The onset of star formation 250 million years after the Big Bang

Abstract

A fundamental quest of modern astronomy is to locate the earliest galaxies and study how they influenced the intergalactic medium a few hundred million years after the Big Bang1,2,3. The abundance of star-forming galaxies is known to decline4,5 from redshifts of about 6 to 10, but a key question is the extent of star formation at even earlier times, corresponding to the period when the first galaxies might have emerged. Here we report spectroscopic observations of MACS1149-JD16, a gravitationally lensed galaxy observed when the Universe was less than four per cent of its present age. We detect an emission line of doubly ionized oxygen at a redshift of 9.1096 ± 0.0006, with an uncertainty of one standard deviation. This precisely determined redshift indicates that the red rest-frame optical colour arises from a dominant stellar component that formed about 250 million years after the Big Bang, corresponding to a redshift of about 15. Our results indicate that it may be possible to detect such early episodes of star formation in similar galaxies with future telescopes.

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Fig. 1: ALMA [O iii] contours and spectrum of MACS1149-JD1.
Fig. 2: The SED of MACS1149-JD1.
Fig. 3: Demonstration of how a dominant phase of early star formation is necessary to reproduce the SED of MACS1149-JD1.

References

  1. 1.

    Robertson, B. E., Ellis, R. S., Furlanetto, S. R. & Dunlop, J. S. Cosmic reionization and early star-forming galaxies: a joint analysis of new constraints from Planck and the Hubble Space Telescope. Astrophys. J. 802, L19 (2015).

    ADS  Article  Google Scholar 

  2. 2.

    Bouwens, R. et al. Reionization after Planck: the derived growth of the cosmic ionizing emissivity now matches the growth of the galaxy UV luminosity density. Astrophys. J. 811, 140 (2015).

    ADS  Article  Google Scholar 

  3. 3.

    Stark, D. Galaxies in the first billion years after the Big Bang. Annu. Rev. Astron. Astrophys. 54, 761–803 (2016).

    ADS  CAS  Article  Google Scholar 

  4. 4.

    McLeod, D., McLure, R. & Dunlop, J. The z = 9−10 galaxy population in the Hubble Frontier Fields and CLASH surveys: the z = 9 luminosity function and further evidence for a smooth decline in ultraviolet luminosity density at z ≥ 8. Mon. Not. R. Astron. Soc. 459, 3812–3824 (2016).

    ADS  CAS  Article  Google Scholar 

  5. 5.

    Oesch, P. et al. The dearth of z ~ 10 galaxies in all HST legacy fields – the rapid evolution of the galaxy population in the first 500 Myr. Astrophys. J. 855, 105 (2018).

    ADS  Article  Google Scholar 

  6. 6.

    Zheng, W. et al. A magnified young galaxy from about 500 million years after the Big Bang. Nature 489, 406–408 (2012).

    ADS  CAS  Article  Google Scholar 

  7. 7.

    Zheng, W. et al. Young galaxy candidates in the Hubble Frontier Fields. IV. MACS J1149.5+2223. Astrophys. J. 836, 210 (2017).

    ADS  Article  Google Scholar 

  8. 8.

    Huang, K. et al. Spitzer UltRa Faint SUrvey Program (SURFS UP). II. IRAC-detected Lyman-break galaxies at 6<z<10 behind strong-lensing clusters. Astrophys. J. 817, 11 (2016).

    ADS  Article  Google Scholar 

  9. 9.

    Kawamata, R. et al. Precise strong lensing mass modeling of four Hubble Frontier Field clusters and a sample of magnified high-redshift galaxies. Astrophys. J. 819, 114 (2016).

    ADS  Article  Google Scholar 

  10. 10.

    Inoue, A. K. et al. Detection of an oxygen emission line from a high-redshift galaxy in the reionization epoch. Science 352, 1559–1562 (2016).

    ADS  CAS  Article  Google Scholar 

  11. 11.

    da Cunha, E. et al. On the effect of the cosmic microwave background in high-redshift (sub-)millimeter observations. Astrophys. J. 766, 13 (2013).

    ADS  Article  Google Scholar 

  12. 12.

    Hildebrand, R. H. The determination of cloud masses and dust characteristics from submillimetre thermal emission. Q. J. R. Astron. Soc. 24, 267–282 (1983).

    ADS  Google Scholar 

  13. 13.

