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Ding X, Onoue M, Silverman JD, Matsuoka Y, Izumi T, Strauss MA, Jahnke K, Phillips CL, Li J, Volonteri M, Haiman Z, Andika IT, Aoki K, Baba S, Bieri R, Bosman SEI, Bottrell C, Eilers AC, Fujimoto S, Habouzit M, Imanishi M, Inayoshi K, Iwasawa K, Kashikawa N, Kawaguchi T, Kohno K, Lee CH, Lupi A, Lyu J, Nagao T, Overzier R, Schindler JT, Schramm M, Shimasaku K, Toba Y, Trakhtenbrot B, Trebitsch M, Treu T, Umehata H, Venemans BP, Vestergaard M, Walter F, Wang F, Yang J. Detection of stellar light from quasar host galaxies at redshifts above 6. Nature 2023; 621:51-55. [PMID: 37380029 DOI: 10.1038/s41586-023-06345-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/25/2022] [Accepted: 06/20/2023] [Indexed: 06/30/2023]
Abstract
The detection of starlight from the host galaxies of quasars during the reionization epoch (z > 6) has been elusive, even with deep Hubble Space Telescope observations1,2. The current highest redshift quasar host detected3, at z = 4.5, required the magnifying effect of a foreground lensing galaxy. Low-luminosity quasars4-6 from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP)7 mitigate the challenge of detecting their underlying, previously undetected host galaxies. Here we report rest-frame optical images and spectroscopy of two HSC-SSP quasars at z > 6 with the JWST. Using near-infrared camera imaging at 3.6 and 1.5 μm and subtracting the light from the unresolved quasars, we find that the host galaxies are massive (stellar masses of 13 × and 3.4 × 1010 M☉, respectively), compact and disc-like. Near-infrared spectroscopy at medium resolution shows stellar absorption lines in the more massive quasar, confirming the detection of the host. Velocity-broadened gas in the vicinity of these quasars enables measurements of their black hole masses (1.4 × 109 and 2.0 × 108 M☉, respectively). Their location in the black hole mass-stellar mass plane is consistent with the distribution at low redshift, suggesting that the relation between black holes and their host galaxies was already in place less than a billion years after the Big Bang.
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Affiliation(s)
- Xuheng Ding
- Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan.
- Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan.
| | - Masafusa Onoue
- Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan.
- Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China.
- Max Planck Institute for Astronomy, Heidelberg, Germany.
| | - John D Silverman
- Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan
- Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan
- Department of Astronomy, School of Science, The University of Tokyo, Bunkyo-ku, Japan
| | - Yoshiki Matsuoka
- Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Japan
| | - Takuma Izumi
- National Astronomical Observatory of Japan, Osawa, Mitaka, Japan
- Department of Physics, Graduate School of Science, Tokyo Metropolitan University, Hachioji, Japan
| | - Michael A Strauss
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - Knud Jahnke
- Max Planck Institute for Astronomy, Heidelberg, Germany
| | - Camryn L Phillips
- Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA
| | - Junyao Li
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
| | - Marta Volonteri
- Institute of Astrophysics of Paris, CNRS, Sorbonne Université, Paris, France
| | - Zoltan Haiman
- Department of Astronomy, Columbia University, New York, NY, USA
- Department of Physics, Columbia University, New York, NY, USA
| | - Irham Taufik Andika
- Physics Department, Technical University of München, Garching bei München, Germany
- Max Planck Institute for Astrophysics, Garching bei München, Germany
| | - Kentaro Aoki
- Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI, USA
| | - Shunsuke Baba
- Graduate School of Science and Engineering, Kagoshima University, Kagoshima, Japan
| | - Rebekka Bieri
- Institute for Computational Science, University of Zurich, Zürich, Switzerland
| | | | - Connor Bottrell
- Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo, Chiba, Japan
- Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Japan
| | | | - Seiji Fujimoto
- Department of Astronomy, The University of Texas at Austin, Austin, TX, USA
| | - Melanie Habouzit
- Max Planck Institute for Astronomy, Heidelberg, Germany
- Centre for Astronomy at the University of Heidelberg (ITA), Heidelberg, Germany
| | - Masatoshi Imanishi
- National Astronomical Observatory of Japan, Osawa, Mitaka, Japan
- Department of Astronomy, School of Science, Graduate University for Advanced Studies (SOKENDAI), Mitaka, Japan
| | - Kohei Inayoshi
- Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, China
| | - Kazushi Iwasawa
- Institute of Sciences of the Cosmos (ICCUB), University of Barcelona (IEEC-UB), Barcelona, Spain
- ICREA, Barcelona, Spain
| | - Nobunari Kashikawa
- Department of Astronomy, School of Science, The University of Tokyo, Bunkyo-ku, Japan
- Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Japan
| | - Toshihiro Kawaguchi
- Department of Economics, Management and Information Science, Onomichi City University, Onomichi, Japan
| | - Kotaro Kohno
- Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Japan
- Institute of Astronomy, Graduate School of Science, The University of Tokyo, Mitaka, Tokyo, Japan
