  We present the results of a broadband radio-to-GeV observing campaign
organized to get a better understanding of the radiation processes responsible
for the $\gamma$-ray flares observed in 3C 279. The total intensity and
polarization observations of the source were carried out between December 28,
2013 and January 03, 2014 using the Fermi-LAT, Swift-XRT, Swift-UVOT, and KVN
telescopes. A prominent flare observed in the optical/near-UV passbands was
found to be correlated with a concurrent $\gamma$-ray flare at a confidence
level $>$95$\%$, which suggests a co-spatial origin of the two. Moreover, the
flaring activity in the two regimes was accompanied by no significant spectral
variations. A peak in the X-ray light curve coincides with the peaks of the
fractional polarization curves at 43 and 86 GHz radio bands. No prominent
variation was noticed for the total intensity and the electric vector position
angle (EVPA) observations at radio bands during this period. We noticed a
possible hint of steepening of the radio spectrum with an increase in
percentage polarization, which suggests that the radio polarization variations
could be simply due to a spectral change. In a simple scenario, the correlated
optical/$\gamma$-ray flares could be caused by the same population of emitting
particles. The coincidence of the increase in radio polarization with the X-ray
flux supports the picture that X-rays are produced via inverse-Compton
scattering of radio photons. The observed fractional variability for the
$\gamma$-ray flare $\sim$0.23 does not exceed that in the optical regime, which
is inconsistent with what we usually observe for 3C 279; it could be due to
different dependencies of the magnetic field and the external radiation field
energy density profiles along the jet.
