1
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Atek H, Labbé I, Furtak LJ, Chemerynska I, Fujimoto S, Setton DJ, Miller TB, Oesch P, Bezanson R, Price SH, Dayal P, Zitrin A, Kokorev V, Weaver JR, Brammer G, Dokkum PV, Williams CC, Cutler SE, Feldmann R, Fudamoto Y, Greene JE, Leja J, Maseda MV, Muzzin A, Pan R, Papovich C, Nelson EJ, Nanayakkara T, Stark DP, Stefanon M, Suess KA, Wang B, Whitaker KE. Most of the photons that reionized the Universe came from dwarf galaxies. Nature 2024; 626:975-978. [PMID: 38418911 DOI: 10.1038/s41586-024-07043-6] [Citation(s) in RCA: 3] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/16/2023] [Accepted: 01/08/2024] [Indexed: 03/02/2024]
Abstract
The identification of sources driving cosmic reionization, a major phase transition from neutral hydrogen to ionized plasma around 600-800 Myr after the Big Bang1-3, has been a matter of debate4. Some models suggest that high ionizing emissivity and escape fractions (fesc) from quasars support their role in driving cosmic reionization5,6. Others propose that the high fesc values from bright galaxies generate sufficient ionizing radiation to drive this process7. Finally, a few studies suggest that the number density of faint galaxies, when combined with a stellar-mass-dependent model of ionizing efficiency and fesc, can effectively dominate cosmic reionization8,9. However, so far, comprehensive spectroscopic studies of low-mass galaxies have not been done because of their extreme faintness. Here we report an analysis of eight ultra-faint galaxies (in a very small field) during the epoch of reionization with absolute magnitudes between MUV ≈ -17 mag and -15 mag (down to 0.005L⋆ (refs. 10,11)). We find that faint galaxies during the first thousand million years of the Universe produce ionizing photons with log[ξion (Hz erg-1)] = 25.80 ± 0.14, a factor of 4 higher than commonly assumed values12. If this field is representative of the large-scale distribution of faint galaxies, the rate of ionizing photons exceeds that needed for reionization, even for escape fractions of the order of 5%.
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Affiliation(s)
- Hakim Atek
- Institut d'Astrophysique de Paris, CNRS, Sorbonne Université, Paris, France.
| | - Ivo Labbé
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria, Australia
| | - Lukas J Furtak
- Physics Department, Ben-Gurion University of the Negev, Be'er Sheva, Israel
| | - Iryna Chemerynska
- Institut d'Astrophysique de Paris, CNRS, Sorbonne Université, Paris, France
| | - Seiji Fujimoto
- Department of Astronomy, The University of Texas at Austin, Austin, TX, USA
| | - David J Setton
- Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA, USA
| | - Tim B Miller
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | - Pascal Oesch
- Department of Astronomy, University of Geneva, Versoix, Switzerland
- Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Rachel Bezanson
- Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA, USA
| | - Sedona H Price
- Department of Physics and Astronomy and PITT PACC, University of Pittsburgh, Pittsburgh, PA, USA
| | - Pratika Dayal
- Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
| | - Adi Zitrin
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria, Australia
| | - Vasily Kokorev
- Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
| | - John R Weaver
- Department of Astronomy, University of Massachusetts, Amherst, MA, USA
| | - Gabriel Brammer
- Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | | | - Christina C Williams
- NSF's National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ, USA
- Steward Observatory, University of Arizona, Tucson, AZ, USA
| | - Sam E Cutler
- Department of Astronomy, University of Massachusetts, Amherst, MA, USA
| | - Robert Feldmann
- Institute for Computational Science, University of Zurich, Zurich, Switzerland
| | - Yoshinobu Fudamoto
- Waseda Research Institute for Science and Engineering, Faculty of Science and Engineering, Waseda University, Tokyo, Japan
- National Astronomical Observatory of Japan, Tokyo, Japan
| | - Jenny E Greene
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - Joel Leja
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, USA
- Institute for Computational and Data Sciences, The Pennsylvania State University, University Park, PA, USA
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA, USA
| | - Michael V Maseda
- Department of Astronomy, University of Wisconsin, Madison, WI, USA
| | - Adam Muzzin
- Department of Physics and Astronomy, York University, Toronto, Ontario, Canada
| | - Richard Pan
- Department of Physics and Astronomy, Tufts University, Medford, MA, USA
| | - Casey Papovich
- Department of Physics and Astronomy, Texas A&M University, College Station, TX, USA
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, College Station, TX, USA
| | - Erica J Nelson
- Department for Astrophysical and Planetary Science, University of Colorado, Boulder, CO, USA
| | - Themiya Nanayakkara
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Melbourne, Victoria, Australia
| | - Daniel P Stark
- Steward Observatory, University of Arizona, Tucson, AZ, USA
| | - Mauro Stefanon
- Departament d'Astronomia i Astrofìsica, Universitat de València, Valencia, Spain
| | - Katherine A Suess
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA, USA
- Kavli Institute for Particle Astrophysics and Cosmology and Department of Physics, Stanford University, Stanford, CA, USA
| | - Bingjie Wang
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, USA
- Institute for Computational and Data Sciences, The Pennsylvania State University, University Park, PA, USA
- Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA, USA
| | - Katherine E Whitaker
- Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
- Department of Astronomy, University of Massachusetts, Amherst, MA, USA
