FSR 0777
(MWSC 546)
0.47
UTI
0.42
CN
1.0
Cdens
0.38
CC3
0.44
Clit
0.88
Cdup
Radius (P>50% members)
4.5 [arcmin]
- CN 0.42 Poorly populated
- Cdens 1.0 Very dense
- CC3 0.38 Low quality
- Clit 0.44 Poorly studied
- Cdup 0.88 Very likely unique
Overview
FSR 0777 is a poorly populated, very dense object of low C3 quality. Its parallax locates it at a moderate* distance, near the mid-plane, affected by moderate extinction. It is catalogued as a low-mass, very young cluster (see Parameters). It is poorly studied in the literature.
(*): The parallax distance estimate (~2.13 kpc) differs significantly from the median photometric distance (~1.08 kpc).
Note: This is very likely a unique object, which shares a small percentage of members with at least one previously reported entry, and a moderate percentage with at least one entry reported in the same catalogue. See table with shared members information.
Relatively close
Moderate extinction
Low mass
Very young
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | â | 81.903 | 34.749 | 0.469 | -0.014 | -2.295 | â |
| Just et al. | 2023 | 81.894 | 34.749 | â | â | â | â |
| Kharchenko et al. | 2016 | 81.894 | 34.749 | â | â | â | â |
| Dias et al. | 2014 | 81.879 | 34.734 | â | -1.14 | -4.54 | â |
| Kharchenko et al. | 2013 | 81.904 | 34.748 | â | 1.4 | -4.27 | 4.7 |
| Kharchenko et al. | 2012 | 81.904 | 34.748 | â | 1.93 | -4.99 | 4.7 |
| Froebrich et al. | 2007 | 81.879 | 34.734 | â | â | â | â |
| Dias et al. | 2002 | 81.879 | 34.734 | â | -1.14 | -4.54 | 2.2 |
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 | 10 | â | 39 | â | â |
| Kharchenko et al. | 2016 | 1.17 | 1.48 | â | 10 | â | â | â | â |
| Kharchenko et al. | 2013 | 1.17 | 1.48 | â | 10 | â | â | â | â |
| Kharchenko et al. | 2012 | 1.00 | 1.24 | â | 42 | â | â | â | â |
| Dias et al. | 2002 | 1.00 | 1.24 | â | 42 | â | â | â | â |
