tokens: the galactic relationship (i.e., Friedman et al. 2011 ) can be applied and it provides the estimate of corresponding to based on the DIB measurement alone, which is in very good agreement with our direct measurement of . Fitting the emission with multiple Gaussians allows an estimate of for the small component at km s as also listed in the table. Figure 6 relates these measurements to those by Welty et al. (2006) , Welty Hobbs (2001) and Friedman et al. (2011) in the Milky Way. The MUSE data allow for excellent measurements of the DIB equivalent widths. The comparison to other DIB data in Fig. A.4 further verifies the method utilized here to measure the equivalent widths in composite fitting residuals of cluster stars as the derived absolute equivalent widths for different DIBs lie within the expected correlation to the strong DIB 5780. Fig. 6 (5780) vs. ( ). The data for the composite spectrum as listed in Table 1 (red star) overlaid to corresponding data for the Milky Way as published in Welty et al. (2006) , Friedman et al. (2011) and Welty Hobbs ( 2001 ; as scatter plot in black). Measurement uncertainties of those data vary between 3 mÅ and 20 mÅ for DIB 5780 and are omitted here for clarity. For our measurement the statistical error is about 12 mÅ and lies within a fraction of the star symbol. 4.2. Spatially resolved Na<inline-formula specific-use="simple-math"><italic>I</italic></inline-formula>, K <inline-formula specific-use="simple-math"><italic>I</italic></inline-formula>, and DIBs 4.2.1. Maps In the previous section we saw that the measurements on the composite spectrum of almost 10 000 cluster stars are in very good agreement with other measurements of individual sight lines in the Milky Way. Rather than finding universal correlations between species, we are in the position to be able to probe correlations between DIBs on very small scales and thus likely in a physically connected absorber. Figure 7 shows a spatial map of and of the DIB ratio 5780/5797 (this ratio is thought to be sensitive to the UV radiation field: Ensor et al. 2017 ). The implications are discussed in Sect. 4.3 . The measured total equivalent width of shows no correlation with the brightness of the GC which would otherwise indicate some underlying systematics in the analysis. Fig. 7 Equivalent width map for the doublet ( top ) and the DIB ratio 5780/5797 ( bottom ). All selected cluster stars are colored in 31 groups according to their Voronoi-bin. The color reflects the measured total equivalent width of the doublet for each composite spectrum per bin with an average of about 960 mÅ. The center of the globular cluster is at coordinate origin and marked with a red star. Brightness contours of the globular cluster are shown as white lines. For the contour plot, the white light image was smoothed to a resolution of 20 arcsec. Further spatial maps are shown in Fig. 8 . The large spatial variations up to a factor of four ( ) or two (DIB 5797) stand out. DIB 6283
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