Melotte 80
(Collinder 170; NGC 2506; MWSC 1406; OCL 593; FSR 1230; FoF 634)
1.0
UTI
1.0
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
N50 (P>50% members)
2044
Stellar density (N50/rad)
73.1 [N/pc2]
- 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
π₯ Members
π Colab
π¬ Bayestar19
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
Overview
Melotte 80 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 very massive, near-solar metallicity, old cluster, but with a large variance across recent sources for the absorption, metallicity, and mass parameters (see Parameters). It is very well-studied in the literature.
Note: This object contains blue stragglers according to at least one source.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999β | 120.009 | -10.774 | 0.281 | -2.557 | 3.966 | 83.937 |
| Li et al. | 2025 | 120.01 | -10.773 | 0.292 | -2.571 | 3.912 | β |
| Hu & Soubiran | 2025 | 120.011 | -10.775 | β | β | β | β |
| Carrasco-Varela et al. | 2025 | 120.225 | -10.835 | β | β | β | β |
| Almeida et al. | 2025 | 120.011 | -10.775 | β | β | β | β |
| Hunt & Reffert | 2024 | 120.002 | -10.77 | 0.279 | -2.561 | 3.965 | 82.351 |
| Cavallo et al. | 2024 | 120.011 | -10.775 | 0.278 | β | β | β |
| Rain et al. | 2024 | 120.009 | -10.774 | 0.282 | -2.557 | 3.969 | β |
| Hunt & Reffert | 2023 | 120.002 | -10.77 | 0.279 | -2.561 | 3.965 | 82.351 |
| Just et al. | 2023 | 119.993 | -10.757 | β | β | β | β |
| Jaehnig et al. | 2021 | 120.008 | -10.773 | 0.317 | -2.568 | 3.917 | β |
| Rain et al. | 2021 | 120.01 | -10.773 | 0.292 | -2.571 | 3.912 | β |
| Dias et al. | 2021 | 120.011 | -10.775 | 0.296 | -2.569 | 3.911 | 83.049 |
| Cantat-Gaudin et al. | 2020 | 120.01 | -10.773 | 0.292 | -2.571 | 3.912 | β |
| SΓ‘nchez et al. | 2020 | 120.004 | -10.77 | β | -2.644 | 3.91 | β |
| Cantat-Gaudin & Anders | 2020 | 120.01 | -10.773 | 0.292 | -2.571 | 3.912 | β |
| Liu & Pang | 2019 | 120.012 | -10.775 | 0.317 | -2.56 | 3.896 | β |
| Soubiran et al. | 2018 | 120.01 | -10.773 | β | β | β | 84.9 |
| Bica et al. | 2019 | 120.012 | -10.773 | β | β | β | β |
| Cantat-Gaudin et al. | 2018 | 120.01 | -10.773 | 0.292 | -2.571 | 3.912 | β |
| Loktin & Popova | 2017 | 120.0 | -10.769 | β | -1.152 | 1.61 | 87.0 |
| Kharchenko et al. | 2016 | 119.993 | -10.757 | β | β | β | β |
| Dias et al. | 2014 | 120.004 | -10.77 | β | -1.87 | 1.96 | β |
| Kharchenko et al. | 2013 | 120.0 | -10.76 | β | -1.62 | 2.14 | 87.0 |
| Gozha et al. | 2012 | 120.004 | -10.77 | β | β | β | β |
| Piskunov et al. | 2008 | 119.998 | -10.769 | β | β | β | β |
| Kharchenko et al. | 2007 | 120.0 | -10.77 | β | 0.2 | β | β |
| van den Bergh | 2006 | 120.004 | -10.77 | β | β | β | β |
| Kharchenko et al. | 2005 | 120.0 | -10.77 | β | -5.87 | 1.79 | β |
| Chen et al. | 2003 | 119.994 | -10.783 | β | β | β | β |
| Dias et al. | 2002 | 120.004 | -10.77 | β | -1.87 | 1.96 | 83.25 |
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] | Bfrac | BSS |
|---|---|---|---|---|---|---|---|---|---|
| UCC | 99999β | 3.23 | 0.25 | 0.27 | 1622 | -0.264 | 7718 | 0.2 | 0.06 |
| Li et al. | 2025 | 3.25 | 0.28 | β | 2031 | -0.281 | β | β | β |
| Hu & Soubiran | 2025 | β | β | β | β | -0.310(5) | β | β | β |
| Carrasco-Varela et al. | 2025 | 3.23 | 0.26 | β | 2099 | -0.310 | β | β | 0.06(1) |
| Almeida et al. | 2025 | 3.23 | 0.26 | β | 2099 | β | 7718 | β | β |
| Hunt & Reffert | 2024 | β | β | β | β | β | 11701(1) | β | β |
| Cavallo et al. | 2024 | 2.51 | 0.56 | β | 2399 | -0.680 | β | β | β |
| Rain et al. | 2024 | 3.22 | 0.08 | β | 2133 | β | 19934 | 0.20 | β |
| Hunt & Reffert | 2023 | 3.17 | 0.03 | 0.27 | 2410 | β | β | β | β |
| Just et al. | 2023 | β | β | β | 1622 | β | 3296 | β | β |
| Jaehnig et al. | 2021 | 3.17(1) | β | β | β | β | β | β | β |
| Rain et al. | 2021 | 3.11 | 0.31 | β | 1000 | β | β | β | 14 |
| Dias et al. | 2021 | 3.23 | 0.26 | β | 2099 | -0.247 | β | β | β |
| Cantat-Gaudin et al. | 2020 | 3.19 | 0.09 | β | 1660 | β | β | β | β |
| Cantat-Gaudin & Anders | 2020 | 3.11 | β | β | β | β | β | β | β |
| Liu & Pang | 2019 | β | β | β | 2630 | 0.000 | β | β | β |
| Soubiran et al. | 2018 | 3.11 | β | β | β | β | β | β | β |
| Cantat-Gaudin et al. | 2018 | 3.11 | β | β | β | β | β | β | β |
| Loktin & Popova | 2017 | 3.67 | 0.30 | β | 1102 | β | β | β | β |
| Kharchenko et al. | 2016 | 3.53 | 0.13 | β | 1622 | β | β | β | β |
| Kharchenko et al. | 2013 | 3.53 | 0.13 | β | 1622 | -0.200 | β | β | β |
| Gozha et al. | 2012 | 3.46 | β | β | 1109 | -0.200 | 6918 | β | β |
| Piskunov et al. | 2008 | 3.46 | 0.25 | β | 1122 | β | β | β | β |
| van den Bergh | 2006 | 3.46 | 0.25 | β | 1096 | β | β | β | β |
| Kharchenko et al. | 2005 | 3.46 | 0.25 | β | 1122 | β | β | β | β |
| Chen et al. | 2003 | 3.46 | 0.25 | β | 1100 | -0.370(1) | β | β | β |
| Dias et al. | 2002 | 3.75 | 0.31 | β | 1000 | -0.200 | β | β | β |
(N): Indicates that there are N extra values assigned to this parameter 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)
Except for one BSS near the ZAMS, all candidates follow binary evolution tracks over a broad luminosity range. The BSS population is small, and no YSSs are detected.