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Home , Faint blue galaxy, HFLS3, Markarian 231

A Dust-Obscured Massive Maximum-Starburst at a of 6.34

Dominik A. Riechers1,2, C.M. Bradford1,3, D.L. Clements4, C.D. Dowell1,3, I. Pérez-Fournon5,6, R.J. Ivison7,8, C. Bridge1, A. Conley9, Hai Fu10, J.D. Vieira1, J. Wardlow10, J. Calanog10, A. Cooray10,1, P. Hurley11, R. Neri12, J. Kamenetzky13, J.E. Aguirre14, B. Altieri15, V. Arumugam8, D.J. Benford16, M. Béthermin17,18, J. Bock1,3, D. Burgarella19, A. Cabrera-Lavers5,6,20, S.C. Chapman21, P. Cox12, J.S. Dunlop8, L. Earle9, D. Farrah22, P. Ferrero5,6, A. Franceschini23, R. Gavazzi24, J. Glenn13,9, E.A. Gonzalez Solares21, M.A. Gurwell25, M. Halpern26, E. Hatziminaoglou27, A. Hyde4, E. Ibar7, A. Kovács1,28, M. Krips12, R.E. Lupu14, P.R. Maloney9, P. Martinez-Navajas5,6, H. Matsuhara29, E.J. Murphy1,30, B.J. Naylor3, H.T. Nguyen3,1, S.J. Oliver11, A. Omont24, M.J. Page31, G. Petitpas25, N. Rangwala13, I.G. Roseboom11,8, D. Scott26, A.J. Smith11, J.G. Staguhn16,32, A. Streblyanska5,6, A.P. Thomson8, I. Valtchanov15, M. Viero1, L. Wang11, M. Zemcov1,3, J. Zmuidzinas1,3

1California Institute of Technology, 1200 East California Blvd., MC 249-17, Pasadena, CA 91125, USA 2Cornell University, 220 Space Sciences Building, Ithaca, NY 14853, USA 3Jet Propulsion Laboratory, 4800 Oak Grove Drive, Pasadena, CA 91109, USA 4Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 5Instituto de Astrofisica de Canarias, E-38200 La Laguna, Tenerife, Spain 6Departamento de Astrofisica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 7UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK 8Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK 9Center for and Space Astronomy 389-UCB, University of Colorado, Boulder, CO 80309, USA 10Dept. of Physics & Astronomy, University of California, Irvine, CA 92697, USA 11Astronomy Centre, Dept. of Physics & Astronomy, University of Sussex, Brighton BN1 9QH, UK 12Institut de RadioAstronomie Millimetrique, 300 Rue de la Piscine, Domaine Universitaire, F-38406 Saint Martin d’Heres, France 13Dept. of Astrophysical and Planetary Sciences, CASA 389-UCB, University of Colorado, Boulder, CO 80309, USA 14Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USA 15Herschel Science Centre, European Space Astronomy Centre, Villanueva de la Cañada, 28691 Madrid, Spain 16Observational Cosmology Lab, Code 665, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 17Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu - CNRS - Universite Paris Diderot, CEA-Saclay, point courrier 131, F-91191 Gif-sur-Yvette, France 18Institut d’Astrophysique Spatiale (IAS), batiment 121, Universite Paris-Sud 11 and CNRS, UMR 8617, F-91405 Orsay, France 19Aix-Marseille Universite, CNRS, Laboratoire d’Astrophysique de Marseille, UMR7326, F-13388 Marseille, France 20Grantecan S.A., Centro de Astrofisica de La Palma, Cuesta de San Jose, E-38712 Brena Baja, La Palma, Spain 21Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 22Department of Physics, Virginia Tech, Blacksburg, VA 24061, USA 23Dipartimento di Fisica e Astronomia, Universita di Padova, vicolo Osservatorio, 3, I-35122 Padova, Italy 24Institut d’Astrophysique de Paris, UMR 7095, CNRS, UPMC Univ. Paris 06, 98bis boulevard Arago, F-75014 Paris, France 25Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 26Department of Physics & Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, BC V6T 1Z1, Canada 27ESO, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, Germany 28Institute for Astrophysics, University of Minnesota, 116 Church Street SE, Minneapolis, MN 55455, USA 29Institute for Space and Astronautical Science, Japan Aerospace and Exploration Agency, Sagamihara, Kanagawa 229-8510, Japan 30Infrared Processing and Analysis Center, MS 100-22, California Institute of Technology, Pasadena, CA 91125, USA 31Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK 32Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, 21218, USA

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 1 Massive present-day early-type (elliptical and scans of the 3-mm and 1-mm bands toward lenticular) probably gained the bulk HFLS3 (also known as 1HERMES S350 of their stellar mass and heavy elements J170647.8+584623; S500µm/S350µm = 1.45), the through intense, dust-enshrouded starbursts brightest candidate discovered in our study. – that is, increased rates of formation – in These observations, augmented by selected the most massive dark matter halos at early follow-up over a broader wavelength range, epochs. However, it remains unknown how unambiguously determine the galaxy redshift to soon after the such massive be z=6.3369+/-0.0009 based on a suite of 7 CO + + starburst progenitors exist. The measured lines, 7 H2O lines, and OH, OH , H2O , NH3, [CI], redshift (z) distribution of dusty, massive and [CII] lines detected in emission and starbursts has long been suspected to be absorption (Figure 1). At this redshift, the biased low in redshift owing to selection Universe was just 880 million years old (or 1/16th effects,1 as confirmed by recent findings of of its present age), and 1” on the sky corresponds systems out to redshift z~5.2,3,4 Here we report to a physical scale of 5.6 kpc. Further the identification of a massive starburst observations from optical to radio wavelengths galaxy at redshift 6.34 through a submillimeter reveal strong continuum emission over virtually color-selection technique. We unambiguously the entire wavelength range between 2.2 µm and determined the redshift from a suite of 20 cm, with no detected emission shortward of molecular and atomic fine structure cooling 1 µm (see Supplementary Information Section 2 lines. These measurements reveal a hundred and Figures S1-S11 for additional details). billion solar masses of highly excited, chemically evolved (ISM) HFLS3 hosts an intense starburst. The 870 µm - in this galaxy, which constitutes at least 40% flux of HFLS3 is >3.5 times higher than those of of the baryonic mass. A "maximum starburst" the brightest high-redshift starbursts in a 0.25-deg2 region containing the Hubble Ultra converts the gas into at a rate more than 8 2,000 times that of the , a rate Deep Field (HUDF). From the continuum spectral among the highest observed at any epoch. energy distribution (Fig. 2), we find that the far- (FIR) luminosity LFIR and inferred star Despite the overall downturn of cosmic star -1 formation towards the highest ,5 it formation rate (SFR) of 2,900 Msunyr of HFLS3 seems that environments mature enough to are 15-20 times those of the prototypical local form the most massive, intense starbursts ultra-luminous starburst Arp 220, and >2,000 existed at least as early as 880 million years times those of the Milky Way (Table 1 and after the Big Bang. Supplementary Information Section 3). The SFR of HFLS3 alone corresponds to ~4.5 times the We have searched 21 deg2 of the -based SFR of all z=5.5-6.5 star-forming Herschel/SPIRE data of the HerMES blank field galaxies in the HUDF combined,9 but the rarity survey6 at 250 – 500 µ m for “ultra-red” sources and dust obscuration of ultra-red sources like with flux densities S250µm < S350µm < S500µm and HFLS3 implies that they do not dominate the UV 10 S500µm/S350µm>1.3, i.e., galaxies that are photon density needed to reionize the universe. significantly redder (and thus, potentially at higher redshift) than massive starbursts discovered thus HFLS3 is a massive, gas-rich galaxy. From the far. This selection yields five candidate ultra-red spectral energy distribution and the intensity of sources down to a flux limit of 30 mJy at 500 µm the CO and [CII] emission, we find a dust mass of 9 Md=1.3 x 10 Msun and total molecular and atomic (>5σ and above the confusion noise; see 11 gas masses of Mgas=1.0 x 10 Msun and Supplementary Information Section 1 for 10 additional details), corresponding to a source MHI=2.0 x 10 Msun. These masses are 15-20 density of ≤0.24 deg-2. For comparison, models of times those of Arp 220, and correspond to a gas- number counts in the Herschel/SPIRE bands to-dust ratio of ~80 and a gas depletion timescale suggest a space density of massive starburst of Mgas/SFR ~36 Myr. These values are -2 comparable to lower-redshift submillimeter- galaxies at z>6 with S500µm>30 mJy of 0.014 deg selected starbursts.11,12 From the [CI] luminosity, (ref. 7). 7 we find an atomic carbon mass of 4.5 x 10 Msun. To understand the nature of galaxies selected by At the current star formation rate of HFLS3, this this technique, we have obtained full frequency level of carbon enrichment could have been

