KMS35

0.40 UTI

0.25

C_N

1.0

C_dens

0.75

C_C3

0.0

C_lit

1.0

C_dup

N_m (P>50%) 25

Core radius and density 0.4 [pc], 18 [pc^-2]

C3 classification BA

C_N 0.25 Poorly populated
C_dens 1.0 Very dense
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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KMS35 is a poorly populated, very dense object of high C3 quality. Its parallax locates it at a very close^* distance, below the mid-plane, affected by very 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 10 years.

(*): The parallax distance estimate (~0.40 kpc) differs significantly from the median photometric distance (~0.64 kpc).

Note: This object shares a moderate percentage of members with at least one entry reported in the same catalogue. See table with shared members information.

Close Very high extinction Very young

Bica et al. (2003)
Classified as infrared cluster (IRC).

Data

🔍 Search references for KMS35 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–	84.482	-6.952	2.518	0.065	-0.722	23.545
Joshi et al.	2016	84.475	-6.956	–	–	–	–
Bica et al.	2003	84.475	-6.95	–	–	–	–

💡 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–	0.64	6.7	–	4	–	–	–	–
Joshi et al.	2016	0.64	6.70	–	4	–	–	–	–

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
LDN1641C	28.0	84.68	-7.02	2.52	-0.06	-1.01	–	0.45

💡 Note: The % column shows the percentage of members that KMS35 shares with each listed object.

Visualization

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