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# Evidence for GN-z11 as a luminous galaxy at redshift 10.957

## Abstract

GN-z11 was photometrically selected as a luminous star-forming galaxy candidate at redshift z > 10 on the basis of Hubble Space Telescope imaging data1. Follow-up Hubble Space Telescope near-infrared grism observations detected a continuum break that was explained as the Lyα break corresponding to $$z = 11.09_{ - 0.12}^{ + 0.08}$$ (ref. 2). However, its accurate redshift remained unclear. Here we report a probable detection of three ultraviolet emission lines from GN-z11, which can be interpreted as the [C iii] λ1907, C iii] λ1909 doublet and O iii] λ1666 at z = 10.957 ± 0.001 (when the Universe was only ~420 Myr old, or ~3% of its current age). This is consistent with the redshift of the previous grism observations, supporting GN-z11 as the most distant galaxy known to date. Its ultraviolet lines probably originate from dense ionized gas that is rarely seen at low redshifts, and its strong [C iii] and C iii] emission is partly due to an active galactic nucleus or enhanced carbon abundance. GN-z11 is luminous and young, yet moderately massive, implying a rapid build-up of stellar mass in the past. Future facilities will be able to find the progenitors of such galaxies at higher redshift and probe the cosmic epoch at the beginning of reionization.

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• ### Exploring nine simultaneously occurring transients on April 12th 1950