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Roberts-Borsani G, Treu T, Chen W, Morishita T, Vanzella E, Zitrin A, Bergamini P, Castellano M, Fontana A, Glazebrook K, Grillo C, Kelly PL, Merlin E, Nanayakkara T, Paris D, Rosati P, Yang L, Acebron A, Bonchi A, Boyett K, Bradač M, Brammer G, Broadhurst T, Calabró A, Diego JM, Dressler A, Furtak LJ, Filippenko AV, Henry A, Koekemoer AM, Leethochawalit N, Malkan MA, Mason C, Mercurio A, Metha B, Pentericci L, Pierel J, Rieck S, Roy N, Santini P, Strait V, Strausbaugh R, Trenti M, Vulcani B, Wang L, Wang X, Windhorst RA. The nature of an ultra-faint galaxy in the cosmic dark ages seen with JWST. Nature 2023:10.1038/s41586-023-05994-w. [PMID: 37198479 DOI: 10.1038/s41586-023-05994-w] [Citation(s) in RCA: 4] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/27/2022] [Accepted: 03/21/2023] [Indexed: 05/19/2023]
Abstract
In the first billion years after the Big Bang, sources of ultraviolet (UV) photons are believed to have ionized intergalactic hydrogen, rendering the Universe transparent to UV radiation. Galaxies brighter than the characteristic luminosity L* (refs. 1,2) do not provide enough ionizing photons to drive this cosmic reionization. Fainter galaxies are thought to dominate the photon budget; however, they are surrounded by neutral gas that prevents the escape of the Lyman-α photons, which has been the dominant way to identify them so far. JD1 was previously identified as a triply-imaged galaxy with a magnification factor of 13 provided by the foreground cluster Abell 2744 (ref. 3), and a photometric redshift of z ≈ 10. Here we report the spectroscopic confirmation of this very low luminosity (≈0.05 L*) galaxy at z = 9.79, observed 480 Myr after the Big Bang, by means of the identification of the Lyman break and redward continuum, as well as multiple ≳4σ emission lines, with the Near-InfraRed Spectrograph (NIRSpec) and Near-InfraRed Camera (NIRCam) instruments. The combination of the James Webb Space Telescope (JWST) and gravitational lensing shows that this ultra-faint galaxy (MUV = -17.35)-with a luminosity typical of the sources responsible for cosmic reionization-has a compact (≈150 pc) and complex morphology, low stellar mass (107.19 M⊙) and subsolar (≈0.6 Z⊙) gas-phase metallicity.
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Affiliation(s)
- Guido Roberts-Borsani
- Department of Physics and Astronomy, University of California, Los Angeles, CA, USA.
| | - Tommaso Treu
- Department of Physics and Astronomy, University of California, Los Angeles, CA, USA
| | - Wenlei Chen
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | | | - Eros Vanzella
- INAF - OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy
| | - Adi Zitrin
- Physics Department, Ben-Gurion University of the Negev, Be'er-Sheva, Israel
| | - Pietro Bergamini
- INAF - OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy
- Dipartimento di Fisica, Università degli Studi di Milano, Milan, Italy
| | - Marco Castellano
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Adriano Fontana
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Karl Glazebrook
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
| | - Claudio Grillo
- Dipartimento di Fisica, Università degli Studi di Milano, Milan, Italy
- INAF - IASF Milano, Milan, Italy
| | - Patrick L Kelly
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - Emiliano Merlin
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Themiya Nanayakkara
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
| | - Diego Paris
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Piero Rosati
- INAF - OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy
- Dipartimento di Fisica e Scienze della Terra, Università degli Studi di Ferrara, Ferrara, Italy
| | - Lilan Yang
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa, Japan
| | - Ana Acebron
- Dipartimento di Fisica, Università degli Studi di Milano, Milan, Italy
- INAF - IASF Milano, Milan, Italy
| | - Andrea Bonchi
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
- ASI-Space Science Data Center, Rome, Italy
| | - Kit Boyett
- School of Physics, University of Melbourne, Parkville, Victoria, Australia
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia
| | - Maruša Bradač
- University of Ljubljana, Department of Mathematics and Physics, Ljubljana, Slovenia
- Department of Physics and Astronomy, University of California, Davis, CA, USA
| | - Gabriel Brammer
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Tom Broadhurst
- Department of Theoretical Physics, University of the Basque Country UPV/EHU, Bilbao, Spain
- Donostia International Physics Center (DIPC), Donostia, Spain
- IKERBASQUE, Basque Foundation for Science, Bilbao, Spain
| | - Antonello Calabró
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Jose M Diego
- Instituto de Física de Cantabria (CSIC-UC), Santander, Spain
| | - Alan Dressler
- The Observatories, The Carnegie Institution for Science, Pasadena, CA, USA
| | - Lukas J Furtak
- Physics Department, Ben-Gurion University of the Negev, Be'er-Sheva, Israel
| | | | - Alaina Henry
- Space Telescope Science Institute, Baltimore, MD, USA
- Center for Astrophysical Sciences, Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | | | | | - Matthew A Malkan
- Department of Physics and Astronomy, University of California, Los Angeles, CA, USA
| | - Charlotte Mason
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Amata Mercurio
- Dipartimento di Fisica 'E.R. Caianiello', Università degli Studi di Salerno, Fisciano (SA), Italy
- INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy
| | - Benjamin Metha
- Department of Physics and Astronomy, University of California, Los Angeles, CA, USA
- School of Physics, University of Melbourne, Parkville, Victoria, Australia
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia
| | - Laura Pentericci
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Justin Pierel
- Space Telescope Science Institute, Baltimore, MD, USA
| | - Steven Rieck
- School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA
| | - Namrata Roy
- Center for Astrophysical Sciences, Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | - Paola Santini
- INAF Osservatorio Astronomico di Roma, Monteporzio Catone, Rome, Italy
| | - Victoria Strait
- Cosmic Dawn Center (DAWN), Copenhagen, Denmark
- Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Robert Strausbaugh
