NGC 1342
(Melotte 21; Collinder 40; MWSC 283; OCL 401; FSR 0679; FoF 2265)
1.0
UTI
1.0
CN
1.0
Cdens
1.0
CC3
1.0
Clit
1.0
Cdup
Stellar density (N50/rad)
52.9 [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 1342 is a very rich, very dense object of very high C3 quality. Its parallax locates it at a close distance, below 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 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 | 52.898 | 37.391 | 1.519 | 0.407 | -1.678 | -10.514 |
| Li et al. | 2025 | 52.894 | 37.38 | 1.502 | 0.52 | -1.604 | â |
| Wei et al. | 2025 | 52.908 | 37.39 | 1.525 | 0.406 | -1.659 | â |
| Almeida et al. | 2025 | 52.87 | 37.397 | â | â | â | â |
| Alfonso et al. | 2024 | 52.909 | 37.39 | 1.485 | 0.414 | -1.661 | â |
| Zhang et al. | 2024 | 52.953 | 37.387 | â | â | â | â |
| Hunt & Reffert | 2024 | 52.953 | 37.387 | 1.525 | 0.425 | -1.665 | -10.159 |
| Cavallo et al. | 2024 | 52.886 | 37.388 | 1.525 | â | â | â |
| Hunt & Reffert | 2023 | 52.953 | 37.387 | 1.525 | 0.425 | -1.665 | -10.159 |
| Almeida et al. | 2023 | 52.868 | 37.396 | â | â | â | â |
| Just et al. | 2023 | 52.995 | 37.356 | â | â | â | â |
| He et al. | 2022 | 52.91 | 37.383 | 1.522 | 0.415 | -1.672 | â |
| Tarricq et al. | 2022 | 52.982 | 37.404 | 1.52 | 0.423 | -1.68 | â |
| Jadhav & Subramaniam | 2021 | 52.894 | 37.38 | â | â | â | â |
| Jaehnig et al. | 2021 | 52.953 | 37.358 | 1.54 | 0.556 | -1.605 | â |
| Rain et al. | 2021 | 52.894 | 37.38 | 1.502 | 0.52 | -1.604 | â |
| Richer et al. | 2021 | 52.939 | 37.374 | 1.504 | 0.546 | -1.609 | â |
| Dias et al. | 2021 | 52.87 | 37.397 | 1.505 | 0.523 | -1.598 | -9.414 |
| Cantat-Gaudin et al. | 2020 | 52.894 | 37.38 | 1.502 | 0.52 | -1.604 | â |
| Zhong et al. | 2020 | 52.894 | 37.38 | â | 0.52 | -1.604 | -18.847 |
| Cantat-Gaudin & Anders | 2020 | 52.894 | 37.38 | 1.502 | 0.52 | -1.604 | â |
| Liu & Pang | 2019 | 52.87 | 37.356 | 1.498 | 0.516 | -1.595 | â |
| Soubiran et al. | 2018 | 52.894 | 37.38 | â | â | â | -9.95 |
| Bica et al. | 2019 | 52.918 | 37.374 | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 52.894 | 37.38 | 1.502 | 0.52 | -1.604 | â |
| Loktin & Popova | 2017 | 52.905 | 37.377 | â | -2.704 | -8.046 | -11.5 |
| Kharchenko et al. | 2016 | 52.995 | 37.356 | â | â | â | â |
| Dias et al. | 2014 | 52.908 | 37.377 | â | -2.99 | -1.82 | â |
| Kharchenko et al. | 2013 | 53.004 | 37.357 | â | -3.12 | -5.5 | -11.5 |
| Gozha et al. | 2012 | 52.908 | 37.377 | â | â | â | â |
| Kharchenko et al. | 2012 | 53.004 | 37.357 | â | -3.12 | -5.5 | -11.5 |
| Bukowiecki et al. | 2011 | 52.908 | 37.376 | â | â | â | â |
| Piskunov et al. | 2008 | 52.898 | 37.336 | â | â | â | â |
| Kharchenko et al. | 2007 | 52.9 | 37.38 | â | 0.25 | â | -11.5 |
| Piskunov et al. | 2007 | 52.898 | 37.336 | â | â | â | â |
| Ahumada & Lapasset | 2007 | 52.95 | 37.383 | â | â | â | â |
| van den Bergh | 2006 | 53.31 | 37.418 | â | â | â | â |
| Kharchenko et al. | 2005 | 52.9 | 37.34 | â | 0.13 | -2.72 | â |
| Kharchenko et al. | 2003 | 52.9 | 37.33 | â | 0.47 | -2.86 | â |
| Chen et al. | 2003 | 52.91 | 37.341 | â | -0.55 | -2.89 | -10.9 |
| Dias et al. | 2002 | 52.908 | 37.377 | â | -2.99 | -1.82 | -10.67 |
| Lynga | 1987 | 52.917 | 37.324 | â | â | â | â |
| Sulentic et al. | 1973 | 52.905 | 37.334 | 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 | 0.67 | 1.04 | 2.41 | 451 | -0.136 | 488 | 0.525 | 1 |
| Li et al. | 2025 | 0.62 | 1.11 | â | 496 | -0.136 | â | â | â |
