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A cold, massive, rotating disk galaxy 1.5 billion years after the Big Bang

Nature volume 581, pages 269–272 (2020)Cite this article

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Abstract

Massive disk galaxies like the Milky Way are expected to form at late times in traditional models of galaxy formation1,2, but recent numerical simulations suggest that such galaxies could form as early as a billion years after the Big Bang through the accretion of cold material and mergers3,4. Observationally, it has been difficult to identify disk galaxies in emission at high redshift5,6 in order to discern between competing models of galaxy formation. Here we report imaging, with a resolution of about 1.3 kiloparsecs, of the 158-micrometre emission line from singly ionized carbon, the far-infrared dust continuum and the near-ultraviolet continuum emission from a galaxy at a redshift of 4.2603, identified by detecting its absorption of quasar light. These observations show that the emission arises from gas inside a cold, dusty, rotating disk with a rotational velocity of about 272 kilometres per second. The detection of emission from carbon monoxide in the galaxy yields a molecular mass that is consistent with the estimate from the ionized carbon emission of about 72 billion solar masses. The existence of such a massive, rotationally supported, cold disk galaxy when the Universe was only 1.5 billion years old favours formation through either cold-mode accretion or mergers, although its large rotational velocity and large content of cold gas remain challenging to reproduce with most numerical simulations7,8.

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Fig. 1: Mean velocity field and p–v diagram for DLA0817g.
Fig. 2: Comparison between the data and the model for DLA0817g.
Fig. 3: Rotation curve for DLA0817g.
Fig. 4: HST imaging of DLA0817g with CO, [C ii] and dust continuum contours.

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Data availability

The data reported in this paper are available though the ALMA archive:(http://almascience.eso.org/aq/) with project code 2017.1.01052.S, the JVLA archive:(https://science.nrao.edu/facilities/vla/archive/index) with project code 17A-279, and the HST/Mikulski Archive for Space Telescopes: (https://archive.stsci.edu/hst/) with project code 15410.

Code availability

All of the code used to generate the kinematic modelling is available online at (https://github.com/mneeleman/qubefit).

References

  1. Rees, M. J. & Ostriker, J. P. Cooling, dynamics and fragmentation of massive gas clouds: clues to the masses and radii of galaxies and clusters. Mon. Not. R. Astron. Soc. 179, 541–559 (1977).

    Article  ADS  CAS  Google Scholar 

  2. Fall, S. M. & Efstathiou, G. Formation and rotation of disc galaxies with haloes. Mon. Not. R. Astron. Soc. 193, 189–206 (1980).

    Article  ADS  Google Scholar 

  3. Kereš, D., Katz, N., Weinberg, D. H. & Davé, R. How do galaxies get their gas? Mon. Not. R. Astron. Soc. 363, 2–28 (2005).

    Article  ADS  CAS  Google Scholar 

  4. Dekel, A. et al. Cold streams in early massive hot haloes as the main mode of galaxy formation. Nature 457, 451–454 (2009).

    Article  ADS  CAS  PubMed  Google Scholar 

  5. Hodge, J. A. et al. Evidence for a clumpy, rotating gas disk in a submillimeter galaxy at z = 4. Astrophys. J. 760, 11 (2012).

    Article  ADS  CAS  Google Scholar 

  6. Smit, R. et al. Rotation in [C ii]-emitting gas in two galaxies at a redshift of 6.8. Nature 553, 178–181 (2018).

    Article  ADS  CAS  PubMed  Google Scholar 

  7. Grand, R. J. J. et al. The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time. Mon. Not. R. Astron. Soc. 467, 179–207 (2017).

    ADS  CAS  Google Scholar 

  8. Pillepich, A. et al. First results from the TNG50 simulation: the evolution of stellar and gaseous disks across cosmic time. Mon. Not. R. Astron. Soc. 490, 3196–3233 (2019).

    Article  ADS  Google Scholar 

  9. Ade, P. A. R. et al. (Planck Collaboration) Planck 2015 results. XIII. Cosmological parameters. Astron. Astrophys. 594, A13 (2016).

    Article  CAS  Google Scholar 

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

    Article  ADS  CAS  Google Scholar 

  11. Price, S. H. et al. The MOSDEF Survey: dynamical and baryonic masses and kinematic structures of star-forming galaxies at 1.4 ≤ z ≤ 2.6. Astrophys. J. 819, 80 (2016).

