%AZhang, Yechi%AOuchi, Masami%AGebhardt, Karl%AMentuch Cooper, Erin%ALiu, Chenxu%ADavis, Dustin%AJeong, Donghui%AFarrow, Daniel%AFinkelstein, Steven%AGawiser, Eric%AHill, Gary%AHarikane, Yuichi%AKakuma, Ryota%AAcquaviva, Viviana%ACasey, Caitlin%AFabricius, Maximilian%AHopp, Ulrich%AJarvis, Matt%ALandriau, Martin%AMawatari, Ken%AMukae, Shiro%AOno, Yoshiaki%ASakai, Nao%ASchneider, Donald%BJournal Name: The Astrophysical Journal; Journal Volume: 922; Journal Issue: 2 %D2021%I %JJournal Name: The Astrophysical Journal; Journal Volume: 922; Journal Issue: 2 %K %MOSTI ID: 10333830 %PMedium: X %TFirst HETDEX Spectroscopic Determinations of Lyα and UV Luminosity Functions at z = 2–3: Bridging a Gap between Faint AGNs and Bright Galaxies %XAbstract We present Ly α and ultraviolet (UV)-continuum luminosity functions (LFs) of galaxies and active galactic nuclei (AGNs) at z = 2.0–3.5 determined by the untargeted optical spectroscopic survey of the Hobby–Eberly Telescope Dark Energy Experiment (HETDEX). We combine deep Subaru imaging with HETDEX spectra resulting in 11.4 deg 2 of fiber spectra sky coverage, obtaining 18,320 galaxies spectroscopically identified with Ly α emission, 2126 of which host type 1 AGNs showing broad (FWHM > 1000 km s −1 ) Ly α emission lines. We derive the Ly α (UV) LF over 2 orders of magnitude covering bright galaxies and AGNs in log L Ly α / [ erg s − 1 ] = 43.3 – 45.5 (−27 < M UV < −20) by the 1/ V max estimator. Our results reveal that the bright-end hump of the Ly α LF is composed of type 1 AGNs. In conjunction with previous spectroscopic results at the faint end, we measure a slope of the best-fit Schechter function to be α Sch = − 1.70 − 0.14 + 0.13 , which indicates that α Sch steepens from z = 2–3 toward high redshift. Our UV LF agrees well with previous AGN UV LFs and extends to faint-AGN and bright-galaxy regimes. The number fraction of Ly α -emitting objects ( X LAE ) increases from M UV * ∼ − 21 to bright magnitude due to the contribution of type 1 AGNs, while previous studies claim that X Ly α decreases from faint magnitudes to M UV * , suggesting a valley in the X Ly α –magnitude relation at M UV * . Comparing our UV LF of type 1 AGNs at z = 2–3 with those at z = 0, we find that the number density of faint ( M UV > −21) type 1 AGNs increases from z ∼ 2 to 0, as opposed to the evolution of bright ( M UV < −21) type 1 AGNs, suggesting AGN downsizing in the rest-frame UV luminosity. %0Journal Article