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tokens: 2010 ) can become carbon-rich, although the transition luminosity is lower in metal-poor populations. Sextans A appears to have a higher relative fraction of carbon stars compared to Leo A (Table 9 ), and its evolved stellar population (above the TRGB) is more luminous. In both galaxies, there are a few stars with bolometric magnitudes brighter than the traditional AGB luminosity limit of (Wood et al. 1983 ). These bright sources represent a small population of RSGs or hot-bottom-burning AGB stars (with ), whose ages are consistent with a recent increase in the SFR ∼1 Gyr ago (Dolphin et al. 2005 ; Cole et al. 2007 ). The discrepancy in the size of the AGB populations unlikely due to the difference in stellar mass of the host galaxy. More likely it is due to differences in both the mean metallicity and SFH. 4.2. Dust Production Stars with have a measurable IR excess due to dust. There are 32 stars in Leo A and 101 stars in Sextans A, which meet this criteria, with a low-moderate relative uncertainty in the DPR. As the uncertainty in the chemical classification is high for most sources (Figure 9 ), we compute four values for the total dust-production rate: (1) using the best-fit models irrespective of dust chemistry; (2) assuming all stars are O-rich; (3) assuming all stars are C-rich; and (4) only including stars identified as variable. Table 10 lists the total DPRs for each galaxy. These estimates exclude any source with a relative uncertainty in the DPR > 0 (see Figure 8 ). Table 10 The Global Dust-production Rates for Leo A and Sextans A Note. Best-fitting chemical type: 25 C-rich and 6 O-rich in Leo A, and 68 C-rich and 33 O-rich in Sextans A. The total DPR in Sextans A should be considered a lower limit, as we do not detect AGB stars to the tip of the RGB. In both galaxies, the total dust input into the ISM is dominated by one or two stars. In Leo A, the star with the highest DPR is LeoA-143, with a DPR of . This is two orders of magnitude greater than the second-highest DPR in Leo A. This object has a rising SED and was identified as a candidate PNe from H α observations by Magrini et al. ( 2003 ), hence we exclude this source from the global dust-budget estimate. In Sextans A, the two sources with the highest DPRs are IDs 17 and 448 (SSTDUSTG J101059.43-044249.3 and J101058.05-044304.1, with and , respectively). These also have rising SEDs; however, both of these sources have been identified as variable x-AGB candidates by DUSTiNGS (Boyer et al. 2015c ). Our fitting routine classified SextansA-17 as an oxygen-rich AGB-star; it is responsible for 89% of the global dust production of Sextans A. If this source is instead carbon rich, then its DPR is significantly lower: . If SextansA-17 is confirmed to be an oxygen-rich AGB star, then it conclusively shows that individual metal-poor ( to −1.40) evolved stars can produce significant amounts of dust, and contribute substantially to the enrichment of the ISM in their host system. Figure 11