Skip to main content

Thank you for visiting nature.com. You are using a browser version with limited support for CSS. To obtain the best experience, we recommend you use a more up to date browser (or turn off compatibility mode in Internet Explorer). In the meantime, to ensure continued support, we are displaying the site without styles and JavaScript.

  • Letter
  • Published:

The gravitationally unstable gas disk of a starburst galaxy 12 billion years ago

Abstract

Galaxies in the early Universe that are bright at submillimetre wavelengths (submillimetre-bright galaxies) are forming stars at a rate roughly 1,000 times higher than the Milky Way. A large fraction of the new stars form in the central kiloparsec of the galaxy1,2,3, a region that is comparable in size to the massive, quiescent galaxies found at the peak of cosmic star-formation history4 and the cores of present-day giant elliptical galaxies. The physical and kinematic properties inside these compact starburst cores are poorly understood because probing them at relevant spatial scales requires extremely high angular resolution. Here we report observations with a linear resolution of 550 parsecs of gas and dust in an unlensed, submillimetre-bright galaxy at a redshift of z = 4.3, when the Universe was less than two billion years old. We resolve the spatial and kinematic structure of the molecular gas inside the heavily dust-obscured core and show that the underlying gas disk is clumpy and rotationally supported (that is, its rotation velocity is larger than the velocity dispersion). Our analysis of the molecular gas mass per unit area suggests that the starburst disk is gravitationally unstable, which implies that the self-gravity of the gas is stronger than the differential rotation of the disk and the internal pressure due to stellar-radiation feedback. As a result of the gravitational instability in the disk, the molecular gas would be consumed by star formation on a timescale of 100 million years, which is comparable to gas depletion times in merging starburst galaxies5.

This is a preview of subscription content, access via your institution

Access options

Buy this article

USD 39.95

Prices may be subject to local taxes which are calculated during checkout

Fig. 1: CO morphology and kinematics of AzTEC-1.
Fig. 2: Spectra and maps of the two large clumps.
Fig. 3: Radially averaged Toomre Q parameter.
Fig. 4: Pixel-to-pixel variations in the physical properties.

Similar content being viewed by others

References

  1. Swinbank, A. M. et al. Intense star formation within resolved compact regions in a galaxy at z = 2.3. Nature 464, 733–736 (2010).

    ArticleĀ  ADSĀ  PubMedĀ  CASĀ  Google ScholarĀ 

  2. Ikarashi, S. et al. Compact starbursts in z ~ 3–6 submillimeter galaxies revealed by ALMA. Astrophys. J. 810, 133 (2015).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  3. Simpson, J. M. et al. The SCUBA-2 cosmology legacy survey: ALMA resolves the rest-frame far-infrared emission of sub-millimeter galaxies. Astrophys. J. 799, 81 (2015).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  4. van Dokkum, P. et al. Forming compact massive galaxies. Astrophys. J. 813, 23 (2015).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  5. Kennicutt, R. C. Jr. The global Schmidt law in star-forming galaxies. Astrophys. J. 498, 541–552 (1998).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  6. Hughes, D. H. et al. High-redshift star formation in the Hubble Deep Field revealed by a submillimetre-wavelength survey. Nature 394, 241–247 (1998).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  7. Barger, A. J. et al. Submillimetre-wavelength detection of dusty star-forming galaxies at high redshift. Nature 394, 248–251 (1998).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  8. Chapman, S. C. et al. A redshift survey of the submillimeter galaxy population. Astrophys. J. 622, 772–796 (2005).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  9. Bothwell, M. S. et al. A survey of molecular gas in luminous sub-millimetre galaxies. Mon. Not. R. Astron. Soc. 429, 3047–3067 (2013).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  10. Ivison, R. J. et al. Herschel-ATLAS: a binary HyLIRG pinpointing a cluster of starbursting protoellipticals. Astrophys. J. 772, 137 (2013).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  11. Tacconi, L. J. et al. Submillimeter galaxies at z ~ 2: evidence for major mergers and constraints on lifetimes, IMF, and CO-H2 conversion factor. Astrophys. J. 680, 246–262 (2008).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