| | | | - Alessandro Lupi
- 'G. Occhialini' Physics Department, University of Studi di Milano-Bicocca, Milano, Italy
| | - Jianwei Lyu
- Steward Observatory, University of Arizona, Tucson, AZ, USA
| | - Tohru Nagao
- Research Center for Space and Cosmic Evolution, Ehime University, Matsuyama, Japan
| | - Roderik Overzier
- Observatoryl/MCTI, Rua General José Cristino, Rio de Janeiro, Brazil
| | | | | | - Kazuhiro Shimasaku
- Department of Astronomy, School of Science, The University of Tokyo, Bunkyo-ku, Japan
- Research Center for the Early Universe, Graduate School of Science, The University of Tokyo, Bunkyo-ku, Japan
| | - Yoshiki Toba
- National Astronomical Observatory of Japan, Osawa, Mitaka, Japan
- Academia Sinica Institute of Astronomy and Astrophysics, Taipei, Taiwan
| | | | - Maxime Trebitsch
- Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands
| | - Tommaso Treu
- Department of Physics and Astronomy, University of California, Los Angeles, CA, USA
| | - Hideki Umehata
- Institute for Advanced Research, Nagoya University, Nagoya, Japan
- Department of Physics, Graduate School of Science, Nagoya University, Nagoya, Japan
| | - Bram P Venemans
- Leiden Observatory, Leiden University, Leiden, The Netherlands
| | - Marianne Vestergaard
- Steward Observatory, University of Arizona, Tucson, AZ, USA
- DARK, Niels Bohr Institute, Copenhagen N, Denmark
| | - Fabian Walter
- Max Planck Institute for Astronomy, Heidelberg, Germany
| | - Feige Wang
- Steward Observatory, University of Arizona, Tucson, AZ, USA
| | - Jinyi Yang
- Steward Observatory, University of Arizona, Tucson, AZ, USA
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Zhao X, Deng S, Gou L. 发现迄今为止最遥远的明亮类星体J0313-1806. CHINESE SCIENCE BULLETIN-CHINESE 2022. [DOI: 10.1360/tb-2022-0182] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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3
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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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4
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Wu X. 发现最古老的超大质量黑洞. CHINESE SCIENCE BULLETIN-CHINESE 2022. [DOI: 10.1360/tb-2022-0082] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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5
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Dynamics and Merger Rate of Primordial Black Holes in a Cluster. UNIVERSE 2022. [DOI: 10.3390/universe8010041] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 01/27/2023]
Abstract
The PBH clusters can be sources of gravitational waves, and the merger rate depends on the spatial distribution of PBHs in the cluster which changes over time. It is well known that gravitational collisional systems experience the core collapse that leads to significant increase of the central density and shrinking of the core. After core collapse, the cluster expands almost self-similarly (i.e., density profile extends in size without changing its shape). These dynamic processes affect the merger rate of PBHs. In this paper, the dynamics of the PBH cluster is considered using the Fokker–Planck equation. We calculate the merger rate of PBHs on cosmic time scales and show that its time dependence has a unique signature. Namely, it grows by about an order of magnitude at the moment of core collapse which depends on the characteristics of the cluster, and then decreases according to the dependence R∝t−1.48. It was obtained for monochromatic and power-law PBH mass distributions with some fixed parameters. Obtained results can be used to test the model of the PBH clusters via observation of gravitational waves at high redshift.
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Koopmans LVE, Barkana R, Bentum M, Bernardi G, Boonstra AJ, Bowman J, Burns J, Chen X, Datta A, Falcke H, Fialkov A, Gehlot B, Gurvits L, Jelić V, Klein-Wolt M, Lazio J, Meerburg D, Mellema G, Mertens F, Mesinger A, Offringa A, Pritchard J, Semelin B, Subrahmanyan R, Silk J, Trott C, Vedantham H, Verde L, Zaroubi S, Zarka P. Peering into the dark (ages) with low-frequency space interferometers: Using the 21-cm signal of neutral hydrogen from the infant universe to probe fundamental (Astro)physics. EXPERIMENTAL ASTRONOMY 2021; 51:1641-1676. [PMID: 34511720 PMCID: PMC8416573 DOI: 10.1007/s10686-021-09743-7] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 01/29/2021] [Accepted: 03/18/2021] [Indexed: 06/13/2023]
Abstract
The Dark Ages and Cosmic Dawn are largely unexplored windows on the infant Universe (z ~ 200-10). Observations of the redshifted 21-cm line of neutral hydrogen can provide valuable new insight into fundamental physics and astrophysics during these eras that no other probe can provide, and drives the design of many future ground-based instruments such as the Square Kilometre Array (SKA) and the Hydrogen Epoch of Reionization Array (HERA). We review progress in the field of high-redshift 21-cm Cosmology, in particular focussing on what questions can be addressed by probing the Dark Ages at z > 30. We conclude that only a space- or lunar-based radio telescope, shielded from the Earth's radio-frequency interference (RFI) signals and its ionosphere, enable the 21-cm signal from the Dark Ages to be detected. We suggest a generic mission design concept, CoDEX, that will enable this in the coming decades.
