HXHWL 54

(H21OC 54)

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0.00 UTI
0.54
CN
1.0
Cdens
0.75
CC3
0.0
Clit
0.0
Cdup
C3 classification AB
Number of members (P>50%) 58
Radius (P>50% members) 9.8 [arcmin]
  • CN 0.54 Moderately populated
  • Cdens 1.0 Very dense
  • CC3 0.75 High quality
  • Clit 0.0 Rarely studied
  • Cdup 0.0 Very likely duplicate
📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview
HXHWL 54 is a moderately populated, very dense object of high C3 quality. Its parallax locates it at a relatively close distance, near the mid-plane, affected by low extinction. It is catalogued as a metal-rich, intermediate-age cluster (see Parameters). It is rarely studied in the literature.

⚠️ Warning: This is very likely a duplicate object, which shares a large percentage of members with at least one previously reported entry. See table with shared members information.

Relatively close Low extinction Metal-rich Intermediate age

Data
Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC – 106.853 -7.663 0.925 -3.94 1.207 32.376
He et al. 2022 106.861 -7.644 0.945 -3.932 1.214 –
He et al. 2021 106.869 -7.659 0.93 -3.94 1.14 –

💡 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
He et al. 2022 – 0.55 – 79 – – – –
He et al. 2021 1.15 0.48 – 263 0.611 – – –

💡 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.

Cluster % RA DEC Plx pmRA pmDE Rv UTI
PHOC 4 100.0 106.82 -7.65 0.92 -3.94 1.18 33.55 0.46
Theia 2649 94.8 106.85 -7.67 0.92 -3.94 1.21 32.25 0.01
CMa01 89.7 106.81 -7.67 0.93 -3.93 1.19 32.25 0.0

💡 Note: The % column shows the percentage of members that HXHWL 54 shares with each listed object.

Visualization
HXHWL 54 UCC
Galactocentric position diagram

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