Clump formation in ram-pressure stripped galaxies: Evidence from mass function

Open Access

Fig. A.2.

Maps of the Hα (top panels) and UV (bottom panels) stacked clumps (left panels) and best-fitting models (right panels) obtained with two 2D Moffat (parameters in Table A.1), residuals. The axes and the fluxes are normalized to scale quantities, as described in Sect. A.

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