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tokens: but not part of the interacting pair (UGC 10549, z = 0.009, 50 kpc projected separation). The integrated spectrum shows a somewhat complex profile, with the velocity of the peak emission at ≳50 km s −1 lower velocity than the redshifts of the two components of dm1647+21. This peak corresponds to the redshift of UGC 10549, suggesting a substantial amount of the single-dish H i flux is associated with that galaxy. In support of this interpretation of the single-dish profile, follow-up interferometric observations with the Very Large Array (VLA) reveal a clumpy H i distribution in dm1647+21 and emission associated with UGC 10549 (S. Stierwalt et al. 2017, in preparation). Unfortunately, the VLA observations (taken in the B-array) do not recover the total single-dish H i flux, so we cannot reliably separate the single-dish H i mass into contributions from dm1647+21 and UGC 10549. Considering the uncertain distribution of the H i mass, the single-dish measurement implies an upper limit to the gas depletion time of 2 Gyr when considering only the SFR of dm1647+21. The true gas depletion time for dm1647+21 is likely shorter than this estimate. 3.3. ISM Properties We use the line images created from the MUSE data to construct optical line ratio maps, based on classic optical diagnostic plots (e.g., Baldwin et al. 1981 ; Veilleux Osterbrock 1987 ; Kewley et al. 2006 ). Maps of [O iii ]/H β , [N ii ]/H α , and [S ii ]/H α are shown in Figure 2 . The system-integrated values for these ratios are: log 10 ([O iii ]/H β ) = 0.51, log 10 ([N ii ]/H α ) = −1.8, and log 10 ([S ii ]/H α ) = −1.0. In Figure 3 , we show the line diagnostic diagrams with the distribution of values from Figure 2 and the source separation lines from Kewley et al. ( 2006 ). The line ratios in the ratio maps and diagnostic diagrams are all consistent with excitation from star formation, and we see no evidence for LINER-like or Seyfert emission. Figure 2. Optical line ratio images. First row, from left to right: [O iii ]/H β , [N ii ]/H α , [S ii ]/H α . Second row, from left to right: A H α and [S ii ] 6718/[S ii ] 6732. The ratio maps were all masked to the fainter of the two lines (Figure 1 ). No extinction corrections have been applied. Figure 3. Optical line diagnostic diagrams based on the narrow-band images in Figure 2 . Left: [O iii ]/H β vs. [N ii ]/H α . Right: [O iii ]/H β vs. [S ii ]/H α . The colored contours and small points show the distribution of values for individual 02 × 02 spaxels in the data cube; the number in the bottom left gives the number of spaxels shown in each panel. The plotted spaxels are those with a ≥5 σ detection in [N ii ] 6585 (left) or [S ii ] 6718 + 6732 (right). The cyan crosses mark the locations of the three brightest clumps identified from the H α map (Section 3.2 , 15 diameter apertures). The colored lines are the Kewley et al. ( 2006 ) separations between star-forming galaxies, Seyferts, and LINERs. The line ratios are consistent with