CWNU 1785

Click to load Aladin Lite
0.46 UTI
0.32
CN
0.5
Cdens
1.0
CC3
0.25
Clit
1.0
Cdup
Radius (P>50% members) 4.1 [arcmin]
  • CN 0.32 Poorly populated
  • Cdens 0.5 Moderately dense
  • CC3 1.0 Very high quality
  • Clit 0.25 Poorly studied
  • Cdup 1.0 Unique

Overview

CWNU 1785 is a poorly populated, moderately dense object of very high C3 quality. Its parallax locates it at a moderate distance, near the mid-plane, affected by high extinction. It is catalogued as a massive, very metal-poor, very young cluster (see Parameters). It was recently reported in the literature.
Relatively close High extinction Massive Very metal-poor Very young

Cavallo et al. (2024): Silver sample.

Data

Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC 267.847 -27.752 0.334 -0.125 -2.124 -2.481
Hunt & Reffert 2024 267.901 -27.742 0.336 -0.128 -2.14 -6.559
Cavallo et al. 2024 267.87 -27.766 0.335
Hunt & Reffert 2023 267.901 -27.742 0.336 -0.128 -2.14 -6.559
He et al. 2023 267.864 -27.758 0.333 -0.098 -2.126 -39.69

💡 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
Hunt & Reffert 2024 1001*
Cavallo et al. 2024 2.65 3.74 71 -1.040
Hunt & Reffert 2023 2.68 3.60 2.61 17
He et al. 2023 2.69 4.40 9

💡 Note: The parameters are sometimes transformed from their original values to match the format of the columns shown here, see FAQ. The columns DAv, Bfr, BSS correspond to differential extinction, binary fraction, and blue stragglers, respectively. BSS values can be listed as fractions or integers.
(*): indicates that this parameter is assigned more than one value in the corresponding reference.

Visualization

Galactocentric position diagram

💡 Note: How are the galactocentric plots generated? See FAQ.