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We test the origin of the 3.5 keV line photons by analyzing the morphology ofthe emission at that energy from the Galactic Center and from the Perseuscluster of galaxies. We employ a variety of different templates to model thecontinuum emission and analyze the resulting radial and azimuthal distributionof the residual emission. We then perform a pixel-by-pixel binned likelihoodanalysis including line emission templates and dark matter templates and assessthe correlation of the 3.5 keV emission with these templates. We conclude thatthe radial and azimuthal distribution of the residual emission is incompatiblewith a dark matter origin for both the Galactic center and Perseus; theGalactic center 3.5 keV line photons trace the morphology of lines atcomparable energy, while the Perseus 3.5 keV photons are highly correlated withthe cluster's cool core, and exhibit a morphology incompatible with dark matterdecay. The template analysis additionally allows us to set the most stringentconstraints to date on lines in the 3.5 keV range from dark matter decay.

Where do the 3.5 keV photons come from? A morphological study of the Galactic Center and of Perseus