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 2 achieved through supernovae on a timescale of From the spectral energy distribution of HFLS3, 7 13 +9 ~10 yr. The profiles of the molecular and atomic we derive a dust temperature of Tdust=56 -12 K, emission lines typically show two velocity ~10 K less than in Arp 220, but ~3 times that of components (Figs. 1, S5, and S7). The gas is the Milky Way. CO radiative transfer models distributed over a 1.7 kpc radius region with a assuming collisional excitation suggest a gas +59 high velocity gradient and dispersion (Fig. 3). This kinetic temperature of Tkin=144 -30 K and a gas +0.28 -3 suggests a dispersion-dominated galaxy with a density of log10(n(H2))=3.80 -0.17 cm 11 dynamical mass of Mdyn = 2.7 x 10 Msun. The gas (Supplementary Information Section 4 and mass fraction in galaxies is a measure of the Figures S13/S14). These models suggest similar relative depletion and replenishment of molecular gas densities as in nearby ULIRGs, and prefer gas, and is expected to be a function of halo mass Tkin>>Tdust, which may imply that the gas and dust and redshift from simulations.14 In HFLS3, we find are not in thermal equilibrium, and that the a high gas mass fraction of fgas = Mgas/Mdyn ~ 40%, excitation of the molecular lines may be partially comparable to what is found in submillimeter- supported by the underlying infrared radiation selected starbursts and massive star-forming field. This is consistent with the finding that we 15,16 galaxies at z~2, but ~3 times higher than in detect H2O and OH lines with upper level nearby ultra-luminous infrared galaxies (ULIRGs) energies of E/kB > 300-450 K and critical densities like Arp 220, and >30 times higher than in the of >108.5 cm-3 at line intensities exceeding those of Milky Way. From population synthesis modeling, the CO lines. The intensities and ratios of the 10 we find a stellar mass of M* = 3.7 x 10 Msun, detected H2O lines cannot be reproduced by comparable to that of Arp 220 and about half that radiative transfer models assuming collisional of the Milky Way. This suggests that at most excitation, but are consistent with being radiatively ~40% of Mdyn within the radius of the gas reservoir pumped by far-infrared photons, at levels 11 are due to dark matter. With up to ~10 Msun of comparable to those observed in Arp 220 (Figures 20,21 dark matter within 3.4 kpc, HFLS3 likely resides in S15/S16). The CO and H2O excitation is a massive enough to grow a inconsistent with what is observed in host present-day .17 The efficiency for galaxies like Mrk 231 and APM08279+5255 at

star formation is given by ε=tdyn x SFR/Mgas, where z=3.9, which lends support to the conclusion that 3 1/2 tdyn=(r /(2GM)) is the dynamical (or free-fall) the gas is excited by a mix of collisions and time, r is the source radius, M is the mass within infrared photons associated with a massive, radius r and G is the gravitational constant. For intense starburst, rather than hard radiation 22 r=1.7kpc and M=Mgas, this suggests ε=0.06, which associated with a luminous AGN. The physical is a few times higher than found in nearby conditions in the ISM of HFLS3 thus are starbursts and in Giant Molecular Cloud cores in comparable to those in the nuclei of the most the Galaxy.18 extreme nearby starbursts, consistent with the finding that it follows the radio-FIR correlation for The properties of the atomic and molecular gas in star-forming galaxies. HFLS3 are fully consistent with a highly enriched, highly excited interstellar medium, as typically HFLS3 is rapidly assembling its stellar bulge found in the nuclei of warm, intense starbursts, through star formation at surface densities close but distributed over a large, ~3.5-kpc-diameter to the theoretically predicted limit for “maximum 23 region. The observed CO and [CII] luminosities starbursts”. At a rest-frame wavelength of suggest that dust is the primary coolant of the gas 158 µm, the FIR emission is distributed over a if both are thermally coupled. The L[CII]/LFIR ratio of relatively compact area of 2.6 kpc x 2.4 kpc ~5 x 10-4 is typical for high radiation environments physical diameter along its major and minor axes in extreme starbursts and respectively (Fig. 3; as determined by elliptical 19 (AGN) host galaxies. The L[CII]/LCO(1-0) ratio of Gaussian fitting). This suggests an extreme star ~3,000 suggests that the bulk of the line emission formation rate surface density of -1 -2 is associated with the photon dominated regions ΣSFR~600 Msunyr kpc over a 1.3-kpc-radius of a massive starburst. At the LFIR of HFLS3, this region, and is consistent with near-Eddington- suggests an infrared radiation field strength and limited star formation if the starburst disk is gas density comparable to nearby ULIRGs supported by radiation pressure.24 This suggests without luminous AGN (Figs. 4 & 5 of ref. 19). the presence of a kiloparsec-scale hyper-starburst similar to that found in the z=6.42 quasar

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 3 25 J1148+5251. Such high ΣSFR are also observed 5. Bouwens, R. et al. A candidate redshift z~10 in the nuclei of local ULIRGs such as Arp 220, galaxy and rapid changes in that population at an albeit on two orders of magnitude smaller scales. age of 500Myr. Nature 469, 504-507 (2011). 6. Oliver, S. et al. The Herschel Multi-tiered A starburst at such high may produce strong ΣSFR Extragalactic Survey: HerMES. winds. Indeed, the relative strength and broad, 2 Mon. Not. R. Astron. Soc. 424, 1614-1635 (2012). asymmetric profile of the OH Π1/2(3/2-1/2) 7. Béthermin, M. et al. A Unified Empirical Model for doublet detected in HFLS3 may indicate a Infrared Galaxy Counts Based on the Observed molecular outflow, reminiscent of the OH outflow Physical Evolution of Distant Galaxies. in Arp 220.21 Astrophys. J. Lett. 757, L23 (2012). 8. Karim, A. et al. An ALMA survey of submillimetre The identification of HFLS3 alone is still galaxies in the Extended Chandra Deep Field consistent with the model-predicted space density South: High resolution 870µm source counts. of massive starburst galaxies at z>6 with Submitted to Mon. Not. R. Astron. Soc.; arXiv -2 preprint at (2012). S500µm > 30 mJy of 0.014 deg (ref. 7). This corresponds to only 10-3-10-4 times the space 9. Bouwens, R.J. et al. Galaxies at z ~ 6: The UV Luminosity Function and Luminosity Density from density of Lyman-break galaxies at the same 506 HUDF, HUDF Parallel ACS Field, and GOODS redshift, but is comparable to the space density of i-Dropouts. Astrophys. J. 653, 53-85 (2006). the most luminous hosting supermassive 10. Robertson, B. et al. Early star-forming galaxies and black holes (SMBHs, i.e., a different population of the reionization of the Universe. 26 massive galaxies) at such early cosmic times. Nature 468, 49-55 (2010). The host galaxies around these very distant 11. Michalowski, M.J. et al. Rapid Dust Production in SMBHs are commonly FIR-luminous, but less Submillimeter Galaxies at z > 4? intensely star-forming, with typically a few times Astrophys. J. 712, 942-950 (2010). 25 12. Riechers, D.A. et al. Extended Cold Molecular Gas lower LFIR than ultra-red sources. This highlights the difference between selecting massive z>6 Reservoirs in z ~= 3.4 Submillimeter Galaxies. Astrophys. J. Lett. 739, L31 (2011). galaxies at the peak of their star formation activity 13. Walter, F. et al. Molecular gas in the host galaxy of through LFIR, and at the peak of their a quasar at redshift z = 6.42. activity through luminous AGN. The substantial Nature 424, 406-408 (2003). population of ultra-red sources discovered with 14. Lagos, C. Del P. et al. On the impact of empirical Herschel will be an ideal probe of early galaxy and theoretical star formation laws on galaxy evolution and heavy element enrichment within formation. the first billion years of cosmic time. These Mon. Not. R. Astron. Soc. 416, 1566-1584 (2011). galaxies are unlikely to dominate the star 15. Tacconi, L.J. et al. Submillimeter Galaxies at z ~ 2: formation history of the Universe at z>6,5 but they Evidence for Major Mergers and Constraints on trace the highest peaks in SFR at early epochs. A Lifetimes, IMF, and CO-H2 Conversion Factor. Astrophys. J. 680, 246-262 (2008). detailed study of this galaxy population will reveal 16. Tacconi, L.J. et al. High molecular gas fractions in the mass and redshift distribution, number density normal massive star-forming galaxies in the young and likely environments of such objects, which if Universe. Nature 463, 781-784 (2010). confirmed in larger numbers may present a stern 17. Overzier, R. et al. ΛCDM predictions for galaxy challenge to current models of early cosmic protoclusters - I. The relation between galaxies, structure formation. protoclusters and quasars at z ~ 6. Mon. Not. R. Astron. Soc. 394, 577-594 (2009). References: 18. Krumholz, M.R. et al. A Universal, Local Star Formation Law in Galactic Clouds, nearby 1. Chapman, S.C. et al. A median redshift of 2.4 for Galaxies, High-redshift Disks, and Starbursts. galaxies bright at submillimetre wavelengths. Astrophys. J. 745, 69 (2012). Nature 422, 695-698 (2003). 19. Stacey, G.J. et al. A 158 µm [C II] Line Survey of 2. Capak, P. et al. A massive protocluster of galaxies Galaxies at z ~ 1-2: An Indicator of Star Formation at a redshift of z~5.3. Nature 470, 233-235 (2011). in the Early Universe. 3. Walter, F. et al. The intense starburst HDF 850.1 in Astrophys. J. 724, 957-974 (2010). a galaxy overdensity at z ≈ 5.2 in the Hubble Deep 20. Rangwala, N. et al. Observations of Arp 220 Using Field. Nature 486, 233-236 (2012). Herschel-SPIRE: An Unprecedented View of the 4. Vieira, J.D. et al. Dusty starburst galaxies in the Molecular Gas in an Extreme Star Formation early Universe as revealed by gravitational lensing. Environment. Astrophys. J. 743, 94 (2011). Nature, in press.

