Fujimoto, SeijiSeijiFujimotoSilverman, John D.John D.SilvermanBethermin, MatthieuMatthieuBetherminGINOLFI, MICHELEMICHELEGINOLFIJones, Gareth C.Gareth C.JonesLe Fèvre, OlivierOlivierLe FèvreDessauges-Zavadsky, MiroslavaMiroslavaDessauges-ZavadskyRujopakarn, WiphuWiphuRujopakarnFaisst, Andreas L.Andreas L.FaisstFudamoto, YoshinobuYoshinobuFudamotoCassata, PaoloPaoloCassataMORSELLI, LAURALAURAMORSELLIMaiolino, RobertoRobertoMaiolinoSchaerer, DanielDanielSchaererCapak, PeterPeterCapakYan, LinLinYanVALLINI, LiviaLiviaVALLINIToft, SuneSuneToftLOIACONO, FedericaFedericaLOIACONOZamorani, GianniGianniZamoraniTalia, MargheritaMargheritaTaliaNarayanan, DesikaDesikaNarayananHathi, Nimish P.Nimish P.HathiLemaux, Brian C.Brian C.LemauxBoquien, MédéricMédéricBoquienAmorin, RicardoRicardoAmorinIbar, EdoEdoIbarKoekemoer, Anton M.Anton M.KoekemoerMéndez-Hernández, HugoHugoMéndez-HernándezBARDELLI, SandroSandroBARDELLIVERGANI, DANIELADANIELAVERGANIZUCCA, ElenaElenaZUCCAROMANO, MICHAELMICHAELROMANOCIMATTI, ANDREAANDREACIMATTI2025-03-122025-03-1220200004-637Xhttp://hdl.handle.net/20.500.12386/36715We present the physical extent of [C II] 158 μm 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 (${r}_{{\rm{e}},[{\rm{C}}{\rm\small{II}}]}$) for individual galaxies and compare them with the rest-frame ultraviolet (UV) continuum (${r}_{{\rm{e}},\mathrm{UV}}$) from Hubble Space Telescope images. The effective radius ${r}_{{\rm{e}},[{\rm{C}}{\rm\small{II}}]}$ exceeds ${r}_{{\rm{e}},\mathrm{UV}}$ by factors of ∼2-3, and the ratio of ${r}_{{\rm{e}},[{\rm{C}}{\rm\small{II}}]}/{r}_{{\rm{e}},\mathrm{UV}}$ increases as a function of M<SUB>star</SUB>. 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 4.1σ-10.9σ 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<SUB>star</SUB>), low Lyα equivalent width, and more blueshifted (redshifted) rest-frame UV metal absorption (Lyα 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.STAMPAenArticle10.3847/1538-4357/ab94b32-s2.0-85091141667https://iopscience.iop.org/article/10.3847/1538-4357/ab94b3https://api.elsevier.com/content/abstract/scopus_id/850911416672020ApJ...900....1FFIS/05 - ASTRONOMIA E ASTROFISICA