NGC 5269
(MWSC 2156; ESO 097 04; FoF 261)
0.96
UTI
0.79
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Stellar density (N50/rad)
40.0 [N/pc2]
- CN 0.79 Rich
- Cdens 1.0 Very dense
- CC3 1.0 Very high quality
- Clit 1.0 Very well-studied
- Cdup 1.0 Unique
đĨ Members
đ Colab
đŦ Bayestar19
MOCA
đ CDS
đ Simbad
đ CDS (Îą, δ)
đ Simbad (Îą, δ)
MOCA
đ CDS
đ Simbad
đ CDS (Îą, δ)
đ Simbad (Îą, δ)
Overview
NGC 5269 is a rich, very dense object of very high C3 quality. Its parallax locates it at a moderate distance, near the mid-plane, affected by moderate extinction. It is catalogued as a near-solar metallicity, intermediate-age cluster, but with a large variance across recent sources for the age, metallicity, and mass parameters (see Parameters). It is very well-studied in the literature.
Note: This object shares a very small 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 | 206.16 | -62.91 | 0.486 | -4.536 | -1.898 | -34.654 |
| Li et al. | 2025 | 206.147 | -62.907 | 0.46 | -4.49 | -1.918 | â |
| Almeida et al. | 2025 | 206.159 | -62.906 | â | â | â | â |
| Hunt & Reffert | 2024 | 206.167 | -62.906 | 0.481 | -4.541 | -1.898 | -37.778 |
| Cavallo et al. | 2024 | 206.177 | -62.906 | 0.483 | â | â | â |
| Hunt & Reffert | 2023 | 206.167 | -62.906 | 0.481 | -4.541 | -1.898 | -37.778 |
| Almeida et al. | 2023 | 206.162 | -62.91 | â | â | â | â |
| Just et al. | 2023 | 206.171 | -62.889 | â | â | â | â |
| Dias et al. | 2021 | 206.159 | -62.906 | 0.463 | -4.498 | -1.921 | -37.259 |
| Cantat-Gaudin et al. | 2020 | 206.147 | -62.907 | 0.46 | -4.49 | -1.918 | â |
| Cantat-Gaudin & Anders | 2020 | 206.147 | -62.907 | 0.46 | -4.49 | -1.918 | â |
| Liu & Pang | 2019 | 206.119 | -62.919 | 0.471 | -4.574 | -1.936 | â |
| Soubiran et al. | 2018 | 206.147 | -62.907 | â | â | â | -36.91 |
| Bica et al. | 2019 | 206.194 | -62.916 | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 206.147 | -62.907 | 0.46 | -4.49 | -1.918 | â |
| Kharchenko et al. | 2016 | 206.171 | -62.889 | â | â | â | â |
| Dias et al. | 2014 | 206.183 | -62.915 | â | -1.68 | -6.25 | â |
| Kharchenko et al. | 2013 | 206.182 | -62.892 | â | -7.03 | -1.19 | â |
| Morales et al. | 2013 | 206.183 | -62.915 | â | â | â | â |
| Dias et al. | 2002 | 206.183 | -62.915 | â | -1.68 | -6.25 | 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 | 1.8 | 1.365 | 2.03 | 174 | 0.000 | 400 | 0.58 | â |
| Li et al. | 2025 | 1.62 | 1.17 | â | 539 | -0.234 | â | â | â |
| Almeida et al. | 2025 | 1.80 | 1.44 | â | 124 | â | 334 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 1143(1) | â | â |
| Cavallo et al. | 2024 | 1.64 | 1.63 | â | 380 | -0.360 | â | â | â |
| Hunt & Reffert | 2023 | 1.91 | 1.29 | 2.03 | 223 | â | â | â | â |
| Almeida et al. | 2023 | 1.85 | 1.48 | â | 168 | 0.168 | 386(1) | 0.58 | â |
| Just et al. | 2023 | â | â | â | 331 | â | 415 | â | â |
| Dias et al. | 2021 | 1.80 | 1.44 | â | 124 | 0.153 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 2.08 | 0.99 | â | 132 | â | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 2.04 | â | â | â | â | â | â | â |
| Liu & Pang | 2019 | â | â | â | 174 | 0.000 | â | â | â |
| Soubiran et al. | 2018 | 2.04 | â | â | â | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 2.04 | â | â | â | â | â | â | â |
| Kharchenko et al. | 2016 | 1.63 | 1.29 | â | 331 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.63 | 1.29 | â | 331 | â | â | â | â |
| Morales et al. | 2013 | 1.41 | â | â | 160 | â | â | â | â |
| Dias et al. | 2002 | 1.41 | 1.61 | â | 158 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
Cantat-Gaudin & Anders (2020)
Marked non-existent historically; some Gaia-based work suggested a small co-moving group, but overall reality remains doubtful. More details in Appendix A of the article.
Palma et al. (2025)
Classified as optical pair P349, along with CWNU_2412.
Morales et al. (2013)
Classified as morphological type 'OC2' (totally exposed cluster without correlation with ATLASGAL emission). Morphological flag: exposed cluster, without submm emission.
Piecka & Paunzen (2021)
Belongs to cluster aggregate 'Agg51' along with SAI 118.
Cavallo et al. (2024)
Gold sample.
Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit. Silver sample.