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tokens: no notable difference in the spatial distribution of variable stars compared to the unclassified (nonvariable) sources according to Gaia DR2. 5.6. P-L Relations Accurately determined periods have been the means to distinguish variable stars, particularly pulsating variables (LPV, Cepheids, RR Lyrae, RV Tauri, etc.) within Gaia (Gaia Collaboration et al. 2019 ). Figure 13 displays the distribution of periods available from Gaia for sources in the local sample. It can be noted that the whole sample contains LPV stars with a wide range of periods, but that those within the solar neighborhood are restricted to stars with periods of ≲1250 days, presumably Mira or SR variables, as classified by Gaia (Molnár et al. 2018 ; Mowlavi et al. 2018 ). Figure 13. Period distributions obtained for variable stars in Gaia DR2 for the Gaia–BAaDE and local samples (see Figure 5 and Section 5.6 ). It has been established that P-L relations are a very powerful tool to distinguish AGB stars of different natures (Wood et al. 1999 ; Ita et al. 2004 ; Lebzelter et al. 2019 ). By recognizing that Mira variables pulsate dominantly in the fundamental mode, they can be promising candidates for distance determinations of remote galaxies, using empirical relations based on the LMC (Whitelock et al. 2008 ). With 2MASS K magnitudes, Gaia DR2 parallaxes, extinction maps, and periods for a subsample of the local sample ( period sample), we are able to make a comparison of the BAaDE targets with previously studied variable stars. In Figure 14 , we present the P-L relation for those BAaDE stars in the local sample with measured Gaia periods ( period sample), where there is a spread in the magnitude, resulting from uncertainties in the apparent K magnitude, extinction, and distance (indicated by the error bars) and IR variability (not indicated). A comparison is made of the P-L distributions with known variability sequences, associated with distinct pulsation modes, that have been derived from Gaia DR2 data for LMC populations as discussed by Lebzelter et al. ( 2019 ). These sequences have been transformed to , using the LMC distance modulus in that work (18.49 mag). Moreover, the established P-L relations for Miras from Whitelock et al. ( 2008 ) and Matsunaga Team ( 2006 ) in the LMC are added. Figure 14. Period–luminosity relations found for the variable stars within the local sample. The sequences marked as C , C ′, and D represent different known variability sequences, associated with distinct pulsation modes derived for the LMC based on Gaia data (Lebzelter et al. 2019 ). Note that the sequences were corrected for a distance modulus of 18.49 mag. Period–luminosity relations reported for LMC using other surveys are also shown (Matsunaga Team 2006 ; Whitelock et al. 2008 ). The local sample appears to be much flatter than the empirical P-L relations for the LMC, and it is clear that most of the stars in the local sample fall below the LMC P-L relations (Matsunaga Team 2006 ;