Seiji FujimotoJohn D. SilvermanMatthieu BetherminMichele GinolfiGareth C. JonesOlivier Le FèvreMiroslava Dessauges-ZavadskyWiphu RujopakarnAndreas L. FaisstYoshinobu FudamotoPaolo CassataLaura MorselliRoberto MaiolinoDaniel SchaererPeter CapakLin YanLivia ValliniSune ToftFederica LoiaconoGianni ZamoraniMargherita TaliaDesika NarayananNimish P. HathiBrian C. LemauxMédéric BoquienRicardo AmorinIbar, EduardoEduardoIbarAnton M. KoekemoerHugo Méndez-HernándezSandro BardelliDaniela VerganiElena ZuccaMichael RomanoAndrea Cimatti2025-04-132025-04-132020-08-2710.3847/1538-4357/ab94b32-s2.0-85091141667https://cris-uv-2.scimago.es/handle/123456789/1866WOS:000566094400001Abstract We present the physical extent of [C ii ] 158 μ m line-emitting gas from 46 star-forming galaxies at z = 4–6 from the ALMA Large Program to INvestigate C ii at Early Times (ALPINE). Using exponential profile fits, we measure the effective radius of the [C ii ] line ( ) for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum ( ) from Hubble Space Telescope images. The effective radius exceeds by factors of ∼2–3, and the ratio of increases as a function of M star . We do not find strong evidence that the [C ii ] line, rest-frame UV, and far-infrared (FIR) continuum are always displaced over ≃1 kpc scale from each other. We identify 30% of isolated ALPINE sources as having an extended [C ii ] component over 10 kpc scales detected at 4.1 σ –10.9 σ beyond the size of rest-frame UV and FIR continuum. One object has tentative rotating features up to ∼10 kpc, where the 3D model fit shows the rotating [C ii ]-gas disk spread over 4 times larger than the rest-frame UV-emitting region. Galaxies with the extended [C ii ] line structure have high star formation rate, high stellar mass ( M star ), low Ly α equivalent width, and more blueshifted (redshifted) rest-frame UV metal absorption (Ly α line), as compared to galaxies without such extended [C ii ] structures. Although we cannot rule out the possibility that a selection bias toward luminous objects may be responsible for such trends, the star-formation-driven outflow also explains all these trends. Deeper observations are essential to test whether the extended [C ii ] line structures are ubiquitous to high- z star-forming galaxies.enacceso abiertoAstronomy And AstrophysicsSpace And Planetary Sciencearticle