    Smit, R. et al. High-precision photometric redshifts from Spitzer/IRAC: extreme [3.6] – [4.5] colors identify galaxies in the redshift range z 6.6 − 6.9. Astrophys. J. 801, 122 (2015).

    ADS  Article  Google Scholar 

  14. 14.

    Roberts-Borsani, G. et al. z ≥ 7 galaxies with red Spitzer/IRAC [3.6]–[4.5] colors in the full CANDELS data set: the brightest-known galaxies at z 7−9 and a probable spectroscopic confirmation at z = 7.48. Astrophys. J. 823, 143 (2016).

    ADS  Article  Google Scholar 

  15. 15.

    Stark, D. et al. Lyα and C iii] emission in z = 7−9 galaxies: accelerated reionization around luminous star-forming systems? Mon. Not. R. Astron. Soc. 464, 469–479 (2017). 

    ADS  CAS  Article  Google Scholar 

  16. 16.

    Hoag, A. et al. HST grism observations of a gravitationally lensed redshift 9.5 galaxy. Astrophys. J. 854, 39 (2018).

    ADS  Article  Google Scholar 

  17. 17.

    Carniani, S. et al. Extended ionised and clumpy gas in a normal galaxy at z=7.1 revealed by ALMA. Astron. Astrophys. 605, A42 (2017).

    Article  Google Scholar 

  18. 18.

    Vernet, J. et al. X-shooter, the new wide band intermediate resolution spectrograph at the ESO Very Large Telescope. Astrophys. J. 536, A105 (2011).

    Google Scholar 

  19. 19.

    Inoue, A. K. et al. ALMA will determine the spectroscopic redshift z>8 with FIR [O iii] emission lines. Astrophys. J. 780, L18 (2013). 

    ADS  Article  Google Scholar 

  20. 20.

    Cen, R. & Haiman, Z. Quasar Strömgren spheres before cosmological reionization. Astrophys. J. 542, L75–L78 (2000).

    ADS  CAS  Article  Google Scholar 

  21. 21.

    Haiman, Z. The detectability of high-redshift Lyα emission lines prior to the reionization of the Universe. Astrophys. J. 576, L1–L4 (2002).

    ADS  Article  Google Scholar 

  22. 22.

    Hu, E. et al. An ultraluminous Lyα emitter with a blue wing at z=6.6. Astrophys. J. 825, L7 (2016).

    ADS  Article  Google Scholar 

  23. 23.

    Dijkstra, M., Haiman, Z. & Spaans, M. Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall. Astrophys. J. 649, 14–36 (2006).

    ADS  Article  Google Scholar 

  24. 24.

    Verhamme, A. et al. Using Lyman-α to detect galaxies that leak Lyman continuum. Astron. Astrophys. 578, A7 (2015).

    Article  Google Scholar 

  25. 25.

    Komatsu, E. et al. Seven-year Wilkinson microwave anisotropy probe (WMAP) observations: cosmological interpretation. Astrophys. J. 192, 18 (2011).

    Article  Google Scholar 

  26. 26.

    Hashimoto, T. et al. A close comparison between observed and modeled Lyα lines for z 2.2 Lyα emitters. Astrophys. J. 812, 157 (2015).

    ADS  Article  Google Scholar 

  27. 27.

    Watson, D. et al. A dusty, normal galaxy in the epoch of reionization. Nature 519, 327–330 (2015).

    ADS  CAS  Article  Google Scholar 

  28. 28.

    Knudsen, K. K. et al. A merger in the dusty, z = 7.5 galaxy A1689-zD1? Mon. Not. R. Astron. Soc. 466, 138–146 (2017).

    ADS  CAS  Article  Google Scholar 

  29. 29.

    Laporte, N. et al. Dust in the reionization era: ALMA observations of a z = 8.38 gravitationally lensed galaxy. Astrophys. J. 837, L21 (2017).

    ADS  Article  Google Scholar 

  30. 30.

    Faisst, A. K. et al. Are high-redshift galaxies hot? Temperature of z > 5 galaxies and implications for their dust properties. Astrophys. J. 847, 21 (2017).

    ADS  Article  Google Scholar 

  31. 31.

    Ota, K. et al. ALMA observation of 158 μm [C ii] line and dust continuum of a z = 7 normally star-forming galaxy in the epoch of reionization. Astrophys. J. 792, 34 (2014). 

    ADS  Article  Google Scholar 

  32. 32.

