NGC 1976
(Trapezium; Ori Trapezium; Trapezium-FG)
0.75
UTI
0.6
CN
1.0
Cdens
0.62
CC3
0.77
Clit
1.0
Cdup
Stellar density (N50/rad)
28.9 [N/pc2]
- CN 0.6 Moderately populated
- Cdens 1.0 Very dense
- CC3 0.62 Intermediate quality
- Clit 0.77 Well-studied
- Cdup 1.0 Unique
Overview
NGC 1976 is a moderately populated, very dense object of intermediate C3 quality. Its parallax locates it at a very close distance, below the mid-plane, affected by low extinction. It is catalogued as a near-solar metallicity, very young cluster, but with a large variance across recent sources for the metallicity and mass parameters (see Parameters). It is well-studied in the literature.
Note: This object shares a moderate percentage of members with at least one entry reported in the same catalogue. 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 | 83.821 | -5.452 | 2.579 | 1.254 | 0.19 | 19.859 |
| Wei et al. | 2025 | 83.823 | -5.418 | 2.564 | 1.156 | 0.246 | â |
| Almeida et al. | 2025 | 83.835 | -5.41 | â | â | â | â |
| Jaehnig et al. | 2021 | 83.829 | -5.417 | 2.57 | 1.276 | 0.176 | â |
| Dias et al. | 2021 | 83.835 | -5.41 | 2.557 | 1.262 | 0.274 | 23.841 |
| Dias et al. | 2018 | â | â | â | 0.02 | 0.37 | â |
| Dib et al. | 2018 | 83.827 | -5.36 | â | â | â | â |
| Loktin & Popova | 2017 | 83.82 | -5.39 | â | 2.05 | 1.56 | 28.9 |
| Sampedro et al. | 2017 | 83.817 | -5.39 | 1.85 | 1.78 | â | â |
| Joshi et al. | 2016 | 83.827 | -5.36 | â | â | â | â |
| Dias et al. | 2014 | 83.817 | -5.39 | â | 2.05 | 1.56 | â |
| Gozha et al. | 2012 | 83.817 | -5.39 | â | â | â | â |
| Bukowiecki et al. | 2011 | 83.821 | -5.385 | â | â | â | â |
| Piskunov et al. | 2008 | 83.813 | -5.392 | â | â | â | â |
| Kharchenko et al. | 2007 | 83.82 | -5.39 | â | 0.4 | â | 28.94 |
| Piskunov et al. | 2007 | 83.813 | -5.392 | â | â | â | â |
| Ahumada & Lapasset | 2007 | 83.825 | -5.383 | â | â | â | â |
| van den Bergh | 2006 | 83.822 | -5.391 | â | â | â | â |
| Kharchenko et al. | 2005 | 83.82 | -5.39 | â | 1.96 | -0.77 | 28.94 |
| Lada & Lada | 2003 | 84.448 | -5.363 | â | â | â | â |
| Kharchenko et al. | 2003 | 83.85 | -5.38 | â | 2.02 | -0.19 | â |
| Bica et al. | 2003 | 83.84 | -5.378 | â | â | â | â |
| Dias et al. | 2002 | 83.817 | -5.39 | â | 2.05 | 1.56 | 31.98 |
| Dambis | 1999 | 83.822 | -5.391 | â | â | â | â |
| Lynga | 1987 | 83.831 | -5.383 | â | â | â | 23.0 |
| Sulentic et al. | 1973 | 83.832 | -5.385 | 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 | 0.41 | 0.19 | â | 13 | 0.177 | 167 | 0.47 | 0 |
| Wei et al. | 2025 | 0.49 | 0.95 | â | 13 | 0.500 | 2585 | 0.47 | â |
| Almeida et al. | 2025 | 0.38 | 0.25 | â | 6 | â | 238 | â | â |
| Jaehnig et al. | 2021 | 0.39(1) | â | â | â | â | â | â | â |
| Dias et al. | 2021 | 0.38 | 0.25 | â | 6 | -0.146 | â | â | â |
| Dib et al. | 2018 | 0.46 | â | â | 1 | â | â | â | â |
| Loktin & Popova | 2017 | 0.49 | 0.98 | â | 10 | â | â | â | â |
| Joshi et al. | 2016 | 0.46 | 0.92 | â | 1 | â | 98 | â | â |
| Gozha et al. | 2012 | 0.41 | â | â | 13 | â | 98 | â | â |
| Piskunov et al. | 2008 | 0.40 | 0.16 | â | 51 | â | 167(1) | â | â |
| Piskunov et al. | 2007 | 0.40 | 0.16 | â | 51 | â | 58 | â | â |
| Ahumada & Lapasset | 2007 | â | 0.16 | â | 13 | â | â | â | 0 |
| van den Bergh | 2006 | 0.40 | 0.16 | â | 13 | â | â | â | â |
| Kharchenko et al. | 2005 | 0.40 | 0.16 | â | 51 | â | â | â | â |
| Lada & Lada | 2003 | 0.50 | â | â | â | â | 413 | â | â |
| Kharchenko et al. | 2003 | 0.45 | 0.19 | â | â | â | â | â | â |
| Dias et al. | 2002 | 0.41 | 0.16 | â | 13 | â | â | â | â |
| Dambis | 1999 | 0.36 | 0.19 | â | 3 | â | â | â | â |
| Lynga | 1987 | 0.45 | â | â | 25 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA

Almeida et al. (2025)
Mass determination: good fit. Isochrone match: good fit.
Ahumada & Lapasset (2007)
= Trapezium. The apparent cluster diameter was taken from (1970PDDO....4....1H). The colour-magnitude diagram of (1952ApJ...116..251S) was dereddened using the reddenings for each star listed in the reference. Star 1891 (WEBDA) = Theta1 Orionis A = HD 37022 (sp. O7Vp,v.sin i=140km/s, var?), appears blueward the ZAMS in the dereddened diagram, but it is a non-member according to (1983A&AS...54..221M).
Bica et al. (2003)
Classified as infrared cluster (IRC).
Lada & Lada (2003)
Embedded cluster within âŧ2 Kpc of the Sun.