    Article  ADS  Google Scholar 

  12. Genzel, R. et al. Strongly baryon-dominated disk galaxies at the peak of galaxy formation ten billion years ago. Nature 543, 397–401 (2017).

    Article  ADS  CAS  PubMed  Google Scholar 

  13. Neeleman, M. et al. [C ii] 158-μm emission from the host galaxies of damped Lyman-alpha systems. Science 355, 1285–1288 (2017).

    Article  ADS  CAS  PubMed  Google Scholar 

  14. Neeleman, M., Kanekar, N., Prochaska, J. X., Rafelski, M. A. & Carilli, C. L. [C ii] 158-μm emission from z ~ 4 H i absorption-selected galaxies. Astrophys. J. 870, L19 (2019).

    Article  ADS  CAS  Google Scholar 

  15. de Blok, W. J. G. et al. High-resolution rotation curves and galaxy mass models from THINGS. Astron. J. 136, 2648–2719 (2008).

    Article  ADS  CAS  Google Scholar 

  16. Burkert, A. et al. High-redshift star-forming galaxies: angular momentum and baryon fraction, turbulent pressure effects, and the origin of turbulence. Astrophys. J. 725, 2324–2332 (2010).

    Article  ADS  CAS  Google Scholar 

  17. Toomre, A. On the gravitational stability of a disk of stars. Astrophys. J. 139, 1217–1238 (1964).

    Article  ADS  Google Scholar 

  18. Goldreich, P. & Lynden-Bell, D. I. Gravitational stability of uniformly rotating disks. Mon. Not. R. Astron. Soc. 130, 97 (1965).

    Article  ADS  Google Scholar 

  19. Elmegreen, B. G., Bournaud, F. & Elmegreen, D. M. Bulge formation by the coalescence of giant clumps in primordial disk galaxies. Astrophys. J. 688, 67–77 (2008).

    Article  ADS  CAS  Google Scholar 

  20. Beuther, H. et al. Carbon in different phases ([C ii], [C i], and CO) in infrared dark clouds: cloud formation signatures and carbon gas fractions. Astron. Astrophys. 571, A53 (2014).

    Article  CAS  Google Scholar 

  21. Riechers, D. A. et al. A dust-obscured massive maximum-starburst galaxy at a redshift of 6.34. Nature 496, 329–333 (2013).

    Article  ADS  CAS  PubMed  Google Scholar 

  22. de Blok, W. J. G. et al. Comparing [C ii], H i, and CO dynamics of nearby galaxies. Astron. J. 152, 51 (2016).

    Article  ADS  CAS  Google Scholar 

  23. Croxall, K. V. et al. The origins of [C ii] emission in local star-forming galaxies. Astrophys. J. 845, 96 (2017).

    Article  ADS  CAS  Google Scholar 

  24. Cormier, D. et al. The Herschel Dwarf Galaxy Survey. II. Physical conditions, origin of [C ii] emission, and porosity of the multiphase low-metallicity ISM. Astron. Astrophys. 626, A23 (2019).

    Article  CAS  Google Scholar 

  25. Carilli, C. L. & Walter, F. Cool gas in high-redshift galaxies. Annu. Rev. Astron. Astrophys. 51, 105–161 (2013).

    Article  ADS  CAS  Google Scholar 

  26. Gullberg, B. et al. The dust and [C ii] morphologies of redshift ~4.5 sub-millimeter galaxies at ~200 pc resolution: the absence of large clumps in the interstellar medium at high-redshift. Astrophys. J. 859, 12 (2018).

    Article  ADS  CAS  Google Scholar 

  27. Jones, M. G., Haynes, M. P., Giovanelli, R. & Moorman, C. The ALFALFA H i mass function: a dichotomy in the low-mass slope and a locally suppressed ‘knee’ mass. Mon. Not. R. Astron. Soc. 477, 2–17 (2018).

    Article  ADS  CAS  Google Scholar 

  28. McMullin, J. P., Waters, B., Schiebel, D., Young, W. & Golap, K. CASA architecture and applications. In Astronomical Data Analysis Software and Systems XVI Vol. 376 (eds Shaw, R. A. et al.) 127 (2007).