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 4 21. Gonzalez-Alfonso, E. et al. Herschel/PACS European-led Principal Investigator consortia and spectroscopy of NGC 4418 and Arp 220: H2O, with important participation from NASA. This 18 18 H2 O, OH, OH, O I, HCN and NH3. research has made use of data from HerMES Astron. Astrophys. 541, A4 (2012). project (http://hermes.sussex.ac.uk/). HerMES is 22. van der Werf, P. et al. Water Vapor Emission a Herschel Key Programme utilising Guaranteed Reveals a Highly Obscured, Star-forming Nuclear Region in the QSO Host Galaxy APM 08279+5255 Time from the SPIRE instrument team, ESAC at z = 3.9. Astrophys. J. Lett. 741, L38 (2011). scientists and a mission scientist. See 23. Elmegreen, B.G. Formation as a Supplementary Information for further Maximum Intensity Starburst. acknowledgments. Astrophys. J. 517, 103-107 (1999). 24. Thompson, T. et al. Radiation Pressure-supported Author Contributions: D.R. had the overall lead Starburst Disks and Active Galactic Nucleus of the project. C.M.B., D.C., I.P.-F., R.I., C.B., Fueling. Astrophys. J. 630, 167-185 (2005). H.F., J.V., and R.N. have contributed significantly 25. Walter, F. et al. A kiloparsec-scale hyper-starburst to the taking and analysis of the follow-up data in a quasar host less than 1 gigayear after the Big with different instruments by leading several Bang. Nature 457, 699-701 (2009). telescope proposals and analysis efforts. C.D.D. 26. Jiang, L. et al. A Survey of z ~ 6 Quasars in the has led the selection of the parent sample. A.C., Sloan Digital Sky Survey Deep Stripe. II. Discovery J.W., J.C., A.C., P.H., and J.K. have contributed of Six Quasars at zAB>21. Astronomical. J. 138, 305-311 (2009). significantly to the data analysis and to fitting and 27. Downes, D. & Solomon, P.M. Rotating Nuclear modeling the results. All other authors contributed Rings and Extreme Starbursts in Ultraluminous to the proposals, source selection, data analysis Galaxies. Astrophys. J. 507, 615-654 (1998). and interpretation, in particular through work on 28. Sodroski, T.J. et al. Large-scale characteristics of the primary Herschel SPIRE data in which the interstellar dust from COBE DIRBE observations. source was discovered through the HerMES Astrophys. J. 428, 638-646 (1994). consortium (led by J.B. and S.O.). All authors 29. Murray, N. & Rahman, M. Star Formation in have reviewed, discussed, and commented on the Massive Clusters Via the Wilkinson Microwave manuscript. Anisotropy Probe and the Spitzer Glimpse Survey. Astrophys. J. 709, 424-435 (2010). Reprints and permissions information is available 30. McMillan, P.J. Mass models of the Milky Way. at www.nature.com/reprints. Mon. Not. R. Astron. Soc. 414, 2446-2457 (2011). Competing Interest Statement: The authors Supplementary Information is linked to the declare that they have no competing financial online version of the paper at interests. www.nature.com/nature. Corresponding authors: Correspondence and Acknowledgments: Herschel is an ESA space requests for material should be addressed to observatory with science instruments provided by Dominik Riechers ([email protected]).

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 5 Figures:

Figure 1: Redshift identification through molecular and atomic spectroscopy of HFLS3. a, Black trace, wide-band spectroscopy in the observed-frame 19 - 0.95-mm (histogram; rest-frame 2,600 - 130 µm) wavelength range with CARMA (3 mm; “blind” frequency scan of the full band), the PdBI (2 mm), the JVLA (19 - 6 mm), and CSO/Z-spec (1 mm; instantaneous coverage). (CARMA, Combined Array for Research in Millimeter-wave Astronomy; PdBI, Plateau de Bure Interferometer; JVLA, Jansky Very Large Array; and CSO, Caltech Submillimeter Observatory) This uniquely determines the redshift + of HFLS3 to be z=6.3369 based on the detection of a series of H2O, CO, OH, OH , NH3, [CI] and [CII] emission and absorption lines. b to o, Detailed profiles of detected lines (histograms; rest frequencies are indicated by corresponding letters in a). 1-mm lines (m-o) are deeper, interferometric confirmation observations for NH3, OH (both PdBI), and [CII] (CARMA) not shown in a. The line profiles are typically asymmetric relative to single Gaussian fits, indicating the presence of two principal velocity components at redshifts of 6.3335 and 6.3427. The implied CO, [CI], and [CII] line luminosities are 5.08+/-0.45 x 106, 8 10 3.0+/-1.9 x 10 , and 1.55+/-0.32 x 10 Lsun. Strong rest-frame submillimeter to far-infrared continuum emission is detected over virtually the entire wavelength range. For comparison, the Herschel/SPIRE spectrum of the nearby ultra- Arp 22020 is overplotted in grey (a). Lines labeled in italic are tentative detections or upper limits (see Table S2). Most of the bright spectral features detected in Arp 22020,21 are also detected in HFLS3 (in spectral regions not blocked by the terrestrial atmosphere). See Supplementary Information Sections 2-4 for more details.

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 6 7 6 5 irest (GHz)4 3 2 1 10 10 10 10 10 10 10 4 102 12 (b) S > S Arp220 (a) HFLS3 350 250 M82 MBB 1 8 HR10 10 Arp220 14 Eyelash M82 7 HR10 3 100 Eyelash 16 18 6 -1 10 350 20 /S 2

500 5 -2 S 8 10 AB mag 7 HFLS3 z=6.34

flux (mJy) 6 22 5 4 S500 > 1.3 S350 3 4 -3 10 24 2 HLock102 z=5.29 S500 > S350 1 z=1 HLS A773 z=5.24 1’ 3 HFLS1 z=4.29 10-4 26 2 HATLAS ID141 z=4.24 z=1 HFLS5 z=4.44 250 µm 350 µm 500 µm 28 10-5 0 10-1 100 101 102 103 104 105 106 0 1 2 3 4 5 h (µm) S /S obs 350 250 Figure 2: Spectral energy distribution (SED) and Herschel/SPIRE colors of HFLS3. a, HFLS3 was identified as a very high redshift candidate, as it appears red between the Herschel/SPIRE 250-, 350-,

and 500-µm bands (inset). The SED of the source (data points; λobs, observed-frame wavelength; νrest, rest-frame frequency; AB mag, magnitudes in the AB system; error bars are 1σ r.m.s. uncertainties in both panels) is fitted with a modified black body (MBB; solid line) and spectral templates for the starburst galaxies Arp 220, M82, HR10, and the Eyelash (broken lines, see key). The implied FIR +0.32 13 luminosity is 2.86 -0.31 x 10 Lsun. The dust in HFLS3 is not optically thick at wavelengths longward of rest-frame 162.7 µm (95.4% confidence; Figure S12). This is in contrast to Arp 220, in which the dust 20 becomes optically thick (i.e., τd=1) shortward of 234+/-3 µm. Other high-redshift massive starburst galaxies (including the Eyelash) typically become optically thick around ~200 µm. This suggests that none of the detected molecular/fine structure emission lines in HFLS3 require correction for extinction. The radio continuum luminosity of HFLS3 is consistent with the radio-FIR correlation for nearby star- forming galaxies. b, 350 µm/250 µm and 500 µm/350 µm flux density ratios of HFLS3. The colored lines are the same templates as in a, but redshifted between 16 for typical SED shapes (except those with low dust temperatures), while red sources typically are at z<5.5. See Supplementary Information Sections 1 and 3 for more details.

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 7 ◦ " "" 2 2 58 46 25 dust continuum [CII]( P3/2 → P1/2) velocity velocity dispersion

"" G1B 24 z = 2.092 −175 220 HFLS3 z = 6.337 +500 800 23"" Declination

"" ."" × ."" −1 −1 22 ab0 35 0 23 cd∆v=100 km s ∆v=100 km s 17h06m48s.0 47s.847s.6 Right Ascension (J2000) Figure 3: Gas dynamics, dust obscuration, and distribution of gas and star formation in HFLS3. a, b, High-resolution (FWHM 0.35”x0.23”) maps of the 158-µm continuum (a) and [CII] line emission (b) obtained at 1.16 mm with the PdBI in A-configuration, overlaid on a Keck/NIRC2 2.2-µm adaptive optics image (rest-frame UV/optical light). The r.m.s. uncertainty in the continuum (a) and line (b) maps is 180 and 400 µJy beam-1, and contours are shown in steps of 3 and 1σ, starting at 5 and 3σ, respectively. A z=2.092 galaxy (labeled G1B) identified through Keck/LRIS spectroscopy is detected ~0.65” north of HFLS3, but is not massive enough to cause significant gravitational lensing at the position of HFLS3. Faint infrared emission is detected toward a region with lower dust obscuration in the north-eastern part of HFLS3 (not detected at <1 µm). The Gaussian diameters of the resolved [CII] and continuum emission are 3.4 kpc x 2.9 kpc and 2.6 kpc x 2.4 kpc, suggesting gas and SFR surface densities of 4 -2 -1 -2 13 -2 Σgas = 1.4 x 10 Msun pc and ΣSFR = 600 Msun yr kpc (~0.6 x 10 Lsun kpc ). The high ΣSFR is consistent with a maximum starburst at near-Eddington-limited intensity. Given the moderate optical depth of τd<~1 at 158 µ m, this estimate is somewhat conservative. Peak velocity (c) and F.W.H.M. velocity dispersion (d) maps of the [CII] emission are obtained by Gaussian fitting to the line emission in each spatial point of the map. Velocity contours are shown in steps of 100 kms-1. High-resolution CO J=7-6 and 10-9 and H2O 321-312 observations show consistent velocity profiles and velocity structure (Figures S5-S7). The large velocity dispersion suggests that the gas dynamics in this system are dispersion-dominated. See Supplementary Information Sections 3 and 5 for more details.