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

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  13. Iono, D. et al. Clumpy and extended starbursts in the brightest unlensed submillimeter galaxies. Astrophys. J. 829, L10 (2016).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  14. Tadaki, K.-i. et al. Bulge-forming galaxies with an extended rotating disk at z ~ 2. Astrophys. J. 834, 135 (2017).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  15. Swinbank, A. M. et al. ALMA resolves the properties of star-forming regions in a dense gas disk at z ~ 3. Astrophys. J. 806, L17 (2015).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  16. Sharda, P. et al. Testing star formation laws in a starburst galaxy at redshift 3 resolved with ALMA. Mon. Not. R. Astron. Soc. 477, 4380–4390 (2018).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  17. Bolatto, A. D. et al. The resolved properties of extragalactic giant molecular clouds. Astrophys. J. 686, 948–965 (2008).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  18. Cappellari, M. Structure and kinematics of early-type galaxies from integral field spectroscopy. Annu. Rev. Astron. Astrophys. 54, 597–665 (2016).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  19. Veale, M. et al. The MASSIVE survey – V. Spatially resolved stellar angular momentum, velocity dispersion, and higher moments of the 41 most massive local early-type galaxies. Mon. Not. R. Astron. Soc. 464, 356–384 (2017).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  20. Naab, T. et al. The ATLAS3D project – XXV. Two-dimensional kinematic analysis of simulated galaxies and the cosmological origin of fast and slow rotators. Mon. Not. R. Astron. Soc. 444, 3357–3387 (2014).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  21. Genzel, R. et al. The Sins survey of z ~ 2 galaxy kinematics: properties of the giant star-forming clumps. Astrophys. J. 733, 101 (2011).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  22. Bournaud, F. et al. The long lives of giant clumps and the birth of outflows in gas-rich galaxies at high-redshift. Astrophys. J. 780, 57–75 (2014).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  23. Mandelker, N. et al. The population of giant clumps in simulated high-z galaxies: in situ and ex situ migration and survival. Mon. Not. R. Astron. Soc. 443, 3675–3702 (2014).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  24. Genzel, R. et al. The SINS/zC-SINF survey of z ~ 2 galaxy kinematics: evidence for gravitational quenching. Astrophys. J. 785, 75 (2014).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  25. Thompson, T. et al. Radiation pressure-supported starburst disks and active galactic nucleus fueling. Astrophys. J. 630, 167–185 (2005).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  26. Cacciato, M. et al. Evolution of violent gravitational disc instability in galaxies: late stabilization by transition from gas to stellar dominance. Mon. Not. R. Astron. Soc. 421, 818–831 (2012).

    ADSĀ  Google ScholarĀ 

  27. Tacconi, L. J. et al. Phibss: molecular gas content and scaling relations in z ~ 1–3 massive, main-sequence star-forming galaxies. Astrophys. J. 768, 74 (2013).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  28. Narayanan, D. et al. The star-forming molecular gas in high-redshift submillimetre galaxies. Mon. Not. R. Astron. Soc. 400, 1919–1935 (2009).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  29. Ueda, J. et al. Cold molecular gas in merger remnants. I. Formation of molecular gas disks. Astrophys. J. Suppl. Ser. 214, 1 (2014).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

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

    ArticleĀ  ADSĀ  PubMedĀ  CASĀ  Google ScholarĀ 

  31. Scott, K. B. et al. AzTEC millimetre survey of the COSMOS field – I. Data reduction and source catalogue. Mon. Not. R. Astron. Soc. 385, 2225–2238 (2008).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  32. Yun, M. S. et al. Early science with the Large Millimeter Telescope: CO and [CĀ ii] emission in the zĀ =Ā 4.3 AzTEC J095942.9+022938 (COSMOS AzTEC-1). Mon. Not. R. Astron. Soc. 454, 3485–3499 (2015).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  33. Toft, S. et al. Submillimeter galaxies as progenitors of compact quiescent galaxies. Astrophys. J. 782, 68 (2014).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  34. Chabrier, G. The galactic disk mass function: reconciliation of the Hubble Space Telescope and nearby determinations. Astrophys. J. 586, L133–L136 (2003).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  35. McMullin, J. P., Waters, B., Schiebel, D., Young, W. & Golap, K. CASA architecture and applications. ASP Conf. Ser. 376, 127–130 (2007).