- Minnesota Institute For Astrophysics, University of Minnesota, Minneapolis, MN, USA
| | - Michele Trenti
- School of Physics, University of Melbourne, Parkville, Victoria, Australia
- ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia
| | | | - Lifan Wang
- Mitchell Institute for Fundamental Physics & Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX, USA
| | - Xin Wang
- School of Astronomy and Space Science, University of Chinese Academy of Sciences (UCAS), Beijing, China
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
- Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University, Beijing, China
| | - Rogier A Windhorst
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ, USA
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3
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Muzio MS, Farrar GR, Unger M. Probing the environments surrounding ultrahigh energy cosmic ray accelerators and their implications for astrophysical neutrinos. Int J Clin Exp Med 2022. [DOI: 10.1103/physrevd.105.023022] [Citation(s) in RCA: 6] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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4
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The Interstellar Medium of Dwarf Galaxies. GALAXIES 2022. [DOI: 10.3390/galaxies10010011] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Dwarf galaxies are by far the most numerous galaxies in the Universe, showing properties that are quite different from those of their larger and more luminous cousins. This review focuses on the physical and chemical properties of the interstellar medium of those dwarfs that are known to host significant amounts of gas and dust. The neutral and ionized gas components and the impact of the dust will be discussed, as well as first indications for the existence of active nuclei in these sources. Cosmological implications are also addressed, considering the primordial helium abundance and the similarity of local Green Pea galaxies with young, sometimes protogalactic sources in the early Universe.
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5
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Hazen RM, Morrison SM, Prabhu A. An evolutionary system of mineralogy. Part III: Primary chondrule mineralogy (4566 to 4561 Ma). THE AMERICAN MINERALOGIST 2021; 106:325-350. [PMID: 33867542 PMCID: PMC8051150 DOI: 10.2138/am-2020-7564] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Information-rich attributes of minerals reveal their physical, chemical, and biological modes of origin in the context of planetary evolution, and thus they provide the basis for an evolutionary system of mineralogy. Part III of this system considers the formation of 43 different primary crystalline and amorphous phases in chondrules, which are diverse igneous droplets that formed in environments with high dust/gas ratios during an interval of planetesimal accretion and differentiation between 4566 and 4561 Ma. Chondrule mineralogy is complex, with several generations of initial droplet formation via various proposed heating mechanisms, followed in many instances by multiple episodes of reheating and partial melting. Primary chondrule mineralogy thus reflects a dynamic stage of mineral evolution, when the diversity and distribution of natural condensed solids expanded significantly.
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Affiliation(s)
- Robert M. Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, D.C. 20015, U.S.A
| | - Shaunna M. Morrison
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, D.C. 20015, U.S.A
| | - Anirudh Prabhu
- Tetherless World Constellation, Department of Earth and Environmental Sciences, Rensselaer Polytechnic Institute, Troy, New York 12180, U.S.A
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6
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Hazra DK, Paoletti D, Finelli F, Smoot GF. Joining Bits and Pieces of Reionization History. PHYSICAL REVIEW LETTERS 2020; 125:071301. [PMID: 32857553 DOI: 10.1103/physrevlett.125.071301] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/04/2019] [Revised: 06/25/2019] [Accepted: 07/15/2020] [Indexed: 06/11/2023]
Abstract
Cosmic microwave background (CMB) temperature and polarization anisotropies from Planck have estimated a lower value of the optical depth to reionization (τ) compared to WMAP. A significant period in the reionization history would then fall within 6<redshift(z)<10, where detection of galaxies with Hubble frontier fields program and independent estimation of neutral hydrogen in the inter galactic medium by Lyman-α observations are also available. This overlap allows an analysis of cosmic reionization which utilizes a direct combination of CMB and these astrophysical measurements and potentially breaks degeneracies in parameters describing the physics of reionization. For the first time we reconstruct reionization histories by assuming photoionization and recombination rates to be free-form and by allowing underlying cosmological parameters to vary with CMB (temperature and polarization anisotropies and lensing) data from Planck 2018 release and a compilation of astrophysical data. We find an excellent agreement between the low-ℓ Planck 2018 High Frequency Instrument polarization likelihood and astrophysical data in determining the integrated optical depth. By combining both data, we report for a minimal reconstruction τ=0.051_{-0.0012-0.002}^{+0.001+0.002} at 68% and 95% C.L., which, for the errors in the current astrophysical measurements quoted in the literature, is nearly twice better than the projected cosmic variance limited CMB measurements. For the duration of reionization, redshift interval between 10%, and complete ionization, we get 2.9_{-0.16-0.26}^{+0.12+0.29} at 68% and 95% C.L., which improves significantly on the corresponding result obtained by using Planck 2015 data. By a Bayesian analysis of the combined results we do not find evidence beyond monotonic reionization histories, therefore a multiphase reionization scenario such as a first burst of reionization followed by recombination plateau and thereafter complete reionization is disfavored compared to minimal alternatives.
