Berkeley 35

(FSR 1075; MWSC 1129; OCL 541; MWSC 1130)

0.84 UTI

0.81

C_N

0.97

C_dens

0.75

C_C3

0.84

C_lit

1.0

C_dup

N_m (P>50%) 259

Core radius and density 1.4 [pc], 4.9 [pc^-2]

C3 classification AB

C_N 0.81 Rich
C_dens 0.97 Very dense
C_C3 0.75 High quality
C_lit 0.84 Well-studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

MOCA 🔍 CDS 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

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Berkeley 35 is a rich, very dense object of high C3 quality. Its parallax locates it at a large distance, above the mid-plane, affected by low extinction. It is catalogued as a near-solar metallicity, old cluster, but with a large variance across recent sources for the metallicity and mass parameters (see Parameters). It is well-studied in the literature.

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

Distant Low extinction Near-solar metallicity Old Contains BSS

Almeida et al. (2025)
Mass determination: invalid due to poor quality CMD. Isochrone match: worst fit.

Cavallo et al. (2024)
Gold sample.

Hunt & Reffert (2024)
Classified as open cluster. CMD class: 0.98 (50th percentile).

Hunt & Reffert (2023)
Classified as open cluster. CMD class: 0.98 (50th percentile).

Hu et al. (2021)
Ellipticities (core, all): e_core=0.0175, e_all=0.0544.

Data

🔍 Search references for Berkeley 35 in: SciX Simbad

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Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	99999–	107.486	2.733	0.181	-0.607	-0.251	81.2
Li et al.	2025	107.491	2.734	0.16	-0.58	-0.235	–
Hu & Soubiran	2025	107.482	2.729	–	–	–	–
Almeida et al.	2025	107.489	2.734	–	–	–	–
Zhang et al.	2024	107.48	2.731	–	–	–	–
Hunt & Reffert	2024	107.48	2.731	0.177	-0.611	-0.255	84.127
Cavallo et al.	2024	107.482	2.729	0.176	–	–	–
Hunt & Reffert	2023	107.48	2.731	0.177	-0.611	-0.255	84.127
Just et al.	2023	107.477	2.735	–	–	–	–
Jadhav & Subramaniam	2021	107.491	2.734	–	–	–	–
Netopil et al.	2022	107.491	2.733	0.17	-0.564	-0.24	101.46
Dias et al.	2021	107.489	2.734	0.162	-0.587	-0.235	–
Cantat-Gaudin et al.	2020	107.491	2.734	0.16	-0.58	-0.235	–
Cantat-Gaudin & Anders	2020	107.491	2.734	0.16	-0.58	-0.235	–
Soubiran et al.	2018	107.491	2.734	–	–	–	101.46
Bica et al.	2019	107.482	2.736	–	–	–	–
Cantat-Gaudin et al.	2018	107.491	2.734	0.16	-0.58	-0.235	–
Dias et al.	2018	–	–	–	-0.1	-0.54	–
Loktin & Popova	2017	107.49	2.734	–	-7.384	-0.022	–
Sampedro et al.	2017	107.483	2.734	–	-1.58	3.76	–
Kharchenko et al.	2016	107.477	2.735	–	–	–	–
Dias et al.	2014	107.483	2.734	–	-3.29	3.34	–
Kharchenko et al.	2013	107.484	2.733	–	-7.78	2.28	–
Bukowiecki et al.	2011	107.483	2.725	–	–	–	–
Froebrich et al.	2007	107.5	2.716	–	–	–	–
Dias et al.	2002	107.483	2.734	–	-3.29	3.34	–
Lynga	1987	107.706	2.738	–	–	–	–

💡 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]	B_frac	BSS
UCC	99999–	4.865	0.41	0.73	1130	-0.206	994	–	2
Li et al.	2025	4.97	0.40	–	1049	-0.075	–	–	–
Hu & Soubiran	2025	–	–	–	–	-0.320⁽⁵⁾	–	–	–
Almeida et al.	2025	4.64	0.65	–	1130	–	264	–	–
Zhang et al.	2024	–	–	–	–	-0.206⁽¹⁾	–	–	–
Hunt & Reffert	2024	5.95	0.23	0.73	827	–	1400⁽¹⁾	–	–
Cavallo et al.	2024	3.25	0.41	–	1905	-0.390	–	–	–
Hunt & Reffert	2023	5.95	0.23	0.73	828	–	–	–	–
Just et al.	2023	–	–	–	1161	–	885	–	–
Jadhav & Subramaniam	2021	4.74	0.43	–	1175	–	994	–	2⁽¹⁾
Netopil et al.	2022	5.89⁽¹⁾	0.41	–	1000	-0.130⁽¹⁾	–	–	–
Dias et al.	2021	4.64	0.65	–	1130	-0.301	–	–	–
Cantat-Gaudin et al.	2020	4.74	0.43	–	1175	–	–	–	–
Kounkel et al.	2020	4.74	0.57	–	708	–	–	–	–
Cantat-Gaudin & Anders	2020	5.28	–	–	–	–	–	–	–
Soubiran et al.	2018	5.28	–	–	–	–	–	–	–
Cantat-Gaudin et al.	2018	5.28	–	–	–	–	–	–	–
Loktin & Popova	2017	3.37	0.00	–	1380	–	–	–	–
Kharchenko et al.	2016	5.01	0.00	–	1161	–	–	–	–
Kharchenko et al.	2013	5.01	0.00	–	1161	–	–	–	–
Bukowiecki et al.	2012	–	–	–	–	–	2942	–	–
Bukowiecki et al.	2011	4.76⁽¹⁾	0.00	–	1000	–	–	–	–
Dias et al.	2002	4.39	1.48	–	891	-0.130	–	–	–

(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.

Visualization

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