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We present Ca-CN-CH-NH photometry for the well-known globular cluster (GC) M3(NGC 5272). We show new evidence for two M3 populations with distinctlydifferent carbon and nitrogen abundances, seen in a sharp division betweenCN-weak and CN-strong red-giant branches (RGBs) in M3. The CN-strong populationshows a C-N anticorrelation that is a natural consequence of the CN cycle,while the CN-weak population shows no or a weak C-N anticorrelation.Additionally, the CN-weak population exhibits an elongated spatial distributionthat is likely linked to its fast rotation. Our derived metallicity revealsbimodal metallicity distributions in both populations, with$\langle$[Fe/H]$\rangle\approx-$1.60 and $-$1.45, which appear to beresponsible for the discrete double RGB bumps in the CN-weak and the large$W^{1G}_{F275W-F814W}$ range. From this discovery, we propose that M3 consistsof two GCs, namely the C1 (23\%, $\langle$[Fe/H]$\rangle\approx-1.60$) and C2(77\%, $\langle$[Fe/H]$\rangle\approx-1.45$), each of which has its own C-Nanticorrelation and structural and kinematical property, which is a strongindication of independent systems in M3. The fractions of the CN-weakpopulation for both the C1 and C2 are high compared to Galactic GCs but theyare in good agreement with GCs in Magellanic Clouds. It is believed that M3 isa merger remnant of the two GCs, most likely in a dwarf galaxy environment, andaccreted to our Galaxy later in time. This is consistent with recent proposalsof an ex-situ origin of M3.

astrophysical journal/the astrophysical journal

Multiple Stellar Populations of Globular Clusters from Homogeneous  Ca-CN-CH-NH Photometry. VI. M3 (NGC 5272) is not a Prototypical Normal  Globular Cluster