Table 1: Observed and derived quantities for HFLS3, Arp 220 and the Galaxy HFLS3 Arp 220* Milky Way* redshift 6.3369 0.0181 - a 11 9 9 Mgas (Msun) (1.04+/-0.09) x 10 5.2 x 10 2.5 x 10 b +0.32 9 8 7 Mdust (Msun) 1.31 -0.30 x 10 ~1 x 10 ~6 x 10 c 10 10 10 M* (Msun) ~3.7 x 10 ~3-5 x 10 ~6.4 x 10 d 11 10 11 Mdyn (Msun) 2.7 x 10 3.45 x 10 2 x 10 (<20 kpc) e fgas 40% 15% 1.2% f +0.32 13 12 10 LFIR (Lsun) 2.86 -0.31 x 10 1.8 x 10 1.1 x 10 -1 g SFR (Msunyr ) 2,900 ~180 1.3 h +9.3 Tdust (K) 55.9 -12.0 66 ~19

For details see Supplementary Information, Section 3. *Literature values for Arp 220 and the Milky Way are adopted from refs. 27, 20, 28, 29, and 30. The total molecular gas mass of the Milky Way is uncertain by at least a factor of 2. Quoted dust masses and stellar masses are typically uncertain by factors of 2-3 due to systematics. The dynamical mass for the Milky Way is quoted within the inner 20 kpc to be comparable to the other systems, not probing the outer regions dominated by dark matter. The dust temperature in the Milky Way varies by at least +/-5 K around the quoted value, which is used as a representative value. Both Arp 220 and the Milky Way are known to contain small fractions of significantly warmer dust. All error bars are 1σ r.m.s. uncertainties. a -1 2 -1 Molecular gas mass, derived assuming αCO = Mgas/L’CO = 1 Msun (K kms pc ) , see Supplementary Information, Section 3.3. bDust mass, derived from spectral energy distribution fitting, see Supplementary Information, Section 3.1. cStellar mass, derived from population synthesis fitting, see Supplementary Information, Section 3.4. dDynamical mass, see Supplementary Information, Section 3.5. e Gas mass fraction, derived assuming fgas=Mgas/Mdyn, see Supplementary Information, Section 3.6. fFar-infrared luminosity as determined over the range of 42.5-122.5 µm from spectral energy distribution fitting, see Supplementary Information, Section 3.1. g -1 -10 Star formation rate, derived assuming SFR[Msunyr ] = 1.0 x 10 LFIR [Lsun], see Supplementary Information, Section 3.2. hDust temperature, derived from spectral energy distribution fitting, see Supplementary Information, Section 3.1.

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 10 2/"*?%, 9(/()$=, ).(%*, *%D%?(0/', /., 4)8, 8)()>, G0(7, ), ?)$04*)(0/',G)2,?)**0%8,/"(,*%$)(03%,(/,#$)'%(2>,G0(7, 2+'(7%20:%8,4%)&,20:%,/.,FB@_", G%, /42%*3%8, 1)*2, /*, 205')$A(/A'/02%, *)(0/, /., EBN, 92%%, Z05"*%2, <, )'8, !N=B, ]%#("'%B,T)224)'8,?)$04*)(0/',G)2,/4()0'%8,/',(7%, W%,)$2/,(%'()(03%$+,8%(%?(%8,(7%,JO, F#,EgFjf>,EgENM>,EgNMNBE>, )'8, OFJ, *o)o?,L, N,S,)'8,S,)'8,(7%,]OE,E2!F),)'8, K")2)*2, ,(7%2%,8)(),#*/308%, , $0&0(2,/',(7%,gJ,*L,)2,G%$$,)2, C7%, 1-R-`V, #)?H)5%, G)2, "2%8, ./*, 8)(), %80(0'5>, /', h]--i, E4, hJ-i, E4, gO, F>EIF!<>, )'8, ?)$04*)(0/'>,)'8,0&)50'5B,-',)880(0/',(/,8%(%?(0'5,gJ, OFJ, *o)o?, L, MFE!M,hg-i, 4F! 4<>,OFJ,*o)o?,L,F<,)'8, g/'(0'""&, %&0220/', G0(7, ), 2(%%#$+, *020'5, 2$/#%, 02, F F hg--i, 4EIF! 4, G%, )$2/, (%'()(03%$+, 8%(%?(%8, /3%*, (7%, %'(0*%, G)3%$%'5(7, *)'5%, 92%%, m 8%(%?(%8, OFJ , *o)o?,L, F@F!F<<, *, L, EIF!EIF, %&0220/', C)4$%, !<, ./*, ?/'(0'""&, .$"6%2, /4()0'%8, ).(%*, 9*%2(A.*)&%, jNYB, )'8, /4()0'%8, "##%*, 2#%?(*)$,)3%*)50'5,0'(/,M,40'2=B, $0&0(2, /', (7%, gJ, *, L, M!N, )'8, , <>PN, )'8,,,, :"M #A+%)(%1#0(#N1&(#;/)(&4(&.<()(&#CA0N;E# jNFB@EEF, \O:d, 2%%, C)4$%, !F, ./*, $0'%, .$"6%2, )'8, # W%, "2%8, (7%, -R`1, T8c-, G0(7, N!Y, )'(%'')2, 0', (7%, $0&0(2>,)'8,Z05"*%2,<,)'8,!<,./*,2#%?(*)=B,g/'(0'""&, ?/&#)?(,g,)'8,V,?/'.05"*)(0/'2,(/,()*5%(,OZ[!E,0', %&0220/', 02, 8%(%?(%8, /3%*, (7%, %'(0*%, G)3%$%'5(7, <@,.*%K"%'?+,2%((0'52,)(,E,&&>,F,&&>,)'8,<,&&,(/, *)'5%, 92%%, C)4$%, !<, ./*, ?/'(0'""&, .$"6%2>, )'8, /42%*3%, ,O J>,JO>,JOm>,gOm>,)'8,]O ,&/$%?"$%2, &)#2, ./*, (7%, gJ, *, L, Y!M, )'8, j!Y>, hg-i, E4 !E4 >,,,,,,, F E F < 9T-2e, R0%?7%*2>, T%*%:AZ/"*'/'=B, J42%*3)(0/'2, G%*%, O J, * L, F !F >, )'8, hg--i, F4 !F4 , $0'%2, G%*%, F o)o?, << @F EIF , @BEN>, G0(7, M!Y, )'(%'')2, 0', (7%, &/2(, %6(%'8%8, `, @BN@>, @BFf>, )'8, FBf, &S+, 4%)&A<, #%*, ffN>, jfM>, MYY>, ?/'.05"*)(0/', (/, ()*5%(, OZ[!E, 0', E, .*%K"%'?+, PME>,)'8,PNN,H&2A<,9E,Ff,F@PBE>,Ff,)'8, 2%((0'52,)(,E,&&>,F,&&>,)'8,<,&&>,(/,0&)5%,(7%,gJ, jFfBF, 1O:=, 40', 92%%, Z05"*%, !E, ./*, $0'%, &)#2, )'8, *, L, j!Y, )'8, <@!f>, hg-i, E4F!E4<>, OFJ, *o)o?,L, EF, 2+'(7%20:%8,4%)&,20:%2=B, F F , )'8, hg--i, 4EIF! 4<-++-<()(&#=>3(&?%).&G#CH*=E#### /42%*3)(0/'2, G%*%, ?)**0%8, /"(, 4%(G%%', F@N<, 2#%?(*/&%(%* /', (7%, g!J, (/, /42%*3%, (7%, C7%, Y, )'(%'')A%K"03)$%'(, /', 2/"*?%, (0&%2, ./*, /"*, ,<, 0', FM@!E@@,/3%*,(7%,?/3%*%8,.*%K"%'?+,*)'5%B,W%, , , , )'8, ), , f@_, ?7/#B, J42%*3)(0/'2,G%*%,?)**0%8, , , F@NB@Fj,,,,, 5//8, <, &&, /42%*30'5, ?/'80(0/'2, 9gJ, *L, FFjBY@N, 9OFJ, *o)o?, L, F, G0(7, ), &%)', /., @B@f@, )'8, ), FF, FN@BEYN, 9]OE, Eo)!Fo2=>, FM@BNf@,,,,,,,,,,,, &%80)',/.,@B@jP=>,+0%$80'5,FFBj,7*,9EfBM,7*=,(0&%,/', 9JO, F#, )'8,,,,,, 2/"*?%, 9(/()$=, ).(%*, *%D%?(0/', /., 4)8, 8)()B, C702, FMfB@Ef,\O:,9hg--i,F4EIF!F4,<@BF>,NBE>,YBj>, , FBN>, jBP>, , , , EB@>, FBE>, )'8, NBM, 7*>, ?/**%2#/'80'5, (/, ), #%*A?7)''%$, *B&B2B, /., FBY, &S+, *%2#%?(03%$+B, C7%, '%)*4+, *)80/, K")2)*2, , 9N@l!M@l, 7057%*, )(, (7%, 4)'8, %85%2>, )'8, G0(7, , /*,

