VDBH 4
(van den Bergh-Hagen 4; BH 4; vdBergh-Hagen 4; ESO 368 06; MWSC 1288)
0.31
UTI
0.35
CN
0.15
Cdens
0.75
CC3
0.16
Clit
1.0
Cdup
Nm (P>50%)
35
Core radius and density
2.8 [pc], 0.8 [pc-2]
- CN 0.35 Poorly populated
- Cdens 0.15 Very loose
- CC3 0.75 High quality
- Clit 0.16 Rarely studied
- Cdup 1.0 Unique
π₯ Members
π Colab
π¬ Bayestar19
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
MOCA
π CDS
π Simbad
π CDS (Ξ±, Ξ΄)
π Simbad (Ξ±, Ξ΄)
Overview
VDBH 4 is a poorly populated, very loose object of high C3 quality. Its parallax locates it at a very large distance, well below the mid-plane, affected by moderate extinction. It is catalogued as a massive, near-solar metallicity, intermediate-age cluster, but with a large variance across recent sources for the age parameter (see Parameters). It is rarely studied in the literature.
Data
| Reference | Year | RA [deg] | DEC [deg] | Plx [mas] | pmRA [mas/yr] | pmDE [mas/yr] | Rv [km/s] |
|---|---|---|---|---|---|---|---|
| UCC | 99999β | 114.437 | -36.061 | 0.1 | -0.862 | 2.175 | β |
| He et al. | 2023 | 114.438 | -36.061 | 0.084 | -0.846 | 2.137 | β |
| Perren et al. | 2022 | 114.45 | -36.033 | β | β | β | β |
| Bica et al. | 2019 | 114.44 | -36.057 | β | β | β | β |
| Bukowiecki et al. | 2011 | 114.438 | -36.075 | β | β | β | β |
| Dias et al. | 2002 | 114.433 | -36.067 | β | β | β | β |
| Lynga | 1987 | 114.45 | -36.03 | β | β | β | β |
| van den Bergh & Hagen | 1975 | 114.0 | -35.917 | β | β | β | 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] | Bfrac | BSS |
|---|---|---|---|---|---|---|---|---|---|
| UCC | 99999β | 9.065 | 1.41 | β | 638 | -0.290 | 1800 | 0.64 | β |
| He et al. | 2023 | 10.00 | 1.75 | β | 16 | β | β | β | β |
| Perren et al. | 2022 | 8.13 | 1.07 | β | 1259 | -0.290 | 1800 | 0.64 | β |
Perren et al. (2022)
Fewer than 70 confirmed members; the CMD shows a very weak but extended main sequence spanning almost 4 magnitudes. ASteCA estimates a distance of 8.1 kpc and an age of 1.3 Gyr, both with large uncertainties (16thβ84th percentile range spans ~3 kpc). Carraro 2007 performed VI CCD photometry and reported 19.3 kpc and 0.2 Gyr β the distance lies outside ASteCA's 2Ο range and is likely inflated by severe field star contamination visible in their CMD.