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Affiliation(s)
- Léon V. E. Koopmans
- Kapteyn Astronomical Institute, University of Groningen, Groningen, Netherlands
| | | | - Mark Bentum
- Eindhoven University of Technology, Eindhoven, Netherlands
- ASTRON, Dwingeloo, Netherlands
| | | | | | | | - Jack Burns
- University of Colorado Boulder, Boulder, CO USA
| | | | | | | | | | | | - Leonid Gurvits
- JIVE and Delft University of Technology, Delft, Netherlands
| | | | | | | | - Daan Meerburg
- VSI, University of Groningen, Groningen, Netherlands
| | | | - Florent Mertens
- Kapteyn Astronomical Institute, University of Groningen, Groningen, Netherlands
- Observatoire de Paris, Paris, France
| | | | | | | | | | | | - Joseph Silk
- Institut d’astrophysique de Paris, Paris, France
- University of Oxford, Oxford, UK
| | | | | | - Licia Verde
- Institute of Cosmological Sciences, Barcelona, Spain
| | - Saleem Zaroubi
- Kapteyn Astronomical Institute, University of Groningen, Groningen, Netherlands
- Open University of Israel, Ra’anana, Israel
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7
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Baibhav V, Barack L, Berti E, Bonga B, Brito R, Cardoso V, Compère G, Das S, Doneva D, Garcia-Bellido J, Heisenberg L, Hughes SA, Isi M, Jani K, Kavanagh C, Lukes-Gerakopoulos G, Mueller G, Pani P, Petiteau A, Rajendran S, Sotiriou TP, Stergioulas N, Taylor A, Vagenas E, van de Meent M, Warburton N, Wardell B, Witzany V, Zimmerman A. Probing the nature of black holes: Deep in the mHz gravitational-wave sky. EXPERIMENTAL ASTRONOMY 2021; 51:1385-1416. [PMID: 34720415 PMCID: PMC8536608 DOI: 10.1007/s10686-021-09741-9] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/22/2020] [Accepted: 03/16/2021] [Indexed: 06/08/2023]
Abstract
Black holes are unique among astrophysical sources: they are the simplest macroscopic objects in the Universe, and they are extraordinary in terms of their ability to convert energy into electromagnetic and gravitational radiation. Our capacity to probe their nature is limited by the sensitivity of our detectors. The LIGO/Virgo interferometers are the gravitational-wave equivalent of Galileo's telescope. The first few detections represent the beginning of a long journey of exploration. At the current pace of technological progress, it is reasonable to expect that the gravitational-wave detectors available in the 2035-2050s will be formidable tools to explore these fascinating objects in the cosmos, and space-based detectors with peak sensitivities in the mHz band represent one class of such tools. These detectors have a staggering discovery potential, and they will address fundamental open questions in physics and astronomy. Are astrophysical black holes adequately described by general relativity? Do we have empirical evidence for event horizons? Can black holes provide a glimpse into quantum gravity, or reveal a classical breakdown of Einstein's gravity? How and when did black holes form, and how do they grow? Are there new long-range interactions or fields in our Universe, potentially related to dark matter and dark energy or a more fundamental description of gravitation? Precision tests of black hole spacetimes with mHz-band gravitational-wave detectors will probe general relativity and fundamental physics in previously inaccessible regimes, and allow us to address some of these fundamental issues in our current understanding of nature.
