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We report on a $\rm{[CII]}_{158\mu\rm{m}}$ search using the Atacama LargeMillimeter/submillimeter Array (ALMA) on three lensed, confirmed {\lya}emitting galaxies at $z \sim 7$. Our targets are ultra-violet (UV) faintsystems with stellar masses on the order of $M_{*} \sim 10^{9} M_{\odot}$. Wedetect a single [CII] line emission ($4\sigma$) from the brightest ($L \sim 2.4\times 10^{10}L_{\odot}$) galaxy in our sample, MACS0454-1251. We determine asystemic redshift ($z_{\rm{[CII]}} = 6.3151 \pm 0.0005$) for MACS0454-1251 andmeasure a {\lya} velocity offset of $\Delta v \approx 300 \pm 70\rm{km\,s}^{-1}$. The remaining two galaxies we detect no {\ct} but provide $3\sigma$ upper limits on their {\ct} line luminosities which we use toinvestigate the $L_{\textrm{[CII]}} - \rm{SFR}$ relation. Overall our single{\ct} detection shows agreement with the relation for dwarf and local starburstgalaxies. Our [CII] deficient galaxies could potentially be exhibiting lowmetallicities ($Z<Z_{\odot}$). Another possible explanation for weaker [CII]emission could be strong feedback from star formation disrupting molecularclouds. We do not detect continuum emission in any of the sources, placingupper limits on their dust masses. Assuming a single dust temperature of$T_{d}=35 \rm{K}$ dust masses ($M_{\rm{dust}}$) range from $< 4.8 \times 10^{7}M_{\odot} $ to $2.3 \times 10^{8} M_{\odot}$. Collectively, our results suggestfaint reionization era sources could be metal poor and/or could have strongfeedback suppressing [CII] emission.

Studying [CII] Emission in Low-mass Galaxies at z ~ 7