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Affiliation(s)
- Dhiraj Kumar Hazra
- The Institute of Mathematical Sciences, HBNI, CIT Campus, Chennai 600113, India; INAF OAS Bologna, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 101, I-40129 Bologna, Italy; and INFN, Sezione di Bologna, via Irnerio 46, 40126 Bologna, Italy
| | - Daniela Paoletti
- INAF OAS Bologna, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 101, I-40129 Bologna, Italy and INFN, Sezione di Bologna, via Irnerio 46, 40126 Bologna, Italy
| | - Fabio Finelli
- INAF OAS Bologna, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, via Gobetti 101, I-40129 Bologna, Italy and INFN, Sezione di Bologna, via Irnerio 46, 40126 Bologna, Italy
| | - George F Smoot
- Paris Centre for Cosmological Physics, Université de Paris, CNRS, Astroparticule et Cosmologie, F-75013 Paris, France; Institute for Advanced Study & Physics Department, Hong Kong University of Science and Technology, Clear Water Bay, Kowloon, Hong Kong; Physics Department and Lawrence Berkeley National Laboratory, University of California, Berkeley, California 94720, USA; and Energetic Cosmos Laboratory, Nazarbayev University, Astana, Kazakhstan
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7
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Hazen RM, Morrison SM. An evolutionary system of mineralogy. Part I: Stellar mineralogy (>13 to 4.6 Ga). THE AMERICAN MINERALOGIST 2020; 105:627-651. [PMID: 33867541 PMCID: PMC8051151 DOI: 10.2138/am-2020-7173] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Minerals preserve records of the physical, chemical, and biological histories of their origins and subsequent alteration, and thus provide a vivid narrative of the evolution of Earth and other worlds through billions of years of cosmic history. Mineral properties, including trace and minor elements, ratios of isotopes, solid and fluid inclusions, external morphologies, and other idiosyncratic attributes, represent information that points to specific modes of formation and subsequent environmental histories-information essential to understanding the co-evolving geosphere and biosphere. This perspective suggests an opportunity to amplify the existing system of mineral classification, by which minerals are defined solely on idealized end-member chemical compositions and crystal structures. Here we present the first in a series of contributions to explore a complementary evolutionary system of mineralogy-a classification scheme that links mineral species to their paragenetic modes. The earliest stage of mineral evolution commenced with the appearance of the first crystals in the universe at >13 Ga and continues today in the expanding, cooling atmospheres of countless evolved stars, which host the high-temperature (T > 1000 K), low-pressure (P < 10-2 atm) condensation of refractory minerals and amorphous phases. Most stardust is thought to originate in three distinct processes in carbon- and/or oxygen-rich mineral-forming stars: (1) condensation in the cooling, expanding atmospheres of asymptotic giant branch stars; (2) during the catastrophic explosions of supernovae, most commonly core collapse (Type II) supernovae; and (3) classical novae explosions, the consequence of runaway fusion reactions at the surface of a binary white dwarf star. Each stellar environment imparts distinctive isotopic and trace element signatures to the micro- and nanoscale stardust grains that are recovered from meteorites and micrometeorites collected on Earth's surface, by atmospheric sampling, and from asteroids and comets. Although our understanding of the diverse mineral-forming environments of stars is as yet incomplete, we present a preliminary catalog of 41 distinct natural kinds of stellar minerals, representing 22 official International Mineralogical Association (IMA) mineral species, as well as 2 as yet unapproved crystalline phases and 3 kinds of non-crystalline condensed phases not codified by the IMA.
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Affiliation(s)
- Robert M. Hazen
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A
| | - Shaunna M. Morrison
- Earth and Planets Laboratory, Carnegie Institution for Science, 5251 Broad Branch Road NW, Washington, DC 20015, U.S.A
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9
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Beyond Optical Depth: Future Determination of Ionization History from the Cosmic Microwave Background. ACTA ACUST UNITED AC 2020; 889. [PMID: 32255818 DOI: 10.3847/1538-4357/ab5fd5] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
We explore the fundamental limits to which reionization histories can be constrained using only large-scale cosmic microwave background (CMB) anisotropy measurements. The redshift distribution of the fractional ionization x e (z) affects the angular distribution of CMB polarization. We project constraints on the reionization history of the universe using low-noise full-sky temperature and E-mode measurements of the CMB. We show that the measured TE power spectrum, C ^ ℓ TE , has roughly one quarter of the constraining power of C ^ ℓ EE on the reionization optical depth τ, and its addition improves the precision on τ by 20% over using C ^ ℓ EE only. We also use a two-step reionization model with an additional high-redshift step, parameterized by an early ionization fraction x e min , and a late reionization step at z re. We find that future high signal-to-noise measurements of the multipoles 10 ⩽ ℓ < 20 are especially important for breaking the degeneracy between x e min and z re. In addition, we show that the uncertainties on these parameters determined from a map with sensitivity 10 μK arcmin are less than 5% larger than the uncertainties in the noiseless case, making this noise level a natural target for future large sky area E-mode measurements.
