Collinder 367
0.73
UTI
0.58
CN
1.0
Cdens
0.75
CC3
0.65
Clit
1.0
Cdup
Stellar density (N50/rad)
6.6 [N/pc2]
- CN 0.58 Moderately populated
- Cdens 1.0 Very dense
- CC3 0.75 High quality
- Clit 0.65 Moderately 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
Collinder 367 is a moderately populated, very dense object of high C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by moderate extinction. It is catalogued as a massive, near-solar metallicity, very young cluster, but with a large variance across recent sources for the absorption parameter (see Parameters). It is moderately studied in the literature.
Note: This object shares a large percentage of members with 2 later reported entries. 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 | 272.447 | -23.645 | 0.775 | 1.899 | -1.517 | â |
| Hunt & Reffert | 2024 | 272.456 | -23.652 | 0.783 | 1.893 | -1.515 | -22.582 |
| Cavallo et al. | 2024 | 272.387 | -23.655 | 0.787 | â | â | â |
| Hunt & Reffert | 2023 | 272.456 | -23.652 | 0.783 | 1.893 | -1.515 | -22.582 |
| Dias et al. | 2014 | 272.462 | -23.828 | â | -0.65 | -3.73 | â |
| Gozha et al. | 2012 | 272.462 | -23.828 | â | â | â | â |
| Piskunov et al. | 2008 | 272.42 | -23.656 | â | â | â | â |
| Kharchenko et al. | 2007 | 272.46 | -23.83 | â | 0.4 | â | -3.17 |
| Kharchenko et al. | 2005 | 272.43 | -23.66 | â | 1.16 | -2.03 | -3.17 |
| Kharchenko et al. | 2003 | 272.44 | -23.66 | â | 0.74 | -2.57 | â |
| Dias et al. | 2002 | 272.462 | -23.828 | â | 0.56 | -3.18 | 0.97 |
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 | 1.215 | 1.08 | 2.5 | 7 | 0.040 | 1793 | â | â |
| Liu et al. | 2025 | 1.19 | 0.41 | â | 16 | â | â | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 424(1) | â | â |
| Cavallo et al. | 2024 | 1.29 | 1.79 | â | 5 | 0.040 | â | â | â |
| Hunt & Reffert | 2023 | 1.23 | 1.66 | 2.50 | 4 | â | â | â | â |
| Gozha et al. | 2012 | 1.25 | â | â | 7 | â | 3162 | â | â |
| Piskunov et al. | 2008 | 1.20 | 1.08 | â | 7 | â | â | â | â |
| Kharchenko et al. | 2005 | 1.20 | 1.08 | â | 7 | â | â | â | â |
| Kharchenko et al. | 2003 | 1.25 | 0.62 | â | â | â | â | â | â |
| Dias et al. | 2002 | 1.20 | 1.08 | â | 7 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
Liu et al. (2025)
Classified as primordial binary cluster 129 along with NGC_6531.
Palma et al. (2025)
Part of multiple system G203, along with ESO_521-38, NGC_6530, UBC_94 and HSC_94.
Cavallo et al. (2024)
Silver sample.