    ADSĀ  Google ScholarĀ 

  36. Smolčić, V. et al. The redshift and nature of AzTEC/COSMOS 1: a starburst galaxy at z = 4.6. Astrophys. J. 731, L27 (2011).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  37. Laigle, C. et al. The COSMOS2015 catalog: exploring the 1Ā <Ā zĀ <Ā 6 universe with half a million galaxies. Astrophys. J. Suppl. Ser. 24, 224 (2016).

    Google ScholarĀ 

  38. Roseboom, I. G. et al. The Herschel multi-tiered extragalactic survey: SPIRE-mm photometric redshifts. Mon. Not. R. Astron. Soc. 419, 2758–2773 (2012).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  39. Oliver, S. J. et al. The Herschel multi-tiered extragalactic survey: HerMES. Mon. Not. R. Astron. Soc. 424, 1614–1635 (2012).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  40. Smolčić, V. et al. The VLA-COSMOS 3 GHz large project: continuum data and source catalog release. Astron. Astrophys. 602, A1 (2017).

    ArticleĀ  CASĀ  Google ScholarĀ 

  41. da Cunha, E., Charlot, S. & Elbaz, D. A simple model to interpret the ultraviolet, optical and infrared emission from galaxies. Mon. Not. R. Astron. Soc. 388, 1595–1617 (2008).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  42. da Cunha, E. et al. An ALMA survey of sub-millimeter galaxies in the extended Chandra deep field south: physical properties derived from ultraviolet-to-radio modeling. Astrophys. J. 806, 110 (2015).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

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

    ArticleĀ  ADSĀ  Google ScholarĀ 

  44. Papadopoulos, P. P., Thi, W.-F. & Viti, S. CĀ i lines as tracers of molecular gas, and their prospects at high redshifts. Mon. Not. R. Astron. Soc. 351, 147–160 (2004).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  45. Weiß, A. et al. Gas and dust in the Cloverleaf quasar at redshift 2.5. Astron. Astrophys. 409, L41–L45 (2003).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  46. Weiß, A. et al. Atomic carbon at redshift ~2.5. Astron. Astrophys. 429, L25–L28 (2005).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  47. Danielson, A. L. R. et al. The properties of the interstellar medium within a star-forming galaxy at z = 2.3. Mon. Not. R. Astron. Soc. 410, 1687–1702 (2011).

    ADSĀ  CASĀ  Google ScholarĀ 

  48. Bothwell, M. S. et al. ALMA observations of atomic carbon in z ~ 4 dusty star-forming galaxies. Mon. Not. R. Astron. Soc. 466, 2825–2841 (2017).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  49. White, G. J. et al. CO and CĀ i maps of the starburst galaxy M 82. Astron. Astrophys. 284, L23–L26 (1994).

    ADSĀ  CASĀ  Google ScholarĀ 

  50. Wilson, C. et al. Luminous infrared galaxies with the submillimeter array. I. Survey overview and the central gas to dust ratio. Astrophys. J. Suppl. Ser. 178, 189–224 (2008).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

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

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  52. Downes, D. & Solomon, P. M. Rotating nuclear rings and extreme starbursts in ultraluminous galaxies. Astrophys. J. 507, 615–654 (1998).

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

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

    ArticleĀ  ADSĀ  CASĀ  Google ScholarĀ 

  54. Bournaud, F. et al. Modeling CO emission from hydrodynamic simulations of nearby spirals, starbursting mergers, and high-redshift galaxies. Astron. Astrophys. 575, A56 (2015).

