DBSB 162
(DBSB2003 162; DBS2003 162; MWSC 2388)
0.07
UTI
0.0
CN
0.04
Cdens
0.12
CC3
0.1
Clit
1.0
Cdup
Nm (P>50%)
13
Core radius and density
2.1 [pc], 0.2 [pc-2]
- CN 0.0 Sparse
- Cdens 0.04 Very loose
- CC3 0.12 Very low quality
- Clit 0.1 Rarely studied
- Cdup 1.0 Unique
Overview
DBSB 162 is a sparse, very loose object of very low C3 quality. Its parallax locates it at a moderate* distance, near the mid-plane, affected by high extinction. It is catalogued as a very young cluster (see Parameters). It is rarely studied in the literature.
(*): The parallax distance estimate (~2.77 kpc) differs significantly from the median photometric distance (~5.52 kpc).
â ī¸ Warning: the low UTI value and no obvious signs of duplication (Cdup=1.0) indicate that this is quite probably an asterism, moving group, or artifact, and not a real open cluster.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 245.176 | -50.693 | 0.361 | -4.125 | -5.012 | -16.449 |
| Just et al. | 2023 | 245.103 | -50.694 | â | â | â | â |
| Kharchenko et al. | 2016 | 245.103 | -50.694 | â | â | â | â |
| Kharchenko et al. | 2013 | 245.115 | -50.695 | â | 0.12 | -6.13 | â |
| Morales et al. | 2013 | 245.146 | -50.69 | â | â | â | â |
| Dutra et al. | 2003 | 245.143 | -50.688 | 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 | 5.52 | 4.79 | â | 2 | â | 197 | â | â |
| Just et al. | 2023 | â | â | â | 2 | â | 197 | â | â |
| Kharchenko et al. | 2016 | 5.52 | 4.79 | â | 2 | â | â | â | â |
| Kharchenko et al. | 2013 | 5.52 | 4.79 | â | 2 | â | â | â | â |
| Morales et al. | 2013 | 3.49 | â | â | â | â | â | â | â |
MOCA

Morales et al. (2013)
Classified as morphological type 'EC2' (partially embedded cluster). Morphological flag: cluster partially embedded, presence of an IR bubble and possible YSOs.
Dutra et al. (2003)
Classified as infrared cluster (IRC).