HXWHB 15

0.15 UTI

0.79

C_N

0.7

C_dens

1.0

C_C3

0.0

C_lit

0.3

C_dup

C3 classification AA

Number of members (P>50%) 197

Radius (P>50% members) 4.0 [arcmin]

C_N 0.79 Rich
C_dens 0.7 Moderately dense
C_C3 1.0 Very high quality
C_lit 0.0 Rarely studied
C_dup 0.3 Possibly duplicate

📥 Members 📊 Colab 🔬 Bayestar19 🔍 SciX 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

HXWHB 15 is a rich, moderately dense object of very high C3 quality. Its parallax locates it at a large distance, below the mid-plane, affected by high extinction. It is catalogued as a very young cluster (see Parameters). It is rarely studied in the literature, with no articles listed in the last 6 years.

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

Very distant High extinction Very young

Data

Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	–	317.615	46.807	0.155	-3.301	-3.644	-66.14
Hao et al.	2020	317.62	46.81	0.14	-3.31	-3.63	–

💡 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
Hao et al.	2020	7.29	3.77	–	7	–	–	–	–

💡 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
Teutsch 157	69.5	317.59	46.79	0.16	-3.3	-3.65	-67.59	0.63

💡 Note: The % column shows the percentage of members that HXWHB 15 shares with each listed object.

Visualization

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