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We examine parallaxes and distances for Galactic luminous blue variables(LBVs) in Gaia DR2. The sample includes 11 LBVs and 14 LBV candidates. Forabout half of the sample, DR2 distances are either similar to commonly adoptedliterature values, or the DR2 values have large uncertainties. For the rest,reliable DR2 distances differ significantly from values in the literature, andin most cases the Gaia DR2 distance is smaller. Two key results are that the SDoradus instability strip may not be as clearly defined as previously thought,and that there exists a population of LBVs at relatively low luminosities. LBVsseem to occupy a wide swath from the end of the main sequence at the blue edgeto 8000 K at the red side, with a spread in luminosity reaching as low aslog(L/Lsun)=4.5. The lower-luminosity group corresponds to effectivesingle-star initial masses of 10-25 Msun, and includes objects that have beenconsidered as confirmed LBVs. We discuss implications for LBVs including (1)their instability and origin in binary evolution, (2) connections to somesupernova (SN) impostors such as the class of SN 2008S-like objects, and (3)LBVs that may be progenitors of SNe with dense circumstellar material across awide initial mass range. Although some of the Gaia DR2 distances for LBVs havelarge uncertainty, this represents the most direct and consistent set ofGalactic LBV distance estimates available in the literature.

On the Gaia DR2 distances for Galactic Luminous Blue Variables