    Ouchi, M. et al. An intensely star-forming galaxy at z 7 with low dust and metal content revealed by deep ALMA and HST observations. Astrophys. J. 778, 102 (2013).

    ADS  Article  Google Scholar 

  33. 33.

    Schaerer, D. et al. New constraints on dust emission and UV attenuation of z = 6.5−7.5 galaxies from millimeter observations. Astron. Astrophys. 574, A19 (2015).

    Article  Google Scholar 

  34. 34.

    Freudling, W. et al. Automated data reduction workflows for astronomy. The ESO Reflex environment. Astrophys. J. 559, A96 (2013).

    Google Scholar 

  35. 35.

    Trainor, R., Steidel, C., Strom, A. & Rudie, G. The spectroscopic properties of Lyα-emitters at z2.7: escaping gas and photons from faint galaxies. Astrophys. J. 809, 89 (2015).

    ADS  Article  Google Scholar 

  36. 36.

    González-López, J. et al. The ALMA Frontier Fields survey. I. 1.1 mm continuum detections in Abell 2744, MACS J0416.1−2403 and MACS J1149.5+2223. Astron. Astrophys. 597, A41 (2017).

    Article  Google Scholar 

  37. 37.

    Dwek, E. et al. Dust formation, evolution, and obscuration effects in the very high-redshift universe. Astrophys. J. 788, L30 (2014).

    ADS  Article  Google Scholar 

  38. 38.

    Dwek, E. et al. Submillimeter observations of CLASH 2882 and the evolution of dust in this galaxy. Astrophys. J. 813, 119 (2015).

    ADS  Article  Google Scholar 

  39. 39.

    Zavala, J. A. et al. Early science with the Large Millimeter Telescope: dust constraints in a z 9.6 galaxy. Mon. Not. R. Astron. Soc. 453, L88–L92 (2015).

    ADS  CAS  Article  Google Scholar 

  40. 40.

    Richard, J. et al. Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies. Mon. Not. R. Astron. Soc. 444, 268–289 (2014).

    ADS  Article  Google Scholar 

  41. 41.

    Johnson, T. L. et al. Lens models and magnification maps of the six Hubble Frontier Fields clusters. Astrophys. J. 797, 48 (2014).

    ADS  Article  Google Scholar 

  42. 42.

    Ishigaki, M. et al. Hubble Frontier Fields first complete cluster data: faint galaxies at z 5−10 for UV luminosity functions and cosmic reionization. Astrophys. J. 799, 12 (2015).

    ADS  Article  Google Scholar 

  43. 43.

    Keeton, C. R. On modeling galaxy-scale strong lens systems. Gen. Relativ. Gravit. 42, 2151–2176 (2010).

    ADS  MathSciNet  Article  Google Scholar 

  44. 44.

    Liesenborgs, J., De Rijcke, S. & Dejonghe, H. A genetic algorithm for the non-parametric inversion of strong lensing systems. Mon. Not. R. Astron. Soc. 367, 1209–1216 (2006).

    ADS  CAS  Article  Google Scholar 

  45. 45.

    Diego, J. M., Protopapas, P., Sandvik, H. B. & Tegmark, M. Non-parametric inversion of strong lensing systems. Mon. Not. R. Astron. Soc. 360, 477–491 (2005).

    ADS  Article  Google Scholar 

  46. 46.

    Merten, J. et al. Creation of cosmic structure in the complex galaxy cluster merger Abell 2744. Mon. Not. R. Astron. Soc. 417, 333–347 (2011).

    ADS  Article  Google Scholar 

  47. 47.

    Mawatari, K. et al. Possible identification of massive and evolved galaxies at z >5. Publ. Astron. Soc. Jpn. 68, 46 (2016).

    ADS  Article  Google Scholar 

  48. 48.

    Bruzual, G. & Charlot, S. Stellar population synthesis at the resolution of 2003. Mon. Not. R. Astron. Soc. 344, 1000–1028 (2003).

    ADS  Article  Google Scholar 

  49. 49.

    Inoue, A. K. Rest-frame ultraviolet-to-optical spectral characteristics of extremely metal-poor and metal-free galaxies. Mon. Not. R. Astron. Soc. 415, 2920–2931 (2011).

    ADS  CAS  Article  Google Scholar 

  50. 50.

