Czernik 17
(OCL 378; MWSC 311)
0.44
UTI
0.4
CN
0.26
Cdens
0.75
CC3
0.39
Clit
1.0
Cdup
Stellar density (N50/rad)
1.3 [N/pc2]
- CN 0.4 Poorly populated
- Cdens 0.26 Loose
- CC3 0.75 High quality
- Clit 0.39 Poorly studied
- Cdup 1.0 Unique
Overview
Czernik 17 is a poorly populated, loose object of high C3 quality. Its parallax locates it at a large* distance, well above the mid-plane, affected by moderate extinction. It is catalogued as a metal-rich, intermediate-age cluster, but with a large variance across recent sources for the age parameter (see Parameters). It is poorly studied in the literature.
(*): The parallax distance estimate (~7.05 kpc) differs significantly from the median photometric distance (~4.90 kpc).
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999â | 58.092 | 61.975 | 0.142 | 0.072 | -0.079 | â |
| Hunt & Reffert | 2024 | 58.075 | 61.972 | 0.139 | 0.059 | -0.103 | â |
| Cavallo et al. | 2024 | 58.099 | 61.969 | 0.14 | â | â | â |
| He et al. | 2023 | 58.093 | 61.975 | 0.142 | 0.062 | -0.104 | â |
| Hunt & Reffert | 2023 | 58.075 | 61.972 | 0.139 | 0.059 | -0.103 | â |
| Bica et al. | 2019 | 58.126 | 61.96 | â | â | â | â |
| Dias et al. | 2018 | â | â | â | -0.34 | 0.33 | â |
| Loktin & Popova | 2017 | 58.11 | 61.951 | â | -0.184 | -2.905 | â |
| Sampedro et al. | 2017 | 58.1 | 61.95 | -2.29 | 1.09 | â | â |
| Tadross | 2014 | 58.1 | 61.95 | â | â | â | â |
| Dias et al. | 2014 | 58.1 | 61.95 | â | -2.3 | 1.81 | â |
| Bukowiecki et al. | 2011 | 58.071 | 61.978 | â | â | â | â |
| Dias et al. | 2002 | 58.1 | 61.95 | â | -2.3 | 1.81 | â |
| Lynga | 1987 | 58.104 | 61.994 | 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 | 4.9 | 2.27 | 0.86 | 190 | 0.660 | 436 | â | â |
| Hunt & Reffert | 2024 | â | â | â | â | â | 625(1) | â | â |
| Cavallo et al. | 2024 | 6.82 | 2.07 | â | 174 | 0.660 | â | â | â |
| He et al. | 2023 | 4.90 | 1.95 | â | 631 | â | â | â | â |
| Hunt & Reffert | 2023 | 6.02 | 2.37 | 0.86 | 190 | â | â | â | â |
| Loktin & Popova | 2017 | 1.80 | 1.68 | â | 631 | â | â | â | â |
| Tadross | 2014 | 2.12 | 2.74 | â | 400 | â | â | â | â |
| Bukowiecki et al. | 2012 | â | â | â | â | â | 246 | â | â |
| Bukowiecki et al. | 2011 | 2.57(1) | 2.65 | â | 63 | â | â | â | â |
| Dias et al. | 2002 | 7.00 | 2.27 | â | 112 | â | â | â | â |
(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.
MOCA


Cavallo et al. (2024)
Gold sample.
Hunt & Reffert (2024)
Classified as open cluster. CMD class: 0.69 (50th percentile).
Hunt & Reffert (2023)
Classified as open cluster. CMD class: 0.69 (50th percentile).