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Surface brightness fluctuation (SBF) magnitudes are a powerful standardcandle to measure distances to semi-resolved galaxies in the local universe, amajority of which are dwarf galaxies that have often bluer colors than brightearly-type galaxies. We present an empirical $i-$band SBF calibration in a blueregime, $0.2 \lesssim (g-i)_0 \lesssim 0.8$ in the Hyper Suprime-Cam (HSC)magnitude system. We measure SBF magnitudes for 12 nearby dwarf galaxies ofvarious morphological types with archival HSC imaging data, and use their tipof the red giant branch (TRGB) distances to derive fluctuation - colorrelations. In order to subtract contributions of fluctuations due to youngstellar populations, we use five different $g-$band magnitude maskingthresholds, $M_{g,{\rm thres}} = -3.5, -4.0, -4.5, -5.0,$ and $-5.5$ mag. Wefind that the rms scatter of the linear fit to the relation is the smallest(rms = 0.16 mag) in the case of $M_{g,{\rm thres}} = -4.0$ mag, $\overline{M_i}= (-2.65\pm0.13)+ (1.28\pm0.24) \times (g-i)_0$. This scatter is much smallerthan those in the previous studies (rms=0.26 mag), and is closer to the valuefor bright red galaxies (rms=0.12 mag). This calibration is consistent withpredictions from metal-poor simple stellar population models.

Calibration of Surface Brightness Fluctuations for Dwarf Galaxies in the Hyper Suprime-Cam $gi$ Filter System