    Calzetti, D. et al. The dust content and opacity of actively star-forming galaxies. Astrophys. J. 533, 682–695 (2000).

    ADS  Article  Google Scholar 

  51. 51.

    Rieke, H. et al. Determining star formation rates for infrared galaxies. Astrophys. J. 692, 556–573 (2009).

    ADS  CAS  Article  Google Scholar 

  52. 52.

    Chabrier, G. Galactic stellar and substellar initial mass function. Publ. Astron. Soc. Pacif. 115, 763–795 (2003).

    ADS  Article  Google Scholar 

  53. 53.

    Inoue, A. K. et al. An updated analytic model for attenuation by the intergalactic medium. Mon. Not. R. Astron. Soc. 442, 1805–1820 (2014).

    ADS  CAS  Article  Google Scholar 

  54. 54.

    Sawicki, M. SEDfit: software for spectral energy distribution fitting of photometric data. Publ. Astron. Soc. Pacif. 124, 1208–1218 (2012).

    ADS  Article  Google Scholar 

  55. 55.

    Förster Schreiber, M. et al. The SINS survey: SINFONI integral field spectroscopy of z 2 star-forming galaxies. Astrophys. J. 706, 1364–1428 (2009).

    ADS  Article  Google Scholar 

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Acknowledgements

We thank K. Umetsu for a discussion of gravitational lensing models; K. Nakanishi, F. Egusa and K. Saigo for discussions about handling ALMA data; S. Kikuchihara for supporting MOSFIRE observations; and H. Yajima and A. Zitrin for discussions. We acknowledge support from: NAOJ ALMA Scientific Research Grant number 2016-01 A (T.H. and A.K.I.); European Research Council Advanced Grant FP7/669253 (N.L. and R.S.E.) and 339177 (C.E.R.); KAKENHI grants 26287034 and 17H01114 (K.M. and A.K.I.), 17H06130 (Y. Tamura), 17H04831 (Y.M.), 16H01085 (T.O.), 16H02166 (Y. Taniguchi), 15K17616 (B.H.), 17K14252 (H.U.), JP17H01111 (I.S.), 16J03329 (Y.H.) and 15H02064 (M.O.); the grant CONICYT-Chile Basal-CATA PFB-06/2007, FONDECYT Regular 1141218 (F.E.B.); NAOJ Visiting Fellow Program (N.H.H.). ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. This work incorporates observations made with ESO Telescopes at the La Silla Paranal Observatory. This work is also partly based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA, as well as observations obtained with the NASA/ESA Hubble Space Telescope at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555.

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Contributions

T.H., N.L., R.S.E., and A.K.I. wrote the paper. T.H. and Y. Tamura reduced and analysed ALMA data. T.H. produced Figs. 1 and 2 and Extended Data Figs. 1, 35. N.L. reduced and analysed X-shooter data and produced Extended Data Figs. 2 and 7. K.M. and E.Z. performed SED fitting analyses. K.M. produced Fig. 3 and Extended Data Fig. 6. W.Z. carried out the astrometry analysis on HST and IRAC data. N.L. and C.E.R. performed lensing analyses. H.M., I.S., T.O., N.Y., Y. Taniguchi, B.H., H.U. and Y.M. contributed to the ALMA observational strategy. N.H.H. independently inspected the ALMA data. G.R.B., T.F. and R.P. inspected independently the X-shooter spectra. G.R.B. contributed to the observations. F.E.B. contributed to the X-shooter observational strategy. Y.H. and M.O. performed MOSFIRE observations and analysed the archival and our own MOSFIRE data. All authors discussed the results and commented on the manuscript.

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Correspondence to Takuya Hashimoto.

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Extended data figures and tables

Extended Data Fig. 1 ALMA dust contours of MACS1149-JD1 and a serendipitous continuum object.

a, ALMA dust contours of MACS1149-JD1 overlaid on the HST F160W image. Contours are drawn at ± 2σ, where σ = 17.7 μJy per beam. Negative contours are shown by the dashed line. The ellipse at the lower left corner indicates the synthesized beam size of ALMA. b, Dust continuum of a dusty galaxy at z = 0.99 in our ALMA field of view, overlaid on the HST F160W image. Contours are drawn at −2σ, 2σ, 4σ, 6σ, 8σ and 9.5σ, where σ = 16.0 μJy per beam.

