  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 distinctly
different carbon and nitrogen abundances, seen in a sharp division between
CN-weak and CN-strong red-giant branches (RGBs) in M3. The CN-strong population
shows 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 distribution
that is likely linked to its fast rotation. Our derived metallicity reveals
bimodal metallicity distributions in both populations, with
$\langle$[Fe/H]$\rangle\approx-$1.60 and $-$1.45, which appear to be
responsible 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 consists
of 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-N
anticorrelation and structural and kinematical property, which is a strong
indication of independent systems in M3. The fractions of the CN-weak
population for both the C1 and C2 are high compared to Galactic GCs but they
are in good agreement with GCs in Magellanic Clouds. It is believed that M3 is
a merger remnant of the two GCs, most likely in a dwarf galaxy environment, and
accreted to our Galaxy later in time. This is consistent with recent proposals
of an ex-situ origin of M3.
