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We study the 3.55 keV X-ray suspected to arise from dark matter in our modelof dark matter consisting of a bubble of a new phase of the vacuum, the surfacetension of which keeps ordinary matter under high pressure inside the bubble.We consider two versions of the model:  Old large pearls model :  We worked for a long time on a pearl picture with pearl / bubbles of cm-sizeadjusted so that the impacts of them on earth could be identified with eventsof the mysterious type that happened in Tunguska in 1908. We fit both the veryfrequency, the 3.55 keV, and the overall intensity of the X-ray line comingfrom the center of the Milky Way and from galaxy clusters with one parameter inthe model in which this radiation comes from collisions of pearls.  New small pearl model:  Our latest idea is to let the pearls be smaller than atoms but bigger thannuclei so as to manage to fit the 3.5 keV X-rays coming from the Tychosupernova remnant in which Jeltema and Profumo observed this line. Further wealso crudely fit the DAMA-LIBRA observation with the small pearls, and even seea possibility for including the electron-recoil-excess seen by the Xenon1Texperiment as being due to de-excitation via electron emission of our pearls.The important point of even our small size pearl model is that the crosssection of our "macroscopic" pearls is so large that the pearls interactseveral times in the shielding but, due to their much larger mass than thetypical nuclei, are {\bf not stopped by only a few interactions}. Neverthelessonly a minute fraction of the relatively strongly interacting pearls reach the1400 m down to the DAMA experiment, but due to the higher cross section we canfit the data anyway.

Dark Matter Macroscopic Pearls, 3.55 keV X-ray line, How big ?