Mayer 2

0.06 UTI

0.0

C_N

0.04

C_dens

0.25

C_C3

0.0

C_lit

1.0

C_dup

C3 classification CC

Number of members (P>50%) 16

Radius (P>50% members) 8.3 [arcmin]

C_N 0.0 Sparse
C_dens 0.04 Very loose
C_C3 0.25 Low quality
C_lit 0.0 Rarely studied
C_dup 1.0 Unique

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

Overview

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Mayer 2 is a sparse, very loose object of low C3 quality. Its parallax locates it at a moderate^* distance, above the mid-plane, affected by high extinction. It is catalogued as a young cluster (see Parameters). It is rarely studied in the literature, with no articles listed in the last 9 years.

(*): The parallax distance estimate (~3.92 kpc) differs significantly from the median photometric distance (~2.33 kpc).

Note: This object shares a small 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 High extinction Young

Data

🔍 Search references for Mayer 2 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	–	64.996	53.161	0.255	0.312	-0.719	-25.204
Loktin & Popova	2017	64.935	53.168	–	-2.923	1.264	–
Dias et al.	2014	64.938	53.167	–	-1.41	-5.88	–
Dias et al.	2002	64.938	53.167	–	-1.41	-5.88	–

💡 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
Loktin & Popova	2017	3.06	2.73	–	32	–	–	–	–
Dias et al.	2002	1.59	3.29	–	25	–	–	–	–

Cluster	%	RA	DEC	Plx	pmRA	pmDE	Rv	UTI
UBC 609	16.0	65.23	53.05	0.22	0.46	-0.73	–	0.18

💡 Note: The % column shows the percentage of members that Mayer 2 shares with each listed object.

Visualization

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