4 candidate dusty WC identifications in IRS 13E (WR101de, WR101df, WR101dh, WR101ea) in VIIth annex
primarily from Maillard et al. (2004, MPS04) were not supported by Fritz et al. (FGD10)
8 stars from original manuscript of Kanarek et al. (2014, KSF14).
1089-117 omitted since spectroscopy reveals MgII 2.13/2.14 micron emission so
LBV candidate Stringfellow et al. (2012).
1626-4FC8 is a [WC6] according to Gvaramadze et al. (2010)
supported by a modest distance according to its Gaia DR3 parallax.
Other sources also omitted 1343-69E, 1353-160A, 1430-AB0, 1443-760, 1547-1DF2, 1547-E0B, some of which are reclassified as PNe or B[e]/LBVs.
1 star (CXOGC J174550.2-284911, WR102-4) is a duplicate of WR102ae as noted by Pantaleoni Gonzalez et al. 2025,
coordinates of Arches WR stars updated according to Clark et al. (2018, CLN18), and 4 Galactic Centre IRS 13E sources (listed above) have been removed. The candidate WR star LAMOST J101509.39-030832.6 from Chang et al. (2025) is the Cataclysmic Variable SW Sex.
1 star (GC IRS 7SE2 = S4-342, WR101nb) a candidate WC (Paumard et al. 2006, PGM06) from VIIth annex following priv. comm. (F. Martins, T. Paumard, R. Bentley)
1 star from Shara et al. (2012), 1023-63L (WC7, a.k.a. WR70-10) has been reclassified as a CSPNe [WC7] by Kanarek et al. 2016 (KSF16) since unrealistically large distance if massive star.
2 candidate WN stars from Liu et al. 2026 are excuded since one (DESI J072423+585705)
is unrealistically faint based on its Gaia DR3 distance (0.74 kpc), and the other (DESI J074300+325629) has no Gaia optical counterpart at this position.