Early galaxy formation initiated by the dark matter and gas assembly evolves through frequent mergers and feedback processes into dynamically hot chaotic structures. In contrast dynamically cold smooth rotating disks have been observed in massive evolved galaxies merely 1.4 billion years after the Big Bang suggesting rapid morphological and dynamical evolution in the early Universe. Probing this evolution mechanism necessitates studies of young galaxies yet efforts have been hindered by observational limitations in both sensitivity and spatial resolution. Here we report highresolution observations of a strongly lensed and quintuply imaged lowluminosity young galaxy at z6.072 dubbed the Cosmic Grapes 930 million years after the Big Bang. Magnified by gravitational lensing the galaxy is resolved into at least 15 individual starforming clumps with effective radii of rrm esimeq 1060 parsec pc which dominate simeq 70 of the galaxys total flux. The cool gas emission unveils a smooth underlying rotating disk characterized by a high rotationaltorandom motion ratio and a gravitationally unstable state Toomre Q simeq 0.20.3 with high surface gas densities comparable to local dusty starbursts with simeq1035 Modotpc2. These gas properties suggest that the numerous starforming clumps are formed through disk instabilities with weak feedback effects. The clumpiness of the Cosmic Grapes significantly exceeds that of galaxies at later epochs and the predictions from current simulations for early galaxies. Our findings shed new light on internal galaxy substructures and their relation to the underlying dynamics and feedback mechanisms at play during their early formation phases potentially explaining the high abundance of bright galaxies observed in the early Universe and the dark matter corecusp problem.
['Astrophysics - Astrophysics of Galaxies', 'Astrophysics - Cosmology and Nongalactic Astrophysics']
Primordial Rotating Disk Composed of geq15 Dense StarForming Clumps at Cosmic Dawn
{'Primordial Rotating Disk Composed of ≥ 15 Dense StarForming Clumps at Cosmic Dawn': "S. Fujimoto 1 , ∗ , M. Ouchi 2 , 3 , 4 , 5 , K. Kohno 6 , 7 , F. Valentino 8 , 9 , C. Giménez-Arteaga 9 , 10 , G. B. Brammer 9 , 10 , L. J. Furtak 11 , M. Kohandel 12 , M. Oguri 13 , 14 , A. Pallottini 12 , J. Richard 15 , A. Zitrin 11 , F. E. Bauer 16 , 17 , 18 , M. Boylan-Kolchin 1 , M. Dessauges-Zavadsky 19 , E. Egami 20 , S. L. Finkelstein 1 , Z. Ma 20 , I. Smail 21 , D. Watson 9 , 10 , T. A. Hutchison 22 , J. R. Rigby 22 , B. D. Welch 22 , 23 , 24 , Y. Ao 25 , 26 , L. D. Bradley 27 , G. B. Caminha 28 , K. I. Caputi 29 , D. Espada 30 , 31 , R. Endsley 1 , Y. Fudamoto 13 , J. González-López 32 , 33 , B. Hatsukade 4 , 6 , 34 , A. M. Koekemoer 26 , V. Kokorev 28 , N. Laporte 35 , M. Lee 9 , 36 , G. E. Magdis 9 , 10 , 36 , Y. Ono 3 , F. Rizzo 9 , 10 , T. Shibuya 37 , K. Shimasaku 6 , 7 , F. Sun 15 , S. Toft 9 , 10 , H. Umehata 38 , 39 , 40 , T. Wang 41 , 42 , and H. Yajima 43  \nEarly galaxy formation, initiated by the dark matter and gas assembly, evolves through frequent mergers and feedback processes into dynamically hot, chaotic structures 1 . In contrast, dynamically cold, smooth rotating disks have been observed in massive evolved galaxies merely 1.4 billion years after the Big Bang 2 , suggesting rapid morphological and dynamical evolution in the early Universe. Probing this evolution mechanism necessitates studies of young galaxies, yet efforts have been hindered by observational limitations in both sensitivity and spatial resolution. Here we report high-resolution observations of a strongly lensed and quintuply imaged, low-luminosity, young galaxy at z = 6 . 072 (dubbed the Cosmic Grapes ), 930 million years after the Big Bang. Magnified by gravitational lensing, the galaxy is resolved into at least 15 individual star-forming clumps with effective radii of r e ≃ 10-60 parsec (pc), which dominate ≃ 70% of the galaxy's total flux. The cool gas emission unveils a smooth, underlying rotating disk characterized by a high rotational-to-random motion ratio and a gravitationally unstable state (Toomre Q ≃ 0.2-0.3), with high surface gas densities comparable to local dusty starbursts with ≃ 10 3 -5 solar mass ( M ⊙ ) per pc 2 . These gas properties suggest that the numerous star-forming clumps are formed through disk instabilities with weak feedback effects. The clumpiness of the Cosmic Grapes significantly exceeds that of galaxies at later epochs and the predictions from current simulations for early galaxies. Our findings shed new light on internal galaxy substructures and their relation to the underlying dynamics and feedback mechanisms at play during their early formation phases, potentially explaining the high abundance of bright galaxies observed in the early Universe 3 and the dark matter core-cusp problem 4 .  \nUsing the James Webb Space Telescope (JWST) with Near Infrared Camera (NIRCam), we obtained deep near-infrared (NIR) imaging over 1-5 µ m wavelengths of a gravitationally-lensed star-forming galaxy, the Cosmic Grapes at z = 6 . 072 . The Cosmic Grapes and the arc were initially discovered as multiply lensed images via the bright [C II] 158 µ m emission lines in the Atacama Large Millimeter Array (ALMA) Lensing Cluster Survey behind the massive galaxy cluster RXCJ0600-2007 5, 6 . A total of five multiple images have been spectroscopically confirmed, which provides stringent constraints from their sky positions and morphology, resulting in a wellconstrained magnification estimate of µ = 32 +0 . 7 -6 . 8 for the Cosmic Grapes , even in this high magni-  \nb)  \nFigure 1: HST and NIRCam near-infrared observed images of Cosmic Grapes without lens correction. (a): HST/F160W image ( 4 '' × 4 '' ) around the Cosmic Grapes , a strongly lensed ( µ = 32) low-luminosity, young galaxy at z = 6 . 072 . b: NIRCam/F150W image ( 4 '' × 4 '' ) showing the same region as a . JWST is able to resolve a single disk-like galaxy into numerous star-forming clumps due to improved spatial resolution. The green circles at bottom right in panels a and b indicate the PSFs of the HST/F160W and NIRCam/F150W images. (c): A zoomed-in view of the galaxy, highlighting 15 identified star-forming clumps (see Methods ), as outlined in white. The right top and bottom panels denote the best-fit Sérsic models for the clumps obtained using GALFIT (see Methods ) and the residual map, respectively.  \n<!-- image -->  \nfication regime (see Methods ; Extended Data Fig. 1). The previous NIR image taken by the Hubble Space Telescope (HST) shows a disk-like galaxy with a circularized intrinsic effective radius of 0 . 68 +0 . 09 -0 . 01 kpc 6 ( 0 . '' 14 ) and absolute ultra-violet (UV) magnitude of -19 . 29 +0 . 02 -0 . 26 with the above µ estimate. Our spectral energy distribution (SED) analysis, using the new NIRCam filters 7 , infers a star-formation rate of SFR = 2 . 6 +1 . 7 -1 . 5 M ⊙ yr -1 and stellar mass of M ⋆ = 4 . 5 +2 . 7 -1 . 1 × 10 8 M ⊙ after lens correction (see Methods ; Extended Data Fig. 2). These SFR and size values are consistent with typical galaxies of similar stellar mass at z ∼ 6 8, 9 ; based on dark-matter halo and stellar mass evolution tracks predicted in cosmological simulations 10 , galaxies like the Cosmic Grapes may represent the progenitor of the Milky Way at z = 6 .  \nOur deep NIRCam F150W-filter image resolves the single-disk-like galaxy into numerous individual star-forming clumps (Fig. 1). These clumps remain visible at longer wavelengths (even at lower spatial resolution), and a modest dust reddening of E ( B -V ) = 0 . 03 ± 0 . 01 is measured in spectroscopic follow-up (see Methods ). These results indicate that the distinct clumps are real and not due to highly inhomogeneous dust obscuration effects. Our source extraction detects at least 15 star-forming clumps with the current sensitivity and spatial resolution of F150W. We apply simultaneous Sérsic profile fitting to the 15 individual star-forming clumps, obtaining r e values of ≃ 10-60 pc after lens correction and find that these clumps dominate ≃ 70% of galaxy's total flux in F150W. From a pixel-by-pixel based SED analysis 7, 11 , we also estimate the SFR and M ⋆ values for the individual star-forming clumps to be ≃ 0.02-0.8 M ⊙ yr -1 and log( M ⋆ /M ⊙ ) ≃ 6.3-8.0 M ⊙ , with stellar ages of 1-140 million years (Myr) (see Methods ). These properties suggest that the individual star-forming clumps have similar size and M ⋆ relations as local young massive clusters (YMCs), while exhibiting elevated SFR surface densities compared to clumps identified in lower-  \nHST/F160W  \nNIRCam/F150W  \nredshift galaxies (Extended Data Fig. 6) 12 . The elevated surface density of SFR (or M ⋆ ) among clumps inside galaxies is consistent with recent JWST/NIRCam results for lensed arc systems at z ≳ 6 13,14 . In previous studies, however, effective areas after lens correction are inevitably too small due to their extremely high magnifications in the arcs, making connections from the host galaxy, the small internal substructures, to their underlying dynamics difficult to uncover. Uniquely, the Cosmic Grapes offers the first opportunity to investigate such connections, owing to its strong µ yet minimal distortion and differential magnification.  \nIn the left panel of Fig. 2, we show the source-plane reconstructed (i.e., lens-corrected) map in F150W. Owing to the strong magnification and the superb spatial resolution of NIRCam in F150W with the Full-width-half-maximum (FWHM) of the point spread function (PSF) being 0 . '' 05 (280 pc) in the image plane, our data effectively achieves the intrinsic spatial resolution of ≃ 0 . '' 01 (58 pc) in the source plane. To reveal how this galaxy appears without lensing magnification, the right panel of Fig. 2 shows a smoothed F150W map in the source plane, which convolves the existing resolution with a Gaussian kernel to downgrade the source-plane spatial resolution from 0 . '' 01 to 0 . '' 05 ; the individual clumps disappear in the smoothed map. Since the Cosmic Grapes represents a typical main-sequence galaxy at z = 6 (Extended Data Fig. 4), this comparison indicates that structures with numerous clumps may be ubiquitous among early galaxies, and have been overlooked even in recent NIRCam observations of z ≳ 6 field galaxies due to its nominal ∼ 0 . '' 05 (280 pc) spatial resolution limit.  \nA unique ensemble of high-resolution IFU observations with JWST Near Infrared Spectrograph (NIRSpec) and ALMA have also been carried out on the Cosmic Grapes . Fig. 3 summarizes the line intensity, velocity, and dispersion maps for the bright emission lines of [C II]158 µ m, H α , and [O III] λ 5008 reconstructed in the source plane. The velocity maps show a smooth velocity gradient from Northeast to Southwest in all emission lines, mostly consistent with the major axis in the galaxy morphology observed in NIRCam. Our high-resolution 3D kinematic analysis shows that the Cosmic Grapes is a rotation-supported system with a symmetric kinematic profile exhibiting a high rotational-to-random motion ratio of 2 . 89 ± 0 . 