SAI 105

0.17 UTI

0.0

C_N

0.11

C_dens

0.75

C_C3

0.0

C_lit

1.0

C_dup

N₅₀ (P>50% members) 23

Stellar density (N₅₀/rad) 0.5 [N/pc²]

C3 classification AB

C_N 0.0 Sparse
C_dens 0.11 Very loose
C_C3 0.75 High quality
C_lit 0.0 Rarely studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

MOCA 🔍 CDS 🔍 Simbad 🔍 CDS (α, δ) 🔍 Simbad (α, δ)

Overview

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SAI 105 is a sparse, very loose object of high C3 quality. Its parallax locates it at a very large^* distance, below the mid-plane, affected by very high extinction. It is catalogued as an old cluster (see Parameters). It is rarely studied in the literature, with no articles listed in the last 7 years.

(*): The parallax distance estimate (~11.82 kpc) differs significantly from the median photometric distance (~2.95 kpc).

Note: This object shares a significant percentage of members with a later reported entry. See table with shared members information.

⚠️ Warning: the low UTI value and no obvious signs of duplication (C_dup=1.0) indicate that this is quite probably an asterism, moving group, or artifact, and not a real open cluster.

Relatively close Very high extinction Old

Data

🔍 Search references for SAI 105 in: SciX Simbad

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Reference	Year	RA [deg]	DEC [deg]	Plx [mas]	pmRA [mas/yr]	pmDE [mas/yr]	Rv [km/s]
UCC	99999–	137.6	-49.901	0.085	-3.303	3.367	46.878
Bica et al.	2019	137.601	-49.92	–	–	–	–
Glushkova et al.	2010	137.602	-49.913	–	–	–	–

💡 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]	B_frac	BSS
UCC	99999–	2.95	5.92	–	1122	–	–	–	–
Glushkova et al.	2010	2.95	5.92	–	1122	–	–	–	–

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
CWNU 3931	64.0	137.6	-49.91	0.04	-3.12	3.36	46.88	0.17

💡 Note: The % column shows the percentage of members that SAI 105 shares with each listed object.

Visualization

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