DBSB 85
(DBSB2003 85; DBS2003 85; MWSC 2104)
0.22
UTI
0.35
CN
0.3
Cdens
0.25
CC3
0.1
Clit
1.0
Cdup
Nm (P>50%)
35
Core radius and density
1.0 [pc], 1.5 [pc-2]
- CN 0.35 Poorly populated
- Cdens 0.3 Loose
- CC3 0.25 Low quality
- Clit 0.1 Rarely studied
- Cdup 1.0 Unique
Overview
DBSB 85 is a poorly populated, loose object of low C3 quality. Its parallax locates it at a moderate distance, near the mid-plane, affected by high extinction. It is catalogued as a low-mass, young cluster (see Parameters). It is rarely studied in the literature.
Note: This object shares a moderate percentage of members with 3 later reported entries. See table with shared members information.
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 | 199.648 | -62.666 | 0.377 | -4.498 | -1.875 | -38.194 |
| Just et al. | 2023 | 199.6 | -62.662 | â | â | â | â |
| Kharchenko et al. | 2016 | 199.6 | -62.662 | â | â | â | â |
| Kharchenko et al. | 2013 | 199.612 | -62.665 | â | -15.7 | 2.0 | â |
| Morales et al. | 2013 | 199.629 | -62.663 | â | â | â | â |
| Dutra et al. | 2003 | 199.617 | -62.659 | 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 | 2.02 | 4.6 | â | 28 | â | 46 | â | â |
| Just et al. | 2023 | â | â | â | 28 | â | 46 | â | â |
| Kharchenko et al. | 2016 | 2.02 | 4.60 | â | 28 | â | â | â | â |
| Kharchenko et al. | 2013 | 2.02 | 4.60 | â | 28 | â | â | â | â |
| Morales et al. | 2013 | 1.98 | â | â | â | â | â | â | â |
MOCA

Morales et al. (2013)
Classified as morphological type 'OC0' (emerging exposed cluster). Morphological flag: possibly associated submm emission surrounding the cluster, presence of an IR bubble.
Dutra et al. (2003)
Classified as stellar group (IRGr).