(J013406.63+304147.8)

This star is also known as [HS80] B416. Despite the detected CO band emission from this object [138], a classification as B[e]SG seems not appropriate (as previously mentioned by Humphreys et al. [98,99]), because its near-IR colors show clearly the lack of warm dust and would place the object to the region populated by LBVs. In addition, no [OI] emission is seen from J013406.63+304147.8 [98]. However, thus far, no photometric variability, typical for LBVs, is recorded [97], and the star can only be considered as a possible LBV candidate, as was previously suggested [99]. The star is found to be surrounded by an expanding ring-like nebula [141] and shows excess emission at 8 μm due to PAHs [138]. The spectral energy distribution leaves space for a companion [98,138], and its spectral lines display radial velocity variations with a period of 16.13 d, leading to the suggestion that the system might be an interacting binary system causing mass loss in the equatorial plane [145].
