Berkeley 25

(MWSC 955; OCL 576)

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0.80 UTI
0.83
CN
1.0
Cdens
0.75
CC3
0.72
Clit
1.0
Cdup
N50 (P>50% members) 308
Stellar density (N50/rad) 10.0 [N/pc2]
C3 classification AB
  • CN 0.83 Rich
  • Cdens 1.0 Very dense
  • CC3 0.75 High quality
  • Clit 0.72 Moderately studied
  • Cdup 1.0 Unique
đŸ“Ĩ Members 📊 Colab đŸ”Ŧ Bayestar19 MOCAMOCA 🔍 CDS 🔍 Simbad 🔍 CDS (Îą, δ) 🔍 Simbad (Îą, δ)

Overview
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Berkeley 25 is a rich, very dense object of 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 very massive, near-solar metallicity, very old cluster, but with a large variance across recent sources for the age, metallicity, and mass parameters (see Parameters). It is moderately studied in the literature.

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

Cavallo et al. (2024)
Gold sample.

Hunt & Reffert (2024)
Classified as open cluster. CMD class: 0.17 (50th percentile).

Perren et al. (2022)
The CMD shows a clear giant branch and several stars above the TO that are BSS candidates. The RDP yields a radius of ~5', the largest in the sample. Carraro 2005 used a much smaller 0.8' radius and obtained 3.0 Gyr and 11.3 kpc; Carraro 2007 gives 5 Gyr and 13.2 kpc. ASteCA estimates 7.4 kpc and 5.2 Gyr, placing the cluster considerably closer than the Carraro et al. values and most databases (>11 kpc). CG20 gives a similar distance of 6.8 kpc but a much younger age of 2.5 Gyr. The underestimated cluster region likely explains the discrepancies with Carraro et al.

Data
🔍 Search references for Berkeley 25 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– 100.314 -16.484 0.105 -0.128 0.865 133.125
Hu & Soubiran 2025 100.318 -16.489 – – – –
Hunt & Reffert 2024 100.312 -16.487 0.096 -0.112 0.877 122.755
Cavallo et al. 2024 100.318 -16.489 0.103 – – –
Hunt & Reffert 2023 100.312 -16.487 0.096 -0.112 0.877 122.755
Just et al. 2023 100.299 -16.493 – – – –
Perren et al. 2022 100.317 -16.487 – – – –
Jadhav & Subramaniam 2021 100.317 -16.487 – – – –
Cantat-Gaudin et al. 2020 100.317 -16.487 0.077 -0.114 0.845 –
Cantat-Gaudin & Anders 2020 100.317 -16.487 0.077 -0.114 0.845 –
Bica et al. 2019 100.31 -16.476 – – – –
Cantat-Gaudin et al. 2018 100.317 -16.487 0.077 -0.114 0.845 –
Loktin & Popova 2017 100.305 -16.495 – -0.215 -0.918 134.3
Kharchenko et al. 2016 100.299 -16.493 – – – –
Dias et al. 2014 100.25 -16.517 – -3.68 -4.17 –
Kharchenko et al. 2013 100.305 -16.495 – 1.53 -2.21 134.3
Gozha et al. 2012 100.25 -16.517 – – – –
Bukowiecki et al. 2011 100.304 -16.493 – – – –
Dias et al. 2002 100.25 -16.517 – -3.68 -4.17 134.3
Lynga 1987 100.258 -16.511 – – – –

💡 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] Bfrac BSS
UCC 99999– 7.605 1.07 2.03 5012 -0.200 8560 0.82 2
Hu & Soubiran 2025 – – – – -0.360(5) – – –
Hunt & Reffert 2024 – – – – – 2119(1) – –
Cavallo et al. 2024 6.31 1.18 – 4169 -0.560 – – –
Hunt & Reffert 2023 7.69 1.65 2.03 929 – – – –
Just et al. 2023 – – – 5012 – 16331 – –
Perren et al. 2022 7.38 1.23 – 5248 -0.200 15000 0.82 –
Spina et al. 2022 – – – – -0.356 – – –
Jadhav & Subramaniam 2021 6.79 1.07 – 2455 – 955 – 2(1)
Cantat-Gaudin et al. 2020 6.79 1.07 – 2455 – – – –
Kounkel et al. 2020 7.50 0.85 – 3236 – – – –
Cantat-Gaudin & Anders 2020 9.47 – – – – – – –
Cantat-Gaudin et al. 2018 9.47 – – – – – – –
Loktin & Popova 2017 2.38 1.76 – 6310 – – – –
Kharchenko et al. 2016 11.40 0.35 – 5012 – – – –
Kharchenko et al. 2013 11.40 0.35 – 5012 -0.200 – – –
Gozha et al. 2012 11.40 – – 5012 -0.200 – – –
Bukowiecki et al. 2011 7.52(1) 0.47 – 6310 – – – –
Dias et al. 2002 11.40 0.35 – 5012 -0.200 – – –

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

Visualization
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Berkeley 25 UCC
Berkeley 25 HUNT23
Berkeley 25 CANTAT20
Galactocentric position diagram