Table 1
Observed sources.
| Name | 2MASS name | RA(J2000) deg | Dec(J2000) deg | distance kpc | Sp. type | Ref. | CSM size arcsec |
|---|---|---|---|---|---|---|---|
| HD 168607 | J18211489–1622318 | 275.3120 | −16.3755 | 1.84 ± 0.08 | B9Ia+ | 1 | − |
| HD 168625 | J18211955–1622260 | 275.3315 | −16.3739 | 1.53 ± 0.06 | B8Ia+ | 1 | 40 |
| MN87 | J18422247–0504300 | 280.5936 | −5.0750 | (2.0–4.0) | − | 28 | |
| MN101 | J19062457+0822015 | 286.6024 | +8.3671 | (3.0–6.2) | − | 20 | |
| G79.29+0.46 | J20314228+4021591 | 307.9262 | +40.3664 | 1.75 ± 0.18 | B:I[e] | 2 | 160 |
Notes. Distances derived from Gaia DR3 (Gaia Collaboration 2022) in HD 168607, HD 168625, and G79.29+0.46. For MN87, the quoted distance range was derived from the angular size of the shell, assuming a physical size of 0.3–0.6 pc, as observed in other LBV stars (Weis 2011). For MN101, the quoted distance range is the most likely range of geometric distances derived from Gaia parallaxes (Bailer-Jones et al. 2021). The quoted references are the papers used for the spectral classification of the target stars. CSM sizes are the angular diameters obtained by visual inspection of the images depicted in the papers cited in Sect. 1. (1) Clark et al. (2012); (2) Voors et al. (2000).
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