23 (Middle panel of Fig 3). These kinematic properties indicate that the numerous star-forming clumps in the Cosmic Grapes are not the result of ongoing merging components but rather are formed through disk-related star-forming activities within the galaxy. The oxygen and nitrogen abundances, measured with the NIRSpec IFU data, are in excellent agreement with local H II regions (Extended Data Fig. 4), which also supports that these clumps are formed through typical star-forming activity within galaxies.  \nWe compute the local Toomre Q -parameter pixel-by-pixel, which expresses the balance between the self-gravity of molecular gas and turbulent pressure by stellar radiation and other sources. We use the [C II] line luminosity for the molecular gas estimate 16,17 , which is confirmed to be consistent with the dynamical mass after subtracting the stellar component in this system 6 . The Q -parameter has critical values of 0.67 and 1.0 for a thick and thin disk, respectively 18 , where the higher values correspond to a gravitationally stable disk. Our local Q measurements are typically ≲ 0.3 over almost the entire disk with general associations with the clump positions (Inset  \nNIRCam+Lensing (Resolution~0. '' 01)  \nNIRCam alone (Resolution~0. '' 05)  \n<!-- image -->  \nFigure 2: Comparison of the views into a typical early galaxy with and without the lensing support. (a): A source plane reconstructed (i.e., lens-corrected) F150W map of the Cosmic Grapes . The high magnification with weak distortion uniquely preserves the global-scale intrinsic galaxy morphology with an effective spatial resolution of ∼ 0 . '' 01 (58 pc) in the source plane. (b): The same map as (a) , smoothed with a Gaussian kernel to downgrade the spatial resolution to ∼ 0 . '' 05 (280 pc), which is comparable to the nominal NIRCam/F150W's resolution without the lensing effect. The morphology appears to be a single, smooth disk-like galaxy. Given the Cosmic Grapes represents a low-mass main-sequence galaxy at z = 6 (Extended Data Fig. 4), many recent HST- and NIRCam-observed early galaxies with similar single-disklike morphologies 15 may in fact also consist of numerous clumps.  \n<!-- image -->  \nin Fig. 3 right). We also evaluate the radially-averaged Q -parameter using the best-fit kinematic parameters that may correct the beam smearing and inclination effects, obtaining similarly low values of ≃ 0 . 2 -0.3. These results imply that gravitational instabilities in the disk indeed induce star formation, leading to the formation of numerous clumps, regardless of the thick or thin disk interpretation. Similarly low Q values have been measured in high gas-density star-forming clumps in the disks of star-forming galaxies at later epochs, while they exhibit higher Q values ( ≈ gravitationally stable) toward the galactic center 19,20 . The low Q values across the entire galaxy in the Cosmic Grapes suggest that the galaxy is dominated by high gas-density star-forming clumps without the presence of a massive bulge. This is consistent with the presence of numerous compact star-forming clumps in NIRCam, where the central regions are dominated by young stellar populations (age < 10 Myr) (Extended Data Fig. 2).  \nWe quantify the clumpiness of the Cosmic Grapes using the non-parametric clumpiness parameter S 22 (see Methods ). We obtain S = 0 . 81 , which is much higher than average values of ≃ 0.1-0.4 measured in local Spirals and irregular dwarfs 22 . We also evaluate the clumpiness of the Cosmic Grapes via the clump luminosity function (LF) in a cumulative format as a function of SFR ( ¯ N clump ) in Fig. 4, together with previous measurements for lensed galaxies at z ∼ 1-3 that have the intrinsic spatial resolution similar to our measurement (see Methods ) 12,25 . While an increasing  \n[CII] 158μm  \nHα  \nFigure 3: Kinematic properties of the Cosmic Grapes measured by high-resolution IFU observations of ALMA and JWST/NIRSpec. (a): Source-plane reconstructed (i.e., lens-corrected) maps of the line intensity (left), velocity (middle), and dispersion (right) for the [C II] 158 µ m, H α , and [O III] λ 5008 lines from top to bottom. The gray ellipse indicates the effective PSF in the source plane. (b): Radial rotation velocity V ( R ) (top) and velocity dispersion σ ( R ) (bottom) measured using 3DBarolo (see Methods ). The red, blue, and green circles and shades indicate the best-fit measurements and 1 σ uncertainties for [C II], H α , and [O III] lines, respectively. Systematically higher σ ( R ) values observed in the H α and [O III] lines, compared to the [C II] line, could be attributed to ionized gas outflows 21 or the limited spectral resolution of NIRSpec ( ≃ 100 km/s). We thus use the [C II] line results to determine an average velocity dispersion σ 0 , while measuring the maximum rotation velocity ( V max ) for each line, and infer V max /σ 0 = 2 . 89 ± 0 . 23 on average. The inset labels indicate the average V max from these three lines and the derived σ 0 . (c): Radially averaged Toomre Q parameter derived from our kinematic modeling results, while the inset panel displaying a local 2-D Q parameter map obtained from the observed [C II] data. Cyan contours from the NIRCam/F150W map are overlaid to guide the clump positions. The vertical bar denotes a possible uncertainty using different conversions between [C II] luminosity and M gas (see Methods ). The grey-shaded area highlights the critical Toomre Q thresholds: 1.0 for thin disks and 0.67 for thick disks, below which the gas becomes gravitationally unstable. The low Q values observed both globally and locally at the clump positions suggest that disk instabilities are the driving force behind numerous clump formations.  \n<!-- image -->  \ntrend of clumpiness has been reported in previous studies from z = 0 to z ∼ 3 12,25 , our results show that this trend continues out to z = 6 at least, with the Cosmic Grapes being consistently a factor of ≳ 2 higher at all SFRs compared to lower-redshift results.  \nTo further investigate the observed clumpiness, we also evaluate the S parameter and the clump LF for galaxies in the state-of-the-art cosmological zoom-in simulations of FIRE 24 and SERRA 23 . We select simulated galaxies at z = 6-8 with physical properties (SFR, M star ) similar to the Cosmic Grapes , generate image cutouts with similar spatial resolution and sensitivity to our F150W data, and evaluate the S parameter and the clump LF in the same manner (see Methods ). We find that these simulated galaxies have lower S values and lower clump LFs compared to the Cosmic Grapes (Fig. 4). SERRA galaxies reproduce smooth-rotating disks but generally only with  \n<!-- image -->  \nFigure 4: Comparison of clumpiness in observed and simulated galaxies. (a): Clumpiness parameter ( S ) 22 . The red line denotes the observed value in the Cosmic Grapes . The blue and grey dashed curves indicate the probability distribution functions (PDFs) drawn from the same measurements for 140 SERRA 23 and 13 FIRE 24 simulated galaxies in their cosmological zoom-in models at z = 6-8, respectively. The PDFs are smoothed with a Gaussian kernel. (b): Cumulative clump luminosity function (LF) as a function of SFR. The red circles represent the measurements of the Cosmic Grapes . The green circles denote lensed galaxies with similar magnifications, SFR = 1 -10 M ⊙ yr -1 at z ∼ 1 -3, and the black and green curves are the best-fit functions for z ∼ 0 and z ∼ 1-3, respectively, from the literature 12,25 . The blue and grey shaded regions represent measurements in the same manner for the simulated galaxies of SERRA and FIRE, respectively. All error bars are calculated assuming Poisson uncertainties. For fair comparisons, we use simulated galaxies whose physical properties (SFR, M ⋆ ) are similar to those of the Cosmic Grapes in both S and clump LF measurements (see Methods ).  \n<!-- image -->  \na few stellar clumps; FIRE galaxies generally have higher clumpiness owing to more frequent starbursts implemented in the model but show chaotic gas motions with no rotating gas disk due to the subsequent feedback effects from the frequent starbursts. These discrepancies highlight the challenges of reproducing the observed clumpy disk without resulting in a system dominated by random motions. Note that the formation of small star-forming clumps is also regulated by the spatial and time resolutions in the simulations 26 . This gap between observations and simulations might suggest that we are reaching a critical resolution limit to compare the substructures inside early galaxies and the zoom-in simulations.  \nOur finding may shed new light on several open questions. Recent JWST studies show the high abundance of bright galaxies at z ≳ 9 , exceeding the theoretical predictions made preJWST 27,28 . It has been suggested that these early galaxies exhibit a high surface gas density ( Σ gas ), leading to ineffective feedback mechanisms and, consequently, a high efficiency of star formation ( ϵ ) 27,28 . This weak feedback scenario also reconciles the presence of the rotating gas disk and the frequent bursts to generate numerous clumps, offering a plausible solution for the current gap  \nbetween observations and simulations described above (Fig. 4a). The bright clumps in the Cosmic Grapes indeed show high surface densities reaching Σ gas ≃ 10 3 -5 M ⊙ pc -2 (Extended Data Fig. 6), where radiation hydrodynamical simulations suggest ϵ may increase out to > 0 . 6 -0 . 9 . 29 The bright galaxies observed at z ≳ 9 may also consist of clumps with similarly high values of Σ gas and ϵ with weak feedback. The numerous star-forming clumps could also be key to the dark matter cuspcore problem. Dynamical friction from the numerous star-forming clumps may provide sufficient energy to heat the central dark matter component, potentially creating a density core in the dark matter distribution 4 . 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ApJ , 303 , 336-346, apr (1986).  \nAcknowledgements We thank Jiyai Sun, Filippo Fraternali, and Amina Helmi for discussions on our target properties based on the comparison from systems in the local Universe; Takashi Kojima for helpful inputs for the optical emission line analyses; John Silverman for engaging discussions regarding the potential impacts of clumps on the dark matter distribution; and researchers at Cosmic Frontier Center for valuable feedback on interpretations for the numerous clumps and the gas dynamics observed in our target. This work is based on the observations of JWST (program ID: 1567), ALMA (program ID: 2021.1.00055.S; 2021.1.00247.S; 2021.1.00181.S; 2022.1.00195.S), and MUSE (program ID: 0103.A-0871(B) and 198.A-2008(E)). We acknowledge support from: the Danish National Research Foundation under grant DNRF140; the NASA Hubble Fellowship grant HST-HF2-51505.001-A awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555; JSPS KAKENHI Grant Numbers JP22K21349, JP20H05856, JP22H01260, JP17H06130, JP22H04939, JP23K20035; the NAOJ ALMA Scientific Research  \nGrant Number 2017-06B; ANID grants for the Millennium Science Initiative Program #ICN12\\_009 (FEB), CATA-BASAL #FB210003 (FEB), and FONDECYT Regular #1200495 (FEB); STFC (ST/X001075/1); Grant No. 2020750 from the United States-Israel Binational Science Foundation (BSF) and Grant No. 2109066 from the United States National Science Foundation (NSF); by the Ministry of Science & Technology, Israel; and by the Israel Science Foundation Grant No. 864/23; the National Natural Science Foundation of China (12173089); NSF CAREER award AST-1752913, NSF grants AST-1910346 and AST-2108962, NASA grant 80NSSC22K0827, and HST-GO-15658, HST-GO-15901, HST-AR-16159, HST-GO-16686, HST-AR-17028, and HSTAR-17043 from STScI; the European Union (ERC, HEAVYMETAL, 101071865); the Netherlands Research School for Astronomy (NOVA) and the Dutch Research Council (NWO) through the award of the Vici Grant VI.C.212.036. Views and opinions expressed are, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them.  \nAuthor contributions Y.A., F.E.B., L.D.B., G.B.B, G.B.C., K.I.C., M.D., D.E., J.G., B.H., E.E., A.M.K, K.K, M.O., N.L. M.L., G.E.M., M.O., M.O., J.R., K.S., I.S., F.S., H.U., F.V., A.Z., and S.F. discussed and planned the follow-up observing strategy of the Cosmic Grapes and its multiple images, writing the telescope proposals. G.B. reduced the JWST/NIRCam images. S.F. reduced the JWST/NIRSpec IFU and ALMA data, and Z.M. and E.E. also reduced the JWST/NIRSpec IFU data independently to cross-check our results. T.H., B.W., and G.R. supported reducing the JWST/NIRSpec data. J.R. reduced the MUSE data and identified the emission lines, generating the spectroscopic sample in the target field. C.G.A. performed the pixel-by-pixel based SED fitting using the NIRCam data and produced the SED output maps. F.V. conducted the far-infrared SED analysis using the constraints from ALMA and Hershel/SPIRE. S.F. and F.R. carried out the kinematic modeling using 3DBarolo . L.J.F. and A.Z. constructed the updated lens model, and M.O., J.R., and G.B.C. supported it. M.K. and A.P. produced image cutouts for the simulated galaxies in the cosmological zoom-in simulation SERRA. S.F. and M.B. producing image cutouts for the simulated galaxies in the cosmological zoom-in simulation FIRE using public resources. All authors discussed the results and commented on the manuscript. S.F. led the team, being the Principal Investigator of the follow-up JWST, ALMA, and MUSE programs, wrote the main text and the Methods section, and produced all figures and tables.  \nCompeting interests The authors declare no competing interests.  \nCorresponding Author Seiji Fujimoto (fujimoto@utexas.edu)", 'Affiliations': "- 1 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712, USA\n- 2 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan\n- 3 Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan  \n- 4 Department of Astronomical Science, SOKENDAI (The Graduate University for Advanced Studies), 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan\n- 5 Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa, Chiba 277-8583, Japan\n- 6 Institute of Astronomy, Graduate School of Science, The University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan\n- 7 Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan\n- 8 European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching, Germany\n- 9 Cosmic Dawn Center (DAWN), Denmark\n- 10 Niels Bohr Institute, University of Copenhagen, Jagtvej 128, 2200, Copenhagen N, Denmark\n- 11 Department of Physics, Ben-Gurion University of the Negev, P.O. Box 653, Beer-Sheva 8410501, Israel\n- 12 Scuola Normale Superiore, Piazza dei Cavalieri 7, I-56126 Pisa, Italy\n- 13 Center for Frontier Science, Chiba University, 1-33 Yayoi-cho, Inage-ku, Chiba 263-8522, Japan\n- 14 Department of Physics, Graduate School of Science, Chiba University, 1-33 Yayoi-Cho, InageKu, Chiba 263-8522, Japan\n- 15 Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230, Saint-Genis-Laval, France\n- 16 Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Campus San Joaquín, Av. Vicuña Mackenna 4860, Macul Santiago, Chile, 7820436\n- 17 Millennium Institute of Astrophysics, Nuncio Monseñor Sótero Sanz 100, Of 104, Providencia, Santiago, Chile\n- 18 Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, Colorado 80301\n- 19 Département d'Astronomie, Université de Genève, Chemin Pegasi 51, 1290 Versoix, Switzerland\n- 20 Steward Observatory, University of Arizona, 933 N. Cherry Ave, Tucson, AZ 85721, USA\n- 21 Centre for Extragalactic Astronomy, Department of Physics, Durham University, South Road, Durham DH1 3LE, UK\n- 22 Astrophysics Science Division, NASA Goddard Space Flight Center, 8800 Greenbelt Rd, Greenbelt, MD 20771, USA\n- 17 Department of Astronomy, University of Maryland, College Park, MD 20742, USA\n- 18 Center for Research and Exploration in Space Science and Technology, NASA/GSFC, Greenbelt, MD 20771 USA\n- 25 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, Jiangsu 210023, People's Republic of China\n- 26 School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei, Anhui 230026, People's Republic of China\n- 27 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21102, USA\n- 28 Max-Planck-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany\n- 29 Kapteyn Astronomical Institute, University of Groningen, P. O. Box 800, 9700AV Groningen,", 'The Netherlands': "- 30 Departamento de Física Teórica y del Cosmos, Campus de Fuentenueva, Edificio Mecenas, Universidad de Granada, E-18071, Granada, Spain\n- 31 Instituto Carlos I de Física Teórica y Computacional, Facultad de Ciencias, E-18071, Granada, Spain\n- 31 Núcleo de Astronomía de la Facultad de Ingeniería y Ciencias, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile\n- 32\n- Las Campanas Observatory, Carnegie Institution of Washington, Casilla 601, La Serena, Chile 34 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan\n- 35 Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d'Astrophysique de Marseille), UMR7326, 13388 Marseille, France\n- 36 37\n- DTU-Space, Technical University of Denmark, Elektrovej 327, 2800, Kgs. Lyngby, Denmark\n- Kitami Institute of Technology, 165, Koen-cho, Kitami, Hokkaido 090-8507, Japan\n- 38 Institute for Advanced Research, Nagoya University, Furocho, Chikusa, Nagoya 464-8602, Japan\n- 39 Department of Physics, Graduate School of Science, Nagoya University, Furocho, Chikusa, Nagoya 464-8602, Japan\n- 40 Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MS249-17, Pasadena, CA91125, USA\n- 41 School of Astronomy and Space Science, Nanjing University, Nanjing, Jiangsu 210093, China\n- 42 Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing 210093, China\n- 43 Center for Computational Sciences, University of Tsukuba, Ten-nodai, 1-1-1 Tsukuba, Ibaraki 305-8577, Japan", 'Methods': "In this paper, error values represent the 1 σ uncertainty, where σ denotes the root-mean-square or standard deviation; upper limits are indicated at the 3 σ level; error values for intrinsic physical properties after the lens correction are obtained by propagating the 1 σ uncertainties of the magnification estimate and the measurement of the physical properties; red symbols in figures denote the Cosmic Grapes , unless otherwise specified. Poisson uncertainty is calculated based on the values presented in Gehrels (1986) 30 . We adopt cosmological parameters measured by the Planck mission 31 , i.e. a Λ cold dark matter ( Λ CDM) model with total matter, vacuum and baryonic densities in units of the critical density, Ω Λ = 0.692, Ω m = 0.308, Ω b = 0.0481, and Hubble constant, H 0 = 100 h km s -1 Mpc -1 , with h = 0 . 678 . Based on these parameters, we adopt the angular size distance of 5.80 kpc/arcsec at the source redshift of z = 6 . 072 in this paper.  \nDec.  \nExtended Data Figure 1: NIRCam and ALMA overviews of the cluster RXCJ0600-2007 and the quintuply lensed images of the Cosmic Grapes at z = 6 . 072 . (a): NIRCam false-color (R: F444W, G: F356W, B: F277W) image. The yellow curves represent the critical lines at z = 6 . 072 . The white dashed circles denote the FoVs of the ALMA follow-up observations. The inset panels show the zoom-in NIRCam false-color images for the multiple images of ID1,2 and the rest in 8 '' × 8 '' and 4 '' × 4 '' scales, respectively. The white contours indicate 3 σ , 4 σ , 5 σ , 10 σ , and 20 σ levels of the [C II] line intensity. (b): Follow-up ALMA Band 6 spectra of [C II] for all multiple images. Black vertical lines indicate the observed [C II] frequency at z = 6 . 072 . Although the [C II] line detected in z 6 \\_ 1 , 2 (arc) is slightly redshifted ( ∼ 90 km s -1 ), this is consistent with the interpretation that z 6 \\_ 1 , 2 (arc) traces the outskirt region of the galaxy where it crosses the caustic line in the source plane 6 .  \n<!-- image -->  \n- 1. Target - A quintuply lensed galaxy the Cosmic Grapes at z = 6 . 072 : The Cosmic Grapes was initially discovered in the RXCJ0600-2007 field 33 as a part of the ALMA Lensing Cluster Survey (ALCS), an ALMA Large Program in Cycle 6 (#2018.1.00035.L, PI: K. Kohno) studying 33 massive lensing clusters observed in the HST treasury programs of RELICS 34 , CLASH 35 , and HFF 36 . In the RXCJ0600-2007 field, two bright emission lines were identified at the same frequency of ∼ 268.7 GHz, exactly at the positions of two Lyman-break galaxies (LBGs) at z ∼ 6 , whose redshifts were confirmed in follow-up Gemini GMOS spectroscopy 5 . This determined the bright lines to be [C II] 158 µ mat z = 6 . 072 . 6 Three independent lens models (Glafic 38 , Lenstool 39 , and Light-Traces-Mass 40 ) consistently suggest that these two [C II] emitters are multiple images of an intrinsically faint, subL ⋆ LBG. These models also predict the presence of two additional multiple images, and the spectroscopic confirmation for the other two multiple images has been achieved in recent ALMA follow-up observations (Section 3). The extended arc structure consists of a pair of two multiple images, and thus a total of five multiple images have been spectroscopically confirmed, referred to as z 6 \\_ 1 , z 6 \\_ 2 , z 6 \\_ 3 , z 6 \\_ 4 , and z 6 \\_ 5 , respectively 6 . In this paper, we focus on the results obtained from z 6 \\_ 3 , dubbed 'the Cosmic Grapes ', while results from the other multiple images will be presented in a separate paper 41 . The sky positions, morphology, and flux ratios among the five multiple images provide stringent constraints on the lens model, which makes the magnification estimate for these sources robust even in the high magnification regime 42 (Section 4). Extended Data Fig. 1 shows the sky positions of all these multiple images.  \nIn the source plane, the outskirt of the background galaxy crosses the caustic and is lensed into the long ( ∼ 6 '' ) arc, corresponding to z 6 \\_ 1 , 2 (arc), with local magnifications of > 100, while the Cosmic Grapes represents a less sheared image of the galaxy on the global scale with a still high magnification of 32 +0 . 7 -6 . 8 (see Figure 4 in Fujimoto et al. 2021 6 ). In contrast to z 6 \\_ 1 , 2 (arc) showing significant distortion tracing a local region, the entire galaxy is magnified with minimal distortion in the Cosmic Grapes , which is an optimal target for this paper to study the galaxy morphology and internal structure.  \n- 2. NIRCam Observations: The massive galaxy cluster RXCJ0600-2007 was observed with JWST/NIRCam as a part of JWST GO cycle 1 program (#1567, PI: S. Fujimoto) in January 2023. The center and position angle of the NIRCam field-of-view (FoV) were optimized to include all five multiple images of the background LBG at z = 6 . 072 and several unique high-redshift sources that were identified in previous HST and ALMA observations 43 . The NIRCam images were taken in five bands: F115W, F150W, F277W, F356W, and F444W with the exposure times of 1890 sec, 4982 sec, 1890 sec, 2491 sec, and 2491 sec, respectively. We adopted the standard subpixel ( N = 3 ) dithering.  \nWe reduced and calibrated the NIRCam data, following the procedure described in the DAWN JWST Archive (DJA) 1 (see also Valentino et al. 44 for the photometry procedure), and here we briefly explain the reduction and calibration procedure. The JWST pipeline calibrated level-2 NIRCam imaging products were retrieved and processed with the grizli pipeline 45,46 . The NIRCam photometric zero-point correction was applied with the Calibration Reference Data  \nExtended Data Figure 2: NIRCam cutouts and spatially-resolved SED fitting outputs for the Cosmic Grapes . Top: NIRCam cutouts ( 2 . '' 6 × 2 . '' 6 ) in the observed frame (i.e., no lens correction). The cyan circles at the bottom right denote the PSF in each filter. The structure remains clumpy in the LW filters (F277W, F356W, F444W), suggesting it is not caused just by patchy dust obscuration. Bottom: NIRCam false-color image and the pixel-by-pixel SED fitting 11 (see Methods ) outputs from left to right, showing the centrally located clumps of young stellar populations ( < 10 Myr), surrounded by an extended region of older stellar populations.  \n<!-- image -->  \nSystem (CRDS) context jwst\\_1039.pmap , including detector variations 2 . The fully-calibrated images in each filter were aligned with the GAIA DR3 catalog 47 , co-added, and drizzled at 20 mas and 40 mas pixel scales for the short-wavelength (SW: F150W, F200W) and long-wavelength (LW: F277W, F356W, F444W) NIRCam bands, respectively. In Extended Data Fig. 1, we show a NIRCam RGB color image for the RXCJ0600-2007 field, and zoom-in cutout RGB images for all the multiple images. We also present the NIRCam cutouts around the Cosmic Grapes in Extended Data Fig. 2.  \n3. ALMA Observations: Follow-up ALMA Band 6 observations were carried out on the five multiple images in RXCJ0600-2007 from January to August 2022 as a part of Cycle 8 program (#2021.1.00055.S, PI: S. Fujimoto), targeting their [C II] 158µ memission line. Because the [C II] line was detected from the brightest multiple images of z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes in the previous ALCS data cube with relatively short exposure, these follow-up observations aimed to perform deep, high-resolution [C II] line spectroscopy to probe the internal structures and kinematics. The configurations of C43-2 and C43-5 were used, with the on-source integration times of 49.4 mins and 107.8 mins, respectively, for z 6 \\_ 1 , 2 (arc) and z 6 \\_ 2 . Note that the [C II] line was not clearly detected in the other two multiple images of z 6 \\_ 4 and z 6 \\_ 5 in the previous ALCS  \ndata cube, and thus, additional follow-up observations for z 6 \\_ 4 and z 6 \\_ 5 were also designed to detect the [C II] line to obtain the spectroscopic confirmations of these multiple images. The C43-2 configuration was used, with the on-source integration time of 12.6 mins for each.  \nWe reduced and calibrated the ALMA data with the Common Astronomy Software Applications package CASA version 6.4.1.12 49 , using the pipeline script in the standard manner. We imaged the calibrated visibilities with a pixel scale of 0 . '' 05 . For z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes , we adopt Briggs weighting with a robust parameter of 0 . 5 to maximize the balance between sensitivity and spatial resolution. For z 6 \\_ 4 and z 6 \\_ 5 , we adopt natural weighting to maximize the sensitivity for a detection experiment. We adopted a common spectral channel bin of 20 km s -1 for the deep data of z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes and 60 km s -1 for z 6 \\_ 4 and z 6 \\_ 5 and applied the tclean routines down to the 2 σ level with a maximum iteration number of 100,000 in the automask mode. The continuum subtraction was applied to the visibility by performing a power-law fit with the line-detected channels masked. The generated cubes achieved full-widthhalf-maximum (FWHM) sizes of the synthesized beam of 0 . '' 28 × 0 . '' 25 ( 0 . '' 80 × 0 . '' 65 ) with 1 σ line sensitivities in a 20-km s -1 (60-km s -1 ) width channel of 0.17 mJy beam -1 (0.18 mJy beam -1 ) for the z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes ( z 6 \\_ 4 and z 6 \\_ 5 ) data. For a high-resolution experiment to study the potential differential distribution of dust, we also generate a high-resolution dust continuum map with Briggs weighting and a robust parameter of 0 . 5 , only using the C43-5 configuration data. This map shows the beam size of 0 . '' 25 × 0 . 21 with 1 σ sensitivity of 12 µ Jy beam -1 .  \n3. NIRSpec IFU Observations: Follow-up JWST/NIRSpec IFU observations were also performed for the brightest multiple images of z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes from September to December 2022, under the same GO program (#1567, PI: S. Fujimoto) as the NIRCam observations (Section 1). We adopted a 4-point dither with the off-scene nod for both z 6 \\_ 1 , 2 (arc) and the Cosmic Grapes in order to probe for potential extended emission. We used the grating/filter setup G395H/F290LP, whose wavelengths cover the rest-frame wavelength from ∼ 4000 to ∼ 7300 for our targets, and thus include key optical emission lines such as H α and [O III] λ 5008. The onsource integration is 3.2 hrs for each target. Because of the scope of this paper, here we present observations on the Cosmic Grapes , while the other observations are presented elsewhere 41 .  \nWe reduced the NIRSpec/IFU raw data using the STScI pipeline (version 1.12.5) with the CRDScontext jwst\\_1039.pmap , following the procedure developed by the ERS TEMPLATES team (PI: Rigby, Co-PI: Vieira; PID 01355; Rigby et al. 50 ). A detailed description is provided in Rigby et al. 50 (also described in 51,52 ) with associated data reduction code publicly available 3 . Here, we briefly explain the reduction and calibration procedure. We processed the raw data through the general three stages with default parameters and added the following steps. After Stage 1, we also applied the NSClean package 53 to the Level1 products, which mitigates the systematic vertical pattern noise and snowballs. We confirmed that the remaining vertical pattern noise and snowballs are less in the products processed with NSClean . In Stage 2, we found that the pipeline background subtraction did not work properly due to the different pixel units between the on-source and background data, and thus, we did not apply it inside the pipeline. Instead, we generated the  \nExtended Data Figure 3: NIRSpec G395H/F290LP 1D spectrum of the Cosmic Grapes . The spectrum is extracted from the IFU data cube with a 0 . '' 7 -radius aperture. The emission lines detected at > 5 σ and consistent with the [C II] line redshift are highlighted with the label.  \n<!-- image -->  \nreduced on-source and background data cubes based on the same procedure, calculated the median count in each channel in the background cube, and performed the subtraction in all channels after all steps. We also confirmed that our background estimate in our target field from the background data is consistent with the JWST background tool prediction within ∼ 5-20% over the 2.8-5.3 µ m range. In Stage 3, although several previous NIRSpec IFU studies 54-56 have reported that this step can lead to false outlier detections corresponding to bright sources in dithered exposures, we find that spurious outlier detections do not occur in our data, likely because our targets are much fainter than those in previous studies such as the luminous quasars 57 . We thus ran the outlier detection step with the default parameters. After completing these procedures, we obtain the final calibrated data cube with the default spatial scale of 0 . '' 1 for each spaxel. Note that we find in the data cube that the structures of the bright emission lines are always shifted by ∼ 0 . '' 1 systematically in the same direction. We speculate that this is due to an uncertainty of the astrometry and correct it by using the Southwest bright object as a reference, whose continuum is also detected within the IFU FoV. We also determine the PSF size of the NIRSpec IFU by analyzing a nearby bright object. By fitting a 2D Gaussian profile using GALFIT 58 to the NIRCam/F444W filter map, we measure an intrinsic source size of FWHM = 0 . '' 06 . From a continuum map generated by collapsing the NIRSpec IFU data cube channels between 3.5-4.5 µ m, we observe an FWHM size of 0 . '' 23 for this object. Consequently, we estimate the PSF size to be 0 . '' 22 , based on Gaussian convolution assumptions.  \nIn Extended Data Fig. 3, we show the 1D spectrum of NIRSpec IFU G395H/F290LP extracted with a 0 . '' 7 -radius aperture for the Cosmic Grapes . In addition to the bright optical emission lines of H α , [O III] λ 5008, and H β , further faint emission lines of H δ , H γ , [O III] λ 4363, HeI λ 5877, [N II], and [S II] are successfully detected at ≳ 5 σ that are all consistent with the redshift determined by the [C II] emission line. We measured the line fluxes by fitting a Gaussian profile with  \na fixed line center based on the source redshift. Several neighboring emission lines were fitted simultaneously by assuming their line widths were the same. We summarize our line flux measurements in Extended Data Table 2. While we show spatially-resolved H α /H β line measurements in Section 8, full spatially-resolved line analyses and results will be presented in a separate paper 41 ,  \n4. Lens model: Several lens models were previously constructed in RXCJ0600-2007 using the HST maps taken in the RELICS program 59 and an 0.8-hour VLT/MUSE IFU dataset (#0100.A0792, P.I.; A. Edge) 5, 6 . Since then, in addition to the JWST/NIRCam observations described above, a new 8.9 hour MUSE observation was obtained (#109.22VV.001, P.I.: S. Fujimoto). Furthermore, new Keck/DEIMOS and Gemini/GMOS observations have also been carried out to confirm the presence of additional massive cluster structures in the northeast, which was hinted at in the previous HST data. These data improve the identification of cluster member galaxies and the multiply lensed images in RXCJ0600-2007, and thus, we use an updated lens model in this study. The details of the new MUSE, DEIMOS, and GMOS data and the construction of the updated lens model are presented in separate papers 41,60 , while here we briefly describe the basic procedure of the lens model.  \nThe model used in this work was constructed using a revised version of the parametric strong lensing (SL) pipline by Zitrin et al. 40 , which was successfully used for modeling several clusters imaged with JWST 61,62 . The smooth dark matter (DM) component of the cluster was modeled by four pseudo-isothermal elliptical mass distributions 63 (PIEMDs). This approach effectively captures the elliptical symmetry and core structures of the DM halos. The individual cluster member galaxies were modeled using dual pseudo-isothermal ellipsoids 64 (dPIEs), accounting for the galaxy profiles' core and truncation radii. The SL model comprises a total of 504 cluster member galaxies, 67 of which have spectroscopic redshifts from the MUSE, DEIMOS or GMOS observations. The final SL model was constrained using a total of 91 multiple images and candidates, belonging to 35 distinct sources. Among these, 31 sources with a total of 83 images have spectroscopic redshifts, providing a robust basis for the lensing analysis. The model was then optimized through a series of Monte-Carlo Markov Chains (MCMCs) of several 10 4 steps in total. The final SL model of the cluster has an average lens plane image reproduction error of ∆ RMS = 0 . 