  29. Brown, A. G. A. et al. (Gaia Collaboration) Gaia Data Release 2. Summary of the contents and survey properties. Astron. Astrophys. 616, A1 (2018).

    Article  Google Scholar 

  30. Bertin, E. & Arnouts, S. SExtractor: software for source extraction. Astron. Astrophys. Suppl. 117, 393–404 (1996).

    ADS  Google Scholar 

  31. Kron, R. G. Photometry of a complete sample of faint galaxies. Astrophys. J. Suppl. 43, 305–325 (1980).

    Article  ADS  Google Scholar 

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

    Article  ADS  CAS  Google Scholar 

  33. Calzetti, D. et al. The calibration of monochromatic far-infrared star formation rate indicators. Astrophys. J. 714, 1256–1279 (2010).

    Article  ADS  Google Scholar 

  34. Lonsdale Persson, C. J. & Helou, G. On the origin of the 40–120 micron emission of galaxy disks: a comparison with Hα fluxes. Astrophys. J. 314, 513–524 (1987).

    Article  ADS  Google Scholar 

  35. Kennicutt, R. C. & Evans, N. J. Star formation in the Milky Way and nearby galaxies. Annu. Rev. Astron. Astrophys. 50, 531–608 (2012).

    Article  ADS  CAS  Google Scholar 

  36. De Looze, I. et al. The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types. Astron. Astrophys. 568, A62 (2014).

    Article  CAS  Google Scholar 

  37. Herrera-Camus, R. et al. [C ii] 158-μm emission as a star formation tracer. Astrophys. J. 800, 1 (2015).

    Article  ADS  CAS  Google Scholar 

  38. Dessauges-Zavadsky, M. et al. Molecular gas content in strongly lensed z ~ 1.5–3 star-forming galaxies with low infrared luminosities. Astron. Astrophys. 577, A50 (2015).

    Article  CAS  Google Scholar 

  39. Bolatto, A. D., Wolfire, M. & Leroy, A. K. The CO-to-H2 conversion factor. Annu. Rev. Astron. Astrophys. 51, 207–268 (2013).

    Article  ADS  CAS  Google Scholar 

  40. Daddi, E. et al. Very high gas fractions and extended gas reservoirs in z = 1.5 disk galaxies. Astrophys. J. 713, 686–707 (2010).

    Article  ADS  CAS  Google Scholar 

  41. Scoville, N. et al. The evolution of interstellar medium mass probed by dust emission: ALMA observations at z = 0.3–2. Astrophys. J. 783, 84 (2014).

    Article  ADS  Google Scholar 

  42. Zanella, A. et al. The [C ii] emission as a molecular gas mass tracer in galaxies at low and high redshifts. Mon. Not. R. Astron. Soc. 481, 1976–1999 (2018).

    Article  ADS  CAS  Google Scholar 

  43. Bañados, E. et al. The z = 7.54 quasar ULAS J1342+0928 is hosted by a galaxy merger. Astrophys. J. 881, L23 (2019).

    Article  ADS  CAS  Google Scholar 

  44. Neeleman, M. et al. Resolved [C ii] emission from z ~ 6 quasar host-companion galaxy pairs. Astrophys. J. 882, 10 (2019).

    Article  ADS  CAS  Google Scholar 

  45. Venemans, B. P. et al. 400 pc imaging of a massive quasar host galaxy at a redshift of 6.6. Astrophys. J. 874, L30 (2019).

    Article  ADS  CAS  Google Scholar 

  46. Bird, J. C. et al. Inside out and upside down: tracing the assembly of a simulated disk galaxy using mono-age stellar populations. Astrophys. J. 773, 43 (2013).

    Article  ADS  Google Scholar 

  47. Simons, R. C. et al. z ~ 2: an epoch of disk assembly. Astrophys. J. 843, 46 (2017).

    Article  ADS  CAS  Google Scholar 

  48. Di Teodoro, E. M. & Fraternali, F. 3DBAROLO: a new 3D algorithm to derive rotation curves of galaxies. Mon. Not. R. Astron. Soc. 451, 3021–3033 (2015).

