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We examine the rest-frame ultra-violet (UV) properties of 10[CII]$\lambda158\,{\rm \mu m}$$-$detected galaxies at $z\sim5.5$ in COSMOSusing new HST/WFC3 near-infrared imaging. Together with pre-existing $158\,{\rm\mu m}-$continuum and [CII] line measurements by ALMA, we study their dustattenuation properties on the IRX-$\beta$ diagram, which connects the totaldust emission ($\propto$ IRX=log($L_{FIR}/L_{1600}$)) to the line-of-sight dustcolumn ($\propto\beta$). We find systematically bluer UV continuum spectralslopes ($\beta$) compared to previous low-resolution ground-based measurements,which relieves some of the tension between models of dust attenuation andobservations at high redshifts. While most of the galaxies are consistent withlocal starburst or Small Magellanic cloud like dust properties, we findgalaxies with low IRX values and a large range in $\beta$ that cannot beexplained by models of a uniform dust distribution well mixed with stars. Astacking analysis of Keck/DEIMOS optical spectra indicates that these galaxiesare metal-poor with young stellar populations which could significantly altertheir spatial dust distribution.

Dust Properties of [CII] Detected z $\sim$ 5.5 Galaxies: New HST/WFC3 Near-IR Observations