Theia 172

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0.05 UTI
0.84
CN
1.0
Cdens
1.0
CC3
0.25
Clit
0.07
Cdup
Stellar density (N50/rad) 7.2 [N/pc2]
  • CN 0.84 Rich
  • Cdens 1.0 Very dense
  • CC3 1.0 Very high quality
  • Clit 0.25 Poorly studied
  • Cdup 0.07 Very likely duplicate

Overview

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Theia 172 is a rich, very dense object of very high C3 quality. Its parallax locates it at a very close distance, above the mid-plane, affected by low extinction. It is catalogued as a near-solar metallicity, young cluster (see Parameters). It was recently reported in the literature.

âš ī¸ 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.

Palma et al. (2025)
Part of multiple system G127, along with Theia_383 and HSC_1707.

Cavallo et al. (2024)
Gold sample.

Data

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Reference Year RA [deg] DEC [deg] Plx [mas] pmRA [mas/yr] pmDE [mas/yr] Rv [km/s]
UCC 99999– 110.209 3.703 2.125 -6.503 -5.118 13.557
Zhang et al. 2024 110.277 4.082 – – – –
Hunt & Reffert 2024 110.277 4.082 2.113 -6.459 -5.036 15.359
Cavallo et al. 2024 110.091 3.188 2.12 – – –
Hunt & Reffert 2023 110.277 4.082 2.113 -6.459 -5.036 15.359

💡 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 99999– 0.47 0.185 0.54 99 0.094 156 – –
Zhang et al. 2024 – – – – -0.002(1) – – –
Hunt & Reffert 2024 – – – – – 156(1) – –
Cavallo et al. 2024 0.49 0.28 – 76 0.190 – – –
Hunt & Reffert 2023 0.45 0.09 0.54 122 – – – –

(N): Indicates that there are N extra values assigned to this parameter in the corresponding reference.

Cluster % RA DEC Plx pmRA pmDE Rv UTI
OCSN 104 92.7 110.2 3.61 2.13 -6.5 -5.1 13.56 0.48
CWWDL 14655 21.8 110.32 3.74 2.14 -6.53 -5.24 13.45 0.0
CWWDL 14656 15.2 109.7 3.37 2.13 -6.46 -5.05 15.02 0.0
CWNU 254 14.8 110.24 3.84 2.16 -6.51 -5.23 12.63 0.45

💡 Note: The % column shows the percentage of members that Theia 172 shares with each listed object.

Visualization

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