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 15 8%*03%,)',/3%*)$$,9.)*A=0'.*)*%8,$"&0'/20(+,@9Z=-R,)'8, !UV,27)#%,*%$)(03%,(/,`*#,FF@,?)',4%,%6#$)0'%8,G0(7, 8"2(, &)22, A8B, W%, "2%, )', )..0'%A0'3)*0)'(, 1)*H/3, ), $/G%*, 8"2(, /#(0?)$, 8%#(7, 0', OZ[!EB, C7%, 8"2(, 0',, g7)0', 1/'(%, g)*$/, 91g1g=, 2)&#$%*, 9#B&##=MN, (/, `*#, FF@, 5%(2, /#(0?)$$+, (70?H, )(, G)3%$%'5(72, ?/&#"(%, M@@>@@@, 2(%#2, .*/&, FM@, 2)&#$%*2B, J"*, 27/*(G)*8, /., *%2(A.*)&%, FEN±E, Q&>F@, G7%*%)2, )##*/)?7,."$$+,&)*50')$0:%2,/3%*,(7%,/#(0?)$,8%#(7>, OZ[!E, 02, /#(0?)$$+, (70', $/'5G)*8, /., *%2(A.*)&%, )'8, ()H%2, ?/3)*0)'?%2, 4%(G%%', (7%, 0'#"(, ,0B%B>,(7%,?7)0'2, $04*)*0%2>Mf>Y@, 4"(, (702, 808, '/(, +0%$8, )'+, 205'0.0?)'(, ?/'3%*5%, 3%*+, G%$$B, C7%, *%2"$(0'5, ?/'2(*)0'(2, )*%, )880(0/')$,?/'2(*)0'(2B, 27/G',0',Z05"*%,!8LMMBfmfBEA,G%,.0((%8,(7%, C7%,#/G%*A$)G,2$/#%,(/,.0(,(7%,4$"%,208%,/.,(7%,!UV, /#(0?)$,8%#(7,/.,/(7%*,7057A*%8270.(,5)$)60%2B,Z/*,(7%, 02, /'$+, #//*$+, ?/'2(*)0'%8, 4+, (7%, 8)(), 9 ;FBM, )(, $ g/2&0?, U+%$)27>, /"*, .0(, +0%$82, ), *F, /., , G0(7, ), 4%2(A.0(, 802?/3%*%8,)2,#)*(,/.,/"*,2"*3%+>,G%,/4()0',),*F,/., 3)$"%,/.,jEEmEFYANYj,Q&,9ffBfmNNBNAYEBY,Q&,*%2(A.*)&%=B, <,)'8,)@LF@@mFfAFM,Q&, C702, 2"55%2(2, (7)(, (7%, /42%*3%8, %&0220/', $0'%2, )(, 0',(7%,*%2(,.*)&%B,Z/*,(7%,:LNBNN,5)$)6+,OZ[!M>,G%, %/42;, )'8, $0'%, %6?0()(0/', &/8%$2B, C7%, .)?(, (7)(, G%, ?)', /'$+, )@LY<, G%, /4()0', ), *F, /., YBP, ./*,,,,,,,,,,,,,,,, %2(0&)(%8, @9Z=-R, )'8, A8B, J"*, .0(2, 0&#$+, )', 0'.*)*%8, Y,8%5*%%2,/.,.*%%8/&>,)'8, L, )@XF@@, Q&, 02, ./"'8, ./*, (7%2%, 7057A @-RL9NB, )'8, ), .)*A0'.*)*%8,,,, 9Z-Rd, NFBM!, G0(7, 0'80308")$, 3)$"%2, (7)(, )*%, ?/&#)(04$%,G0(7,(7)(,&%)2"*%8,0',`*#,FF@B,C)H%',)(, @Z-RL9FBPYm@BEFA@BE<="<@,(702,G/"$8,0'80?)(%,(7)(,(7%,/#(0?)$,8%#(7, , 0', OZ[!E, 02, 2/&%G7)(, $/G%*, (7)', (+#0?)$, ./*, A8L)%,C[F,h9=iA<,"%,h, n[-R\2,)'8,7057A:,&)2203%,2()*4"*2(,5)$)60%2B, , # )22"&0'5, ), &)22, )42/*#(0/', ?/%..0?0%'(, /.,,,,,,# F, A< MM K":#*)%&#^.&<%)-./#8%)(# $%LFBYN,& H5 ,)(,, G70?7, )*%, )(, $%)2(, ), ."'?(0/',9-1Z=>YF,(/,8%*03%,(7%,2()*,./*&)(0/',*)(%,/., .)?(/*,/.,EB, OZ[!E,.*/&,(7%,Z-R,$"&0'/20(+,4)2%8,/',), # YE # o%''0?"((,?/'3%*20/'e , , K"!":#$(<@+%)(#^-))-/', A< " A<@ , !ZRh12"'+* i,L,, G%, )$2/, "2%8, *F, Z/*+@Z-RL9FBPYm@BEFA@BE<="<@, (702, 2"55%2(2, ), 2()*, ./*&)(0/', #7/(/&%(*+,/.,OZ[!EB,W%,2%$%?(%8,(%&#$)(%2,./*,(7%, *)(%,9!ZR=,/.,,XF>f@@,12"'+*A, (7%, '%)*4+, "$(*)A ), .)?(/*, /., X, (7%, !L,XN>f@@,12"'+*A<=>YE,)'8,4+,),.)?(/*, 5)$)6+,OR<@>,)'8,(7%,5*)30()(0/')$$+,$%'2%8,!LFBEF, /.,,XFBY,$/G%*,G7%',)8/#(0'5,),.$)(,c)"57,-1Z,90B%B>, 5)$)6+, !11, SF<@@,12"'+*A<=BYN>YM,`,.$)(,-1Z,&)+,4%,#*%.%**%8,(/, MY>Mj>MP Z05"*%,F=B ,C7%,Z-R,!UV,27)#%,02,'/(,?/'202(%'(, %6#$)0', (7%, ./*&)(0/', /., :XF, 2"4&0$$0&%(%*, G0(7,OR<@,/*,(7%,U+%$)27B,C7%,'%)*I&08A0'.*)*%8,(/, 5)$)60%2BYN,J',(7%,/(7%*,7)'8>,#*%2%'(A8)+,%$$0#(0?)$, Z-R, .$"6, *)(0/, 02, /'$+, &)*50')$$+, ?/'202(%'(, G0(7, 5)$)60%2, 27/G, %308%'?%, ./*, 4/((/&A7%)3+, 1PFB, O/G%3%*>, (7%, /3%*)$$, !UV, 27)#%, 02, .)0*$+, -1Z2BYY>Yj>YP, `22"&0'5, (7)(, 2"4&0$$0&%(%*, 5)$)60%2, ?/'202(%'(,G0(7,`*#,FF@B,C7%,80..%*%'?%2,0',(7%,Z-R,

