NGC 6940
(Melotte 232; Collinder 424; MWSC 3370; OCL 141; FoF 2054)
1.0
UTI
1.0
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Stellar density (N50/rad)
45.1 [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
Overview
NGC 6940 is a very rich, very dense object of very high C3 quality. Its parallax locates it at a relatively close distance, below the mid-plane, affected by low extinction. It is catalogued as a massive, near-solar metallicity, intermediate-age 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 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 | 99999â | 308.639 | 28.284 | 0.956 | -1.952 | -9.431 | 8.069 |
| Malhotra et al. | 2026 | 308.618 | 28.285 | â | â | â | â |
| Li et al. | 2025 | 308.626 | 28.278 | 0.947 | -1.954 | -9.413 | â |
| Hu & Soubiran | 2025 | 308.633 | 28.292 | â | â | â | â |
| Wei et al. | 2025 | 308.634 | 28.28 | 0.961 | -1.939 | -9.43 | â |
| Almeida et al. | 2025 | 308.615 | 28.273 | â | â | â | â |
| Hunt & Reffert | 2024 | 308.591 | 28.258 | 0.958 | -1.954 | -9.437 | 8.023 |
| Cavallo et al. | 2024 | 308.633 | 28.292 | 0.959 | â | â | â |
| Hunt & Reffert | 2023 | 308.591 | 28.258 | 0.958 | -1.954 | -9.437 | 8.023 |
| Almeida et al. | 2023 | 308.557 | 28.304 | â | â | â | â |
| Cordoni et al. | 2023 | 308.615 | 28.273 | 0.95 | -1.958 | -9.411 | â |
| Just et al. | 2023 | 308.604 | 28.277 | â | â | â | â |
| He et al. | 2022 | 308.628 | 28.294 | 0.958 | -1.949 | -9.437 | â |
| Tarricq et al. | 2022 | 308.626 | 28.249 | 0.959 | -1.941 | -9.43 | â |
| Jadhav & Subramaniam | 2021 | 308.626 | 28.278 | â | â | â | â |
| Jaehnig et al. | 2021 | 308.619 | 28.269 | 0.977 | -1.977 | -9.415 | â |
| Rain et al. | 2021 | 308.626 | 28.278 | 0.947 | -1.954 | -9.413 | â |
| Dias et al. | 2021 | 308.615 | 28.273 | 0.95 | -1.958 | -9.411 | 8.047 |
| Cantat-Gaudin et al. | 2020 | 308.626 | 28.278 | 0.947 | -1.954 | -9.413 | â |
| Cantat-Gaudin & Anders | 2020 | 308.626 | 28.278 | 0.947 | -1.954 | -9.413 | â |
| Liu & Pang | 2019 | 308.632 | 28.299 | 0.951 | -1.971 | -9.398 | â |
| Bossini et al. | 2019 | 308.626 | 28.278 | â | â | â | â |
| Soubiran et al. | 2018 | 308.626 | 28.278 | â | â | â | 8.1 |
| Bica et al. | 2019 | 308.612 | 28.317 | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 308.626 | 28.278 | 0.947 | -1.954 | -9.413 | â |
| Loktin & Popova | 2017 | 308.61 | 28.283 | â | -0.935 | -1.834 | 4.7 |
| Kharchenko et al. | 2016 | 308.604 | 28.277 | â | â | â | â |
| Dias et al. | 2014 | 308.608 | 28.283 | â | -3.4 | -4.47 | â |
| Kharchenko et al. | 2013 | 308.61 | 28.28 | â | -1.6 | -8.69 | 4.7 |
| Gozha et al. | 2012 | 308.608 | 28.283 | â | â | â | â |
| Piskunov et al. | 2008 | 308.604 | 28.273 | â | â | â | â |
| Kharchenko et al. | 2007 | 308.61 | 28.28 | â | 0.5 | â | 4.66 |
| Piskunov et al. | 2007 | 308.604 | 28.273 | â | â | â | â |
| Ahumada & Lapasset | 2007 | 308.6 | 28.283 | â | â | â | â |
| van den Bergh | 2006 | 308.6 | 28.283 | â | â | â | â |
| Kharchenko et al. | 2005 | 308.61 | 28.28 | â | -1.5 | -8.93 | 4.42 |
| Kharchenko et al. | 2003 | 308.62 | 28.28 | â | -1.74 | -9.11 | â |
| Chen et al. | 2003 | 308.656 | 28.302 | â | -2.23 | -9.7 | 7.7 |
| Dias et al. | 2002 | 308.608 | 28.283 | â | -3.4 | -4.47 | 7.89 |
| Lynga | 1987 | 308.647 | 28.308 | â | â | â | 4.0 |
| Sulentic et al. | 1973 | 308.637 | 28.303 | â | â | â | 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 | 0.99 | 0.66 | 0.67 | 934 | 0.010 | 1302 | 0.43 | 2 |
| Malhotra et al. | 2026 | 1.01 | 0.45 | â | 975 | 0.009 | â | â | â |