Scientific Reports Open Access 17 June 2021

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$32.00 All prices are NET prices. ## Data availability The Keck MOSFIRE data of this work are publicly available from the Keck Observatory Archive (https://www2.keck.hawaii.edu/koa/public/koa.php). Source data are provided with this paper. Other data of this study are available from the corresponding authors upon reasonable request. ## Code availability The Keck MOSFIRE data were reduced using a publicly available data reduction pipeline (https://github.com/Keck-DataReductionPipelines/MosfireDRP). ## References 1. Oesch, P. A. et al. The most luminous z ~ 9–10 galaxy candidates yet found: the luminosity function, cosmic star-formation rate, and the first mass density estimate at 500 Myr. Astrophys. J. 786, 108–126 (2014). 2. Oesch, P. A. et al. A remarkably luminous galaxy at z = 11.1 measured with Hubble Space Telescope grism spectroscopy. Astrophys. J. 819, 129–139 (2016). 3. Zheng, W. et al. A magnified young galaxy from about 500 million years after the Big Bang. Nature 489, 406–408 (2012). 4. Coe, D. et al. CLASH: three strongly lensed images of a candidate z ≈ 11 galaxy. Astrophys. J. 762, 32–52 (2013). 5. Ellis, R. S. et al. The abundance of star-forming galaxies in the redshift range 8.5–12: new results from the 2012 Hubble ultra-deep field campaign. Astrophys. J. Lett. 763, 7–12 (2013). 6. Zitrin, A. et al. A geometrically supported z ~ 10 candidate multiply imaged by the Hubble Frontier Fields Cluster A2744. Astrophys. J. Lett. 793, 12–17 (2014). 7. Bouwens, R. J. et al. The bright end of the z ~ 9 and z ~ 10 UV luminosity functions using all five CANDELS fields. Astrophys. J. 830, 67–88 (2016). 8. Shibuya, T. et al. The first systematic survey for Lyα emitters at z = 7.3 with red-sensitive Subaru/Suprime-Cam. Astrophys. J. 752, 114–124 (2012). 9. Finkelstein, S. L. et al. A galaxy rapidly forming stars 700 million years after the Big Bang at redshift 7.51. Nature 502, 524–527 (2013). 10. Tilvi, V. et al. First results from the Faint Infrared Grism Survey (FIGS): first simultaneous detection of Lyα emission and Lyman break from a galaxy at z = 7.51. Astrophys. J. Lett. 827, 14–19 (2016). 11. Laporte, N. et al. Dust in the reionization era: ALMA observations of a z = 8.38 gravitationally lensed galaxy. Astrophys. J. Lett. 837, 21–26 (2017). 12. Hashimoto, T. et al. The onset of star formation 250 million years after the Big Bang. Nature 557, 392–395 (2018). 13. McLean, I. S. et al. MOSFIRE, the Multi-Object Spectrometer For Infra-Red Exploration at the Keck Observatory. Proc. SPIE 8446, 17 (2012). 14. Stark, D. P. et al. Spectroscopic detections of C iii] λ1909 Å at z 6–7: a new probe of early star-forming galaxies and cosmic reionization. Mon. Not. R. Astron. Soc. 450, 1846–1855 (2015). 15. Mainali, R. et al. Spectroscopic constraints on UV metal line emission at z 6–9: the nature of Lyα emitting galaxies in the reionization era. Mon. Not. R. Astron. Soc. 479, 1180–1193 (2018). 16. Fosbury, R. A. E. et al. Massive star formation in a gravitationally lensed H ii galaxy at z = 3.357. Astrophys. J. 596, 797–809 (2003). 17. Nakajima, K. et al. The VIMOS Ultra Deep Survey: nature, ISM properties, and ionizing spectra of C iii] λ1909 emitters at z = 2–4. Astron. Astrophys. 612, A94 (2018). 18. Le Fèvre, O. et al. The VIMOS Ultra-Deep Survey: evidence for AGN feedback in galaxies with C iii]-λ1908 Å emission 10.8 to 12.5 Gyr ago. Astron. Astrophys. 625, A51 (2019). 19. Quider, A. M. et al. The ultraviolet spectrum of the gravitationally lensed galaxy ‘the Cosmic Horseshoe’: a close-up of a star-forming galaxy at z ~ 2. Mon. Not. R. Astron. Soc. 398, 1263–1278 (2009). 20. James, B. L. et al. Testing metallicity indicators at z ~ 1.4 with the gravitationally lensed galaxy CASSOWARY 20. Mon. Not. R. Astron. Soc. 440, 1794–1809 (2014). 21. Stark, D. P. et al. Ultraviolet emission lines in young low-mass galaxies at z ~ 2: physical properties and implications for studies at z > 7. Mon. Not. R. Astron. Soc. 445, 3200–3220 (2014). 22. Nanayakkara, T. et al. Exploring He ii λ1640 emission line properties at z ~ 2–4. Astron. Astrophys. 624, A89 (2019). 23. Feltre, A., Charlot, S. & Gutkin, J. Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths. Mon. Not. R. Astron. Soc. 456, 3354–3374 (2016). 24. Cassata, P. et al. He ii emitters in the VIMOS VLT Deep Survey: Population III star formation or peculiar stellar populations in galaxies at 2 < z < 4.6? Astron. Astrophys. 556, 68–90 (2013). 25. Maiolino, R. et al. The assembly of ‘normal’ galaxies at z ~ 7 probed by ALMA. Mon. Not. R. Astron. Soc. 452, 54–68 (2015). 26. Carniani, S. et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Mon. Not. R. Astron. Soc. 478, 1170–1184 (2018). 27. Jiang, L. et al. Physical properties of spectroscopically confirmed galaxies at z ≥ 6. III. Stellar populations from SED modeling with secure Lyα emission and redshifts. Astrophys. J. 816, 16–33 (2016). 28. Mutch, S. J. et al. Dark-ages reionization and galaxy-formation simulation—VI. The origins and fate of the highest known redshift galaxy. Mon. Not. R. Astron. Soc. 463, 3556–3562 (2016). 29. Waters, D. et al. Monsters in the dark: predictions for luminous galaxies in the early Universe from the BLUETIDES simulation. Mon. Not. R. Astron. Soc. 461, 51–55 (2016). 30. Shapley, A. et al. Rest-frame ultraviolet spectra of z ~ 3 Lyman break galaxies. Astrophys. J. 588, 65–89 (2003). 31. Kriek, M. et al. The MOSFIRE Deep Evolution Field (MOSDEF) survey: rest-frame optical spectroscopy for ~1500 H-selected galaxies at 1.37 < z < 3.8. Astrophys. J. Suppl. 218, 15–41 (2015). 