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Affiliation(s)
- Vishal Baibhav
- Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 USA
| | - Leor Barack
- Mathematical Sciences, University of Southampton, Southampton, SO17 1BJ UK
| | - Emanuele Berti
- Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 USA
| | | | - Richard Brito
- Dipartimento di Fisica, “Sapienza” Università di Roma & Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185 Roma, Italy
| | - Vitor Cardoso
- CENTRA, Departamento de Física, Instituto Superior Técnico – IST, Universidade de Lisboa – UL, Avenida Rovisco Pais 1, 1049 Lisboa, Portugal
| | - Geoffrey Compère
- Université Libre de Bruxelles, Centre for Gravitational Waves, International Solvay Institutes, CP 231, B-1050 Brussels, Belgium
| | - Saurya Das
- Theoretical Physics Group and Quantum Alberta, Department of Physics and Astronomy, University of Lethbridge, 4401 University Drive, Lethhbridge, Alberta T1K 3M4 Canada
| | - Daniela Doneva
- Theoretical Astrophysics, IAAT, University of Tuebingen, Tuebingen, 72076 Germany
| | - Juan Garcia-Bellido
- Instituto de F ísica Teórica UAM-CSIC, Universidad Autonóma de Madrid, Cantoblanco, 28049 Madrid, Spain
| | - Lavinia Heisenberg
- Institute of Theoretical Physics, ETH Zurich, CH-8093 Zurich, Switzerland
| | - Scott A. Hughes
- Department of Physics and MIT Kavli Institute, Massachusetts Institute of Technology, Cambridge, MA 02139 USA
| | - Maximiliano Isi
- Department of Physics and MIT Kavli Institute, Massachusetts Institute of Technology, Cambridge, MA 02139 USA
| | - Karan Jani
- Center for Relativistic Astrophysics and School of Physics, Georgia Institute of Technology, Atlanta, GA 30332 USA
| | - Chris Kavanagh
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Muhlenberg 1, Potsdam, 14476 Germany
| | | | - Guido Mueller
- Department of Physics, University of Florida, 2001 Museum Road, Gainesville, FL 32611 USA
| | - Paolo Pani
- Dipartimento di Fisica, “Sapienza” Università di Roma & Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185 Roma, Italy
| | - Antoine Petiteau
- AstroParticule et Cosmologie (APC), Université de Paris/CNRS, 75013 Paris, France
| | - Surjeet Rajendran
- Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 USA
| | - Thomas P. Sotiriou
- School of Mathematical Sciences & School of Physics and Astronomy, University of Nottingham, University Park, Nottingham, NG7 2RD UK
| | - Nikolaos Stergioulas
- Department of Physics, Aristotle University of Thessaloniki, Thessaloniki, 54124 Greece
| | - Alasdair Taylor
- School of Physics and Astronomy, University of Glasgow, Glasgow, G12 8QQ Scotland UK
| | - Elias Vagenas
- Theoretical Physics Group, Department of Physics, Kuwait University, P.O. Box 5969, Safat, 13060 Kuwait
| | - Maarten van de Meent
- Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Muhlenberg 1, Potsdam, 14476 Germany
| | - Niels Warburton
- School of Mathematics and Statistics, University College Dublin, Belfield, Dublin 4, D04 V1W8 Ireland
| | - Barry Wardell
- School of Mathematics and Statistics, University College Dublin, Belfield, Dublin 4, D04 V1W8 Ireland
| | - Vojtěch Witzany
- Astronomical Institute of the Czech Academy of Sciences, Bocní II 1401/1a, CZ-141 00 Prague, Czech Republic
| | - Aaron Zimmerman
- Theory Group, Department of Physics, University of Texas at Austin, Austin, TX 78712 USA
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Multi-Field versus Single-Field in the Supergravity Models of Inflation and Primordial Black Holes. UNIVERSE 2021. [DOI: 10.3390/universe7050115] [Citation(s) in RCA: 11] [Impact Index Per Article: 3.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We review the models unifying inflation and Primordial Black Hole (PBH) formation, which are based on the modified (Starobinsky-type) supergravity. We begin with the basic (Starobinsky) inflationary model of modified gravity and its alpha-attractor-type generalizations for PBH production, and recall how all those single-field models can be embedded into the minimal supergravity. Then, we focus on the effective two-field models arising from the modified (Starobinsky-type) supergravity and compare them to the single-field models under review. Those two-field models describe double inflation whose first stage is driven by Starobinsky’s scalaron and whose second stage is driven by another scalar belonging to the supergravity multiplet. The power spectra are numerically computed, and it is found that the ultra-slow-roll regime gives rise to the enhancement (peak) in the scalar power spectrum leading to an efficient PBH formation. The resulting PBH masses and their density fraction (as part of dark matter) are found to be in agreement with cosmological observations. The PBH-induced gravitational waves, if any, are shown to be detectable by the ground-based and space-based gravitational interferometers under construction.
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9
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Silk J. The limits of cosmology: role of the Moon. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2021; 379:20190561. [PMID: 33222642 DOI: 10.1098/rsta.2019.0561] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 07/30/2020] [Indexed: 06/11/2023]
Abstract
The lunar surface allows a unique way forward in cosmology, to go beyond current limits. The far side provides an unexcelled radio-quiet environment for probing the dark ages via 21 cm interferometry to seek elusive clues on the nature of the infinitesimal fluctuations that seeded galaxy formation. Far-infrared telescopes in cold and dark lunar polar craters will probe back to the first months of the Big Bang and study associated spectral distortions in the CMB. Optical and IR megatelescopes will image the first star clusters in the Universe and seek biosignatures in the atmospheres of unprecedented numbers of nearby habitable zone exoplanets. The goals are compelling and a stable lunar platform will enable construction of telescopes that can access trillions of modes in the sky, providing the key to exploration of our cosmic origins. This article is part of a discussion meeting issue 'Astronomy from the Moon: the next decades'.