| Li et al. | 2025 | 0.97 | 0.58 | â | 1209 | -0.050 | â | â | â |
| Hu & Soubiran | 2025 | â | â | â | â | -0.120(5) | â | â | â |
| Wei et al. | 2025 | 0.98 | 0.30 | â | 912 | 0.500 | 1356 | 0.32 | â |
| Almeida et al. | 2025 | 0.99 | 0.69 | â | 1175 | â | 1293 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 2132(1) | â | â |
| Cavallo et al. | 2024 | 1.06 | 0.78 | â | 851 | 0.170 | â | â | â |
| Hunt & Reffert | 2023 | 0.99 | 0.45 | 0.67 | 769 | â | â | â | â |
| Almeida et al. | 2023 | 1.00 | 0.71 | â | 1052 | 0.008 | 1393(1) | 0.49 | â |
| Cordoni et al. | 2023 | 0.99 | 0.69 | â | 1175 | -0.032 | 1310 | 0.43 | 1(1) |
| Just et al. | 2023 | â | â | â | 955 | â | 149 | â | â |
| He et al. | 2022 | â | 0.80 | â | 891 | â | â | â | â |
| Tarricq et al. | 2022 | 1.07 | â | â | 1380 | â | â | â | â |
| Jadhav & Subramaniam | 2021 | 1.10 | 0.41 | â | 1349 | â | 2698 | â | 2(1) |
| Jaehnig et al. | 2021 | 1.03(1) | â | â | â | â | â | â | â |
| Rain et al. | 2021 | 1.02 | 0.66 | â | 708 | â | â | â | 2 |
| Dias et al. | 2021 | 0.99 | 0.69 | â | 1175 | -0.032 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 1.10 | 0.41 | â | 1349 | â | â | â | â |
| Kounkel et al. | 2020 | 1.03 | 0.88 | â | 724 | â | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 1.02 | â | â | â | â | â | â | â |
| Liu & Pang | 2019 | â | â | â | 1950 | -0.500 | â | â | â |
| Bossini et al. | 2019 | 1.03 | 0.46 | â | 1023 | 0.150 | â | â | â |
| Soubiran et al. | 2018 | 1.02 | â | â | â | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 1.02 | â | â | â | â | â | â | â |
| Loktin & Popova | 2017 | 0.84 | 0.65 | â | 757 | â | â | â | â |
| Kharchenko et al. | 2016 | 0.84 | 0.66 | â | 955 | â | â | â | â |
| Kharchenko et al. | 2013 | 0.84 | 0.66 | â | 955 | 0.013 | â | â | â |
| Gozha et al. | 2012 | 0.77 | â | â | 721 | 0.010 | 363 | â | â |
| Piskunov et al. | 2008 | 0.77 | 0.66 | â | 871 | â | 589(1) | â | â |
| Piskunov et al. | 2007 | 0.77 | 0.66 | â | 871 | â | 185 | â | â |
| Ahumada & Lapasset | 2007 | â | 0.66 | â | 724 | â | â | â | 6 |
| van den Bergh | 2006 | 0.77 | 0.66 | â | 724 | â | â | â | â |
| Kharchenko et al. | 2005 | 0.77 | 0.66 | â | 871 | â | â | â | â |
| Kharchenko et al. | 2003 | 0.77 | 0.66 | â | â | â | â | â | â |
| Chen et al. | 2003 | 0.77 | 0.68 | â | 720 | 0.010(1) | â | â | â |
| Dias et al. | 2002 | 0.77 | 0.68 | â | 721 | 0.013 | â | â | â |
| Lynga | 1987 | 0.80 | 0.76 | â | 1096 | 0.040 | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Malhotra et al. (2026)
Lowest/Highest stellar mass in the catalogue with a mass-ratio estimate: 0.5/1.83 Msun
Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit. Gold sample.
Cavallo et al. (2024)
Gold sample.
Hunt & Reffert (2024)
Classified as open cluster. CMD class: 1.00 (50th percentile).
Rain et al. (2021)
This cluster was include in (Dias et al., 2002A&A...389..871D, Cat. B/ocl) however, parameters log(t)=9.010, Av =0.455, [Fe/H]=+ 0.150 were taken from Bossini et al. (2019A&A...623A.108B, Cat. J/A+A/623/A108). Apparently, star Gaia DR2 1857459766532229248 is a massive straggler.
Ahumada & Lapasset (2007)
The following membership probabilities are from (1972A&A....16...58S): star 50, 83%; star 70, 90%; star 153, 90%; star 172=HD 334735, 89%; star 175, 85%; star 179=HD 334755, 83%. Some spectra: star 50, F0 (1957AJ.....62..175V); star 70, F5II-III (1958ApJ...128..562W); star 153, A0 (1960StoAn..20i...1L); star 175, A5 (1960StoAn..20i...1L); star 179, A0 (1960StoAn..20i...1L). Stars 70 and 77 are cited as blue stragglers in (1988PASP..100..338G).