Collinder 140
(MWSC 1199; FoF 2397; OCSN 191)
- CN 0.82 Rich
- Cdens 1.0 Very dense
- CC3 1.0 Very high quality
- Clit 1.0 Very well-studied
- Cdup 1.0 Unique
Overview
Collinder 140 is a rich, very dense object of very high C3 quality. Its parallax locates it at a very close distance, near the mid-plane. It is catalogued as a near-solar metallicity, young cluster, but with a large variance across recent sources for the absorption parameter (see Parameters). It is very well-studied in the literature.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | – | 110.904 | -31.986 | 2.601 | -8.079 | 4.766 | 16.809 |
| Almeida et al. | 2025 | 110.846 | -32.004 | – | – | – | – |
| Alfonso et al. | 2024 | 110.907 | -31.984 | 2.574 | -8.055 | 4.767 | – |
| Hunt & Reffert | 2024 | 110.802 | -32.012 | 2.591 | -8.088 | 4.756 | 14.576 |
| Celli et al. | 2024 | 110.882 | -31.966 | – | – | – | – |
| Cavallo et al. | 2024 | 110.899 | -32.087 | 2.596 | – | – | – |
| Hunt & Reffert | 2023 | 110.802 | -32.012 | 2.591 | -8.088 | 4.756 | 14.576 |
| Qin et al. | 2023 | 110.91 | -31.99 | 2.57 | -8.06 | 4.73 | 17.78 |
| Just et al. | 2023 | 111.024 | -31.888 | – | – | – | – |
| He et al. | 2022 | 110.813 | -32.051 | 2.624 | -8.141 | 4.811 | – |
| Jaehnig et al. | 2021 | 110.909 | -31.969 | 2.603 | -8.14 | 4.727 | – |
| Rain et al. | 2021 | 110.882 | -31.966 | 2.594 | -8.074 | 4.789 | – |
| Dias et al. | 2021 | 110.846 | -32.004 | 2.553 | -8.045 | 4.783 | 19.669 |
| Cantat-Gaudin et al. | 2020 | 110.882 | -31.966 | 2.594 | -8.074 | 4.789 | – |
| Liu & Pang | 2019 | 110.758 | -31.887 | 2.547 | -8.023 | 4.695 | – |
| Dias et al. | 2019 | 111.883 | -31.966 | 2.594 | -8.074 | 4.789 | 16.018 |
| Bossini et al. | 2019 | 110.882 | -31.966 | – | – | – | – |
| Soubiran et al. | 2018 | 110.882 | -31.966 | – | – | – | 19.65 |
| Cantat-Gaudin et al. | 2018 | 110.882 | -31.966 | 2.594 | -8.074 | 4.789 | – |
| Loktin & Popova | 2017 | 111.105 | -31.849 | – | -1.751 | 2.975 | 22.9 |
| Kharchenko et al. | 2016 | 111.024 | -31.888 | – | – | – | – |
| Kharchenko et al. | 2013 | 111.03 | -31.89 | – | -7.9 | 4.28 | 22.9 |
| Piskunov et al. | 2008 | 110.816 | -32.058 | – | – | – | – |
| Kharchenko et al. | 2007 | 111.1 | -31.85 | – | 0.5 | – | 22.93 |
| Kharchenko et al. | 2005 | 110.82 | -32.06 | – | -8.5 | 3.67 | 22.93 |
| Kharchenko et al. | 2003 | 110.82 | -32.06 | – | -8.93 | 3.91 | – |
| Chen et al. | 2003 | 110.866 | -32.13 | – | -8.27 | 4.52 | 10.5 |
| Dias et al. | 2002 | 111.112 | -31.85 | – | -7.33 | 2.7 | 19.34 |
| Dambis | 1999 | 111.112 | -31.85 | – | – | – | – |
💡 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 |
|---|---|---|---|---|---|---|---|---|---|
| Almeida et al. | 2025 | 0.38 | 0.14 | – | 40 | – | 165 | – | – |
| Alfonso et al. | 2024 | 0.39 | 0.00 | – | 28 | 0.011 | – | – | – |
| Hunt & Reffert | 2024 | – | – | – | – | – | 130* | – | – |
| Celli et al. | 2024 | – | – | – | 27 | – | 135 | – | – |
| Cavallo et al. | 2024 | 0.40 | 0.49 | – | 15 | -0.070 | – | – | – |
| Hunt & Reffert | 2023 | 0.37 | 0.10 | 0.59 | 17 | – | – | – | – |
| Qin et al. | 2023 | 0.43 | 0.22 | – | 32 | – | – | – | – |
| Just et al. | 2023 | – | – | – | 50 | – | 34 | – | – |
| He et al. | 2022 | – | 0.15 | – | 32 | – | – | – | – |
| Jaehnig et al. | 2021 | 0.39* | – | – | – | – | – | – | – |
| Rain et al. | 2021 | 0.38 | 0.09 | – | 30 | – | – | – | 0 |
| Dias et al. | 2021 | 0.38 | 0.14 | – | 40 | 0.011 | – | – | – |
| Cantat-Gaudin et al. | 2020 | 0.39 | 0.00 | – | 27 | – | – | – | – |
| Liu & Pang | 2019 | – | – | – | 32 | 0.000 | – | – | – |
| Dias et al. | 2019 | 0.40 | 0.09 | – | 45 | 0.223 | – | – | – |
| Bossini et al. | 2019 | 0.36 | 0.10 | – | 30 | 0.010 | – | – | – |
| Soubiran et al. | 2018 | 0.38 | – | – | – | – | – | – | – |
| Cantat-Gaudin et al. | 2018 | 0.38 | – | – | – | – | – | – | – |
| Loktin & Popova | 2017 | 0.40 | 0.09 | – | 35 | – | – | – | – |
| Kharchenko et al. | 2016 | 0.39 | 0.16 | – | 50 | – | – | – | – |
| Kharchenko et al. | 2013 | 0.39 | 0.16 | – | 50 | -0.100 | – | – | – |
| Piskunov et al. | 2008 | 0.40 | 0.09 | – | 37 | – | – | – | – |
| Kharchenko et al. | 2005 | 0.40 | 0.09 | – | 37 | – | – | – | – |
| Kharchenko et al. | 2003 | 0.41 | 0.09 | – | – | – | – | – | – |
| Chen et al. | 2003 | 0.41 | 0.09 | – | 30 | -0.100* | – | – | – |
| Dias et al. | 2002 | 0.41 | 0.09 | – | 35 | -0.100 | – | – | – |
| Dambis | 1999 | 0.35 | 0.08 | – | 40 | – | – | – | – |
💡 Note: The parameters are sometimes
transformed from their original values to match the format of the
columns shown here, see FAQ.
The columns DAv, Bfr, BSS correspond to differential
extinction, binary fraction, and blue stragglers, respectively.
BSS values can be listed as fractions or integers.
(*): indicates that this parameter is
assigned more than one value in the corresponding reference.
