Melotte 39
(Collinder 78; NGC 2126; FSR 0730; MWSC 708; OCL 418)
0.96
UTI
0.8
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Stellar density (N50/rad)
20.2 [N/pc2]
- CN 0.8 Rich
- Cdens 1.0 Very dense
- CC3 1.0 Very high quality
- Clit 1.0 Very well-studied
- Cdup 1.0 Unique
Overview
Melotte 39 is a rich, very dense object of very high C3 quality. Its parallax locates it at a relatively close 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 very well-studied in the literature.
Note: This object shares a large percentage of members with a later reported entry. See table with shared members information.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 90.662 | 49.88 | 0.756 | 0.813 | -2.6 | -12.886 |
| Li et al. | 2025 | 90.658 | 49.883 | 0.747 | 0.848 | -2.615 | â |
| Hu & Soubiran | 2025 | 90.671 | 49.89 | â | â | â | â |
| Almeida et al. | 2025 | 90.657 | 49.895 | â | â | â | â |
| Zhang et al. | 2024 | 90.65 | 49.872 | â | â | â | â |
| Hunt & Reffert | 2024 | 90.65 | 49.872 | 0.76 | 0.817 | -2.601 | -12.705 |
| Cavallo et al. | 2024 | 90.671 | 49.89 | 0.761 | â | â | â |
| Hunt & Reffert | 2023 | 90.65 | 49.872 | 0.76 | 0.817 | -2.601 | -12.705 |
| Almeida et al. | 2023 | 90.639 | 49.896 | â | â | â | â |
| Just et al. | 2023 | 90.636 | 49.873 | â | â | â | â |
| Tarricq et al. | 2022 | 90.638 | 49.883 | 0.759 | 0.822 | -2.589 | â |
| Jaehnig et al. | 2021 | 90.655 | 49.879 | 0.78 | 0.863 | -2.603 | â |
| Dias et al. | 2021 | 90.657 | 49.895 | 0.743 | 0.841 | -2.606 | -11.741 |
| Cantat-Gaudin et al. | 2020 | 90.658 | 49.883 | 0.747 | 0.848 | -2.615 | â |
| Cantat-Gaudin & Anders | 2020 | 90.658 | 49.883 | 0.747 | 0.848 | -2.615 | â |
| Bica et al. | 2019 | 90.631 | 49.873 | â | â | â | â |
| Loktin & Popova | 2017 | 90.645 | 49.872 | â | -0.152 | -0.8 | â |
| Kharchenko et al. | 2016 | 90.636 | 49.873 | â | â | â | â |
| Dias et al. | 2014 | 90.621 | 49.918 | â | -0.63 | -1.62 | â |
| Kharchenko et al. | 2013 | 90.648 | 49.872 | â | -1.38 | -1.71 | â |
| Kharchenko et al. | 2012 | 90.648 | 49.872 | â | -1.38 | -1.71 | â |
| Froebrich et al. | 2007 | 90.638 | 49.873 | â | â | â | â |
| Dias et al. | 2002 | 90.621 | 49.918 | â | -0.63 | -1.62 | â |
đĄ 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 | 99999â | 1.24 | 0.675 | 0.41 | 1535 | -0.175 | 314 | 0.63 | â |
| Li et al. | 2025 | 1.20 | 0.69 | â | 1811 | -0.240 | â | â | â |
| Hu & Soubiran | 2025 | â | â | â | â | -0.210(5) | â | â | â |
| Almeida et al. | 2025 | 1.23 | 0.67 | â | 1535 | â | 352 | â | â |
| Zhang et al. | 2024 | â | â | â | â | -0.221(1) | â | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 610(1) | â | â |
| Cavallo et al. | 2024 | 1.29 | 0.77 | â | 1413 | 0.080 | â | â | â |
| Hunt & Reffert | 2023 | 1.24 | 0.35 | 0.41 | 1778 | â | â | â | â |
| Almeida et al. | 2023 | 1.25 | 0.81 | â | 1517 | -0.141 | 275(1) | 0.63 | â |
| Just et al. | 2023 | â | â | â | 2818 | â | 97 | â | â |
| Tarricq et al. | 2022 | 1.26 | â | â | 977 | â | â | â | â |
| Jaehnig et al. | 2021 | 1.28(1) | â | â | â | â | â | â | â |
| Dias et al. | 2021 | 1.23 | 0.67 | â | 1535 | 0.016 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 1.31 | 0.68 | â | 977 | â | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 1.29 | â | â | â | â | â | â | â |
| Loktin & Popova | 2017 | 2.14 | 0.78 | â | 891 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.10 | 0.16 | â | 2818 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.10 | 0.16 | â | 2818 | â | â | â | â |
| Kharchenko et al. | 2012 | 1.10 | 0.16 | â | 2818 | â | â | â | â |
| Dias et al. | 2002 | 1.09 | 0.84 | â | 1259 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit.
Cavallo et al. (2024)
Gold sample.