We report on the detection of the [CII] 157.7 $mu$m emission from the Lyman break galaxy (LBG) MACS0416_Y1 at z = 8.3113, by using the Atacama Large Millimeter/submillimeter Array (ALMA). The luminosity ratio of [OIII] 88 $mu$m (from previous campaigns) to [CII] is 9.31 $pm$ 2.6, indicative of hard interstellar radiation fields and/or a low covering fraction of photo-dissociation regions. The emission of [CII] is cospatial to the 850 $mu$m dust emission (90 $mu$m rest-frame, from previous campaigns), however the peak [CII] emission does not agree with the peak [OIII] emission, suggesting that the lines originate from different conditions in the interstellar medium. We fail to detect continuum emission at 1.5 mm (160 $mu$m rest-frame) down to 18 $mu$Jy (3$sigma$). This nondetection places a strong limit on the dust spectrum, considering the 137 $pm$ 26 $mu$Jy continuum emission at 850 $mu$m. This suggests an unusually warm dust component (T $>$ 80 K, 90% confidence limit), and/or a steep dust-emissivity index ($beta_{rm dust}$ $>$ 2), compared to galaxy-wide dust emission found at lower redshifts (typically T $sim$ 30 - 50 K, $beta_{rm dust}$ $sim$ 1 - 2). If such temperatures are common, this would reduce the required dust mass and relax the dust production problem at the highest redshifts. We therefore warn against the use of only single-wavelength information to derive physical properties, recommend a more thorough examination of dust temperatures in the early Universe, and stress the need for instrumentation that probes the peak of warm dust in the Epoch of Reionization.
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