Extended Data Fig. 2 X-shooter observations and Lyα spectra of MACS1149-JD1.

a, Orientation of the X-shooter slit (white dashed-line rectangle), demonstrating the successful acquisition of MACS1149-JD1 data by alignment of the slit to follow the lensed elongation, as well as the inclusion of a bright foreground galaxy. b, Two-dimensional X-shooter spectra of MACS1149-JD1, with the position of Lyα marked with a green arrow and the two negative counterparts shown by red arrows. Sky lines are highlighted by blue rectangles. c, Extracted one-dimensional spectra in a 0.8″ aperture. Lyα is shaded in yellow, 2σ is shown in grey, and the sky lines are marked by blue rectangles.

Extended Data Fig. 3 ALMA [O iii] 88-μm emission and X-shooter Lyα spectra in velocity space.

The flux densities Fν of [O iii] and Lyα emissions are shown with a resolution of 42 km s−1 and 15 km s−1, respectively. The values are normalized by the peak flux densities. The zero-velocity point corresponds to the [O iii] redshift, z = 9.1096 (red dashed line), and the Lyα offset is 450 km s−1 (blue dashed line). Grey rectangles show regions contaminated by night-sky emission. The data at around −100 km s−1 to 0 km s−1 were removed from the analysis because the night-sky emission was too strong. The black solid lines indicate the 1σ noise level for these velocity resolutions.

Extended Data Fig. 4 Best-fit SEDs of MACS1149-JD1 with various SFHs.

a, b, Best-fit SEDs obtained with a single stellar component, assuming an exponentially declining (a) and a constant (b) SFH. c, d, Best-fit SEDs obtained with two stellar components, assuming a constant SFH. The star formation duration of the old component is τ = 10 Myr (c) and 200 Myr (d). The reduced χ2 value, \({\chi }_{\nu }^{<mml:mpadded xmlns:xlink="http://www.w3.org/1999/xlink" lspace="-.15em">2</mml:mpadded>}\), and the best-fit stellar age for each model is shown in the upper left corner. The meanings of the symbols are the same as those in Fig. 2.

Extended Data Fig. 5 Schematic overview of the SFHs of our two-components models.

The red and blue rectangles show the old and young stellar components with constant SFRs, respectively. The old component stops its star formation activity after a fixed duration, τ. The black vertical dashed line indicates the observation at z = 9.1 (Universe age of ~550 Myr). Each component is described using age and SFR parameters. For simplicity, both components have a common dust attenuation, Av, and metallicity, Z.

Extended Data Fig. 6 Comparisons of constant SFH models and observational constraints.

ac, \({\chi }_{\nu }^{<mml:mpadded xmlns:xlink="http://www.w3.org/1999/xlink" lspace="-.15em">2</mml:mpadded>}\) (a), IRAC colour (b) and dust emission (c), plotted against stellar age. All model grids are shown with grey dots, and the best-fit models at given stellar ages are indicated with red circles. In b, the black horizontal dashed line indicates the observed value and the yellow shaded region its 1σ uncertainty. In c, the black horizontal dashed line refers to the 2σ upper limit. df, Best-fit SEDs at ages of 1 Myr, 10 Myr and 100 Myr indicated by the blue squares in a. The insets show the flux density of the dust continuum (in μJy) and the [O iii] 88-μm flux (in 10−18 erg cm−2 s−1). In d we demonstrate that a strong nebular continuum plus [O ii] 3,727-Å emission counteracts intense Hβ plus [O iii] 4,959-Å emission, producing an ‘inverse Balmer break’ for very young metal-poor cases.

Extended Data Fig. 7 Evolution of the ultraviolet luminosity of MACS1149-JD1 as a function of redshift.

For each redshift bin (Δz = 1), we extrapolated the magnitude by assuming a constant SFR over the redshift interval (blue curve). We over-plotted the sensitivity of the NIRCam filters (pink and grey) covering the 1,500-Å rest frame (10σ in ~20 min) and the NIRSpec sensitivity (dashed black line) at the same wavelength (10σ in 3 h).

Extended Data Table 1 Upper limits on the infrared luminosity and dust mass
Extended Data Table 2 Summary of our SED parameters
Extended Data Table 3 Summary of SED fit results of our fiducial model

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Hashimoto, T., Laporte, N., Mawatari, K. et al. The onset of star formation 250 million years after the Big Bang. Nature 557, 392–395 (2018). https://doi.org/10.1038/s41586-018-0117-z

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