    Article  ADS  CAS  Google Scholar 

  49. Wang, R. et al. Star formation and gas kinematics of quasar host galaxies at z ~ 6: new insights from ALMA. Astrophys. J. 773, 44 (2013).

    Article  ADS  CAS  Google Scholar 

  50. Walter, F., Brinks, E., Duric, N. & Klein, U. A dynamical analysis of the H ii galaxy ii Zwicky 33 and its low surface brightness companion. Astron. J. 113, 2031–2045 (1997).

    Article  ADS  CAS  Google Scholar 

  51. Ho, L. C. The CO Tully–Fisher relation and implications for the host galaxies of high-redshift quasars. Astrophys. J. 669, 821–829 (2007).

    Article  ADS  CAS  Google Scholar 

  52. Decarli, R. et al. An ALMA [C ii] survey of 27 quasars at z > 5.94. Astrophys. J. 854, 97 (2018).

    Article  ADS  CAS  Google Scholar 

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Acknowledgements

This work would not have been possible without the insights of the late A. M. Wolfe. M.N. thanks F. Walter for discussions, and S. Simha for extracting effective radii from the HST and ALMA imaging. ALMA is a partnership of the European Southern Observatory (ESO; representing its member states), the National Science Foundation (NSF; United States) and the National Institutes of Natural Sciences (Japan), together with the National Research Council (Canada), the National Science Council and the Academia Sinica Institute of Astronomy and Astrophysics (Taiwan), and the Korean Astronomy and Space Science Institute (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities Incorporated (AUI) National Radio Astronomy Observatory (NRAO) and the National Astronomical Observatory of Japan. NRAO is a facility of the NSF operated under cooperative agreement by AUI. M.N. acknowledges support from the European Research Council advanced grant 740246 (Cosmic_Gas). N.K. acknowledges support from the Department of Science and Technology via a Swarnajayanti Fellowship (DST/SJF/PSA-01/2012-13), and from the Department of Atomic Energy under project 12-R&D-TFR-5.02-0700. Support for programme no. 15410 was provided by the National Aeronautics and Space Administration (NASA) through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy Incorporated, under NASA contract NAS 5-26555.

Author information

Authors and Affiliations

  1. Max-Planck-Institut für Astronomie, Heidelberg, Germany

    Marcel Neeleman

  2. Department of Astronomy and Astrophysics, UCO/Lick Observatory, University of California, Santa Cruz, CA, USA

    J. Xavier Prochaska

  3. Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU), The University of Tokyo, Kashiwa, Japan

    J. Xavier Prochaska

  4. National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University, Pune, India

    Nissim Kanekar

  5. Space Telescope Science Institute, Baltimore, MD, USA

    Marc Rafelski

  6. Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA

    Marc Rafelski

Authors
  1. Marcel Neeleman
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  2. J. Xavier Prochaska
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  4. Marc Rafelski
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Contributions

M.N. is the PI of the observing programmes. M.N. and N.K. contributed to the analysis of the ALMA and JVLA data. M.R. reduced and analysed the HST data. All authors contributed to analysis of the data and writing and editing of the manuscript.

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Correspondence to Marcel Neeleman.

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Peer review information Nature thanks Robert Grand and Alfred Tiley for their contribution to the peer review of this work.

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Extended data figures and tables

Extended Data Fig. 1 Spectrum of the [C ii] line from DLA0817g.

The velocity is relative to the systemic velocity of the [C ii] line. The velocity range used to estimate the velocity-integrated [C ii] flux density and the integrated [C ii] contours is marked by the solid black bar. The 1σ (standard deviation) uncertainty of the measurements is indicated by the dotted red lines, and has been estimated by bootstrapping flux density measurements at random positions within each channel chosen to be devoid of any line emission. A double Gaussian model fit to the data is shown in green. Both the peak flux density of 16.8 ± 1.3 mJy and the velocity-integrated [C ii] line flux density of 5.8 ± 0.4 Jy km s−1 are consistent with values obtained from the lower-resolution data, indicating that no emission is resolved out by the higher-resolution observations.

Extended Data Fig. 2 Channel maps of the [C ii] emission line from DLA0817g.