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 16 )*%, (7%, )'?%2(/*2, /., (7%2%, 5)$)60%2>, 0(, &)+, 4%, K"K"K#F).<-,#W%3#I%33# %6#%?(%8,(7)(,(7%0*,-1Z,?/"$8,)$2/,4%,4/((/&A7%)3+B, , C702>, 7/G%3%*>, ?/"$8, 0&#$+, )', %3%', 7057%*, 2()*, C/,8%(%*&0'%,(7%,)(/&0?,5)2,9O-=,&)22,0',OZ[!E,90', ./*&)(0/', *)(%, (7)', 0', )'+, /., (7%, ?)2%2, K"/(%8, 12"'=,4)2%8,/',hg--i>,G%,"2%,(7%,./$$/G0'5,%K")(0/', )4/3%B, `22"&0'5>, (7)(, (7%, (7%/*%(0?)$, $0&0(, /.,,,,,,,,9G70?7,)22"&%2,(7)(,(7%,hg--i,%&0220/',02,/#(0?)$$+, (70'=e, %!ZR, L, <>@@@, 12"'+*A<, H#?AF, )##$0%2, (/, OZ[!E>, -1Z2, , (7)(, )*%, &/*%, 4/((/&A7%)3+, (7)', !)$#%(%*, )*%, AO-,L,@Bjj,9@Bj,@hg--i=,9=mE?*0(IE=,9F,%6#9!f<,oI>==A<,>, g7)4*0%*,-1Z,./*,(7%,*%&)0'8%*,/.,(702,G/*HB, , # G7%*%, D L,)'8,E?*0(LFBj"<@ ,?& ,02,(7%,?*0(0?)$, # 8%'20(+, /., hg--iBjF, `22"&0'5, EL<@EBP, ?&AE, )'8,,,, K"K"!##I.+(,1+%&#W%3#I%33# >L, , G%, .0'8,,,,,,,, $"&0'/20(+,/.,OZ[!E>,G%,)22"&%,),$/G,?/'3%*20/', AO-LFB@"<@<@,12"'B,C702,?/**%2#/'82,(/,XF@l,/.,(7%, .)?(/*,/.,&gJ,L,A5)2I@tgJ,L,<,12"',9o,H&2A<,#?F=A<,.*/&, &/$%?"$)*,5)2,&)22B, gJ, $0'%, $"&0'/20(+, (/, A5)2>, )2, ?/&&/'$+, "2%8, ./*, # # n[-R\2,9(+#0?)$,3)$"%2,/.,&gJ,L@BY!,G0(7,/"($0%*2, K"M#*)(++%&#I%33# /"(, (/, @BE!jN, G%, /4()0', ), 2(%$$)*, &)22, /., (/()$, &/$%?"$)*, 5)2, &)22, /., AvLNBMm, 4"(, 503%', 7057,?/'3%*20/',.)?(/*,/.,&gJ,L,N,12"',9o,H&2A<,#?F=A<, (7%, 7057, *%8270.(, )'8, 7057, 8"2(, /42?"*)(0/', /., (7%, )2, ./"'8, ./*, '%)*4+, 2#0*)$, 5)$)60%2, 0'?$"80'5, (7%, 2/"*?%>, (7%, 8)(), )$$/G, ./*, ), 4*/)8, *)'5%, 0', Av, j@ 10$H+, W)+, )'8, 7057A*%8270.(, 802H, 5)$)60%2> , (7%, 4%(G%%', F"<@P, )'8, Y"<@<<, 12"'>, G0(7, )', &/$%?"$)*, 5)2, &)22, G/"$8, %6?%%8, (7%, 8+')&0?)$, 0'(%*K")*(0$%, *)'5%, /., @BF!F"<@<@, 12"'B, \03%', (7%, &)22B, `'+, &gJ, ;, FBj, 12"', 9o, H&2A<, #?F=A<,,,,,,,,,,,,,,,,,&)22, /., (7%, 8"2(, )'8, 80..%*%'(, 5)2, #7)2%, &)22%2>, A<, F A< 9;FB@,12"',9o,H&2 #? = ,G7%',0'?$"80'5,A8>,Av>,Ag->, 2(%$$)*, &)22%2, /., ;./#I%33, &)((%*,.*)?(0/',/.,FMl>,(702,$0&0(,G/"$8,8%?*%)2%,(/, # ;jBj"<@<@, 12"'=>, )'8, (7"2>, )*%, 802.)3/*%8, 8"%, (/, C/,8%*03%,(7%,'%"(*)$,)(/&0?,?)*4/',&)22,0',OZ[!E, /(7%*,/42%*3)(0/')$,?/'2(*)0'(2B,[0H%G02%>,503%',(7%, 90',12"'=>,G%,"2%,(7%,./$$/G0'5,%K")(0/'e, ?/'208%*)4$%, 8"2(, &)22>, 2(%$$)*, &)22%2, )(, (7%, $/G, , %'8, /., (7%, ./*&)$$+, )$$/G%8, *)'5%, )*%, 802.)3/*%8>, Ag-,L,MBj@Y"<@AN,79>%6=,%6=,@thg-i,>, )22"&0'5,(7)(,),205'0.0?)'(,.*)?(0/',/.,(7%,8"2(,G)2, , #*/8"?%8, 4+, 2()*2, 0', (7%, 5)$)6+B, 1)H0'5, (7%, G7%*%,79>%6=,L,<,m,E,%6#9!>%6=,m,M,%6#9!>FI>%6=, ?/'2%*3)(03%,)22"&#(0/',(7)(,(7%,5)$)6+,?/'()0'2,)(, 02, (7%, hg-i, #)*(0(0/', ."'?(0/'>, >F,L,YFBM,o,)*%,(7%,%'%*50%2,)4/3%,(7%,5*/"'8,2()(%, 2(%$$)*, &)22%2, /., a,)'8,@thg-i,02,(7%,$0'%,$"&0'/20(+,0', (7%, $/G%*, $0&0(, /., (7%, 0'(%*K")*(0$%, *)'5%=B, C7%, (7%,$/G%*,hg-i,$0'%Bj<,C7%,hg-i,$"&0'/20(+,/.,OZ[!E,02, 0'(%*K")*(0$%,*)'5%,G/"$8,2"55%2(,(7)(,(7%,4)*+/'0?, @hg-iLEB@±, )'8, (7"2>, (7)(, (7%, /'5/0'5, (%&#%*)("*%,*)(0/,/.,@BM,4%(G%%',(7%,hg-i,$%3%$2>,G%, 2()*4"*2(,02,0',),*%$)(03%$+,%)*$+,#7)2%B, .0'8,)',)(/&0?,?)*4/',&)22,/.,NBM"<@j,1 B, 2"' , , jM , W%,7)3%,)$2/,.0((%8,(7%,!UV,/.,OZ[!E,G0(7,FGHI@J> , # "20'5, 8"2(, %&0220/', (%&#$)(%2, 90B%B>, ()H0'5, (7%, ."$$, # 2#%?(*)$, %'%*5+, 802(*04"(0/', 0'(/, )??/"'(=>Mf,

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 20 T"#*1@@+(<(/)%&G#$%>+(3# # $%>+(#*!`#I1+)-7J%?(+(/')B#@B.).<()&G#.4#Z^S*K"# # Wavelength Frequency Flux Density Error Observatory [!m] [GHz] [mJy] [mJy] 0.4686 640,000 <0.052e-3 GTC (g) 0.6165 485,000 <0.083e-3 GTC (r) 0.7481 400,000 <0.052e-3 GTC (i) 0.8931 335,000 <0.157e-3 GTC (z) 2.2 135,000 1.823e-3 0.305e-3 WHT+Keck (Ks) 3.4 88,000 <0.08 WISE 3.6 83,000 2.39e-3 0.25e-3 IRAC 4.5 67,000 3.16e-3 0.52e-3 IRAC 4.6 65,000 <0.11 WISE 12 25,000 <0.8 WISE 22 13,600 <6 WISE 70 4,300 <2.0 PACS 110 2,700 <2.2 PACS 160 1,900 <4.0 PACS 250 1,200 12.0 2.3* SPIRE 350 850 32.4 2.3* SPIRE 500 600 47.3 2.8* SPIRE 880 341 33.0 2.4 SMA 1,055.0 284.161 20.57 0.45 Z-spec 1,110 270 21.3 1.1 SMA 1,151.6 260.329 17.10 0.37 Z-spec 1,157.5 259.106 17.12 0.81 PdBI 1,157.5 259.106 13.9 1.9 CARMA 1,190.1 251.906 13.51 1.22 CARMA 1,196.8 250.490 14.07 0.60 PdBI 1,247.2 240.364 15.05 0.19 PdBI 1,247.7 240.284 14.17 0.38 Z-spec 1,317.2 227.604 10.13 0.29 PdBI 1,349.4 222.167 11.76 0.40 Z-spec 1,448.2 207.013 9.78 0.45 Z-spec 1,469.4 204.027 9.79 0.29 PdBI 1,821.4 164.598 6.57 0.18 PdBI 1,900.3 157.757 4.59 0.39 PdBI 2,000 150 2.93 0.37 GISMO 2,014.7 148.800 3.35 0.12 PdBI 2,121.2 141.328 3.22 0.12 PdBI 2,226.5 134.650 2.38 0.11 PdBI 2,633.9 113.819 1.25 0.09 PdBI 2,722.2 110.128 1.21 0.10 PdBI 2,722.2 110.128 1.59 0.12 CARMA 2,924.8 102.500 0.705 0.134 CARMA 3,181.0 94.246 0.527 0.078 CARMA 6,360.8 47.1311 0.139 0.030 JVLA (Q) 9,540.9 31.4217 0.0469 0.0093 JVLA (Ka) 19,081.5 15.7112 <0.015 JVLA (U) 214,000 1.4 0.059 0.011 JVLA (L) v%**/*,4)*2,/',!T-RU,.$"6%2,)*%,/4()0'%8,.*/&,.0((0'5,)'8,8/,'/(,)??/"'(,./*,?/'."20/','/02%>,G70?7,02,)(, $%)2(,XY&S+,0',)$$,!T-RU,4)'82B,

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 21 $%>+(#*:`#*@(,)&%+#+-/(#@%&%<()(&3#C3(,./0#(/)&-(3#-/#,.+1

H2O 211-202 752.033227 2.68 0.78 927 330 2.63 0.76 8.1 2.3 CARMA

H2O 202-111 987.926764 2.56 0.31 805 129 2.19 0.33 3.9 0.5 PdBI

H2O 312-303 1,097.364791 2.59 0.43 672 146 1.83 0.45 2.7 0.5 PdBI

H2O 312-221 1,153.126822 2.51 2.08 937 165 2.49 1.74 3.3 2.3 PdBI

H2O 321-312 1,162.911593 4.84 0.77 937 165 4.81 0.76 6.2 0.9 PdBI

H2O 422-413 1,207.638714 1.56 0.60 1.25 0.48 1.5 0.5 PdBI*

H2O 523-514 1,410.618074 <5.9 <5.2 Z-spec

H2O 413-404 1,602.219182 3.96 2.70 2.7 1.8 Z-spec*

H2O 221-212 1,661.007637 <1.92 <1.2 PdBI

H2O 212-101 1,669.904775 <2.26 <1.4 PdBI

H2O 303-212 1,716.769633 <6.7 <4.0 Z-spec

H2O 633-624 1,762.042791 <6.2 <3.5 Z-spec

H2O 624-615 1,794.788953 <7.5 <4.1 Z-spec

H2O 734-725 1,797.158762 <7.5 <4.1 Z-spec

H2O 532-523 1,867.748594 <6.8 <3.4 Z-spec

H2O 523-432 1,918.485324 <7.3 <3.5 Z-spec

H2O 322-313 1,919.359531 <7.5 <3.6 Z-spec

H2O 431-422 2,040.476810 <10.5 <4.4 Z-spec

H2O 413-322 2,074.432305 <11.6 <4.7 Z-spec

H2O 313-202 2,164.131980 <11.4 <4.2 Z-spec

H2O 330-321 2,196.345756 <16.0 <5.8 Z-spec

H2O 514-505 2,221.750500 <16.8 <5.9 Z-spec + H2O 202-111 J=5/2-3/2 742.0332 <1.08 <3.4 CARMA J=3/2-3/2 746.1938 1.64 0.99 542 410 0.94 0.57 3.0 1.8 CARMA*

