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Fig. 1.

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Submillimeter observations towards MACS1931. Upper left: Gaussian fit to the 12CO(1−0) line in the NRO 45-m observations of MACS1931. The black histogram shows the spectrum. The blue solid curve shows the Gaussian fit to the line. Upper right: Gaussian fit to the [CI](2−1) and 12CO(7−6) lines in the APEX observations of MACS1931. The black histogram shows the spectrum. The green and red solid curves show the Gaussian fits to the [CI](2−1) and 12CO(7−6) lines, respectively. The magenta solid lines show the regions of the spectrum excluded because of the atmospheric lines. Lower left: Best-fit line profiles of 12CO(1−0), 12CO(3−2), and 12CO(4−3) from Fogarty et al. (2019) (dashed curves) and Lorentzian fits on 12CO(1−0), 12CO(7−6), and [CI](2−1) from this work (solid curves) displayed on the same plot for comparison (see Sect. 3 and Table 1). The CGM tail peak of the 12CO(4−3) line from Fogarty et al. (2019) is the best fit to a partially truncated spectrum due to a spectral window gap in the ALMA Band 7 observations. Lower right: The ALMA 12CO(3−2) intensity map of the MACS1931 BCG and the tail. The moment zero map is calculated over a range of [ − 500, 600] km s−1. ALMA beam is shown by an ellipse on the bottom left side of the image. The APEX and NRO 45-m HPBWs are shown by solid red and dashed yellow circles. Contours are calculated on the moment map with levels [0.2, 0.5, 1, 2]σ and σ = 0.297 Jy beam−1 km s−1. The CGM tail component of the spectra is detectable in the [CI](2−1) line as well as all lines from Fogarty et al. (2019).

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