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10
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Abstract
Elements heavier than helium are produced in the lives and deaths of stars. This Review discusses when and how the process of nucleosynthesis made elements. High-mass stars fuse elements much faster, fuse heavier nuclei, and die more catastrophically than low-mass stars. The explosions of high-mass stars as supernovae release elements into their surroundings. Supernovae can leave behind neutron stars, which may later merge to produce additional heavy elements. Dying low-mass stars throw off their enriched outer layers, leaving behind white dwarfs. These white dwarfs may also later merge and synthesize elements as well. Because these processes occur on different time scales and produce a different pattern of elements, the composition of the Universe changes over time as stars populate the periodic table.
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Affiliation(s)
- Jennifer A Johnson
- Department of Astronomy and Center for Cosmology and AstroParticle Physics, Ohio State University, Columbus, OH, USA.
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11
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12
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A gamma-ray determination of the Universe's star formation history. Science 2018; 362:1031-1034. [PMID: 30498122 DOI: 10.1126/science.aat8123] [Citation(s) in RCA: 69] [Impact Index Per Article: 11.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/06/2018] [Accepted: 10/11/2018] [Indexed: 11/02/2022]
Abstract
The light emitted by all galaxies over the history of the Universe produces the extragalactic background light (EBL) at ultraviolet, optical, and infrared wavelengths. The EBL is a source of opacity for gamma rays via photon-photon interactions, leaving an imprint in the spectra of distant gamma-ray sources. We measured this attenuation using 739 active galaxies and one gamma-ray burst detected by the Fermi Large Area Telescope. This allowed us to reconstruct the evolution of the EBL and determine the star formation history of the Universe over 90% of cosmic time. Our star formation history is consistent with independent measurements from galaxy surveys, peaking at redshift z ~ 2. Upper limits of the EBL at the epoch of reionization suggest a turnover in the abundance of faint galaxies at z ~ 6.
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Quantitative Constraints on the Reionization History from the IGM Damping Wing Signature in Two Quasars at z > 7. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aad6dc] [Citation(s) in RCA: 142] [Impact Index Per Article: 23.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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14
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Lovell MR, Zavala J, Vogelsberger M, Shen X, Cyr-Racine FY, Pfrommer C, Sigurdson K, Boylan-Kolchin M, Pillepich A. ETHOS - an effective theory of structure formation: predictions for the high-redshift Universe - abundance of galaxies and reionization. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 477:2886-2899. [PMID: 30598558 PMCID: PMC6310026 DOI: 10.1093/mnras/sty818] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We contrast predictions for the high-redshift galaxy population and reionization history between cold dark matter (CDM) and an alternative self-interacting dark matter model based on the recently developed ETHOS framework that alleviates the small-scale CDM challenges within the Local Group. We perform the highest resolution hydrodynamical cosmological simulations (a 36 Mpc3 volume with gas cell mass of ∼ 105 M⊙ and minimum gas softening of ∼ 180 pc) within ETHOS to date - plus a CDM counterpart - to quantify the abundance of galaxies at high redshift and their impact on reionization. We find that ETHOS predicts galaxies with higher ultraviolet (UV) luminosities than their CDM counterparts and a faster build-up of the faint end of the UV luminosity function. These effects, however, make the optical depth to reionization less sensitive to the power spectrum cut-off: the ETHOS model differs from the CDM τ value by only 10 per cent and is consistent with Planck limits if the effective escape fraction of UV photons is 0.1-0.5. We conclude that current observations of high-redshift luminosity functions cannot differentiate between ETHOS and CDM models, but deep James Webb Space Telescope surveys of strongly lensed, inherently faint galaxies have the potential to test non-CDM models that offer attractive solutions to CDM's Local Group problems.
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Affiliation(s)
- Mark R Lovell
- Center for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland
- Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK
- Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
| | - Jesús Zavala
- Center for Astrophysics and Cosmology, Science Institute, University of Iceland, Dunhagi 5, 107 Reykjavik, Iceland
| | - Mark Vogelsberger
- Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | - Xuejian Shen
- Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
| | | | - Christoph Pfrommer
- Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany
| | - Kris Sigurdson
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia V6T 1Z1, Canada
| | - Michael Boylan-Kolchin
- Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA
| | - Annalisa Pillepich
- Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany
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15
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Zick TO, Weisz DR, Boylan-Kolchin M. Globular clusters in high-redshift dwarf galaxies: a case study from the Local Group. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 477:480-490. [PMID: 30598557 PMCID: PMC6310024 DOI: 10.1093/mnras/sty662] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We present the reconstructed evolution of rest-frame ultraviolet (UV) luminosities of the most massive Milky Way dwarf spheroidal satellite galaxy, Fornax, and its five globular clusters (GCs) across redshift, based on analysis of the stellar fossil record and stellar population synthesis modelling. We find that (1) Fornax's (proto-)GCs can generate 10-100 times more UV flux than the field population, despite comprising <~ 5 per cent of the stellar mass at the relevant redshifts; (2) due to their respective surface brightnesses, it is more likely that faint, compact sources in the Hubble Frontier Fields (HFFs) are GCs hosted by faint galaxies, than faint galaxies themselves. This may significantly complicate the construction of a galaxy UV luminosity function at z > 3. (3) GC formation can introduce order-of-magnitude errors in abundance matching. We also find that some compact HFF objects are consistent with the reconstructed properties of Fornax's GCs at the same redshifts (e.g. surface brightness, star formation rate), suggesting we may have already detected proto-GCs in the early Universe. Finally, we discuss the prospects for improving the connections between local GCs and proto-GCs detected in the early Universe.
