Berkeley 22

(MWSC 698; OCL 490)

0.97 UTI

0.86

C_N

1.0

C_dens

1.0

C_C3

1.0

C_lit

1.0

C_dup

C3 classification AA

Number of members (P>50%) 406

Radius (P>50% members) 1.9 [arcmin]

C_N 0.86 Rich
C_dens 1.0 Very dense
C_C3 1.0 Very high quality
C_lit 1.0 Very well-studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

Berkeley 22 is a rich, very dense object of very high C3 quality. Its parallax locates it at a large distance, well below the mid-plane, affected by moderate extinction. It is catalogued as a massive, near-solar metallicity, old cluster, but with a large variance across recent sources for the age parameter (see Parameters). It is very well-studied in the literature.

Note: This object contains blue stragglers according to at least one source.

Note: This object shares a very small percentage of members with a later reported entry. See table with shared members information.

Very distant Moderate extinction Massive Near-solar metallicity Old Contains BSS

Cavallo et al. (2024): Gold sample.

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	89.615	7.757	0.13	0.629	-0.404	90.907
Hu & Soubiran	2025	89.617	7.753	–	–	–	–
Hunt & Reffert	2024	89.615	7.759	0.134	0.564	-0.39	87.412
Cavallo et al.	2024	89.617	7.753	0.148	–	–	–
Hunt & Reffert	2023	89.615	7.759	0.134	0.564	-0.39	87.412
Just et al.	2023	89.624	7.758	–	–	–	–
Jaehnig et al.	2021	89.623	7.764	0.1	0.616	-0.456	–
Rain et al.	2021	89.618	7.763	0.069	0.648	-0.473	–
Cantat-Gaudin et al.	2020	89.618	7.763	0.069	0.648	-0.473	–
Soubiran et al.	2018	89.618	7.763	–	–	–	92.45
Bica et al.	2019	89.622	7.758	–	–	–	–
Cantat-Gaudin et al.	2018	89.618	7.763	0.069	0.648	-0.473	–
Loktin & Popova	2017	89.61	7.757	–	0.395	-1.002	95.3
Kharchenko et al.	2016	89.624	7.758	–	–	–	–
Kharchenko et al.	2013	89.631	7.757	–	1.81	-3.93	95.3
Kharchenko et al.	2007	89.61	7.76	–	0.01	–	–
Chen et al.	2003	89.601	7.837	–	–	–	–
Dias et al.	2002	89.612	7.757	–	1.81	-3.93	95.3

💡 Note: The UCC values are estimated from its identified members.

Reference	Year	Dist [kpc]	Av [mag]	DAv [mag]	Age [Myr]	[Fe/H] [dex]	Mass [Msun]	Bfr	BSS
Hu & Soubiran	2025	–	–	–	–	-0.300*	–	–	–
Hunt & Reffert	2024	–	–	–	–	–	1410*	–	–
Cavallo et al.	2024	6.22	1.52	–	2884	-0.260	–	–	–
Hunt & Reffert	2023	5.26	1.81	2.54	789	–	–	–	–
Just et al.	2023	–	–	–	3162	–	703	–	–
Jaehnig et al.	2021	9.69*	–	–	–	–	–	–	–
Rain et al.	2021	10.15	1.83	–	3311	–	–	–	3
Cantat-Gaudin et al.	2020	6.22	1.99	–	2455	–	–	–	–
Soubiran et al.	2018	10.15	–	–	–	–	–	–	–
Cantat-Gaudin et al.	2018	10.15	–	–	–	–	–	–	–
Loktin & Popova	2017	7.32	2.20	–	995	–	–	–	–
Kharchenko et al.	2016	5.49	1.94	–	3162	–	–	–	–
Kharchenko et al.	2013	5.49	1.94	–	3162	-0.320	–	–	–
Chen et al.	2003	7.66	2.17	–	1060	-0.300*	–	–	–
Dias et al.	2002	6.00	1.83	–	3311	-0.320	–	–	–

💡 Note: The parameters are sometimes transformed from their original values to match the format of the columns shown here, see FAQ. The columns DAv, Bfr, BSS correspond to differential extinction, binary fraction, and blue stragglers, respectively. BSS values can be listed as fractions or integers.
(*): indicates that this parameter is assigned more than one value in the corresponding reference.

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
HSC 1586	6.2	89.61	7.76	0.25	0.67	-0.42	89.74	0.0

💡 Note: The % column shows the percentage of members that Berkeley 22 shares with each listed object.

Visualization

1 2 3

💡 Note: How are the galactocentric plots generated? See FAQ.