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Affiliation(s)
- Joseph Silk
- Institut d'Astrophysique de Paris, UMR7095:CNRS & UPMC-Sorbonne University, 75014 Paris, France
- Department of Physics and Astronomy, The Johns Hopkins University Homewood Campus, Baltimore, MD 21218, USA
- BIPAC, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
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10
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Kashlinsky A. Cosmological Advection Flows in the Presence of Primordial Black Holes as Dark Matter and Formation of First Sources. PHYSICAL REVIEW LETTERS 2021; 126:011101. [PMID: 33480799 DOI: 10.1103/physrevlett.126.011101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/06/2020] [Revised: 11/16/2020] [Accepted: 12/07/2020] [Indexed: 06/12/2023]
Abstract
In the inflation-based cosmology the dark matter (DM) density component starts moving with respect to the universal expansion at z_{eq}∼3200 while baryons remain frozen until z_{rec}∼1100. It has been suggested that in this case postlinear corrections to the evolution of small fluctuations would result, for the standard Λ-dominated cold DM (CDM) model, in delayed formation of early objects as supersonic advection flows develop after recombination, so baryons are not immediately captured by the DM gravity on small scales. We develop the hydrodynamical description of such two-component advection and show that, in the supersonic regime, the advection within irrotational fluids is governed by the gradient of the difference of the kinetic energies of the two (DM and baryonic here) components. We then apply this formalism to the case where DM is made up of LIGO-type black holes (BHs) and show that there the advection process on scales relevant for early structure collapse will differ significantly from the earlier discussed (CDM) case because of the additional granulation component to the density field produced during inflation. The advection here will lead efficiently to the common motion of the DM and baryon components on scales relevant for collapse and formation of first luminous sources. This leads to early collapse, making it easier to explain the existence of supermassive BHs observed in quasars at high z>7. The resultant net advection rate reaches minimum around ≲10^{9} M_{⊙} and subsequently rises to a secondary maximum near the typical mass of ∼10^{12} M_{⊙}, which may be an important consideration for formation of galaxies at z≲(a few).
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Affiliation(s)
- A Kashlinsky
- Code 665, Observational Cosmology Lab, NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA and SSAI, Lanham, Maryland 20770, USA
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11
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Abstract
Supermassive black holes lying in the center of galaxies can launch relativistic jets of plasma along their polar axis. The physics of black-hole jets is a very active research topic in astrophysics, owing to the fact that many questions remain open on the physical mechanisms of jet launching, of particle acceleration in the jet, and on the radiative processes. In this work I focus on the last item, and present a review of the current understanding of radiative emission processes in supermassive-black-hole jets.
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12
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Zhang Y, An T, Frey S. Fast jet proper motion discovered in a blazar at z=4.72. Sci Bull (Beijing) 2020; 65:525-530. [PMID: 36659183 DOI: 10.1016/j.scib.2020.01.008] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/20/2019] [Revised: 12/16/2019] [Accepted: 01/02/2020] [Indexed: 01/21/2023]
Abstract
High-resolution observations of high-redshift (z>4) radio quasars offer a unique insight into jet kinematics at early cosmological epochs, as well as constraints on cosmological model parameters. Due to the general weakness of extremely distant objects and the apparently slow structural changes caused by cosmological time dilation, only a couple of high-redshift quasars (HRQs) have been studied with parsec-scale resolutions, and with limited number of observing epochs. Here we report on very long baseline interferometry (VLBI) observations of a high-redshift blazar J1430 + 4204 (z=4.72) in the 8 GHz frequency band at five different epochs spanning 22 years. The source shows a compact core-jet structure with two jet components being identified within 3 milli-arcsecond (mas) scale. The long time span and multiple-epoch data allow for the kinematic studies of the jet components. That results in a jet proper motion of μ(J1) = 0.017 ± 0.002 mas a-1 and μ(J2) = 0.156 ± 0.015 mas a-1, respectively. For the fastest-moving outer jet component J2, the corresponding apparent transverse speed is (19.5±1.9)c. The inferred bulk jet Lorentz factor Γ=14.6±3.8 and viewing angle θ=2.2°±1.6° indicate highly relativistic beaming. The Lorentz factor and apparent proper motion are the highest measured to date among the z>4 jetted radio sources, while the jet kinematics is still consistent with the cosmological interpretation of quasar redshifts.
