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We present Very Long Baseline Array polarimetric observations of theinnermost jet of 3C$\sim$84 (NGC$\sim$1275) at 43$\sim$GHz. A significantpolarized emission is detected at the hotspot of the innermost re-started jet,which is located $\sim$1 pc south from the radio core. While the previousreport presented a hotspot at the southern end of the western limb, the hotspotlocation has been moved to the southern end of the eastern limb. Faradayrotation is detected within an entire bandwidth of the 43-GHz band. Themeasured rotation measure (RM) is at most(6.3$\pm$1.9)$\times10^{5}$$\sim$rad$\sim$m$^{-2}$ and might be slightly timevariable on the timescale of a month by a factor of a few. Our measured RM andthe RM previously reported by the CARMA and SMA observations cannot beconsistently explained by the spherical accretion flow with a power-lawprofile. We propose that a clumpy/inhomogeneous ambient medium is responsiblefor the observed rotation measure. Using equipartition magnetic field, wederive the electron density of $2\times10^{4}$$\sim$cm$^{-3}$. Such an electrondensity is consistent with the cloud of narrow line emission region around thecentral engine. We also discuss the magnetic field configuration from blackhole scale to pc scale and the origin of low polarization.

Enhanced Polarized Emission from the One-Parsec-Scale Hotspot of 3C 84 as a Result of the Interaction with Clumpy Ambient Medium