Berkeley 39
(MWSC 1336; OCL 561; FSR 1174; FoF 633)
1.0
UTI
1.0
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Radius (P>50% members)
4.3 [arcmin]
- CN 1.0 Very rich
- Cdens 1.0 Very dense
- CC3 1.0 Very high quality
- Clit 1.0 Very well-studied
- Cdup 1.0 Unique
Overview
Berkeley 39 is a very rich, very dense object of very high C3 quality. Its parallax locates it at a moderate distance, well above the mid-plane, affected by low extinction. It is catalogued as a massive, near-solar metallicity, very old cluster, but with a large variance across recent sources for the metallicity and mass parameters (see Parameters). It is very well-studied in the literature.
Distant
Low extinction
Massive
Near-solar metallicity
Very old
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | β | 116.7 | -4.669 | 0.233 | -1.722 | -1.618 | 59.332 |
| Li et al. | 2025 | 116.702 | -4.665 | 0.201 | -1.73 | -1.645 | β |
| Hu & Soubiran | 2025 | 116.697 | -4.664 | β | β | β | β |
| Carrasco-Varela et al. | 2025 | 116.893 | -4.735 | β | β | β | β |
| Almeida et al. | 2025 | 116.695 | -4.658 | β | β | β | β |
| Zhang et al. | 2024 | 116.707 | -4.673 | β | β | β | β |
| Hunt & Reffert | 2024 | 116.707 | -4.673 | 0.231 | -1.732 | -1.631 | 59.873 |
| Cavallo et al. | 2024 | 116.697 | -4.664 | 0.228 | β | β | β |
| Hunt & Reffert | 2023 | 116.707 | -4.673 | 0.231 | -1.732 | -1.631 | 59.873 |
| Just et al. | 2023 | 116.701 | -4.678 | β | β | β | β |
| Jaehnig et al. | 2021 | 116.706 | -4.669 | 0.225 | -1.739 | -1.646 | β |
| Rain et al. | 2021 | 116.702 | -4.665 | 0.201 | -1.73 | -1.645 | β |
| Dias et al. | 2021 | 116.695 | -4.658 | 0.207 | -1.724 | -1.648 | 60.117 |
| Cantat-Gaudin et al. | 2020 | 116.702 | -4.665 | 0.201 | -1.73 | -1.645 | β |
| SΓ‘nchez et al. | 2020 | 116.675 | -4.6 | β | -1.605 | -1.63 | β |
| Cantat-Gaudin & Anders | 2020 | 116.702 | -4.665 | 0.201 | -1.73 | -1.645 | β |
| Liu & Pang | 2019 | 116.695 | -4.655 | 0.268 | -1.679 | -1.643 | β |
| Soubiran et al. | 2018 | 116.702 | -4.665 | β | β | β | 59.89 |
| Bica et al. | 2019 | 116.695 | -4.666 | β | β | β | β |
| Cantat-Gaudin et al. | 2018 | 116.702 | -4.665 | 0.201 | -1.73 | -1.645 | β |
| Loktin & Popova | 2017 | 116.7 | -4.68 | β | -1.373 | -3.361 | 55.0 |
| Kharchenko et al. | 2016 | 116.701 | -4.678 | β | β | β | β |
| Dias et al. | 2014 | 116.675 | -4.6 | β | -2.97 | -2.57 | β |
| Kharchenko et al. | 2013 | 116.707 | -4.68 | β | -2.5 | -1.01 | 55.0 |
| Gozha et al. | 2012 | 116.675 | -4.6 | β | β | β | β |
| Kharchenko et al. | 2007 | 116.67 | -4.6 | β | 0.06 | β | β |
| van den Bergh | 2006 | 116.675 | -4.6 | β | β | β | β |
| Chen et al. | 2003 | 116.67 | -4.601 | β | β | β | β |
| Dias et al. | 2002 | 116.675 | -4.6 | β | -2.97 | -2.57 | 57.8 |
π‘ 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 |
|---|---|---|---|---|---|---|---|---|---|
| Li et al. | 2025 | 4.25 | 0.51 | β | 5919 | -0.156 | β | β | β |
| Hu & Soubiran | 2025 | β | β | β | β | -0.250* | β | β | β |
| Carrasco-Varela et al. | 2025 | 4.16 | 0.39 | β | 6471 | 0.000 | β | β | 0.14* |
| Almeida et al. | 2025 | 4.36 | 0.39 | β | 6471 | β | 6456 | β | β |
| Zhang et al. | 2024 | β | β | β | β | -0.196* | β | β | β |
| Hunt & Reffert | 2024 | β | β | β | β | β | 3576* | β | β |
| Cavallo et al. | 2024 | 3.27 | 0.72 | β | 6918 | -0.550 | β | β | β |
| Hunt & Reffert | 2023 | 3.90 | 0.25 | 1.10 | 3126 | β | β | β | β |
| Just et al. | 2023 | β | β | β | 3162 | β | 1312 | β | β |
| Jaehnig et al. | 2021 | 4.67* | β | β | β | β | β | β | β |
| Rain et al. | 2021 | 4.36 | 0.37 | β | 7943 | β | β | β | 18 |
| Dias et al. | 2021 | 4.36 | 0.39 | β | 6471 | -0.109 | β | β | β |
| Cantat-Gaudin et al. | 2020 | 3.96 | 0.29 | β | 5623 | β | β | β | β |
| Cantat-Gaudin & Anders | 2020 | 4.36 | β | β | β | β | β | β | β |
| Liu & Pang | 2019 | β | β | β | 12300 | -1.750 | β | β | β |
| Soubiran et al. | 2018 | 4.36 | β | β | β | β | β | β | β |
| Cantat-Gaudin et al. | 2018 | 4.36 | β | β | β | β | β | β | β |
| Loktin & Popova | 2017 | 3.66 | 1.34 | β | 1230 | β | β | β | β |
| Kharchenko et al. | 2016 | 4.84 | 0.13 | β | 3162 | β | β | β | β |
| Kharchenko et al. | 2013 | 4.84 | 0.13 | β | 3162 | -0.260 | β | β | β |
| Gozha et al. | 2012 | 4.78 | β | β | 7943 | -0.210 | β | β | β |
| van den Bergh | 2006 | 4.73 | 0.37 | β | 7943 | β | β | β | β |
| Chen et al. | 2003 | 4.78 | 0.37 | β | 7940 | -0.170* | β | β | β |
| Dias et al. | 2002 | 4.78 | 0.37 | β | 7943 | -0.200 | β | β | β |
(*): Indicates that this parameter is assigned more than one value in the corresponding reference.


Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit. Gold sample.
Cavallo et al. (2024)
Gold sample.
Rain et al. (2024)
BSS candidates form two groups: faint objects consistent with low-mass donors and redder, brighter BSSs matched by higher-mass donor models. Two YSSs are present. Some stars may be misidentified or require alternative binary parameters.