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 22 Transition Rest Peak flux Velocity Line Line Obs. Frequency density FWHM Intensity Luminosity 10 # [GHz] [mJy] [km/s] [Jy km/s] [10 Ll ] 2 OH # 1/2 3/2-1/2 1,834.74735/ 7.82 0.80 1493 222 12.37 1.43 6.4 0.7 PdBI 1,837.81682 5.98 3.25 3.1 1.7 Z-spec* + OH 11F-01F ~1,033.0582 -0.56 0.18 -0.92 0.29 PdBI* CH+ J=1-0 835.07895 <1.1 <2.8 PdBI CH+ J=2-1 1,669.15951 <2.3 <1.4 PdBI

NH3 3Ka-2Ks ~1,763.6496 -1.56 0.51 648 290 -1.07 0.37 -0.60 0.21 PdBI* -5.68 2.83 -3.2 1.6 Z-spec*

NH 22-11 ~1,958.2068 -7.06 3.10 -3.2 1.4 Z-spec* HF J=2-1 2,463.42814 <19.6 <5.6 SMA 3 3 [CI] P2- P1 809.343500 1.82 1.30 276 240 0.53 0.37 1.4 1.0 CARMA* 0.76 0.45 419 341 0.34 0.21 0.91 0.57 PdBI 2 2 [CII] P3/2- P1/2 1,900.543 29.34 6.12 470 135 14.62 3.05 7.1 1.6 CARMA 9.99 2.86 4.8 1.4 Z-Spec 13.66 2.07 6.6 1.0 PdBI 3 3 [NII] P1- P0 1,461.132 <6.3 <5.2 Z-spec 3 3 [NII] P2- P1 2,459.380 <19.6 <5.7 SMA 3 3 [OI] P1- P0 2,060.068 <7.4 <3.0 Z-spec w$0'%,$"&0'/20(+,02,503%',0',"'0(2,/.,@(,L,o,H&I2,#?F, v(%'()(03%,8%(%?(0/'2,/'$+>,0'8%#%'8%'(,?/'.0*&)(0/',*%K"0*%8, # # $%>+(#*K`#H=#(_,-)%)-./#<.0(+-/'`#@%&%<()(&3# # Parameter Median value 1! range 1D Max 4D Max Tkin [K] 143.59 113.64-202.21 138.04 138.04 -3 log10 n(H2) [cm ] 3.84 3.63-4.08 3.80 3.80 -2 log10 NCO [cm ] 20.84 20.63-21.03 20.92 21.02 log10 ' A !1.78 !1.88 - !1.68 !1.70 !1.70 -2 log10 P [K cm ] 6.02 5.82-6.24 6.12 6.12 -2 log10 [cm ] 19.08 18.83-19.30 19.21 19.21 dv/dr [kms-1pc-1] 1.4 0.8-3.5 1.3 1.3 # # # # # # # # # # # # #

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 23 $%>+(#*M`#I(%31&(0#%/0#0(&-?(0#3.1&,(#@&.@(&)-(3# # Parameter Value 11 -1 2 L’CO 1.04±0.09"10 K kms pc 6 LCO 5.08±0.45"10 Lsun 8 L[CI] 3.0±1.9"10 Lsun 10 L[CII] 1.55±0.32"10 Lsun +0.32 13 LFIR 2.86 -0.31"10 Lsun a 11 Mgas 1.0"10 Msun b 7 MCI 4.5"10 Msun c 10 MHI 2.0"10 Msun +0.32 9 Mdust 1.31 -0.30"10 Msun 10 M* 3.7"10 Msun 11 Mdyn 2.7"10 Msun d -1 SFR 2,900 Msunyr 4 -2 % gas 1.4"10 Msun pc -1 -2 % SFR 600 Msunyr kpc fgas 40% gas-to-dust ratio 80 tdep 36Myr

( 0.06 d[CII] 3.4 kpc"2.9 kpc dFIR 2.6 kpc"2.4 kpc +9.3 Tdust 55.9 -12.0K # 1.92±0.12 ))22"&0'5 &gJ,L,A5)2I@tgJ,L,<,12"',9o,H&2A<,#?F=A<,9*%.2B,Fj>Yf=, 4)22"&0'5,),hg-i,%6?0()(0/',(%&#%*)("*%,/.,E@,o,)'8,),4*057('%22,(%&#%*)("*%,*)(0/,/.,@BM,4%(G%%',(7%,(G/, hg-i,.0'%,2(*"?("*%,$0'%2j<, ?4)2%8,/',hg--i,)22"&0'5,),#7/(/',8/&0')(%8,*%50/',9TVR=,2"*.)?%,(%&#%*)("*%,/.,,4)2%8,/',),g7)4*0%*,0'0(0)$,&)22,."'?(0/'YF>YE, # # # # # # # # # # # # # # # # # # # #

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 24 U"#*1@@+(<(/)%&G#^-'1&(3#

a b c d

f g h e Flux density [mJy]

velocity offset [km/s] # , ^-'1&(# *!`, `880(0/')$, 80)5'/2(0?, $0'%2, /., (7%, 2()*A./*&0'5, 0'(%*2(%$$)*, &%80"&, 0', OZ[!EB, C%'()(03%, 8%(%?(0/'2,)'8,"##%*,$0&0(2,/',(7%,gJ,*LM!N>,,)'8,,(7%,OFJ,*o)o?,L,F,FF,(7%,gOm,*L,)'8,(7%,h]--i,E4F!E4<,$0'%,9'=,(/G)*8, OZ[!E,9gJ,*LM!N,)'8,,h]--i,)'8,OZ,.*/&,(7%,!1`>,)$$,/(7%*,(%'()(03%,8%(%?(0/'2I$0&0(2, .*/&,(7%,T8c-=B,`,&/*%,2%'20(03%,?/'2(*)0'(,/',(7%,gJ,*L, .$"6A0'3%*(%8, #*/.0$%, /., (7%, OFJ, *o)o?, L, EF,(7%,2#%?(*"&,27/G2,),70'(,/.,),2%$.A)42/*4%8,$0'%B, , a b c d e

f ghi j

,, ^-'1&(#*:`,g/'(0'""&,%&0220/',(/G)*8,OZ[!EB,%!(>,1)#2,/.,(7%,/42%*3%8A.*)&%,E,&&,9%>,g`R1`=>,F,&&, 9>=>,,T8c-=>,,)'8,PP@,Q&,9(>,!1`=,?/'(0'""&,%&0220/'>,)2,/4()0'%8,4+,?/$$)#20'5,8)(), /3%*, &"$(0#$%, .*%K"%'?+, 2%("#2, )'8, )**)+, ?/'.05"*)(0/'2B, C7%,*%2/$"(0/',/.,%)?7,&)#,02,0'80?)(%8,0', (7%, 4/((/&, $%.(, ?/*'%*, /., %)?7, #)'%$B, U&0220/', 02, 8%(%?(%8, )(, , , ,

, )'8, , *%2#%?(03%$+, 97057, 205')$A(/A'/02%, *)(0/, &)#2, 27/G, 4%)&, *%208")$2, ).(%*, ?$%)'0'5, 8"%, (/, $0&0(%8, Q0, ?/3%*)5%=B, 4Aa>, O057A*%2/$"(0/', &)#2, /., (7%, /42%*3%8A.*)&%, FBj, &&, 94=>, , , T8c-=>,,,,,,,,, ,)'8,PP@,Q&,9a>,!1`=,?/'(0'""&,%&0220/'>,)2,/4()0'%8,4+,?/$$)#20'5,T8c-,`,?/'.05"*)(0/',)'8, !1`,, , )'8, PP@, Q&=, /*, ±M! 9, , )'8,,,,,,,, PP@,Q&=,/*,M!,9,G0(7/"(,%308%'?%,./*,%&0220/',/',;X<_,2?)$%2,)(,)'+,G)3%$%'5(7B,

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 25 a b c d

e f g h

i j kl

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 26 , a bc d

ef

, # ^-'1&(# *O`, !#)(0)$$+, *%2/$3%8, )(/&0?, )'8, &/$%?"$)*, $0'%, %&0220/', (/G)*82, OZ[!EB, T8c-, 7057A*%2/$"(0/', &)#2,9%!0=,)'8,#%)H,2#%?(*),9(,)'8,4=,/.,(7%,hg-i>,gJ,*Lj!Y,)'8,<@!f,)'8,OFJ,EF,gJ,*Lj!Y,)'8,OFJ=,/*,±M!, 9gJ,*L<@!f=>,)'8,)*%,0',2(%#2,/.,,F!,9gJ,*Lj!Y=>,/*,M!,9gJ,*L<@!f,)'8,OFJ=B, , , , , , , ab c

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 27 b a d

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 28 abc d e f g

h i j k l m n , , ^-'1&(# *[`, J#(0?)$,(/,&08A0'.*)*%8, 0&)5%2,/.,(7%,*%50/',)*/"'8,OZ[!EB, %!'>,E@_"E@_,20:%,*%50/'2, 0',(7%, /#(0?)$,8>,$>,9>,!,9%!0=>,'%)*A0'.*)*%8,5%,9(=>,)'8,&08A0'.*)*%8,EBY,)'8,NBM,Q&,4)'82,94,)'8,'=B,B!/>,://&A0', /',<@_"<@_,20:%,*%50/'2,0',(7%,2)&%,4)'82B,g/'(/"*2,/.,(7%,<,&&,?/'(0'""&,%&0220/',)*%,/3%*$)+%8,/',)$$, #)'%$2B,OZ[!E,02,'/(,8%(%?(%8,0',(7%,/#(0?)$,4)'82>,4"(,02,8%(%?(%8,0',5%,4)'8,)'8,$/'5G)*82B,C7%,%&0220/', ?$/2%,(/,OZ[!E,02,8/&0')(%8,4+,(7%,./*%5*/"'8,5)$)6+,\