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Affiliation(s)
- Yingkang Zhang
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China; University of Chinese Academy of Sciences, Beijing 100049, China
| | - Tao An
- Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing 210008, China.
| | - Sándor Frey
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary
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Arvanitaki A, Dimopoulos S, Galanis M, Lehner L, Thompson JO, Van Tilburg K. Large-misalignment mechanism for the formation of compact axion structures: Signatures from the QCD axion to fuzzy dark matter. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.083014] [Citation(s) in RCA: 77] [Impact Index Per Article: 19.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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14
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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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Wang HT, Jiang Z, Sesana A, Barausse E, Huang SJ, Wang YF, Feng WF, Wang Y, Hu YM, Mei J, Luo J. Science with the TianQin observatory: Preliminary results on massive black hole binaries. Int J Clin Exp Med 2019. [DOI: 10.1103/physrevd.100.043003] [Citation(s) in RCA: 35] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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16
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Reverberation Mapping of the Narrow-line Seyfert 1 Galaxy I Zwicky 1: Black Hole Mass. ACTA ACUST UNITED AC 2019. [DOI: 10.3847/1538-4357/ab16ef] [Citation(s) in RCA: 16] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Ferrer F, Masso E, Panico G, Pujolas O, Rompineve F. Primordial Black Holes from the QCD Axion. PHYSICAL REVIEW LETTERS 2019; 122:101301. [PMID: 30932654 DOI: 10.1103/physrevlett.122.101301] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/24/2018] [Revised: 10/31/2018] [Indexed: 06/09/2023]
Abstract
We propose a mechanism to generate primordial black holes (PBHs) that is independent of cosmological inflation and occurs slightly below the QCD phase transition. Our setup relies on the collapse of long-lived string-domain wall networks and is naturally realized in QCD axion models with domain wall number N_{DW}>1 and Peccei-Quinn symmetry broken after inflation. In our framework, dark matter is mostly composed of axions in the meV mass range along with a small fraction, Ω_{PBH}≳10^{-6}Ω_{CDM} of heavy M∼10^{4}-10^{7} M_{⊙} PBHs. The latter could play a role in alleviating some of the shortcomings of the standard cosmological model on subgalactic scales. The scenario might have distinct signatures in ongoing axion searches as well as gravitational wave observatories.
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Affiliation(s)
- Francesc Ferrer
- Department of Physics, McDonnell Center for the Space Sciences, Washington University, St. Louis, Missouri 63130, USA
- IFAE and BIST, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
| | - Eduard Masso
- IFAE and BIST, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
- Departament de Física, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
| | - Giuliano Panico
- IFAE and BIST, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
- Laboratory of High Energy and Computational Physics, National Institute of Chemical Physics and Biophysics, Rävala pst. 10, 10143 Tallinn, Estonia
| | - Oriol Pujolas
- IFAE and BIST, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
| | - Fabrizio Rompineve
- IFAE and BIST, Universitat Autònoma de Barcelona, E-08193 Bellaterra, Barcelona, Spain
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Wise JH, Regan JA, O'Shea BW, Norman ML, Downes TP, Xu H. Formation of massive black holes in rapidly growing pre-galactic gas clouds. Nature 2019; 566:85-88. [PMID: 30675066 DOI: 10.1038/s41586-019-0873-4] [Citation(s) in RCA: 79] [Impact Index Per Article: 15.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/21/2018] [Accepted: 11/30/2018] [Indexed: 11/09/2022]
Abstract
The origin of the supermassive black holes that inhabit the centres of massive galaxies remains unclear1,2. Direct-collapse black holes-remnants of supermassive stars, with masses around 10,000 times that of the Sun-are ideal seed candidates3-6. However, their very existence and their formation environment in the early Universe are still under debate, and their supposed rarity makes modelling their formation difficult7,8. Models have shown that rapid collapse of pre-galactic gas (with a mass infall rate above some critical value) in metal-free haloes is a requirement for the formation of a protostellar core that will then form a supermassive star9,10. Here we report a radiation hydrodynamics simulation of early galaxy formation11,12 that produces metal-free haloes massive enough and with sufficiently high mass infall rates to form supermassive stars. We find that pre-galactic haloes and their associated gas clouds that are exposed to a Lyman-Werner intensity roughly three times the intensity of the background radiation and that undergo at least one period of rapid mass growth early in their evolution are ideal environments for the formation of supermassive stars. The rapid growth induces substantial dynamical heating13,14, amplifying the Lyman-Werner suppression that originates from a group of young galaxies 20 kiloparsecs away. Our results strongly indicate that the dynamics of structure formation, rather than a critical Lyman-Werner flux, is the main driver of the formation of massive black holes in the early Universe. We find that the seeds of massive black holes may be much more common than previously considered in overdense regions of the early Universe, with a co-moving number density up to 10-3 per cubic megaparsec.