| Wei et al. | 2025 | 0.98 | 1.51 | â | 380 | 0.000 | 792 | 0.49 | â |
| Almeida et al. | 2025 | 0.63 | 1.23 | â | 578 | â | 880 | â | â |
| Alfonso et al. | 2024 | 0.69 | 0.71 | â | 1113 | -0.113 | â | â | â |
| Zhang et al. | 2024 | â | â | â | â | -0.200(1) | â | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 1311(1) | â | â |
| Cavallo et al. | 2024 | 0.66 | 1.27 | â | 288 | 0.260 | â | â | â |
| Hunt & Reffert | 2023 | 0.63 | 1.37 | 2.41 | 160 | â | â | â | â |
| Almeida et al. | 2023 | 0.64 | 1.26 | â | 403 | -0.005 | 925(1) | 0.56 | â |
| Just et al. | 2023 | â | â | â | 398 | â | 42 | â | â |
| He et al. | 2022 | â | 1.50 | â | 316 | â | â | â | â |
| Tarricq et al. | 2022 | 0.68 | â | â | 851 | â | â | â | â |
| Jadhav & Subramaniam | 2021 | 0.69 | 0.71 | â | 813 | â | 1204 | â | 0(1) |
| Jaehnig et al. | 2021 | 0.65(1) | â | â | â | â | â | â | â |
| Rain et al. | 2021 | 0.65 | 0.98 | â | 447 | â | â | â | 1 |
| Richer et al. | 2021 | â | 1.05 | â | 600 | â | â | â | â |
| Dias et al. | 2021 | 0.63 | 1.23 | â | 578 | -0.115 | â | â | â |
| Cantat-Gaudin et al. | 2020 | 0.69 | 0.71 | â | 813 | â | â | â | â |
| Kounkel et al. | 2020 | 0.65 | 1.19 | â | 398 | â | â | â | â |
| Zhong et al. | 2020 | 0.65(1) | 1.04 | â | 8600 | -0.205 | â | â | â |
| Cantat-Gaudin & Anders | 2020 | 0.65 | â | â | â | â | â | â | â |
| Liu & Pang | 2019 | â | â | â | 871 | 0.250 | â | â | â |
| Soubiran et al. | 2018 | 0.65 | â | â | â | â | â | â | â |
| Cantat-Gaudin et al. | 2018 | 0.65 | â | â | â | â | â | â | â |
| Loktin & Popova | 2017 | 0.67 | 1.09 | â | 452 | â | â | â | â |
| Kharchenko et al. | 2016 | 0.67 | 1.04 | â | 398 | â | â | â | â |
| Kharchenko et al. | 2013 | 0.67 | 1.04 | â | 398 | -0.160 | â | â | â |
| Bukowiecki et al. | 2012 | â | â | â | â | â | 184 | â | â |
| Gozha et al. | 2012 | 0.67 | â | â | 452 | -0.160 | 155 | â | â |
| Kharchenko et al. | 2012 | 0.67 | 1.04 | â | 398 | -0.160 | â | â | â |
| Bukowiecki et al. | 2011 | 0.43(1) | 0.76 | â | 501 | â | â | â | â |
| Piskunov et al. | 2008 | 0.67 | 1.01 | â | 162 | â | 132(1) | â | â |
| Piskunov et al. | 2007 | 0.67 | 1.01 | â | 162 | â | 33 | â | â |
| Ahumada & Lapasset | 2007 | â | 1.01 | â | 457 | â | â | â | 2 |
| van den Bergh | 2006 | 0.67 | 1.01 | â | 457 | â | â | â | â |
| Kharchenko et al. | 2005 | 0.67 | 1.01 | â | 162 | â | â | â | â |
| Kharchenko et al. | 2003 | 0.67 | 1.01 | â | â | â | â | â | â |
| Chen et al. | 2003 | 0.67 | 1.01 | â | 450 | -0.160(1) | â | â | â |
| Dias et al. | 2002 | 0.67 | 1.01 | â | 452 | -0.160 | â | â | â |
| Lynga | 1987 | 0.55 | 0.85 | â | 302 | -0.130 | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Palma et al. (2025)
Classified as optical pair P261, along with Alessi-Teutsch_9.
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: 0.40 (50th percentile).
Richer et al. (2021)
The expected number of WDs is 37.7, 0 WD candidates found, and 0 WD candidates found in the wide search.
Ahumada & Lapasset (2007)
Only the photoelectric data of (1961PUSNO..17..343H) were examined. References (1985ApJ...294L.103A) and (1982A&A...109...37M) cite star 2=HD 21728 as a blue straggler. In (1985ApJ...294L.103A) this star is given a spectrum A0II-IIIp(Si(st),Mg(wk)) and a projected velocity v.sin i<40km/s. Star 4=HD 275501 has a spectrum G8II according to (2000AJ....120..333S). Both stars have a membership probability of 99% (ref. 148).