Quantifying the scale of star formation across the Perseus spiral arm using young clusters around Cas OB5

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Table 1

Properties of the main open clusters related to Cas OB5 in Hunt & Reffert (2024) and our identified clusters, ordered by increasing median distance.

OC	OC (HR24)	N_HM/N_all	d (kpc)	Age (Myr) (HR24)	Age (Myr) (Others)	Age references
6, 8	NGC 7788	58/98	${2.70}_{- 0.01}^{+ 0.02}$ $\[2.70_{-0.01}^{+0.02}\]$	$20_{- 8}^{+ 9}$ $\[20_{-8}^{+9}\]$	17–40	[1], [2], [4]–[7], [8], [11], [12]
6, 8	FSR 451	118/186	${2.80}_{- 0.01}^{+ 0.02}$ $\[2.80_{-0.01}^{+0.02}\]$	$27_{- 15}^{+ 9}$ $\[27_{-15}^{+9}\]$	11–14	[5], [11], [12]
6	King 12	58/81	${2.80}_{- 0.01}^{+ 0.02}$ $\[2.80_{-0.01}^{+0.02}\]$	20 ± 8	10–14	[1]–[7], [11], [12]
9	King 21	82/153	${2.89}_{- 0.03}^{+ 0.01}$ $\[2.89_{-0.03}^{+0.01}\]$	$52_{- 17}^{+ 34}$ $\[52_{-17}^{+34}\]$	10–117	[1], [2], [5]–[7], [10]–[12]
9	Teutsch 23	17/19	${2.89}_{- 0.05}^{+ 0.04}$ $\[2.89_{-0.05}^{+0.04}\]$	$13_{- 5}^{+ 9}$ $\[13_{-5}^{+9}\]$	8–64	[2], [5]–[7], [11],
6	Stock 17	47/64	${2.93}_{- 0.02}^{+ 0.03}$ $\[2.93_{-0.02}^{+0.03}\]$	12 ± 5	6–10	[5]–[7], [11]
9	Negueruela 1	11/11	2.95 ± 0.04	4 ± 1	3–17	[5]–[7], [9], [11], [12]
8, 11	Berkeley 58	91/173	3.01 ± 0.02	$91_{- 36}^{+ 47}$ $\[91_{-36}^{+47}\]$	158–372	[2], [5]–[8] [11], [12]
8, 11	NGC 7790	77/143	3.13 ± 0.02	$67_{- 25}^{+ 36}$ $\[67_{-25}^{+36}\]$	57–126	[2], [4]–[7], [11], [12]

Notes. N_HM stands for the number of cluster members in HR24 with a 50 th percentile of the mass greater than 1.88 M_⊙, whilst N_all corresponds to the total number of cluster members. For comparison, the ages from other references have also been indicated on the second to last column, with the corresponding references written on the last column. References are [1]: Pandey et al. (1989), [2]: Kharchenko et al. (2005), [3]: Hancock et al. (2008), [4]: Davidge (2012), [5]: Kharchenko et al. (2013), [6]: Kharchenko et al. (2016), [7]: Loktin & Popova (2017), [8]: Bossini et al. (2019), [9]: Monteiro & Dias (2019), [10]: Maurya et al. (2020), [11]: Dias et al. (2021), and [12]: Tarricq et al. (2021).

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