NGC 1663
(MWSC 426)
0.23
UTI
0.0
CN
0.01
Cdens
0.38
CC3
0.38
Clit
1.0
Cdup
Radius (P>50% members)
7.2 [arcmin]
- CN 0.0 Sparse
- Cdens 0.01 Very loose
- CC3 0.38 Low quality
- Clit 0.38 Poorly studied
- Cdup 1.0 Unique
Overview
NGC 1663 is a sparse, very loose object of low C3 quality. Its parallax locates it at a large* distance, well below the mid-plane, affected by moderate extinction. It is catalogued as an old cluster (see Parameters). It is poorly studied in the literature.
(*): The parallax distance estimate (~7.65 kpc) differs significantly from the median photometric distance (~1.49 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.
Relatively close
Moderate extinction
Old
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | â | 72.344 | 13.114 | 0.131 | 0.516 | -0.786 | 23.774 |
| Just et al. | 2023 | 72.307 | 13.169 | â | â | â | â |
| Angelo et al. | 2019 | 72.35 | 13.14 | â | â | â | â |
| Loktin & Popova | 2017 | 72.315 | 13.148 | â | 1.462 | -7.315 | â |
| Kharchenko et al. | 2016 | 72.307 | 13.169 | â | â | â | â |
| Dias et al. | 2014 | 72.242 | 13.148 | â | 2.18 | -2.9 | â |
| Kharchenko et al. | 2013 | 72.315 | 13.17 | â | 2.56 | -5.07 | 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] | Bfr | BSS |
|---|---|---|---|---|---|---|---|---|---|
| Just et al. | 2023 | â | â | â | 2512 | â | 309 | â | â |
| Angelo et al. | 2019 | 2.40 | â | â | 5010 | â | 15 | â | â |
| Loktin & Popova | 2017 | 1.16 | 1.41 | â | 631 | â | â | â | â |
| Kharchenko et al. | 2016 | 1.49 | 1.29 | â | 2512 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.49 | 1.29 | â | 2512 | â | â | â | â |

Cantat-Gaudin et al. (2020)
Historically described as poor and irregular. Gaia DR2 data show large dispersion in proper motion and parallax, inconsistent with a physical cluster. More details in Appendix A of the article.