32. Pettini, M. et al. The rest-frame optical spectra of Lyman break galaxies: star formation, extinction, abundances, and kinematics. Astrophys. J. 554, 981–1000 (2001). 33. Erb, D. K. et al. The stellar, gas, and dynamical masses of star-forming galaxies at z ~ 2. Astrophys. J. 646, 107–132 (2006). 34. Erb, D. K. et al. Physical conditions in a young, unreddened, low-metallicity galaxy at high redshift. Astrophys. J. 719, 1168–1190 (2010). 35. Boquien, M. et al. CIGALE: a python Code Investigating GALaxy Emission. Astron. Astrophys. 622, 103–135 (2019). 36. Finlator, K., Oppenheimer, B. D. & Davé, R. Smoothly rising star formation histories during the reionization epoch. Mon. Not. R. Astron. Soc. 410, 1703–1724 (2011). 37. Kennicutt, R. C. Star formation in galaxies along the Hubble sequence. Annu. Rev. Astron. Astrophys. 36, 189–232 (1998). 38. Madau, P., Pozzetti, L. & Dickinson, M. The star formation history of field galaxies. Astrophys. J. 498, 106–116 (1998). Download references ## Acknowledgements We acknowledge support from the National Science Foundation of China (11721303, 11890693, 11991052), the National Key R&D Program of China (2016YFA0400702, 2016YFA0400703) and the Chinese Academy of Sciences (CAS) through a China–Chile Joint Research Fund (1503) administered by the CAS South America Center for Astronomy. N.K. acknowledges support from JSPS grant 15H03645. We thank P. Oesch and C. Steidel for discussions on observations and data reduction. We thank A. Feltre, K. Nakajima and T. Nanayakkara for providing data shown in Fig. 3. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The observatory was made possible by the financial support of the W. M. Keck Foundation. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. ## Author information ### Authors and Affiliations Authors ### Contributions L.J. designed the programme, carried out the Keck observations, analysed the data and prepared the manuscript. N.K. designed the programme and carried out the observations. S.W. and G.W. reduced the images. L.C.H. helped to prepare the manuscript. K.I. and Y.L. assisted with the observations. All authors helped with the scientific interpretations and commented on the manuscript. ### Corresponding authors Correspondence to Linhua Jiang or Nobunari Kashikawa. ## Ethics declarations ### Competing interests The authors declare no competing interests. ## Additional information Peer review information Nature Astronomy thanks Fergus Cullen, Norbert Pirzkal and the other, anonymous, reviewer(s) for their contribution to the peer review of this work. Publisher’s note Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations. ## Extended data ### Extended Data Fig. 1 Detection of the [C III] and C III] emission lines from the first half of the K-band data. Detection of the [C III] λ1907 and C III] λ1909 emission lines. Same as Fig. 2, but for the first half of the K-band data. ### Extended Data Fig. 2 Detection of the [C III] and C III] emission lines from the second half of the K-band data. Detection of the [C III] λ1907 and C III] λ1909 emission lines. Same as Fig. 2, but for the second half of the K-band data. ### Extended Data Fig. 3 Detection of the O III] emission line. Detection of the O III] λ1666 emission line. a, Part of the K-band 2D spectrum with the line (enclosed by the yellow circle) detected at 3.3σ significance. The two negative signals enclosed by the blue circles are the same pattern shown in Fig. 2. b, A smoothed version of the 2D spectrum to better illustrate the line detection; a Gaussian filter with a size of 2.5 pixels is used. c, Extracted 1D spectrum. The grey area represents the 1σ uncertainty region. The hatched areas indicate regions affected by OH skylines. The emission line is shown in green, with the vermillion solid profile being the best-fit Gaussian. d, Same as (c), but from the smoothed 2D spectrum (b). ### Extended Data Fig. 4 SED modelling of GN-z11. SED modelling of GN-z11. a, SED modelling result using a fixed redshift z = 3.558, that is, the emission line at 22823 Å is assumed to be [O III] λ5007. The red points with 1σ error bars are the observed photometric data points. The downward arrows indicate the 2σ detection upper limits. The horizontal errors indicate the wavelength ranges of the filters. The light blue spectrum represents the best model. The dark blue crosses represent the photometric points predicted by the model. They are inconsistent with the observed values. For comparison, the grey spectrum represents the best model using a fixed redshift z = 10.957. The model photometry (black crosses) is well consistent with the observed photometry. b, Same as (a), but for a fixed redshift z = 5.124, that is, the emission line at 22823 Å is assumed to be [O II] λ3727. The best model is also inconsistent with the observed photometry. ## Source data ### Source Data Fig. 1 Source data for Fig. 1. ### Source Data Fig. 2 Source data for Fig. 2. ## Rights and permissions Reprints and Permissions ## About this article ### Cite this article Jiang, L., Kashikawa, N., Wang, S. et al. Evidence for GN-z11 as a luminous galaxy at redshift 10.957. Nat Astron 5, 256–261 (2021). https://doi.org/10.1038/s41550-020-01275-y Download citation • Received: • Accepted: • Published: • Issue Date: • DOI: https://doi.org/10.1038/s41550-020-01275-y ## Further reading • ### Four revelations from the Webb telescope about distant galaxies • Alexandra Witze Nature (2022) • ### Observational Manifestations of First Galaxies in the Far Infrared Range • T. I. Larchenkova • A. A. Ermash • Yu. A. Shchenkov Astrophysics (2022) • ### L. 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