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Affiliation(s)
- John H Wise
- Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA, USA.
| | - John A Regan
- Centre for Astrophysics and Relativity, School of Mathematical Sciences, Dublin City University, Dublin, Ireland
| | - Brian W O'Shea
- Department of Computational Mathematics, Science and Engineering, Michigan State University, East Lansing, MI, USA.,Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - Michael L Norman
- Center for Astrophysics and Space Sciences, University of California, San Diego, CA, USA.,San Diego Supercomputer Center, San Diego, CA, USA
| | - Turlough P Downes
- Centre for Astrophysics and Relativity, School of Mathematical Sciences, Dublin City University, Dublin, Ireland
| | - Hao Xu
- Center for Astrophysics and Space Sciences, University of California, San Diego, CA, USA.,San Diego Supercomputer Center, San Diego, CA, USA.,IBM, Poughkeepsie, NY, USA
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YOSHIDA N. Formation of the first generation of stars and blackholes in the Universe. PROCEEDINGS OF THE JAPAN ACADEMY. SERIES B, PHYSICAL AND BIOLOGICAL SCIENCES 2019; 95:17-28. [PMID: 30643093 PMCID: PMC6395782 DOI: 10.2183/pjab.95.002] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 03/20/2018] [Accepted: 10/23/2018] [Indexed: 06/09/2023]
Abstract
Modern sky surveys using large ground-based telescopes have discovered a variety of celestial objects. Prominent structures such as galaxies and galaxy clusters are found virtually everywhere, and their collective distribution forms the large-scale structure of the Universe. It is thought that all of the rich content in the present-day Universe developed through gravitational amplification of primeval density fluctuations generated in the very early phase of cosmic evolution. The standard theoretical model based on an array of recent observations accurately predicts the physical conditions in the early Universe, and powerful super-computers allow us to simulate in detail the formation and evolution of cosmic structure to the present epoch. We review recent progress in the study on the first generation of stars and blackholes. We focus on the physics of early structure formation, while identifying several key issues and open questions. Finally, we discuss prospects for future observations of the first stars, galaxies and blackholes.
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Affiliation(s)
- Naoki YOSHIDA
- Department of Physics, School of Science, The University of Tokyo, Tokyo, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIAS, The University of Tokyo, Chiba, Japan
- Research Center for the Early Universe, The University of Tokyo, Tokyo, Japan
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Mayer L, Bonoli S. The route to massive black hole formation via merger-driven direct collapse: a review. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:016901. [PMID: 30057369 DOI: 10.1088/1361-6633/aad6a5] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
The direct collapse model for the formation of massive black holes has gained increased support as it provides a natural explanation for the appearance of bright quasars already less than a billion years from the Big Bang. In this paper we review a recent scenario for direct collapse that relies on multi-scale gas inflows initiated by the major merger of massive gas-rich galaxies at z > 6, where gas has already achieved solar composition. Hydrodynamical simulations undertaken to explore our scenario show that supermassive, gravitationally bound compact gaseous disks weighing a billion solar masses, only a few pc in size, form in the nuclei of merger remnants in less than 105 yr. These could later produce a supermassive protostar or supermassive star at their center via various mechanisms. Moreover, we present a new analytical model, based on angular momentum transport in mass-loaded gravitoturbulent disks. This naturally predicts that a nuclear disk accreting at rates exceeding [Formula: see text] yr-1, as seen in the simulations, is stable against fragmentation irrespective of its metallicity. This is at variance with conventional direct collapse scenarios, which require the suppression of gas cooling in metal-free protogalaxies for gas collapse to take place. Such high accretion rates reflect the high free-fall velocities in massive halos appearing only at z < 10, and occur naturally as a result of the efficient angular momentum loss provided by the merger dynamics. We discuss the implications of our scenario on the observed population of high-z quasars and on its evolution to lower redshifts using a semi-analytical galaxy formation model. Finally, we consider the intriguing possibility that the secondary gas inflows in the unstable disks might drive gas to collapse into a supermassive black hole directly via the General Relativistic radial instability. Such dark collapse route could generate gravitational wave emission detectable via the future Laser Interferometer Space Antenna (LISA).
