Authors

Daizhong Liu, Max Planck Institute for Extraterrestrial Physics
Natascha M. Förster Schreiber, Max Planck Institute for Extraterrestrial Physics
Kevin C. Harrington, Universidad Diego Portales
Lilian L. Lee, Max Planck Institute for Extraterrestrial Physics
Patrick S. Kamieneski, School of Earth and Space Exploration
Richard I. Davies, Max Planck Institute for Extraterrestrial Physics
Dieter Lutz, Max Planck Institute for Extraterrestrial Physics
Alvio Renzini, Osservatorio Astronomico di Padova
Stijn Wuyts, University of Bath, Department of Physics
Linda J. Tacconi, Max Planck Institute for Extraterrestrial Physics
Reinhard Genzel, Max Planck Institute for Extraterrestrial Physics
Andreas Burkert, Ludwig-Maximilians-Universität München
Rodrigo Herrera-Camus, Universidad de Concepcion
Belén Alcalde Pampliega, European Southern Observatory Santiago
Amit Vishwas, Cornell Center for Astrophysics and Planetary Science
Melanie Kaasinen, European Southern Observatory Santiago
Q. Daniel Wang, University of Massachusetts Amherst
Eric F. Jiménez-Andrade, Instituto de Radioastronomía y Astrofísica
James Lowenthal, Smith CollegeFollow
Nicholas Foo, School of Earth and Space Exploration
Brenda L. Frye, The University of Arizona
Jinyi Shangguan, Max Planck Institute for Extraterrestrial Physics
Yixian Cao, Max Planck Institute for Extraterrestrial Physics
Guido Agapito, Osservatorio Astrofisico Di Arcetri
Alex Agudo Berbel, Max Planck Institute for Extraterrestrial Physics
Capucine Barfety, Max Planck Institute for Extraterrestrial Physics
Andrea Baruffolo, Osservatorio Astronomico di Padova
Derek Berman, Cornell Center for Astrophysics and Planetary Science
Martin Black, Royal Observatory
Marco Bonaglia, Istituto Nazionale Di Astrofisica, Rome
Runa Briguglio, Osservatorio Astrofisico Di Arcetri
Luca Carbonaro, Osservatorio Astrofisico Di Arcetri

Author ORCID Identifier

Daizhong Liu: 0000-0001-9773-7479

Kevin C. Harrington: 0000-0001-5429-5762

Lilian L. Lee: 0000-0001-7457-4371

Patrick S. Kamieneski: 0000-0001-9394-6732

Richard I. Davies: 0000-0003-4949-7217

Dieter Lutz: 0000-0003-0291-9582

Alvio Renzini: 0000-0002-7093-7355

Stijn Wuyts: 0000-0003-3735-1931

Linda J. Tacconi: 0000-0002-1485-9401

Reinhard Genzel: 0000-0002-2767-9653

Andreas Burkert: 0000-0001-6879-9822

Rodrigo Herrera-Camus: 0000-0002-2775-0595

Belén Alcalde Pampliega: 0000-0002-4140-0428

Amit Vishwas: 0000-0002-4444-8929

Melanie Kaasinen: 0000-0002-1173-2579

Q. Daniel Wang: 0000-0002-9279-4041

Eric F. Jiménez-Andrade: 0000-0002-2640-5917

James Lowenthal: 0000-0001-9969-3115

Nicholas Foo: 0000-0002-7460-8460

Brenda L. Frye: 0000-0003-1625-8009

Jinyi Shangguan: 0000-0002-4569-9009

Yixian Cao: 0000-0001-5301-1326

Guido Agapito: 0000-0002-6382-2613

Capucine Barfety: 0000-0002-1952-3966

Andrea Baruffolo: 0000-0002-1114-4355

Derek Berman: 0000-0002-9800-0249

Marco Bonaglia: 0000-0002-4236-2339

Runa Briguglio: 0000-0002-0495-0543

Luca Carbonaro: 0000-0003-1492-1591

Document Type

Article

Publication Date

9-1-2024

Publication Title

Nature Astronomy

Abstract

Hyperluminous infrared galaxies (HyLIRGs) are the rarest and most extreme starbursts and found only in the distant Universe (z ≳ 1). They have intrinsic infrared (IR) luminosities LIR ≥ 1013 L⊙ and are commonly found to be major mergers. Recently, the Planck All-Sky Survey to Analyze Gravitationally-lensed Extreme Starbursts project (PASSAGES) searched ~104 deg2 of the sky and found ~20 HyLIRGs. We describe a detailed study of PJ0116-24, the brightest (μLIR ≈ 2.6 × 1014 L⊙, magnified with μ ≈ 17) Einstein-ring HyLIRG in the southern sky, at z = 2.125, with observations from the near-IR integral-field spectrograph VLT/ERIS and the submillimetre interferometer ALMA. We detected Hα, Hβ, [N ii] and [S ii] lines and obtained an extreme Balmer decrement (Hα/Hβ ≈ 8.73 ± 1.14). We modelled the molecular-gas and ionized-gas kinematics with CO(3–2) and Hα data at ~100–300 pc and (sub)kiloparsec delensed scales, respectively, finding consistent regular rotation. We found PJ0116-24 to be highly rotationally supported (vrot/σ0, mol. gas ≈ 9.4) with a richer gaseous substructure than other known HyLIRGs. Our results imply that PJ0116-24 is an intrinsically massive (Mbaryon ≈ 1011.3 M⊙) and rare starbursty disk (star-formation rate, SFR = 1,490 M⊙ yr−1) probably undergoing secular evolution. This indicates that the maximal SFR (≳1,000 M⊙ yr−1) predicted by simulations could occur during a galaxy’s secular evolution, away from major mergers.

Volume

8

Issue

9

First Page

1181

Last Page

1194

DOI

10.1038/s41550-024-02296-7

Comments

Archived as published.

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