NGC 6618

(M17; BDB2003 G015.05-00.69)

0.31 UTI

0.0

C_N

0.03

C_dens

0.25

C_C3

0.65

C_lit

1.0

C_dup

N_m (P>50%) 20

Core radius and density 5.3 [pc], 0.1 [pc^-2]

C3 classification CC

C_N 0.0 Sparse
C_dens 0.03 Very loose
C_C3 0.25 Low quality
C_lit 0.65 Moderately studied
C_dup 1.0 Unique

📥 Members 📊 Colab 🔬 Bayestar19

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

Overview

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NGC 6618 is a sparse, very loose object of low C3 quality. Its parallax locates it at a close^* distance, near the mid-plane, affected by high extinction. It is catalogued as an extremely massive, near-solar metallicity, very young cluster (see Parameters). It is moderately studied in the literature.

(*): The parallax distance estimate (~0.62 kpc) differs significantly from the median photometric distance (~1.50 kpc).

Relatively close High extinction Extremely massive Near-solar metallicity Very young

Palma et al. (2025)
Part of multiple system G131, along with HSC_181 and Alessi_40.

Cavallo et al. (2024)
Gold sample.

Hunt & Reffert (2024)
Classified as moving group. CMD class: 0.97 (50th percentile).

Hunt & Reffert (2023)
Classified as open cluster. CMD class: 0.97 (50th percentile).

Morales et al. (2013)
Classified as morphological type 'EC2' (partially embedded cluster). Morphological flag: cluster partially embedded, presence of an IR bubble.

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

Lada & Lada (2003)
Embedded cluster within ∼2 Kpc of the Sun.

Data

🔍 Search references for NGC 6618 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–	275.097	-15.456	1.626	1.81	-5.377	-16.67
Cavallo et al.	2024	275.479	-14.741	1.634	–	–	–
Hunt & Reffert	2023	275.065	-15.982	1.635	1.757	-5.381	-16.956
Dias et al.	2018	–	–	–	-0.08	-3.03	–
Dib et al.	2018	275.145	-16.15	–	–	–	–
Loktin & Popova	2017	275.19	-16.173	–	1.51	-1.74	-4.0
Sampedro et al.	2017	275.196	-16.172	–	1.95	-1.47	–
Joshi et al.	2016	275.145	-16.15	–	–	–	–
Dias et al.	2014	275.196	-16.172	–	1.51	-1.74	–
Morales et al.	2013	275.125	-16.182	–	–	–	–
Gozha et al.	2012	275.196	-16.172	–	–	–	–
Piskunov et al.	2008	275.132	-16.19	–	–	–	–
Kharchenko et al.	2007	275.19	-16.17	–	0.3	–	-17.0
Piskunov et al.	2007	275.132	-16.19	–	–	–	–
van den Bergh	2006	275.108	-16.177	–	–	–	–
Kharchenko et al.	2005	275.14	-16.19	–	3.04	0.33	-17.0
Lada & Lada	2003	275.108	-16.177	–	–	–	–
Kharchenko et al.	2003	275.16	-16.17	–	2.36	0.79	–
Bica et al.	2003	275.123	-16.185	–	–	–	–
Dias et al.	2002	275.196	-16.172	–	1.51	-1.74	-25.3
Lynga	1987	275.188	-16.174	–	–	–	–
Sulentic et al.	1973	275.186	-16.171	–	–	–	–

💡 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–	1.5	4.905	1.47	4	0.041	10617	–	–
Cavallo et al.	2024	0.59	1.53	–	209	-0.050	–	–	–
Hunt & Reffert	2023	0.59	1.13	1.47	390	–	–	–	–
Dib et al.	2018	1.31	–	–	1	–	–	–	–
Loktin & Popova	2017	1.81	5.06	–	11	–	–	–	–
Joshi et al.	2016	1.31	5.07	–	1	–	30200	–	–
Morales et al.	2013	1.99	–	–	1	–	–	–	–
Gozha et al.	2012	1.30	–	–	1	–	30200	–	–
Piskunov et al.	2008	1.81	5.05	–	6	–	10617⁽¹⁾	–	–
Piskunov et al.	2007	1.81	5.05	–	6	–	838	–	–
van den Bergh	2006	1.30	4.76	–	1	–	–	–	–
Kharchenko et al.	2005	1.81	5.05	–	6	–	–	–	–
Lada & Lada	2003	1.80	–	–	–	–	890	–	–
Kharchenko et al.	2003	1.50	1.26	–	–	–	–	–	–
Dias et al.	2002	1.30	4.76	–	1	0.132	–	–	–
Lynga	1987	1.50	–	–	–	–	–	–	–

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

Visualization

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