Young nearby open clusters and their luminosity functions

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Table A.1.

Extinction and E(B-V) from dustmaps for the bound clusters.

Cluster	Distance	E(B-V)	A_V	N	E(B-V) ref	Ref

	pc	mag	mag		mag
Blanco 1	243	0.01	0.03	53	0.02	Westerlund et al. (1988)
Melotte 111	86	0.01	0.04	29	negligible	Feltz (1972)
Alessi 13	103	0.02	0.06	12	0.02	He et al. (2022), derived from A₀ = 0.05
Mamajek 4	441	0.07	0.21	24
Alessi 24	478	0.08	0.24	12	0.1	He et al. (2022), derived from A₀ = 0.3
NGC 1039	492	0.09	0.27	71	0.12	Malofeeva et al. (2023), derived from A_V = 0.328
UBC 9	344	0.10	0.32	13
Alessi 10	434	0.14	0.43	14	0.2	He et al. (2022), derived from A₀ = 0.6
Alessi 3	275	0.14	0.44	10	0.16	He et al. (2022), derived from A₀ = 0.5
NGC 2516	407	0.20	0.61	418	0.14	Sagar (1987)
Melotte 22	135	0.20	0.61	142	0.03	O’dell et al. (1994)
UBC 7	274	0.21	0.64	11
NGC 1901	415	0.21	0.66	18	0.04	Carraro et al. (2007)
Melotte 25	46	0.48^a	1.50	82	≤0.001	Taylor (2006)
IC 2391	151	0.58^a	1.79	34	0.006	Patten & Simon (1996)
Melotte 20	173	0.58^a	1.80	79	negligible	Ayres (2017)
IC 2602	150	0.67^a	2.07	35	0	Arenou et al. (2018), most likely A_g = 0

Notes. Some reference reddenings are determined from the reported extinction. In both cases, we assumed R_V = 3.1. ^a These are upper limits. Most of the extinction comes from behind the clusters. This is true for all clusters in our list, but we emphasise this specifically for clusters with higher E(B-V) from dustmaps.

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