Dolidze 17
(MWSC 513)
0.06
UTI
0.0
CN
0.0
Cdens
0.12
CC3
0.1
Clit
1.0
Cdup
Nm (P>50%)
22
Core radius and density
3.8 [pc], 0.02 [pc-2]
- CN 0.0 Sparse
- Cdens 0.0 Very loose
- CC3 0.12 Very low quality
- Clit 0.1 Rarely studied
- Cdup 1.0 Unique
Overview
Dolidze 17 is a sparse, very loose object of very low C3 quality. Its parallax locates it at a large* distance, well below the mid-plane, affected by moderate extinction. It is catalogued as a low-mass, old cluster (see Parameters). It is rarely studied in the literature.
(*): The parallax distance estimate (~8.13 kpc) differs significantly from the median photometric distance (~1.03 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 | 80.605 | 7.157 | 0.123 | 0.083 | -0.641 | 122.596 |
| Just et al. | 2023 | 80.625 | 7.161 | â | â | â | â |
| Dib et al. | 2018 | 80.632 | 7.16 | â | â | â | â |
| Joshi et al. | 2016 | 80.632 | 7.16 | â | â | â | â |
| Kharchenko et al. | 2016 | 80.625 | 7.161 | â | â | â | â |
| Kharchenko et al. | 2013 | 80.632 | 7.16 | â | -0.5 | -6.51 | 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 | 1.03 | 1.31 | â | 1514 | â | 20 | â | â |
| Just et al. | 2023 | â | â | â | 1514 | â | 20 | â | â |
| Dib et al. | 2018 | 1.03 | â | â | 1514 | â | â | â | â |
| Joshi et al. | 2016 | 1.03 | 1.31 | â | 1514 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.03 | 1.31 | â | 1514 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.03 | 1.31 | â | 1514 | â | â | â | â |
MOCA

Bica et al. (2019)
Analysis of Dolidze objects by M. Kronberger reported in DAML02. Web updates in DAML02, some were later removed (2003 to 2010).
Dias et al. (2002)
Asterism (Archinal, B. A. & Hynes, S. J. 2003); cat V3.5 (Jan 2016)