Hogg 12
(MWSC 1918; OCL 851; ESO 129 11)
0.37
UTI
0.28
CN
0.05
Cdens
0.5
CC3
0.5
Clit
1.0
Cdup
Radius (P>50% members)
4.7 [arcmin]
- CN 0.28 Poorly populated
- Cdens 0.05 Very loose
- CC3 0.5 Intermediate quality
- Clit 0.5 Moderately studied
- Cdup 1.0 Unique
Overview
Hogg 12 is a poorly populated, very loose object of intermediate C3 quality. Its parallax locates it at a large* distance, near the mid-plane, affected by moderate extinction. It is catalogued as a low-mass, young cluster (see Parameters). It is moderately studied in the literature.
(*): The parallax distance estimate (~7.84 kpc) differs significantly from the median photometric distance (~1.66 kpc).
Note: This object shares a moderate percentage of members with a later reported entry. See table with shared members information.
Relatively close
Moderate extinction
Low mass
Young
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | β | 168.059 | -60.772 | 0.128 | -5.541 | 1.998 | 7.429 |
| Just et al. | 2023 | 168.052 | -60.761 | β | β | β | β |
| SΓ‘nchez et al. | 2020 | 168.254 | -60.783 | β | -6.234 | 1.005 | β |
| Bica et al. | 2019 | 168.066 | -60.755 | β | β | β | β |
| Kharchenko et al. | 2016 | 168.052 | -60.761 | β | β | β | β |
| Dias et al. | 2014 | 168.254 | -60.783 | β | -3.43 | -1.84 | β |
| Kharchenko et al. | 2013 | 168.06 | -60.765 | β | -7.04 | 1.34 | -3.0 |
| Kharchenko et al. | 2003 | 168.07 | -60.75 | β | -8.99 | 2.0 | β |
| Dias et al. | 2002 | 168.254 | -60.783 | β | -3.43 | -1.84 | β |
π‘ 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 | β | β | β | 40 | β | 20 | β | β |
| Kharchenko et al. | 2016 | 1.66 | 1.24 | β | 40 | β | β | β | β |
| Kharchenko et al. | 2013 | 1.66 | 1.24 | β | 40 | β | β | β | β |
| Kharchenko et al. | 2003 | 1.43 | 0.93 | β | β | β | β | β | β |
| Dias et al. | 2002 | 2.00 | 1.24 | β | 30 | β | β | β | β |
