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tokens: are the amplitude index (Belokurov et al. 2017 ) and the Gaia DR2 variability classification (Mowlavi et al. 2018 ), in the left and right panels, respectively. The local sample (without YSOs and MS/RGB stars) is also shown for comparison as a black unfilled histograms. We found that the amplitude index method seems to find variability in objects that were not classified as variables in the Gaia DR2. 5.2. Absolute Magnitudes for the Foreground Mira Population Several studies have been carried out to estimate IR absolute magnitudes of the AGB populations in the LMC, where the distance to the stellar system is known, and therefore, the distance modulus (and presumably also the IR extinction) can be assumed to be the same for each object (see e.g., Whitelock et al. 2008 ). From Figure 6 , we can determine an average absolute K magnitude of mag for the local sample. Although the magnitude values found roughly correspond to those found in the LMC (i.e., between −8.0 and −6.0 mag; see, e.g., Whitelock et al. 2008 ), one should keep in mind that we established a fainter limit of . Nevertheless, with the aim of analyzing the absolute magnitude distribution using the variability classification defined by Gaia (Mowlavi et al. 2018 ) and the amplitude index (Belokurov et al. 2017 ), we made Figure 9 , where the distribution of absolute magnitude for the local sample without considering the filtering of YSOs and MS/RGB (made in Section 4.3 ) is shown. Figure 9 shows that by including these younger sources, the distributions are much broader in terms of absolute magnitude range. This can be partly explained by the current sample being mostly based on a single 2MASS observation and including the effects of large amplitude variability. However, when we filter the sample by a variability qualification (as shown in both panels of Figure 9 ), the low-luminosity tail (in ) is cut out. In this sense, the Gaia classification as Mira or SR variable seems to narrow the distribution more. Following a similar discussion in Mowlavi et al. ( 2018 ), we argue that the low-luminosity tail in Figure 9 and also Figure 7 is due to contamination with YSOs and MS/RGB stars that can also peak in the IR but do not show the same variability (Lewis et al. 2020b ; Y. M. Pihlström et al. 2020, in preparation). 5.3. Bolometric Magnitudes for the Foreground Mira Population The bolometric luminosity is a fundamental property useful for classifying stellar populations and evolutionary stages (Srinivasan et al. 2009 ), as it measures the intrinsic stellar power. Although its definition is straightforwardly formulated as the total integrated power over all frequencies, in practice, complete photometric measurements that allow a direct bolometric luminosity estimate are hardly ever available. Therefore, under various assumptions, a limited set of photometric measurements, preferably near the peak of the SED, can be used to apply a bolometric correction (BC) in order to determine the