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Affiliation(s)
- Tom O. Zick
- Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA
- Lawrence Livermore National Laboratory, PO Box 808 L-210, Livermore, CA 94551, USA
| | - Daniel R. Weisz
- Department of Astronomy, University of California Berkeley, Berkeley, CA 94720, USA
| | - Michael Boylan-Kolchin
- Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712, USA
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16
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Hashimoto T, Laporte N, Mawatari K, Ellis RS, Inoue AK, Zackrisson E, Roberts-Borsani G, Zheng W, Tamura Y, Bauer FE, Fletcher T, Harikane Y, Hatsukade B, Hayatsu NH, Matsuda Y, Matsuo H, Okamoto T, Ouchi M, Pelló R, Rydberg CE, Shimizu I, Taniguchi Y, Umehata H, Yoshida N. The onset of star formation 250 million years after the Big Bang. Nature 2018; 557:392-395. [PMID: 29769675 DOI: 10.1038/s41586-018-0117-z] [Citation(s) in RCA: 181] [Impact Index Per Article: 30.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/24/2017] [Accepted: 03/14/2018] [Indexed: 11/09/2022]
Abstract
A fundamental quest of modern astronomy is to locate the earliest galaxies and study how they influenced the intergalactic medium a few hundred million years after the Big Bang1-3. The abundance of star-forming galaxies is known to decline4,5 from redshifts of about 6 to 10, but a key question is the extent of star formation at even earlier times, corresponding to the period when the first galaxies might have emerged. Here we report spectroscopic observations of MACS1149-JD1 6 , a gravitationally lensed galaxy observed when the Universe was less than four per cent of its present age. We detect an emission line of doubly ionized oxygen at a redshift of 9.1096 ± 0.0006, with an uncertainty of one standard deviation. This precisely determined redshift indicates that the red rest-frame optical colour arises from a dominant stellar component that formed about 250 million years after the Big Bang, corresponding to a redshift of about 15. Our results indicate that it may be possible to detect such early episodes of star formation in similar galaxies with future telescopes.
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Affiliation(s)
- Takuya Hashimoto
- Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan. .,National Astronomical Observatory of Japan, Tokyo, Japan.
| | - Nicolas Laporte
- Department of Physics and Astronomy, University College London, London, UK.,IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
| | - Ken Mawatari
- Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan
| | - Richard S Ellis
- Department of Physics and Astronomy, University College London, London, UK
| | - Akio K Inoue
- Department of Environmental Science and Technology, Faculty of Design Technology, Osaka Sangyo University, Osaka, Japan
| | - Erik Zackrisson
- Department of Physics and Astronomy, Uppsala University, Uppsala, Sweden
| | | | - Wei Zheng
- Department of Physics & Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | - Yoichi Tamura
- Division of Particle and Astrophysical Science, Graduate School of Science, Nagoya University, Nagoya, Japan
| | - Franz E Bauer
- Instituto de Astrofísica and Centro de Astroingeniería, Facultad de Física, Pontificia Universidad Católica de Chile, Santiago, Chile.,Millennium Institute of Astrophysics (MAS), Santiago, Chile.,Space Science Institute, Boulder, CO, USA
| | - Thomas Fletcher
- Department of Physics and Astronomy, University College London, London, UK
| | - Yuichi Harikane
- Institute for Cosmic Ray Research, The University of Tokyo, Chiba, Japan.,Department of Physics, Graduate School of Science, The University of Tokyo, Tokyo, Japan
| | - Bunyo Hatsukade
- Institute of Astronomy, The University of Tokyo, Tokyo, Japan
| | - Natsuki H Hayatsu
- Department of Physics, Graduate School of Science, The University of Tokyo, Tokyo, Japan.,European Southern Observatory, Garching bei München, Germany
| | - Yuichi Matsuda
- National Astronomical Observatory of Japan, Tokyo, Japan.,Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), Tokyo, Japan
| | - Hiroshi Matsuo
- National Astronomical Observatory of Japan, Tokyo, Japan.,Department of Astronomical Science, School of Physical Sciences, The Graduate University for Advanced Studies (SOKENDAI), Tokyo, Japan
| | - Takashi Okamoto
- Department of Cosmosciences, Graduates School of Science, Hokakido University, Sapporo, Japan
| | - Masami Ouchi
- Institute for Cosmic Ray Research, The University of Tokyo, Chiba, Japan.,Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Chiba, Japan
| | - Roser Pelló
- IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
| | - Claes-Erik Rydberg
- Universität Heidelberg, Zentrum für Astronomie, Institut für Theoretische Astrophysik, Heidelberg, Germany
| | - Ikkoh Shimizu
- Theoretical Astrophysics, Department of Earth and Space Science, Osaka University, Osaka, Japan
| | | | - Hideki Umehata
- Institute of Astronomy, The University of Tokyo, Tokyo, Japan.,The Open University of Japan, Chiba, Japan.,The Institute of Physical and Chemical Research (RIKEN), Saitama, Japan
| | - Naoki Yoshida
- Department of Physics, Graduate School of Science, The University of Tokyo, Tokyo, Japan.,Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, Chiba, Japan
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17
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The Universe Is Reionizing atz∼ 7: Bayesian Inference of the IGM Neutral Fraction Using LyαEmission from Galaxies. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aab0a7] [Citation(s) in RCA: 159] [Impact Index Per Article: 26.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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18