72 '' which corresponds to reduced χ 2 ≃ 4 . 2 . In particular, the five images of the object studied in this work were exceptionally well reproduced with an average image reproduction error of ∆ RMS = 0 . 12 '' . The lens model and the discovery of the extended structures of MACS0600 will be published in Furtak et al. (in prep.) 60 .  \n5. SED analysis: Taking advantage of the superb sensitivity and spatial resolution of JWST/NIRCam, we conduct the SED fitting in a spatially-resolved manner, which reduces the so-called 'outshining' effect 65,66 due to UV-luminous young stellar populations formed in recent bursts 11 . Note that the PSF size is much worse in NIRSpec/IFU ( ∼ 0 . '' 22 ; Section 3) than those in NIRCam ( ∼ 0 . '' 04 -0 . '' 14 4 ), and thus we adopt the outputs from the spatially-resolved SED analyses for characterizing the basic physical properties (SFR, M ⋆ , age) of the Cosmic Grapes and clumps inside in this paper.  \nWe basically follow the pixel-by-pixel method presented in Giménez-Arteaga et al. (2023) 11 . The details of the method and the results are presented in Giménez-Arteaga et al. (2024) 7 , while here we briefly provide the analysis procedure. Again, we focus on ID3 in this paper to study the SED properties of the Cosmic Grapes from the global scale of the galaxy and the individual star-forming clumps inside, and the SED fitting results in the other multiple images are further presented in a separate paper 41 . Note that we do not include the ALMA measurements in the SED fitting in this study because of the lower-spatial resolution of that data (beam FWHM = 0 . '' 28 × 0 . '' 25 ) compared to NIRCam.  \nWe first matched PSFs in all NIRCam images to the one in F444W using the PSF models generated with WebbPSF 68,69 and Gaussian kernel. We then resized the PSF-matched images to a commonpixel scale of 40 mas per pixel. We use Agglomerative Clustering ( sklearn.cluster ) with a 'single' linkage method and a 1.5 distance threshold in the pixel selection for the SED fitting. After initial S/N > 1 thresholding in all bands and subsequent masking, a secondary threshold was applied based on the mean S/N per band. The final pixel selection was determined by combining these thresholds, resulting in 625 pixels satisfying the S/N criteria across all bands, ensuring a ∼ 2 σ detection minimum. The following analysis was performed only for these selected pixels.  \nWe ran the SED fitting code of BAGPIPES 70 on the photometry obtained in each selected pixel, fixing the redshift to z = 6 . 072 . The ionisation parameter was varied ( -3 < log 10 U < -1 ), incorporating nebular emission with CLOUDY 71 and stellar population synthesis (SPS) models by Bruzual & Charlot 72 . We assumed a Calzetti 73 attenuation curve and a constant star-formation history (SFH). We adhered to a 74 IMF, setting t bc = 10 Myr, and established uniform priors for A V ∈ [0 , 3] and log 10 ( M ∗ /M ⊙ ) ∈ [5 , 11] . A Gaussian prior centered at 0.1 solar metallicity Z ⊙ (with σ = 0 . 2 Z ⊙ ) was used for metallicity.  \nIn Extended Data Fig. 2, we show the SED outputs of stellar mass M ⋆ , star-formation rate (SFR) averaged over the past 100 Myr, and age of the stellar populations weighted by mass ( t age ). We find that young ( t age < 10 Myr) stellar populations are formed in the central regions surrounded by older stellar populations ( t age > 100 Myr). We confirm that predicted line fluxes and spatial distributions of H α and [O III] λ 5008 from our NIRCam-based SED fitting remain in excellent agreement with the observed values obtained from our NIRSpec IFU, assuring our SED results 7 . Adopting a pixel-by-pixel lens correction, we obtain the total M ⋆ and SFR values of 2 . 6 +1 . 7 -1 . 5 M ⊙ yr -1 and M ⋆ = 4 . 5 +2 . 7 -1 . 1 × 10 8 M ⊙ , respectively.  \n- 6. Global-scale galaxy properties of the Cosmic Grapes : In Extended Data Fig. 4, we show the global galaxy scale SFRM ⋆ relation of the Cosmic Grapes . We find that the Cosmic Grapes falls on the main sequence at z = 6 9 , indicating that the Cosmic Grapes represents a typical star-forming galaxy.  \nUsing the optical line fluxes measured with NIRSpec IFU, we further evaluate the Balmer decrement, electron density n e , oxygen abundance of 12+ log (O/H), nitrogen abundance of log (N/O), and BPT diagnostic for the Cosmic Grapes on the global galaxy scale. For the Balmer decrement,  \nExtended Data Figure 4: Global-scale physical properties of the Cosmic Grapes . Top: Relations of SFR, metallicity, and Balmer decrement as a function of M ⋆ , from left to right. The blue and black symbols, lines, and shades present the typical relations estimated in the literature 9, 76-78 . the Cosmic Grapes falls well within the scatter or 1 σ errors of these typical relations at similar redshifts. Bottom: Relations of N/O and O/H abundances, line ratio of the [SII] doublet ( ≈ electron density n e ) and Σ SFR , and the BPT diagram from left to right. The black and blue symbols denote the typical relations estimated in the literature 79-81 . The black dashed horizontal lines in the middle panel are obtained from the PyNeb package. The black curve in the right panel is the diagnostical line between star-forming and AGN populations, taken from the literature 82 the Cosmic Grapes falls in the regimes generally consistent within the scatter or the ∼ 1-2 σ errors of the previous measurements. These results suggest that the Cosmic Grapes represents a typical star-forming galaxy at z = 6 .  \n<!-- image -->  \nwe use H α /H β and obtain the line ratio of H α /H β = 3 . 33 ± 0 . 07 . Assuming an intrinsic ratio of 2.86 under the case B recombination 83 , we estimate a dust reddening of E ( B -V ) = 0 . 03 ± 0 . 01 . We apply the dust correction based on this E ( B -V ) value in the following analyses. For n e , we use the [S II] λλ 6718,6733 doublet. Based on the line ratio of [S II] λ 6718/[S II] λ 6733 = 1 . 22 ± 0 . 20 , we obtain n e = 260 +400 -230 using the nebular emission code of PyNeb 5 . For 12+ log (O/H), we use the direct electron temperature T e method with the auroral [O III] λ 4364 line. Based on the line ratio of [O III] λ 4363/[O III] λ 5008, we obtain T e of 14 , 100 ± 600 Kusing PyNeb . We then estimate the oxygen abundance, following the equations in Izotov et al. (2006) 84 , where we ignore oxygen ions of O 3+ due to their exceptionally high ionization potential (54.9 eV). Because our NIR-  \nExtended Data Figure 5: Comparison of metallicity measurements for the Cosmic Grapes with different calibrations . The red horizontal line indicates our fiducial estimate based on the T e method (see Methods ). The blue circles are estimated from the strong line methods based on calibrations in the literature 88 , showing the general consistency among the calibrations.  \n<!-- image -->  \nSpec G395H/F290LP data does not cover the wavelength of the [O II] λ 3727 line from the Cosmic Grapes , we infer the [O II] line flux from the tight correlation between R ( ≡ I [OIII] λ 4363 / I [OIII] λ 5008 ) and R 23 ( ≡ ( I [OII] λλ 3727 , 3729 + I [OIII] λ 4960 , 5008 ) / I H β ), calibrated in Pilyugin & Thuan (2005) 85 as log R = -4 . 264 + 3 . 087 log R 23 . Because auroral lines of [O II] λλ 7320,7330 are not observed in our data, we also assume t 2 = 0 . 7 t 3 +0 . 3 , 86,87 where t 3 = 10 -4 T e ([O III]) and t 2 = 10 -4 T e ([O II]). We obtain 12+ log (O/H) = 8 . 11 ± 0 . 03 . We confirm the general consistency between our T e -based measurement and those from other strong line methods with R3 ( ≡ I [OIII] λ 5008 / I H β ), N2 ( ≡ I [NII] λ 6585 / I H α ), O3N2 ( ≡ R3/N2), S2 ( ≡ I [SII] λλ 6718 , 6733 / I H α ), and O3S2 ( ≡ R3/S2) calibrated in the literature 88,89 (Extended Data Fig. 5). For log (N/O), we follow the equations in Izotov et al. (2006) 84 , assuming N/O ≃ N + /O + , as their ionization potentials are almost the same. Here, we use the [O II] line flux inferred above. We obtain log (N/O) = -1 . 46 ± 0 . 04 . We summarize these estimates in Extended Data Table 3.  \nIn Extended Data Fig. 4, we summarize the physical properties of the Cosmic Grapes evaluated on the global galaxy scale described above. For comparison, we also show previous measurements among high-redshift galaxies in the literature, including recent JWST results when available. We find that the chemical enrichment, dust attenuation, and nebular conditions (density, ionization state) in the Cosmic Grapes agree well with the typical relations measured in similarly high-redshift galaxies, indicating again that the Cosmic Grapes represents a typical star-forming galaxy at z = 6 . In the log (N/O)-12+ log (O/H) relation, the Cosmic Grapes is in excellent agreement with the measurements obtained in local H II regions. Although recent JWST studies report the presence of significantly nitrogen-abundant systems with log (N/O) ≳ -0 . 5 , hinting at their possible connection to Globular cluster and intermediate blackhole formations 90-93 , our results indicate that it is not the case in the Cosmic Grapes . In the BPT diagram, the Cosmic Grapes falls on the border between star-forming and AGN activities 82 . However, the location remains consistent within the 1-2 σ range with the recent JWST measurements for galaxies at similar redshifts 81 . Besides, the  \ndifficulty in using the BPT diagram to distinguish the star formation and AGN in metal-poor systems with the gas-phase metallicity of Z gas ≲ 0 . 2 Z ⊙ has been argued and become clear at z > 5 , 94 which is likely the case in the Cosmic Grapes . In the NIRSpec IFU spectrum, we find that the line profiles of the Balmer emission lines and [O III] λ 5008 are consistent. We thus conclude that the current data does not show any clear evidence of the presence of AGN.", 'SExtractor': "7. Properties of the individual star-forming clumps inside the Cosmic Grapes : Weuse version 2.25.0 101 to quantify the number of individual star-forming clumps that appear in the JWST/NIRCam maps (Extended Data Fig. 2). Here, we adopt the NIRCam/F150W map, which provides one of the highest spatial resolutions (PSF FWHM ≃ 0 . '' 05 ) and the best sensitivity owing to the longest exposure among our data. We run SExtractor using the default parameter values 6 , except for DETECT\\_MINAREA = 9, DETECT\\_THRESH = 2.0, DEBLEND\\_NTHRESH = 64, and DEBLEND\\_MINCONT = 0.0001 that are optimized to identify the small individual star-forming clumps separately. Fig. 1 shows the segmentation map obtained from the above parameter set, resulting in the identification of 15 individual star-forming clumps. Despite a different methodology adopted for clump identification, visual inspections already tell a stark difference from the number of clumps identified in lower redshift galaxies in recent JWST/NIRCam studies ( N < 5 ) 102 , which is likely because of a possible redshift evolution of the morphology 103 and the higher spatial resolution achieved in this study aided by the gravitational lensing effect. Given the remarkably low likelihood of capturing extraordinary phenomena through strong lensing twice, these numerous clumpy structures observed by the JWST, in conjunction with lensing effects, might be a common feature in early galaxies. In this paper, we regard N = 15 as the count of the individual star-forming clumps in the Cosmic Grapes , while this number could be increased with further high-resolution observations in the future.  \nUsing our pixel-by-pixel SED outputs and the [C II] line intensity map, we characterize the physical properties of M ⋆ , SFR, and gas mass M gas for these individual star-forming clumps. We sum the pixel-based output values for M ⋆ and SFR, following the segmentation presented in Fig. 1. We note that the pixels of star-forming clump-13 did not pass the pixel mask procedure in our SED fitting, so characterizations are performed for all of the clumps except that one. For M gas , we first convert the [C II] luminosity L [CII] to M gas pixel-by-pixel using the conversion factor calibrated in the literature 16 , and sum the values in the same manner as above. We discuss potential uncertainties in this conversion in Section 10. Note that because the ALMA beam size in the [C II] map ( 0 . '' 28 × 0 . '' 25 ) is larger than those in NIRCam, the M gas estimate is only performed for star-forming clump-1, 3, 4, 6, 7, 8, and 9 whose segmentation areas are larger than the ALMA beam size. We summarize the M ⋆ , SFR, and M gas values for each star-forming clump in Extended Data Table 4. We also derive M gas in the global galaxy scale in the same manner, resulting in 1 . 1 +0 . 4 -0 . 1 × 10 9 M ⊙ , which is listed in Extended Data Table 3.  \nThe spatial sizes of the individual star-forming clumps are also constrained by Sérsic profile fitting to the NIRCam/F150W map using the GALFIT software 58 . In the fitting, we adopt 16 Sérsic profiles for the 15 individual star-forming clumps and an underlying diffuse stellar disk component,  \n<!-- image -->  \nd)  \nExtended Data Figure 6: Physical properties of the individual star-forming clumps identified in the Cosmic Grapes . (a): SizeM ⋆ relation. The red circles represent the star-forming clumps, while the open red pentagon shows the measurement as the entire galaxy. For comparison, the other symbols indicate local objects of elliptical/S0 galaxies (E/S0; black circles), dwarf elliptical/S0 galaxies (dEs/dS0; open black triangles), dwarf spheroids (dSph; grey squares), ultra-compact dwarfs/compact elliptical galaxies (UCD/cE; magenta crosses), young massive star clusters (YMC; blue pentagon), nuclear star clusters (NSCs; green diamonds), globular clusters (GCs; orange triangles), young star clusters (YSC; cyan pentagon) taken from the compilation in the literature 95 . (b): Size-SFR relation. For comparison, the other symbols represent lower-redshift star-forming clumps at z ∼ 0 (black crosses), z ∼ 1 . 0 -1 . 5 (blue open squares), z ∼ 1 . 5 -3 . 0 (orange open pentagons), and z ∼ 3 . 0 -4 . 0 (green open pentagons), with the best-fit power-law functions (dashed lines) estimated in the literature 12 . (c): Σ SFR -Σ gas relation. The color symbols indicate different classes of local star-forming galaxies compiled in the literature 97 . The dashed line presents the KennicuttSchmidt (KS) law with the power-law slope of 1.4 97 . d: Same as b , but comparing with other z ≳ 6 objects recently observed with NIRCam. The green triangles represent the field galaxies at z ∼ 6 -10 98 , and the magenta diamonds 13 and squares 14 show the individual clumps identified in strongly lensed arc systems. The filled and open symbols indicate spectroscopic and photometric samples, respectively. The horizontal labels denote the typical physical scales of star clusters, star-forming clumps, and galaxies, where the Cosmic Grapes and its star-forming clumps uniquely bridge the relation between the galaxy and the star-forming clumps inside. 23  \nrespectively, where we fix the Sérsic index to n = 1 . 0 for all cases except star-forming clump-1 and the underlying disk component. Other parameters are used as free parameters with initial values of r e = 1 pix (pix = 0 . '' 02 = 116 pc), axis ratio q = 0 . 9 , position angle PA = 0 deg, spatial position ( x, y ) taken from the center of the segmentation area for each clump, and magnitude calculated by summing the pixel fluxes within the segmentation area for each clump. For the underlying disk component, we adopt the luminosity-weighted center and 50% of the total flux of the Cosmic Grapes for the initial values of the spatial position and the magnitude in the fitting. We also set the boundary limits of x = [ -3 : 3] pix, y = [ -3 : 3] pix (from the initial values), r e = [0 . 1 : 10 . 0] pix, and q = [0 . 1 : 1 . 0] for the 15 star-forming clumps, and n = [0 . 5 : 5] , r e = [10 : 60] pix, and q = [0 . 3 : 0 . 8] for the underlying disk component. To ensure a balanced fit of both compact and diffuse components, the area defined by the segmentation map is expanded by applying smoothing to the outer edge, extending the fitting mask by approximately 0 . '' 2 . All 16 components are then fitted simultaneously within this adjusted region. In Fig. 1, we show the best-fit model and the residual maps. We confirm that the individual star-forming clumps are reasonably modeled. Based on the best-fit models, the sum of the fluxes from the 15 clumps accounts for 69.9% of the total flux of the Cosmic Grapes in F150W, indicating that these clumps are the dominant luminosity component of the galaxy. We summarize the best-fit Sérsic profiles for each star-forming clump in Extended Data Table 4. Note that although the emission from the Cosmic Grapes observed in F150W corresponds to the rest-frame UV continuum, recent JWST/NIRCam studies show that spatial sizes in rest-UV and optical are comparable 98 . We thus refer to the rest-frame UV-based size measurement as the size throughout this paper.  \nIn Extended Data Fig. 6, we summarize the sizeM ⋆ , size-SFR, and surface gas density Σ gas - surface SFR density Σ SFR relations. In the calculation of Σ gas , we assume that the size of the gas clouds is two times larger than that of the rest-UV emitting region based on previous studies suggesting r e ([C II]) ≃ 2 × r e (UV) in high-redshift galaxies 105 . In panels of a and b , we find that our numerous star-forming clumps identified in the Cosmic Grapes fall in the same parameter space as young massive clusters (YMCs) in the local galaxies on the sizeM ⋆ plane, while their Σ SFR is much higher than that of the star-forming clumps at lower redshifts. Such an increasing trend of Σ SFR in star-forming clumps towards high redshifts is consistent with recent studies for high-redshift lensed systems 12-14,25,107 . In panel c , we find that our star-forming clumps have very high Σ gas and Σ SFR values comparable to dusty starburst systems, following the local Kennicutt-Schmidt law with the power-law slope of 1.4 97 . The panel d is the same as the panel b , but comparing the size-SFR relation with those measured in recent NIRCam-observed objects at z ≳ 6 13,14,98 . This comparison shows that our star-forming clumps are ∼ 1-2 orders magnitude more compact than galaxies (green triangles 98 ), while ∼ 1-2 orders magnitude larger than the compact star clusters (SCs) recently identified in the strongly lensed arc system at z ≃ 10 . 2 14 . Although spectroscopic confirmation has not yet been made for the lensed arc system at z ≃ 10 . 2 , this indicates that we are witnessing the three important regimes in early galaxies from our and recent NIRCam+lensing studies: global galaxy scales, star-forming clumps, and SCs. In this context, the Cosmic Grapes and its numerous star-forming clumps uniquely bridge the galaxy and SC layers, enabling us to study their roles in early galaxy formation and evolution through the multi-layered components. Examining the details of the internal structures while maintaining a comprehensive  \n<!-- image -->  \na)  \nb)  \nExtended Data Figure 7: Spatially-resolved views of modest dust reddening in the Cosmic Grapes . (a): Overlaid dust continuum on the NIRCam/F150W image cutout ( 2 . '' 2 × 2 . '' 2 ) in the image plane (i.e., before lens correction). The orange contour represents the 3 σ level dust continuum detected in a high-resolution ALMA map, utilizing only the C43-5 configuration. The orange ellipse at bottom left denotes the ALMA beam. A single component, recently detected in lower-resolution deep ALMA follow-up observations 108 is resolved into two peaks that align with the bright clumps seen in F150W. (b): Pixel-by-pixel E ( B -V ) and error estimates derived from H α /H β ratios observed with NIRSpec IFU, covering the same field as (a) . the Cosmic Grapes is characterized by modestly dust-reddened regions, with E ( B -V ) ≲ 0 . 06 . These results indicate that the distinctively clumpy morphology of the Cosmic Grapes is not a consequence of dust reddening.  \npicture of the entire galaxy has been challenging in strongly distorted arc systems because of the difficulty in reconstructing the entire galaxy from the significant local magnification in a specific narrow region in the source plane. Therefore, the Cosmic Grapes is offering us an invaluable laboratory at the epoch of reionization, not only because of its strong magnification ( µ = 32 ), but also because of its weak distortion and differential magnification.  \n8. Dust reddening in the Cosmic Grapes : While the Cosmic Grapes represents a subL ⋆ galaxy ( 0 . 025 L ⋆ of UV LF at z = 6 109 ), characterized by its youth ( 0 . 26 Z ⊙ ), lower mass ( 4 . 5 × 10 8 M ⊙ ), and typical dust reddening ( E ( B -V ) = 0 . 03 ) for its mass range at z = 6 , the modest dust emission is successfully detected in deep ALMA follow-up observations aided by the strong lensing effect 108 . To explore the influence of dust reddening on the observed clumpy morphology of the Cosmic Grapes , we examine the spatial distributions of dust continuum and dust reddening via the Balmer decrement of H α /H β .  \nIn Extended Data Fig.7a, we overlay the high-resolution ALMA dust continuum map, produced using only the C43-5 configuration (Section 3), on the NIRCam/F150W map to pinpoint dust-emitting peak positions, relative to the rest-frame UV continuum seen in F150W. The dust continuum is resolved into two peaks above the 3 σ level, coinciding with bright clumps in F150W. The absence of dust emission peaks at the gaps between the F150W clumps suggests that the clumpy morphology of the Cosmic Grapes is unlikely due to the presence of heavily dust-obscured star-forming regions. Additionally, we analyze spatially-resolved H α /H β line ratios on a pixel-by-  \n<!-- image -->  \nExtended Data Figure 8: Cool gas dynamics observed in the Cosmic Grapes via [C II ] 158 µ m line with ALMA. These maps are obtained in the source plane (i.e., after the lens correction). (a): Positionvelocity (PV) diagram along the major axis for the disk extracted using 3DBarolo . (b): Same as a , but along with the minor axis for the disk. (c): Channel maps for the [C II] line. The green cross denotes the kinematic center, and the magenta ellipse at left bottom indicates the effective beam in the source plane (i.e., after lens correction). These maps show a symmetric 3D structure, indicating that the Cosmic Grapes is a rotation-supported system 110 , rather than an ongoing merging system.  \npixel basis using NIRSpec IFU data, considering only pixels where both lines are detected at ≥ 3 σ . In Extended Data Fig.7b, we present E ( B -V ) and its error distributions, assuming a Calzetti 73 attenuation curve. Apart from several pixels at the edges, the Cosmic Grapes predominantly features modestly dust-reddened regions with E ( B -V ) ≲ 0 . 06 , aligning with the E ( B -V ) = 0 . 03 ± 0 . 01 measured in the global galaxy scale (Section 6). The minimal variation within E ( B -V ) ≲ 0 . 06 further suggests that the gaps between the clumps do not always show slightly high E ( B -V ) values across the Cosmic Grapes . We, therefore, conclude that the remarkably clumpy morphology of the Cosmic Grapes is not driven by dust reddening.  \n- 9. Kinematic modeling: Weanalyze the kinematic properties of [C II] 158 µ m, H α , and [O III] λ 5008 observed with ALMA and JWST/NIRSpec IFU. We perform the following analyses using 3D data cubes in the source plane, reconstructed in a pixel-by-pixel approach. First, we extracted radial rotation velocity ( V ( R ) ) and velocity dispersion ( σ ( R ) ) profiles, using the 3D-based analysis tool 3DBarolo 111 . A 3D tilted-ring model is employed in 3DBarolo , allowing us to derive rotation  \n[CII] 158μm (ALMA)  \nHα (JWST)  \n[OIII]λ5008 (JWST)  \nExtended Data Figure 9: Kinematic modeling of the [C II ] 158 µ m, H α , and [O III ] λ 5008 lines across the galaxy , using 3DBarolo . All maps are reconstructed in the source plane (i.e., lens-corrected). Top row: Line intensity maps for each emission line, with the observed data, model fit, and residuals displayed from left to right. Middle row: Line of sight velocity ( V LOS ), probing the rotational dynamics and any potential perturbations. Bottom row: Velocity dispersion maps, highlighting the kinematic thermal and non-thermal broadening effects. Contours overlaying the V LOS maps denote the V LOS = 0 km s -1 , and crosses mark the galaxy's dynamical center. The dashed line is the positional angle, which is fixed during the fitting.  \n<!-- image -->  \ncurves and gas dynamics in a non-parametric fashion, under the assumption of circular rotation. The smearing effects by the spectral and spatial resolutions are taken into account in 3DBarolo . Each tilted ring has flexibility with parameters such as rotation velocity V , velocity dispersion σ , inclination ( i ), position angle (PA), and scale height ( Z 0 ). From the target morphology in NIRCam, we obtain the axis ratio of q = 0 . 53 and calculate i = arccos( q ) ≃ 57 . 9 deg, which is fixed during the fitting. We adopt the AZIM normalization to study the global scale kinematics. We confirm that the PA value does not change much when we derive it with the emission line morphology. The dynamical center is fixed based on an iterative fitting output that initiates at the peak of the line intensity and velocity dispersion. The Z 0 value is also fixed around the effective spatial resolution of each instrument in the source plane. We use V , σ , and PA as free parameters. Owing to the weak distortion and differential magnification of our target, variations of the PSF shape in the source plane are minimal, and we adopt an average PSF shape over the target area. We set the width of the tilted ring between (0.5-1.0) × FWHMof the average PSF.  \nIn Extended Data Fig. 8, we highlight the position and velocity (PV) diagram and velocity channel maps for the [C II] line observed with the high spatial and spectral resolution ALMA data. The PV diagram shows a symmetric distribution with the two peaks, providing strong evidence that the Cosmic Grapes is a rotation-supported system 110 , rather than the result of ongoing  \nmerging components 112,113 . In Extended Data Fig. 9, we also summarize the observed, best-fit model, and residual maps for the [C II] (left), H α (middle), and [O III] (right) lines. While some residual components stand in the line intensity map, this is a natural consequence of the AZIM normalization in the fitting, and they are interpreted as the elevated line emissivity due to localscale substructures (e.g., clumps). The residuals in the velocity and dispersion maps are generally within ≃ ± 20 km s -1 along with the dynamical major axis, and the global-scale 3D structures of these emission lines are well modeled by 3DBarolo . A red-shifted velocity component along the dynamical major axis is identified in both H α and [O III] lines, which is likely an outflowing ionized gas component and further addressed in a separated paper 41 . In Fig. 3b, the red, blue, and green points indicate the measurements obtained for [C II], H α , and [O III] lines, respectively. While the V ( R ) measurements are generally consistent among the lines, we find that H α and [O III] lines show systematically higher σ ( R ) measurements than [C II]. This is consistent with predictions from cosmological zoom-in simulations and is interpreted that ionized gas is likely more influenced by feedback in galaxies 21 . We caution that the limited spectral resolution of NIRSpec ( ≃ 100 km s -1 ) might also contribute to the elevated σ ( R ) measurements in the H α and [O III] lines. We thus determine an average velocity dispersion σ 0 from the [C II] results, while we assume the maximum rotation velocity V max is not significantly affected by the feedback in H α and [O III]. We obtain V max /σ 0 = 3 . 47 ± 0 . 77 , 3 . 05 ± 0 . 78 , and 2 . 66 ± 0 . 43 for the [C II], H α , and [O III] lines, respectively, resulting in an average value of 2 . 89 ± 0 . 23 . In Extended Data Table 5, we list the best-fit V and σ measurements and the derived V max /σ 0 values.  \n10. Toomre Q parameter: We estimate the Toomre Q parameter, which gauges the stability of the disk against gravitational fragmentation. The critical threshold of Q crit is 1.0 (0.67) for a thin (thick) gas disk galaxy 18,19 , where the self-gravity of gas overcomes the repelling forces by pressure and differential rotation at Q < Q crit . The Q parameter is given by  \nQ = κσ πG Σ gas , (1)  \nwhere G is the gravitational constant, σ is the velocity dispersion of the gas, and Σ gas is the surface density of M gas , and κ is the epicyclic frequency defined by  \nκ 2 = 2Ω ( 2Ω R + d Ω dR ) , (2)  \nwhere Ω = V/R is the angular velocity.  \nTo compute Σ gas , we first convert L [CII] to M gas using a conversion factor of α [CII] = 31 M ⊙ /L ⊙ calibrated with star-forming galaxies at z ∼ 2 16 . While a systematic uncertainty may remain in this conversion, a consistent M gas value is obtained from the dynamical mass M dyn estimate, after subtracting M ⋆ in the Cosmic Grapes in the global galaxy scale 6 . Based on our latest [C II] data and the kinematic modeling results (Section 9), we obtain M dyn = 1 . 7 +0 . 7 -0 . 8 × 10 9 M ⊙ within 2 × r e of the rest-UV emitting region, and infer M gas ≈ M dyn -M ⋆ = (1 . 3 ± 0 . 8) × 10 9 M ⊙ , assuming that the dark matter contribution is negligible. This is in excellent agreement with the M gas estimate of 1 . 1 +0 . 4 -0 . 1 × 10 9 M ⊙ in the global galaxy scale using the above conversion. With an  \nanalytical model proposed based on the KS law, empirical relations, and a star-formation burstiness parameter (i.e., deviation from the KS relation) 117 , we infer α [CII]] ≃ 15 M ⊙ /L ⊙ , which is consistent with α [CII] = 18 M ⊙ /L ⊙ predicated from cosmological simulations for z ∼ 6 galaxies 17 . These models imply that using α [CII] = 31 M ⊙ /L ⊙ could result in overestimating M gas by a factor of ∼ 2. On the other hand, the dust mass is also estimated to be M dust = 1 . 2 +1 . 2 -0 . 7 × 10 6 M ⊙ for the Cosmic Grapes 108 , based on a dedicated far-infrared (FIR) SED analysis for the Cosmic Grapes with Hershel and ALMA multiple band constraints that cover observed wavelengths of 0.35-4 mm. Using the gas-to-dust mass ratio of ∼ 10 3 calibrated at a low-metallicity regime 119 like the Cosmic Grapes , we obtain M gas = 1 . 2 +1 . 2 -0 . 7 × 10 9 M ⊙ , which is again well consistent with the estimate based on α [CII] = 31 M ⊙ /L ⊙ . In this paper, we adopt the M gas estimate using α [CII] = 31 , M ⊙ /L ⊙ as our fiducial estimate, while we acknowledge a potential uncertainty up to a factor of 2 in Fig. 3c. In Extended Data Table 3, we also list the M gas estimates from M dyn and M dust .  \nWe applied the following approaches to assess the Q parameter. First, we derived the radial profile of the Toomre Q parameter by employing non-parametric radial profiles of the best-fit V ( R ) and σ ( R ) and the radial-averaged profile of the L [CII] luminosity obtained from 3DBarolo . This approach allowed us to correct for the beam-smearing effect, with the results presented in Fig. 3c. Second, as a complementary check, while retaining the beam-smearing effect, we directly computed the 2D distribution of the Q parameter by computing the V and σ pixel-by-pixel across the observed [C II] cube. In both approaches, we used the best-fit non-parametric V ( R ) profile obtained from 3DBarolo to compute κ via the numerical fashion. The results of this direct computation are displayed in the inset panel of Fig. 3c. Both approaches yielded consistent values of the Toomre Q parameter in a range of ≃ 0.2-0.3, well below Q crit = 0.67-1.0, suggesting that the gas is unstable over the entire galaxy. This instability likely facilitates star formation throughout the disk and forms numerous star-forming clumps (Fig. 1).  \n11. Clumpiness parameter S : To quantify the clumpy structure observed in the Cosmic Grapes , we evaluate the clumpiness parameter S , defined as  \nS = 10 × Σ N,N x , y=1 , 1 ( I x , y -I σ x , y ) -B x , y I x , y , (3)  \nwhere I x , y is the sky-subtracted flux values of the galaxy at position ( x, y ) , I x , y is the value of the galaxy's flux at ( x, y ) once it has been reduced in resolution by a smoothing filter of width σ , N is the size of the galaxy in pixels, and B x , y is the background pixel values in an area of the sky which is equal to the galaxy's area 22 . For this measurement, we adopt σ = 0 . '' 2 and use the pixels in NIRCam/F150W map within a circular area with r = 0 . '' 7 ( ≈ 0.7 kpc in the source plane) from the peak pixel in the Cosmic Grapes , given that circularized r e of the Cosmic Grapes on the global galaxy scale is estimated to be 0.7 kpc 6 . We obtain S = 0 . 81 , which is much higher than the average values observed among local Spirals ( 0 . 08 ± 0 . 08 ), dwarf irregulars ( 0 . 40 ± 0 . 20 ), and dwarf ellipticals ( 0 . 00 ± 0 . 06 ) 22 (Fig. 4). While the spatial resolutions are different between our and these local observations, the S parameter increases with better resolution, and the gap could be even larger in the same resolution. On the other hand, remarkably clumpy local dwarf galaxies, similar to the Cosmic Grapes , have also been identified in recent studies (see  \ne.g., Mrk178, DDO155 121 ), while these galaxies are much less massive than the Cosmic Grapes by ∼ 1-2 dex. Albeit less clumpy, dynamical studies with H I gas for local dwarf irregulars show their global-scale rotations 122 , while their velocity dispersions are even much smaller ( < 10 km s -1 ) than the Cosmic Grapes . Although it falls outside the scope of this study, investigating whether analogs of the Cosmic Grapes exist in the local Universe across various aspects (e.g., size, mass, kinematics, chemical enrichment) is crucial, offering valuable insights on whether the physical properties observed in the Cosmic Grapes result from unique processes exclusive to the early Universe or certain mechanisms observable in the local Universe as well.  \n- 12. Clump Luminosity Function: We also derive the cumulative clump luminosity function (LF) 12,25 as a function of SFR in each clump to independently evaluate the clumpiness in the Cosmic Grapes . In Fig. 4, we show our cumulative clump LF measurements for the Cosmic Grapes . For comparison, we also show measurements for similarly lensed galaxies at z ∼ 1 -3 using the H α line in the literature 12 . Here we convert the H α line luminosity to SFR 123 and select galaxies with SFR = 1 -10 M ⊙ yr -1 , which is comparable to that of the Cosmic Grapes , and recalculate the average cumulative LF per galaxy. We find that the cumulative clump LF in the Cosmic Grapes is systematically higher than that of the lower-redshift measurement, indicating the increasing trend of the clumpiness towards high redshifts.\n- 13. Cosmological zoom-in simulations: To investigate whether such a highly clumpy structure observed in the Cosmic Grapes is reproduced in state-of-the-art cosmological zoom-in simulations for early galaxies, we also quantify the S value and the cumulative clump LF using simulated galaxies in SERRA 21,23,126 and FIRE 24,127 . We refer the reader to the details of the SERRA and FIRE simulations in Pallottini et al. (2022) 23 and Wetzel et al. (2023) 24 , respectively, while here we briefly describe each simulation.  \nThe first set is SERRA, using a customized version of the adaptive mesh refinement (AMR) code RAMSES 128 to simulate the dynamics of dark matter, gas, and stars. Gas evolution is modeled using a second-order Godunov scheme, while dark matter and stars are handled via a multigrid particle-mesh solver. Radiative transfer processes are integrated on-the-fly with RAMSES-RT 129 , utilizing a momentum-based framework with M1 closure for the Eddington tensor 130 . Gas-photon interactions, along with the system of equations governing the thermal evolution of the gas, are managed using the KROME package 131 , which employs a detailed non-equilibrium chemical network. The integration of KROME with RAMSES-RT is achieved by sub-cycling the absorption steps to ensure convergence 132,133 . Emission lines are computed by interpolating grids from the photoionization code CLOUDY c17 71 , extending the models from Vallini et al. (2017) 134 as detailed in Pallottini et al. (2019) 133 . Attenuation of UV and continuum FIR emissions is calculated with the Monte Carlo code SKIRT V8 135,136 , informed by the modeling provided by Behrens et al. (2018) 137 . The spatial resolution reaches ≃ 30 pc in the densest regions at z = 6 , closely modeling the characteristics of Galactic Molecular Clouds. We select a total of 140 SERRA galaxies at z = 6 -8 for our comparison, whose physical properties are similar to the Cosmic Grapes with SFR ≃ 1-10 M ⊙ yr -1 , M ⋆ ≃ 10 8 -9 M ⊙ , and the gas kinematics likely to be rotation supported via the visual checks.  \nSERRA  \nFIRE  \nExtended Data Figure 10: Examples of simulated early galaxies in the cosmological zoom-in models of SERRA 23 (top) and FIRE 24 (bottom) . The panels show the noise-free maps of stellar (all), young stellar ( < 100 Myr), gas mass, and gas velocity distributions in the physical scale of 3 kpc × 3 kpc (see Methods ). The simulated maps are smoothed with Gaussian kernels to match the spatial resolution with the NIRCam/F150W observation of ≃ 0 . '' 01 after the lens correction (Fig. 2). For a fair comparison, we use simulated galaxies whose physical properties are close to the Cosmic Grapes ; SFR ≃ 1-10 M ⊙ yr -1 , M ⋆ ≃ 10 8 -9 M ⊙ , and z ≃ 6-8. We also select rotation-dominated galaxies when available, while no similarly rotation-dominated systems are identified in FIRE due to frequent starbursts and associated feedback effects. Thus, kinematic properties are not considered when selecting the FIRE galaxies for our comparison.  \n<!-- image -->  \nThe second set is FIRE, utilizing the N-body+hydrodynamics code GIZMO to re-simulate a set of haloes from the MassiveFIRE galaxy simulations, originally presented without black hole (BH) physics by Feldman et al. (2017) 138 . The updated simulations, employing the FIRE-2 code 139 , cover diverse halo formation histories with halo masses around 10 12 . 5 M ⊙ at z = 2 , and are evolved down to z = 1 with baryonic and dark matter particle masses of 3 . 3 × 10 4 M ⊙ and 1 . 7 × 10 5 M ⊙ with force softenings of 0.7 pc, 7 pc, and 57 pc for gas, stellar, and DM particles, respectively. The FIRE-2 enhancements include the meshless finite mass (MFM) hydrodynamics solver and refined stellar feedback algorithms. These improvements, alongside the assumed Λ CDMcosmology consistent with 140 , enable detailed modeling of galaxy evolution. Among the simulated galaxies publicly available 7 , we choose four galaxies of z5m11c, z5m11d, z5m11e, and z5m12a whose M ⋆ values evolve to (0 . 5 -3 . 0) × 10 9 M ⊙ at z = 5 141 , comparable to that of the Cosmic Grapes , and use their simulated maps at redshift slices of z = 6 . 0 , 6 . 5 , 7 . 0 , 7 . 5 , and 8 . 0 . Note that the systems with the rotating gas disk are rarely found among the simulated galaxies in FIRE due to more busty SFH implemented, where the gas disk is blown away 142,143 . Thus, we do not consider the  \nAll stellar  \nYoung stellar (<100Myr)  \nGas  \nGas velocity  \nkinematic properties in selecting the FIRE galaxies, while we do not use obvious major merger systems for our comparison. We select a total of 13 FIRE galaxies at z = 6 -8.  \nTo perform the comparison, we produce four cutout images of the stellar distribution, young ( < 100 Myr) stellar distribution, gas mass, and gas velocity in the physical scale of 3 kpc × 3 kpc around galaxies at z = 6 -8 from random lines of sight. We then inject random noise and smooth the maps using a Gaussian kernel to match the sensitivity and the spatial resolution as the observation of 0 . '' 01 (after the lens correction) to achieve a fair comparison. In Extended Data Fig. 10, we show four maps of example simulated galaxies in the SERRA and FIRE models after smoothing. As highlighted in these examples, we find that SEERA (FIRE) galaxies are generally characterized as rotation- (dispersion-) dominated systems with one or two (a few) stellar clump components. The difference between SERRA and FIRE simulations may originate from their different handling of star formation and feedback, which results in a burstier star formation history 142,143 - and, accordingly, more intense starbursts - in FIRE compared SERRA. Such frequent starbursts may produce more small clumps 26 , while it leads to more dynamically chaotic structures due to subsequent feedback effects. The FIRE galaxy in Extended Data Fig. 10 actually shows the situation that the gas disk is blown away due to a strong feedback effect.  \nGiven the NIRCam/F150W map corresponds to the rest-frame UV continuum representing the young stellar distribution of the Cosmic Grapes at z = 6 . 072 , we measure the S parameter and the clump LF in the same manner as the procedures done for the observed map. The results are summarized in Fig. 4. We find that the clumpiness in the Cosmic Grapes exceeds the values measured in the SERRA and FIRE galaxies in both quantities of S and the clump LF. These results indicate challenges in the current simulations to reconcile the two distinct properties - the numerous clumps and the rotating disk; more frequent starbursts may be required to reproduce the numerous clumps observed in the Cosmic Grapes , while the smooth rotating disk needs to remain in the galaxy. One plausible solution is that the feedback effects are significantly weaker than what is implemented in the current simulations. When the surface gas density exceeds 1,000 M ⊙ pc -2 , the star-formation efficiency is estimated to be larger than 0.6 in radiation hydrodynamical simulations 29 for clouds with 10% Z ⊙ and M gas = 10 6 M ⊙ , which are comparable to the individual clumps identified in the Cosmic Grapes . In the same context, we might be witnessing the effect of a feedback-free scenario 146 , as the low Q Toomre parameter promotes disk fragmentation, which leads to clump formation, boosting the already relatively high gas density ( ≃ 100 M ⊙ pc -2 ; see Extended Data Fig. 6c) and making star formation very efficient, i.e. effectively feedback free up in the burst phase. On one hand, however, the low dust obscuration observed in the Cosmic Grapes may imply that radiation pressure is effectively driving out the gas and dust from the system, a mechanism which is invoked to explain the overabundance of highz galaxies 147 . Due to the clumpy structure and the high gas surface density, the dust might be ejected from caves towards the face-on directions, which reconciles this scenario with the weak feedback scenarios described above. We note that the galaxies at z = 6 -8 in SERRA simulations show the gas fraction ( ≡ M gas / ( M gas + M ⋆ ) ) of ≃ 40 %at maximum. On the other hand, the gas fraction in the Cosmic Grapes is estimated to be ≃ 80-90% (see Extended Data Table 3). This indicates that a part of the gap between the observation and simulation results may also be ascribed to the physical  \nmechanisms related to the gas fraction such as the gas supply from the circum- and inter-galactic media.  \nExtended Data Table 1 | Optical-NIR observed photometry of the Cosmic Grapes  \nCode availability. The NIRCam data were processed with GRIZLI available at https://github. com/gbrammer/grizli . The NIRCam F160W image is analyzed with GALFIT available at https://users.obs.carnegiescience.edu/peng/work/galfit/galfit.html . The ALMA data were reduced using the CASA software version 6.4.1.12 available at https:// casa.nrao.edu/casa\\_obtaining.shtml . The NIRSpec data reduction code developed by the TEMPLATE team, which is available at https://github.com/JWST-Templates/ Notebooks/blob/main/nirspec\\_ifu\\_cookbook.ipynb . The [C II], H α , and [O III] λ 5008 data cubes are analyzed with 3DBarolo available at https://editeodoro.github.io/ Bbarolo/ .  \nData availability. This paper makes use of the JWST data from #GO-1567, available at https: //archive.stsci.edu/ . The reduced JWST NIRCam images are available at https:// dawn-cph.github.io/dja/ . The ALMA data supporting our finding is from #2021.1.00055.S, available at http://almascience.nao.ac.jp/ . The simulated galaxies in FIRE used in this study are all available at https://flathub.flatironinstitute.org/fire . Other datasets generated and/or analyzed during the current study are available from the corresponding author upon reasonable request.  \nExtended Data Table 2 | Observed line fluxes of the Cosmic Grapes with NIRSpec IFU", 'References for Methods': "- 31. Planck Collaboration, Ade, P. A. R., Aghanim, N., Armitage-Caplan, C. et al., 'Planck 2013 results. XVI. Cosmological parameters'. A&A , 571 , A16, November (2014).\n- 32. 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