The evolution of the UV luminosity and stellar mass functions of Lyman-α emitters from <i>z</i> ∼ 2 to <i>z</i> ∼ 6

ABSTRACT We measure the evolution of rest-frame UV luminosity function (LF) and stellar mass (SMF) Lyman-α (Ly α) emitters (LAEs) from z ∼ 2 to 6 by exploring ∼4000 LAEs SC4K sample. find a correlation between Ly α (LLy (MUV), with best fit M$_{\rm UV}=-1.6_{-0.3}^{+0.2}\log _{10} (\rm L_{Ly\,\alpha }/erg\, s^{-1})+47_{-11}^{+12}$ shallower relation LLy (M⋆), $\log M_\star /{\rm M}_\odot)=0.9_{-0.1}^{+0.1}\log s^{-1})-28_{-3.8}^{+4.0}$. An increasing cut predominantly lowers number density faint MUV low M⋆ LAEs. estimate proxy for full LFs SMFs simple assumptions end slope. For LF, we brightening characteristic (M$_{\rm UV}^*$) redshift decrease (Φ*). SMF, (${\rm ^*/{\rm M}_\odot }$) increase redshift, Φ* decline. However, if apply uniform s^{-1}) \ge 43.0$, much milder no in SMF The (ρUV) sample shows moderate (ρM) decreases, both being always lower than total ρUV ρM more typical galaxies but slowly approaching them redshift. Overall, our results indicate that approach measurements continuum-selected at &amp;gt; 6, which suggests key role epoch reionization.