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A Model Connecting Galaxy Masses, Star Formation Rates, and Dust Temperatures across Cosmic Time. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aaa3f0] [Citation(s) in RCA: 18] [Impact Index Per Article: 3.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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19
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van de Bruck C, Mifsud J. Searching for dark matter-dark energy interactions: Going beyond the conformal case. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.023506] [Citation(s) in RCA: 44] [Impact Index Per Article: 7.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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20
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Boylan-Kolchin M. The globular cluster-dark matter halo connection. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2017; 472:3120-3130. [PMID: 30546160 PMCID: PMC6288678 DOI: 10.1093/mnras/stx2164] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
I present a simple phenomenological model for the observed linear scaling of the stellar mass in old globular clusters (GCs) with z = 0 halo mass in which the stellar mass in GCs scales linearly with progenitor halo mass at z = 6 above a minimum halo mass for GC formation. This model reproduces the observed M GCs-M halo relation at z = 0 and results in a prediction for the minimum halo mass at z = 6 required for hosting one GC: M min(z = 6) = 1.07 × 109 M⊙. Translated to z = 0, the mean threshold mass is M halo(z = 0) ≈ 2 × 1010 M⊙. I explore the observability of GCs in the reionization era and their contribution to cosmic reionization, both of which depend sensitively on the (unknown) ratio of GC birth mass to present-day stellar mass, ξ. Based on current detections of z ≳ 6 objects with M 1500<-17, values of ξ > 10 are strongly disfavoured; this, in turn, has potentially important implications for GC formation scenarios. Even for low values of ξ, some observed high-z galaxies may actually be GCs, complicating estimates of reionization-era galaxy ultraviolet luminosity functions and constraints on dark matter models. GCs are likely important reionization sources if 5 ≲ ξ ≲ 10. I also explore predictions for the fraction of accreted versus in situ GCs in the local Universe and for descendants of systems at the halo mass threshold of GC formation (dwarf galaxies). An appealing feature of the model presented here is the ability to make predictions for GC properties based solely on dark matter halo merger trees.
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Affiliation(s)
- Michael Boylan-Kolchin
- Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA
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21
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Emulating Simulations of Cosmic Dawn for 21 cm Power Spectrum Constraints on Cosmology, Reionization, and X-Ray Heating. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/aa8bb4] [Citation(s) in RCA: 60] [Impact Index Per Article: 8.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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22
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Results from EDGES High-band. I. Constraints on Phenomenological Models for the Global 21 cm Signal. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/aa88d1] [Citation(s) in RCA: 68] [Impact Index Per Article: 9.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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23
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Upper Limits on the 21 cm Epoch of Reionization Power Spectrum from One Night with LOFAR. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/aa63e7] [Citation(s) in RCA: 170] [Impact Index Per Article: 24.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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24
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25
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CALIBRATION OF THE EDGES HIGH-BAND RECEIVER TO OBSERVE THE GLOBAL 21 cm SIGNATURE FROM THE EPOCH OF REIONIZATION. ACTA ACUST UNITED AC 2017. [DOI: 10.3847/1538-4357/835/1/49] [Citation(s) in RCA: 39] [Impact Index Per Article: 5.6] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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26
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27
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Abstract
AbstractAn important effort has been recently made to detect spectroscopically galaxies at z ~ 6 and higher where the cosmic reionization is thought to occur. The drop of the fraction of Lyman Alpha Emitters (LAEs) at z>6 is currently interpreted as an effect of the increasing neutral hydrogen density.We present preliminary results from the latest VLT/FORS2 programs, combined with ESO archival data, to perform a large census of z ~ 6 galaxies. We derive their physical properties as stellar mass and dust attenuation with an SED fitting tool including nebular emission which is of primeval importance because IRAC channels are strongly contaminated by emission lines at those redshifts. We take a special care to derive with precision the redshift of non LAEs to perform a comparison of their properties with the LAE population and derive as accurately as possible the fraction of LAEs. In particular, we compare the UV beta slope with the Lyα equivalent width which are known to correlate at lower redshift.We also report the detection of few peculiar z ~ 6 galaxies with extremely blue UV β slope (~−3), which can be a signature of unusual stellar populations (e.g., very hot and massive stars).