The plus symbol indicates the central position of the [C ii] emission derived from the kinematic analysis. This agrees within the uncertainties with the position derived from fitting a 2D-Gaussian profile to both the velocity-integrated [C ii] emission and the far-infrared continuum emission, using the imfit routine in CASA (Extended Data Table 1). The outer black contour is 3σ, where σ = 0.35 mJy per beam, with subsequent contours increasing in powers of \(\sqrt{2}\). Velocities are relative to the kinematically derived [C ii] redshift, z = 4.2603. The synthesized beam is shown in the bottom left corner of the bottom left panel.

Extended Data Fig. 3 Channel maps of the residuals, after subtracting the model from the data, of the [C ii] emission from DLA0817g.

The colour scaling, contour levels and annotations are the same as Extended Data Fig. 2. Little excess emission (at >3σ significance) is seen in the individual 25 km s−1 channels, indicating that the exponential thin disk model is a good approximation for the bulk of the [C ii] emission. Only two features are seen in the channel maps with >3σ emission in two or more consecutive channels: 2.8 kpc south of the centre at 88 km s−1 and 113 km s−1, and 3 kpc east of the centre at 113 km s−1, 138 km s−1 and 163 km s−1. This emission arises from clumps that are not rotating with the bulk of the gas, possibly arising in outflows or satellite galaxies.

Extended Data Fig. 4 Position–velocity diagram for DLA0817g.

a, The p–v diagram along the major axis of DLA0817g. b, The p–v diagram along the minor axis. The contours in both panels are the p–v diagrams derived from the rotating disk model with constant velocity. The outer contour is 2σ where σ = 0.35 mJy per beam, and the contours increase in powers of \(\sqrt{2}\). Distances are given with respect to the kinematic centre of the emission (Fig. 1).

Extended Data Fig. 5 Velocity dispersion profile for DLA0817g.

The observed velocity dispersion profile is measured from the standard deviation of a Gaussian fit to each pixel, and is shown by the data points where the data have been binned into bins equal to the size of the horizontal error bars. The vertical error bars reflect the 16 to 84 percentile spread in measurements per bin. The radius has been de-projected for the inclination of DLA0817g. The dashed line is the value derived from the kinematic modelling. The solid coloured region is the 16 to 84 percentile spread in the constant velocity dispersion model, showing that the increase in velocity dispersion at the galactic centre is due to beam-smearing.

Extended Data Fig. 6 Light profile for dust continuum, [C ii] line and UV emission.

The light profiles are scaled by the emission at the kinematic centre. Distances from the kinematic centre are de-projected, taking into account the inclination of the disk. Both the dust continuum and the [C ii] emission are convolved with a Gaussian kernel to the slightly worse resolution of the UV observations. This increases the width of the surface density profile by about 10%. Vertical error bars give the 16 to 84 percentile range in the measurements within the bins defined by the horizontal error bars. The [C ii] surface density profile, the dust continuum profile and the UV surface density profile—within the uncertainties—are consistent with each other. This can also be seen by the effective radii (marked by solid vertical lines), whose 1σ uncertainties (marked by the vertical coloured regions) overlap at a value of approximately 3 kpc.

Extended Data Fig. 7 The Toomre-Q parameter for DLA0817g.

a, The spatial distribution of the Toomre-Q parameter, assuming that the gas density is traced by the [C ii] emission. This spatial distribution is still convolved with the ALMA synthesized beam. Over the entire disk, Q is roughly constant and below 1, indicating that the disk is unstable against axisymmetric perturbations. The white cross shows the kinematic centre of the emission, and the inset shows the ALMA beam for the [C ii] emission. b, The radial profile of the Toomre-Q parameter. The solid dark line shows Q, assuming that the gas density falls off exponentially, at the same rate as the [C ii] emission. The coloured squares are the observed data, as in a, corrected for the projected radius. This panel shows that the observed data underestimate Q at large radii owing to beam smearing, which increases the emission, and thus the gas surface density.

Extended Data Table 1 Physical properties of DLA0817g
Full size table
Extended Data Table 2 Results from the kinematic analysis of DLA0817g
Full size table

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Neeleman, M., Prochaska, J.X., Kanekar, N. et al. A cold, massive, rotating disk galaxy 1.5 billion years after the Big Bang. Nature 581, 269–272 (2020). https://doi.org/10.1038/s41586-020-2276-y

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