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The two red clumps (RCs) observed in the color-magnitude diagram of the MilkyWay bulge is widely accepted as evidence for an X-shaped structure originatedfrom the bar instability. A drastically different interpretation has beensuggested, however, based on the He-enhanced multiple stellar populationphenomenon as is observed in globular clusters (GCs). Because these twoscenarios imply very different pictures on the formation of the bulge andelliptical galaxies, understanding the origin of the double RC is of crucialimportance. Here we report our discovery that the stars in the two RCs show asignificant (> 5.3 {\sigma}) difference in CN-band strength, in stark contrastto that expected in the X-shaped bulge scenario. The difference in CN abundanceand the population ratio between the two RCs are comparable to those observedin GCs between the first- and later generation stars. Since CN-strong starstrace a population with enhanced N, Na, and He abundances originated in GCs,this is direct evidence that the double RC is due to the multiple populationphenomenon, and that a significant population of stars in the Milky Way bulgewere assembled from disrupted proto-GCs. Our result also calls for the majorrevision of the 3D structure of the Milky Way bulge given that the current viewis based on the previous interpretation of the double RC phenomenon.

Assembling the Milky Way bulge from globular clusters: Evidence from the double red clump