass corrected for incompleteness ( $M_{corr}^{cls}$ $M^{\mathrm{cls}}_{\mathrm{corr}}$ ); minimum Sun–cluster distance ( $D_{\min}^{Sun - cls}$ $D^{\mathrm{Sun-cls}}_{\mathrm{min}}$ ); time of minimum approach (t_{D_min}^{Sun − cls}); time during which the Sun and the cluster are within 100 pc ( $t_{\leq 100 pc}^{Sun - cls}$ $t^{\mathrm{Sun-cls}}_{\le100\,\mathrm{pc}}$ ); and probability for the Sun and the cluster to be within 100 pc $P_{\leq 100 pc}^{Sun - cls}$ $\mathrm{P}^{\mathrm{Sun-cls}}_{\le100\,\mathrm{pc}}$ . The expected number of massive stars was estimated using the initial cluster mass corrected for incompleteness and a synthetic stellar population assuming a Kroupa IMF.

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