    ArticleĀ  CASĀ  Google ScholarĀ 

  55. Bouche, N. et al. GalPak3D: a Bayesian parametric tool for extracting morphokinematics of galaxies from 3D data. Astrophys. J. 150, 92 (2015).

    Google ScholarĀ 

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

    ArticleĀ  ADSĀ  Google ScholarĀ 

  57. Wang, B. et al. Gravitational instability and disk star formation. Astrophys. J. 427, 759–769 (1994).

    ArticleĀ  ADSĀ  Google ScholarĀ 

  58. Binney, J. & Tremaine, S. Galactic Dynamics 2nd edn, 494–496 (Princeton Univ. Press, Princeton, 2008).

    MATHĀ  Google ScholarĀ 

  59. Romeo, A. B. & Wiegert, J. The effective stability parameter for two-component galactic discs: is \({Q}^{-1}\approx {Q}_{{\rm{stars}}}^{-1}+{Q}_{{\rm{gas}}}^{-1}\)? Mon. Not. R. Astron. Soc. 416, 1191–1196 (2011).

    ArticleĀ  ADSĀ  Google ScholarĀ 

Download references

Acknowledgements

We thank J. Baba for discussions about a gravitational instability in SMGs. This work was supported by JSPS KAKENHI JP17J04449. We thank the ALMA staff and in particular the EA-ARC staff for their support. This research has made use of data from ALMA and HerMES project (http://hermes.sussex.ac.uk/). ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (South Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. HerMES is a Herschel Key Programme utilizing Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. Data analysis was in part carried out on the common-use data analysis computer system at the Astronomy Data Center (ADC) of the National Astronomical Observatory of Japan.

Reviewer information

Nature thanks F. Bournaud and the other anonymous reviewer(s) for their contribution to the peer review of this work.

Author information

Authors and Affiliations

Authors

Contributions

K.T. led the project and reduced the ALMA data. K.T. and D.I. wrote the manuscript. M.S.Y. reduced the Large Millimeter Telescope data and edited the final manuscript. Other authors contributed to the interpretation and commented on the ALMA proposal and the paper.

Corresponding author

Correspondence to K. Tadaki.

Ethics declarations

Competing interests

The authors declare no competing interests.

Additional information

Publisher’s note: Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

Extended data figures and tables

Extended Data Fig. 1 Galaxy-integrated CO (4–3), CO (1–0) and C i (2–1) spectra of AzTEC-1.

The CO (4–3) spectrum is extracted using an 0.8″-diameter aperture in the natural-weighted map cube. The CĀ i (1–0) and CĀ i (2–1) spectra are extracted from the peak positions in map cubes with 1.7″ × 1.1″ and 0.8″ × 0.7″ resolution, respectively. Yellow shaded regions show the velocity range v =ā€‰āˆ’315Ā kmĀ sāˆ’1 to v = +315Ā kmĀ sāˆ’1, in which the velocity-integrated line fluxes are measured.

Extended Data Fig. 2 Galaxy-integrated SED of AzTEC-1.

Red circles show the photometric data from Subaru (r′, i′, z′)37, VISTA (Ks)37, Spitzer (3.6 μm, 4.4 μm)37, Herschel (250 μm, 350 μm, 500 μm)38,39, ALMA (860 μm, 2.1Ā mm, 3.2Ā mm) and JVLA (10Ā cm)40. The black line shows the best-fitting SED model from MAGPHYS41,42.

Extended Data Fig. 3 CO spectra along the kinematic major axis.

Spectra are extracted at a position angle of PA =ā€‰āˆ’64°. The spatial offset x from the galactic centre is shown at the upper left of each panel. Red lines indicate the spectra of the best-fitting dynamical model produced by GalPaK3D.

Extended Data Fig. 4 Full MCMC chain for 20,000 iterations.

Red solid lines and black dashed lines indicate the median and 95% confidence interval of the last 60% of the MCMC chain.