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Affiliation(s)
- Lucio Mayer
- Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, CH-8057 Zurich, Switzerland. Kavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106, United States of America
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22
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Monitoring AGNs with Hβ Asymmetry. I. First Results: Velocity-resolved Reverberation Mapping. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aaed2c] [Citation(s) in RCA: 36] [Impact Index Per Article: 6.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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23
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Modeling the Radio Background from the First Black Holes at Cosmic Dawn: Implications for the 21 cm Absorption Amplitude. ACTA ACUST UNITED AC 2018. [DOI: 10.3847/1538-4357/aae51d] [Citation(s) in RCA: 100] [Impact Index Per Article: 16.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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24
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Sun L, Ruiz M, Shapiro SL. Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles. PHYSICAL REVIEW. D. (2016) 2018; 98:103008. [PMID: 34589637 PMCID: PMC8477203 DOI: 10.1103/physrevd.98.103008] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
Collapsing supermassive stars (SMSs) with masses M ≳ 104-6 M ⊙ have long been speculated to be the seeds that can grow and become supermassive black holes (SMBHs). We previously performed general relativistic magnetohydrodynamic (GRMHD) simulations of marginally stable Γ = 4/3 polytropes uniformly rotating at the mass-shedding limit and endowed initially with a dynamically unimportant dipole magnetic field to model the direct collapse of SMSs. These configurations are supported entirely by thermal radiation pressure and reliably model SMSs with M ≳ 106 M ⊙. We found that around 90% of the initial stellar mass forms a spinning black hole (BH) remnant surrounded by a massive, hot, magnetized torus, which eventually launches a magnetically-driven jet. SMSs could be therefore sources of ultra-long gamma-ray bursts (ULGRBs). Here we perform GRMHD simulations of Γ ≳ 4/3, polytropes to account for the perturbative role of gas pressure in SMSs with M ≲ 106 M ⊙. We also consider different initial stellar rotation profiles. The stars are initially seeded with a dynamically weak dipole magnetic field that is either confined to the stellar interior or extended from its interior into the stellar exterior. We calculate the gravitational wave burst signal for the different cases. We find that the mass of the black hole remnant is 90%-99% of the initial stellar mass, depending sharply on Γ - 4/3 as well as on the initial stellar rotation profile. After t ~ 250-550M ≈ 1 - 2 × 103(M/106 M ⊙) s following the appearance of the BH horizon, an incipient jet is launched and it lasts for ~104-105(M/106 M ⊙) s, consistent with the duration of long gamma-ray bursts. Our numerical results suggest that the Blandford-Znajek mechanism powers the incipient jet. They are also in rough agreement with our recently proposed universal model that estimates accretion rates and electromagnetic (Poynting) luminosities that characterize magnetized BH-disk remnant systems that launch a jet. This model helps explain why the outgoing electromagnetic luminosities computed for vastly different BH-disk formation scenarios all reside within a narrow range (~1052±1 erg s-1), roughly independent of M.
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Affiliation(s)
- Lunan Sun
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Milton Ruiz
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
| | - Stuart L Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
- Department of Astronomy & NCSA, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801, USA
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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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27
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Li JT, Fuller GM, Kishimoto CT. Neutrino burst-generated gravitational radiation from collapsing supermassive stars. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.023002] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Butler SP, Lima AR, Baumgarte TW, Shapiro SL. Maximally rotating supermassive stars at the onset of collapse: the perturbative effects of gas pressure, magnetic fields, dark matter, and dark energy. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 477:3694-3710. [PMID: 30008487 PMCID: PMC6042249 DOI: 10.1093/mnras/sty834] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/08/2023]
Abstract
The discovery of quasars at increasingly large cosmological redshifts may favour 'direct collapse' as the most promising evolutionary route to the formation of supermassive black holes. In this scenario, supermassive black holes form when their progenitors - supermassive stars - become unstable to gravitational collapse. For uniformly rotating stars supported by pure radiation pressure and spinning at the mass-shedding limit, the critical configuration at the onset of collapse is characterized by universal values of the dimensionless spin and radius parameters J/M2 and R/M, independent of mass M. We consider perturbative effects of gas pressure, magnetic fields, dark matter, and dark energy on these parameters, and thereby determine the domain of validity of this universality. We obtain leading-order corrections for the critical parameters and establish their scaling with the relevant physical parameters. We compare two different approaches to approximate the effects of gas pressure, which plays the most important role, find identical results for the above dimensionless parameters, and also find good agreement with recent numerical results.
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Affiliation(s)
- Satya P. Butler
- Department of Physics and Astronomy, Bowdoin College, Brunswick, ME 04011, USA
| | - Alicia R. Lima
- Department of Physics and Astronomy, Bowdoin College, Brunswick, ME 04011, USA
| | - Thomas W. Baumgarte
- Department of Physics and Astronomy, Bowdoin College, Brunswick, ME 04011, USA
| | - Stuart L. Shapiro
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA
- Department of Astronomy and NCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA
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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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30
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A beacon at the dawn of the Universe. Nature 2018; 553:410-411. [DOI: 10.1038/d41586-018-00818-8] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/08/2022]
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