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 29 ^-'1&(# *!!`, J#(0?)$, 2#%?(*/2?/#+, (/G)*82, OZ[!E, )'8, ./*%5*/"'8, 2/"*?%2B, o%?HI[R-!, 2#%?(*/2?/#+, (/G)*8, OZ[!EB,C7%,(/#,#)'%$,27/G2,(7%,#/20(0/',)'8,)$05'&%'(,/., (7%, 2$0(>, /3%*$)+%8, /', ), \Cg, 9A4)'8, 0&)5%B, C7%, G70(%, ?/'(/"*2,?/**%2#/'8,(/,(7%,,c,0'80?)(%2, (7%,#/20(0/',/.,\,),5)$)6+,X@BYM_,'/*(7,/.,OZ[!EB,g,)'8, V, 0'80?)(%, *%.%*%'?%, 2/"*?%2B, C7%, 4$"%, $0'%2, 0'80?)(%, (7%, 802()'?%, /., 2/"*?%2, `, )'8, c, .*/&, gB, C7%, 4/((/&, #)'%$2, 27/G,(7%,/'%A80&%'20/')$,2#%?(*),%6(*)?(%8,)(,#/20(0/'2,`, )'8,c>,G70?7,)*%,?/'202(%'(,G0(7,[+A$,%&0220/',)(,!LFBF@F, 9`=,)'8,G0(7,),[+&)'A?/'(0'""&,4*%)H,)'8,g-q,9

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 30 ab

, , ^-'1&(# *!K`, 1/8%$,.0(2,(/,(7%,gJ,*/()(0/')$,$0'%,$)88%*,/.,OZ[!EB,J42%*3%8,gJ,%6?0()(0/',$)88%*,(/G)*8, OZ[!E, 92K")*%, 2+&4/$2=, )'8, &)60&"&, $0H%$07//8, R`VUk, &/8%$, 92/$08, $0'%=, /', $0'%, 0'(%'20(+, 2?)$%, 9%>, 27)$$/G,$0&0(2,./*,2/&%,$0'%2,)*%,/..A2?)$%=>,)'8,'/*&)$0:%8,(/,(7%,gJ9*LF!<=,4*057('%22,(%&#%*)("*%,9>=B, ,

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 31 7 a b Mrk231 11 01 02 21 12 04 Arp220 14 -1 -1 -2 -2 -3 -4 -5

6 02 12 11 12 21 13 APM08279 23 2 2 2 3 3 4 HFLS3 5 12 03 13 -2 -3 -4

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Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 32 1 21 3.2 ab c 0.5 20.5 3

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(7%,WB1B,o%?H,J42%*3)(/*+>,G70?7,02,/#%*)(%8,)2,), Lett. 741, L37 (2011). 2?0%'(0.0?,#)*('%*270#,)&/'5,(7%,g)$0./*'0),-'2(0("(%, , /.,C%?7'/$/5+>,(7%,n'03%*20(+,/.,g)$0./*'0),)'8,(7%, # ])(0/')$, `%*/')"(0?2, )'8, !#)?%, `8&0'02(*)(0/'B, F,Q/.J+(0'<(/)3# # C7%, J42%*3)(/*+, G)2, &)8%, #/2204$%, 4+, (7%, W%,(7)'H,[%%,`*&"2,)'8,C)'0/,V0):A!)'(/2,./*,7%$#, 5%'%*/"2, .0')'?0)$, 2"##/*(, /., (7%, WB1B, o%?H, G0(7,8%(%*&0'0'5,(7%,2(%$$)*,&)22,/.,`*#,FF@B,!T-RU, Z/"'8)(0/'B, C7%, )"(7/*2, G027, (/, *%?/5'0:%, )'8, 7)2, 4%%', 8%3%$/#%8, 4+, ), ?/'2/*(0"&, /., 0'2(0("(%2, )?H'/G$%85%, (7%, 3%*+, 205'0.0?)'(, ?"$("*)$, */$%, )'8, $%8, 4+, g)*80.., n'03B, 9no=, )'8, 0'?$"80'5, n'03B, *%3%*%'?%,(7)(,(7%,2"&&0(,/.,1)"'),o%),7)2,)$G)+2, [%(74*085%, 9g)')8)=d, ]`Jg, 9g70')=d, gU`>, [`1, 7)8, G0(70', (7%, 0'805%'/"2, O)G)00)', 9Z*)'?%=d, -Z!->, n'03B, T)8"), 9-()$+=d, -`g, 9!#)0'=d, ?/&&"'0(+B,, W%, )*%, &/2(, ./*("')(%, (/, 7)3%, (7%, !(/?H7/$&,J42%*3)(/*+,9!G%8%'=d,-&#%*0)$,g/$$%5%, /##/*("'0(+, (/, ?/'8"?(, /42%*3)(0/'2, .*/&, (702, [/'8/'>,R`[>,ng[A1!![>,no`Cg>,n'03B,!"22%6,9no=d, &/"'()0'B, c)2%8, /', /42%*3)(0/'2, &)8%, G0(7, (7%, g)$(%?7>, ST[>, ]O!g>, n'03B, g/$/*)8/, 9n!`=B, C702, W0$$0)&, O%*2?7%$, C%$%2?/#%, 9WOC=>, 0', #)*(, "'8%*, 8%3%$/#&%'(, 7)2, 4%%', 2"##/*(%8, 4+, ')(0/')$, V0*%?(/*r2,V02?*%(0/')*+,C0&%,/.,!#)0'r2,-'2(0("(/,8%, ."'80'5, )5%'?0%2e, g!`, 9g)')8)=d, ]`Jg, 9g70')=d, `2(*/.020?), 8%, g)')*0)2, 9-`g=>, )'8, G0(7, (7%, \*)', gU`>, g]U!>, g]R!, 9Z*)'?%=d, `!-, 9-()$+=d, 1g-]], C%$%2?/#0/,g)')*0)2,9\Cg=>,0'2()$$%8,0',(7%,!#)'027, 9!#)0'=d, !]!c, 9!G%8%'=d, !CZg, 9no=d, )'8, ]`!`, J42%*3)(/*0/, 8%$, R/K"%, 8%, $/2, 1"?7)?7/2, /., (7%, 9n!`=B,T`g!,7)2,4%%',8%3%$/#%8,4+,),?/'2/*(0"&,/., -`g>,0',(7%,02$)'8,/.,[),T)$&)B,C7%,WOC,02,/#%*)(%8, 0'2(0("(%2, $%8, 4+, 1TU, 9\%*&)'+=, )'8, 0'?$"80'5, /', (7%, 02$)'8, /., [), T)$&), 4+, (7%, -2))?, ]%G(/', nq-U, 9`"2(*0)=d, on, [%"3%'>, g![>, -1Ug, 9c%$50"&=d, \*/"#B,C7%,\Cg,)'8,2/&%,/.,(7%,WOC,/42%*3)(0/'2, gU`>, [`1, 9Z*)'?%=d, 1T-`, 9\%*&)'+=d, -]`ZA, )*%, #)*(, /., (7%, -'(%*')(0/')$, C0&%, T*/5*)&&%, -Z!-IJ``IJ`TIJ`C>, [U]!>, !-!!`, 9-()$+=d, -`g, F@<@!F@<<, 9T-e, T%*%:AZ/"*'/'=B, C702, #"4$0?)(0/', 9!#)0'=B, C702, 8%3%$/#&%'(, 7)2, 4%%', 2"##/*(%8, 4+, &)H%2, "2%, /., 8)(), #*/8"?(2, .*/&, (7%, W08%A.0%$8, (7%,."'80'5,)5%'?0%2,c1q-C,9`"2(*0)=>,U!`ATRJVUk, -'.*)*%8,!"*3%+,U6#$/*%*>,G70?7,02,),D/0'(,#*/D%?(,/., 9c%$50"&=>, gU`Ig]U!, 9Z*)'?%=>, V[R, 9\%*&)'+=>, (7%,n'03%*20(+,/.,g)$0./*'0)>,[/2,`'5%$%2>,)'8,(7%,S%(, `!-I-]`Z,9-()$+=>,)'8,g-gyCI1gyC,9!#)0'=B,!"##/*(, T*/#"$20/', [)4/*)(/*+Ig)$0./*'0), -'2(0("(%, /., ./*, g`R1`, ?/'2(*"?(0/', G)2, 8%*03%8, .*/&, (7%, C%?7'/$/5+>, ."'8%8, 4+, (7%, ])(0/')$, `%*/')"(0?2, 2()(%2,/.,g)$0./*'0)>,-$$0'/02>,)'8,1)*+$)'8>,(7%,S)&%2, )'8,!#)?%,`8&0'02(*)(0/'B, !B, 1?V/''%$$, Z/"'8)(0/'>, (7%, \/*8/', )'8, c%((+, 1//*%, Z/"'8)(0/'>, (7%, o%''%(7, CB, )'8, U0$%%', [B,

Riechers et al. (2013), Nature, in the press (under press embargo until 13:00 US Eastern time on 17 April 2013) 35