Extended Data Table 1 Line fluxes in AzTEC-1

Rights and permissions

Reprints and permissions

About this article

Check for updates. Verify currency and authenticity via CrossMark

Cite this article

Tadaki, K., Iono, D., Yun, M.S. et al. The gravitationally unstable gas disk of a starburst galaxy 12 billion years ago. Nature 560, 613–616 (2018). https://doi.org/10.1038/s41586-018-0443-1

Download citation

  • Received:

  • Accepted:

  • Published:

  • Version of record:

  • Issue date:

  • DOI: https://doi.org/10.1038/s41586-018-0443-1

This article is cited by

Comments

Commenting on this article is now closed.

  1. As Einstein's relativity and the Big Bang theory have been disproved, the discovery of this paper gives us a completely new idea about the age of the universe. For 12 billion years, the light of the galaxy has just reached the earth. If the universe then were at the age of 1.8 billion years and it kept expanding in a fixed acceleration from its birth to now, the distance between the earth and the galaxy should be ignorable at that time. The fact that the light has caught the earth now means that the current speed of the earth leaving the location of the galaxy at 12 billion years ago is still smaller than the speed of light. Then the speed of the earth 12 billion years ago leaving the location of the galaxy at 12 billion years ago should be much much smaller than the speed of light. Thus, how could the light needed 12 billion years to catch such a slow moving earth in an ignorable distance? It is obvious a contradiction which tells us that the distance between the earth and the galaxy at 12 billion years ago was not ignorable, but close to 12 billion light years, as the move of the earth during the 12 billion year period is ignorable compared with the distance the light has traveled. As the universe already had such a large size at that moment, the age of the universe then should not be 1.8 billion years old, but much older.

    Therefore, the age of the universe now should be much older than 13.8 billion years.

  2. Good question showing a major flaw of GR based time concept, also shared by some basic mistakes of traditional QM foundations such as Planck energy constant that actually includes the variable speed C4 of the decelerating expansion of Riemann 4-radius R4. The speed of light C along the 3-D space direction orthogonal to R4 direction is closely coupled to the dynamic contraction/expansion speed C4 such that the balance of the motion and gravitational energies of total mass M in universe is continually preserved. The ticking rate of atomic clocks and other processes (such as decay rate) at small values of R4 such as 1.8B l.y was close to 1,000 times higher than today such that in terms of today's definition of 'prolonged' second the GR based age 13.8 B yrs reduces to 9.2B yrs. This explains the fast star formation process of the ALMA observed disk while also revealing some 5-10 other blunders of GR/QM based postulates, including the 'epicycle mistakes' of Dark Energy/Matter, GW etc. See the books and papers of 'Suntola Dynamic Universe' bounce (vs BB) theory since 1995, collected today at PFS web site for open view.

    Also note the 'cosmic entanglement' principle of DU where the motion of any mass object, such as Earth from its birth to today, has been continually interconnected (in a 'pipeline' fashion) to the gravitational states of ALL other mass objects of universe, acting as its 'anti-matter counterpart'. The same principle applies to binary star/NS/BH pairs during millions/billions of years before their local merge event - no or little unbalanced energy left to cause the GR postulated emission of GW for detection at the global optical or 'gravitational' distance of over 100 M years. See DU explanation of the 'indirect GR proof of GW' granted Nobel award in 1990's and paving the funding of LIGO related developments, unaware of the more general digital software/hardware developments of array algebra in digital photogrammetry and geodesy since 1975. The learned lessons of both DE/DM, GW and related automated multi-ray stereo image matching and range sensing/ultra-accurate time keeping technologies of array calculus are valuable for the new technologies of cosmic mapping projects. WFIRST and Gaia/Hubble efforts are partially wasted as they were inspired by the 2011 and 2017 Nobel 'confirmations' of GR based DE and GW mistakes.

Search

Quick links

Nature Briefing

Sign up for the Nature Briefing newsletter — what matters in science, free to your inbox daily.

Get the most important science stories of the day, free in your inbox. Sign up for Nature Briefing