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Ginolfi M, Piconcelli E, Zappacosta L, Jones GC, Pentericci L, Maiolino R, Travascio A, Menci N, Carniani S, Rizzo F, Arrigoni Battaia F, Cantalupo S, De Breuck C, Graziani L, Knudsen K, Laursen P, Mainieri V, Schneider R, Stanley F, Valiante R, Verhamme A. Detection of companion galaxies around hot dust-obscured hyper-luminous galaxy W0410-0913. Nat Commun 2022; 13:4574. [PMID: 35931777 PMCID: PMC9355969 DOI: 10.1038/s41467-022-32297-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 01/12/2022] [Accepted: 07/22/2022] [Indexed: 11/28/2022] Open
Abstract
The phase transition between galaxies and quasars is often identified with the rare population of hyper-luminous, hot dust-obscured galaxies. Galaxy formation models predict these systems to grow via mergers, that can deliver large amounts of gas toward their centers, induce intense bursts of star formation and feed their supermassive black holes. Here we report the detection of 24 galaxies emitting Lyman-α emission on projected physical scales of about 400 kpc around the hyper-luminous hot dust-obscured galaxy W0410-0913, at redshift z = 3.631, using Very Large Telescope observations. While this indicates that W0410-0913 evolves in a very dense environment, we do not find clear signs of mergers that could sustain its growth. Data suggest that if mergers occurred, as models expect, these would involve less massive satellites, with only a moderate impact on the internal interstellar medium of W0410-0913, which is sustained by a rotationally-supported fast-rotating molecular disk, as Atacama Large Millimeter Array observations suggest. Lyman-alpha emission is one of the observational probes for the high-redshift universe. Here, the authors show several Lyman-alpha emitting companion galaxies around the hot dust-obscured galaxy W0410-091 suggesting that the galaxy evolves in a very dense environment.
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Affiliation(s)
- M Ginolfi
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany.
| | - E Piconcelli
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - L Zappacosta
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - G C Jones
- Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 4RH, UK.,Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - L Pentericci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - R Maiolino
- Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge, CB3 0HE, UK.,Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK
| | - A Travascio
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - N Menci
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - S Carniani
- Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126, Pisa, Italy
| | - F Rizzo
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - F Arrigoni Battaia
- Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748, Garching bei München, Germany
| | - S Cantalupo
- Department of Physics, University of Milan Bicocca, Piazza della Scienza 3, I-20126, Milano, Italy
| | - C De Breuck
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - L Graziani
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - K Knudsen
- Department of Space, Earth, and Environment, Chalmers University of Technology, Onsala Space Observatory, SE-439 92, Onsala, Sweden
| | - P Laursen
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark.,Niels Bohr Institute, University of Copenhagen, Jagtvej 128, DK-2200, Copenhagen N, Denmark
| | - V Mainieri
- European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748, Garching bei München, Germany
| | - R Schneider
- Dipartimento di Fisica, Sapienza, Universita di Roma, Piazzale Aldo Moro 5, I-00185, Roma, Italy
| | - F Stanley
- Sorbonne Université, UPMC Université Paris 6 & CNRS, UMR 7095, Institut d'Astrophysique de Paris, 98b boulevard Arago, 75014, Paris, France
| | - R Valiante
- INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040, Monte Porzio Catone, Italy
| | - A Verhamme
- Observatoire de Genéve, Université de Genève, 51 Ch. des Maillettes, 1290, Versoix, Switzerland
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A dusty compact object bridging galaxies and quasars at cosmic dawn. Nature 2022; 604:261-265. [PMID: 35418632 DOI: 10.1038/s41586-022-04454-1] [Citation(s) in RCA: 6] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/23/2021] [Accepted: 01/24/2022] [Indexed: 11/08/2022]
Abstract
Understanding how super-massive black holes form and grow in the early Universe has become a major challenge1,2 since it was discovered that luminous quasars existed only 700 million years after the Big Bang3,4. Simulations indicate an evolutionary sequence of dust-reddened quasars emerging from heavily dust-obscured starbursts that then transition to unobscured luminous quasars by expelling gas and dust5. Although the last phase has been identified out to a redshift of 7.6 (ref. 6), a transitioning quasar has not been found at similar redshifts owing to their faintness at optical and near-infrared wavelengths. Here we report observations of an ultraviolet compact object, GNz7q, associated with a dust-enshrouded starburst at a redshift of 7.1899 ± 0.0005. The host galaxy is more luminous in dust emission than any other known object at this epoch, forming 1,600 solar masses of stars per year within a central radius of 480 parsec. A red point source in the far-ultraviolet is identified in deep, high-resolution imaging and slitless spectroscopy. GNz7q is extremely faint in X-rays, which indicates the emergence of a uniquely ultraviolet compact star-forming region or a Compton-thick super-Eddington black-hole accretion disk at the dusty starburst core. In the latter case, the observed properties are consistent with predictions from cosmological simulations7 and suggest that GNz7q is an antecedent to unobscured luminous quasars at later epochs.
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Hodge JA, da Cunha E. High-redshift star formation in the Atacama large millimetre/submillimetre array era. ROYAL SOCIETY OPEN SCIENCE 2020; 7:200556. [PMID: 33489252 PMCID: PMC7813222 DOI: 10.1098/rsos.200556] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 04/01/2020] [Accepted: 11/02/2020] [Indexed: 06/12/2023]
Abstract
The Atacama Large Millimetre/submillimetre Array (ALMA) is currently in the process of transforming our view of star-forming galaxies in the distant ( z ≳ 1 ) universe. Before ALMA, most of what we knew about dust-obscured star formation in distant galaxies was limited to the brightest submillimetre sources-the so-called submillimetre galaxies (SMGs)-and even the information on those sources was sparse, with resolved (i.e. sub-galactic) observations of the obscured star formation and gas reservoirs typically restricted to the most extreme and/or strongly lensed sources. Starting with the beginning of early science operations in 2011, the last 9 years of ALMA observations have ushered in a new era for studies of high-redshift star formation. With its long baselines, ALMA has allowed observations of distant dust-obscured star formation with angular resolutions comparable to-or even far surpassing-the best current optical telescopes. With its bandwidth and frequency coverage, it has provided an unprecedented look at the associated molecular and atomic gas in these distant galaxies through targeted follow-up and serendipitous detections/blind line scans. Finally, with its leap in sensitivity compared to previous (sub-)millimetre arrays, it has enabled the detection of these powerful dust/gas tracers much further down the luminosity function through both statistical studies of colour/mass-selected galaxy populations and dedicated deep fields. We review the main advances ALMA has helped bring about in our understanding of the dust and gas properties of high-redshift ( z ≳ 1 ) star-forming galaxies during these first 9 years of its science operations, and we highlight the interesting questions that may be answered by ALMA in the years to come.
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Affiliation(s)
- J. A. Hodge
- Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
| | - E. da Cunha
- International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, Western Australia 6009, Australia
- Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australian Capital Territory 2611, Australia
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)
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