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28
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29
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Inoue AK, Tamura Y, Matsuo H, Mawatari K, Shimizu I, Shibuya T, Ota K, Yoshida N, Zackrisson E, Kashikawa N, Kohno K, Umehata H, Hatsukade B, Iye M, Matsuda Y, Okamoto T, Yamaguchi Y. Detection of an oxygen emission line from a high-redshift galaxy in the reionization epoch. Science 2016; 352:1559-62. [PMID: 27312046 DOI: 10.1126/science.aaf0714] [Citation(s) in RCA: 133] [Impact Index Per Article: 16.6] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/14/2015] [Accepted: 05/16/2016] [Indexed: 11/02/2022]
Abstract
The physical properties and elemental abundances of the interstellar medium in galaxies during cosmic reionization are important for understanding the role of galaxies in this process. We report the Atacama Large Millimeter/submillimeter Array detection of an oxygen emission line at a wavelength of 88 micrometers from a galaxy at an epoch about 700 million years after the Big Bang. The oxygen abundance of this galaxy is estimated at about one-tenth that of the Sun. The nondetection of far-infrared continuum emission indicates a deficiency of interstellar dust in the galaxy. A carbon emission line at a wavelength of 158 micrometers is also not detected, implying an unusually small amount of neutral gas. These properties might allow ionizing photons to escape into the intergalactic medium.
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Affiliation(s)
- Akio K Inoue
- College of General Education, Osaka Sangyo University, 3-1-1 Nakagaito, Daito, Osaka 574-8530, Japan.
| | - Yoichi Tamura
- Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
| | - Hiroshi Matsuo
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Ken Mawatari
- College of General Education, Osaka Sangyo University, 3-1-1 Nakagaito, Daito, Osaka 574-8530, Japan
| | - Ikkoh Shimizu
- Department of Earth and Space Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, Japan
| | - Takatoshi Shibuya
- Institute for Cosmic Ray Research, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan
| | - Kazuaki Ota
- Kavli Institute for Cosmology, University of Cambridge, Cambridge CB3 0HA, UK. Cavendish Laboratory, University of Cambridge, Cambridge CB3 0HE, UK
| | - Naoki Yoshida
- Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan. Kavli IPMU, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan
| | - Erik Zackrisson
- Department of Physics and Astronomy, Uppsala University, SE-751 20 Uppsala, Sweden
| | - Nobunari Kashikawa
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Kotaro Kohno
- Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
| | - Hideki Umehata
- Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan. European Southern Observatory, D-85748 Garching, Germany
| | - Bunyo Hatsukade
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Masanori Iye
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Yuichi Matsuda
- National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Takashi Okamoto
- Department of Cosmosciences, Graduate School of Science, Hokkaido University, N10 W8, Kitaku, Sapporo, Hokkaido 060-0810, Japan
| | - Yuki Yamaguchi
- Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan
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30
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THESWIFTGRB HOST GALAXY LEGACY SURVEY. II. REST-FRAME NEAR-IR LUMINOSITY DISTRIBUTION AND EVIDENCE FOR A NEAR-SOLAR METALLICITY THRESHOLD. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0004-637x/817/1/8] [Citation(s) in RCA: 119] [Impact Index Per Article: 14.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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31
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Atek H, Richard J, Jauzac M, Kneib JP, Natarajan P, Limousin M, Schaerer D, Jullo E, Ebeling H, Egami E, Clement B. ARE ULTRA-FAINT GALAXIES ATz= 6–8 RESPONSIBLE FOR COSMIC REIONIZATION? COMBINED CONSTRAINTS FROM THE HUBBLE FRONTIER FIELDS CLUSTERS AND PARALLELS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/814/1/69] [Citation(s) in RCA: 142] [Impact Index Per Article: 15.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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32
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Bouwens RJ, Illingworth GD, Oesch PA, Caruana J, Holwerda B, Smit R, Wilkins S. REIONIZATION AFTERPLANCK: THE DERIVED GROWTH OF THE COSMIC IONIZING EMISSIVITY NOW MATCHES THE GROWTH OF THE GALAXY UV LUMINOSITY DENSITY. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/811/2/140] [Citation(s) in RCA: 278] [Impact Index Per Article: 30.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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33
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Zitrin A, Labbé I, Belli S, Bouwens R, Ellis RS, Roberts-Borsani G, Stark DP, Oesch PA, Smit R. Ly
α
EMISSION FROM A LUMINOUS
z
= 8.68 GALAXY: IMPLICATIONS FOR GALAXIES AS TRACERS OF COSMIC REIONIZATION. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/2041-8205/810/1/l12] [Citation(s) in RCA: 153] [Impact Index Per Article: 17.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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34
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Ali ZS, Parsons AR, Zheng H, Pober JC, Liu A, Aguirre JE, Bradley RF, Bernardi G, Carilli CL, Cheng C, DeBoer DR, Dexter MR, Grobbelaar J, Horrell J, Jacobs DC, Klima P, MacMahon DHE, Maree M, Moore DF, Razavi N, Stefan II, Walbrugh WP, Walker A. PAPER-64 CONSTRAINTS ON REIONIZATION: THE 21 cm POWER SPECTRUM ATz= 8.4. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/809/1/61] [Citation(s) in RCA: 213] [Impact Index Per Article: 23.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/11/2022]
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