1
|
Bruni G, Piro L, Yang YP, Quai S, Zhang B, Palazzi E, Nicastro L, Feruglio C, Tripodi R, O'Connor B, Gardini A, Savaglio S, Rossi A, Nicuesa Guelbenzu AM, Paladino R. A nebular origin for the persistent radio emission of fast radio bursts. Nature 2024; 632:1014-1016. [PMID: 39112707 DOI: 10.1038/s41586-024-07782-6] [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: 12/22/2023] [Accepted: 07/03/2024] [Indexed: 08/17/2024]
Abstract
Fast radio bursts (FRBs) are millisecond-duration, bright (approximately Jy) extragalactic bursts, whose production mechanism is still unclear1. Recently, two repeating FRBs were found to have a physically associated persistent radio source of non-thermal origin2,3. These two FRBs have unusually large Faraday rotation measure values2,3, probably tracing a dense magneto-ionic medium, consistent with synchrotron radiation originating from a nebula surrounding the FRB source4-8. Recent theoretical arguments predict that, if the observed Faraday rotation measure mostly arises from the persistent radio source region, there should be a simple relation between the persistent radio source luminosity and the rotation measure itself7,9. Here we report the detection of a third, less luminous persistent radio source associated with the repeating FRB source FRB 20201124A at a distance of 413 Mpc, substantially expanding the predicted relation into the low luminosity-low Faraday rotation measure regime (<1,000 rad m-2). At lower values of the Faraday rotation measure, the expected radio luminosity falls below the limit-of-detection threshold for present-day radio telescopes. These findings support the idea that the persistent radio sources observed so far are generated by a nebula in the FRB environment and that FRBs with low Faraday rotation measure may not show a persistent radio source because of a weaker magneto-ionic medium. This is generally consistent with models invoking a young magnetar as the central engine of the FRB, in which the surrounding ionized nebula-or the interacting shock in a binary system-powers the persistent radio source.
Collapse
Affiliation(s)
- Gabriele Bruni
- IAPS - Institute for Space Astrophysics and Planetology, INAF (Istituto Nazionale di Astrofisica), Rome, Italy.
| | - Luigi Piro
- IAPS - Institute for Space Astrophysics and Planetology, INAF (Istituto Nazionale di Astrofisica), Rome, Italy
| | - Yuan-Pei Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, China
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Salvatore Quai
- Dipartimento di Fisica e Astronomia "Augusto Righi", Università degli Studi di Bologna (UNIBO), Bologna, Italy
- Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
| | - Bing Zhang
- Nevada Center for Astrophysics, University of Nevada, Las Vegas, NV, USA
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA
| | - Eliana Palazzi
- Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
| | - Luciano Nicastro
- Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
| | - Chiara Feruglio
- Osservatorio Astronomico di Trieste, INAF (Istituto Nazionale di Astrofisica), Trieste, Italy
- IFPU: Institute for Fundamental Physics of the Universe, Trieste, Italy
| | - Roberta Tripodi
- Osservatorio Astronomico di Trieste, INAF (Istituto Nazionale di Astrofisica), Trieste, Italy
- IFPU: Institute for Fundamental Physics of the Universe, Trieste, Italy
- Dipartimento di Fisica, Università degli Studi di Trieste, Trieste, Italy
| | - Brendan O'Connor
- McWilliams Center for Cosmology & Astrophysics, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Angela Gardini
- Instituto de Astrofísica de Andalucía, CSIC (Consejo Superior de Investigaciones Científicas), Granada, Spain
| | - Sandra Savaglio
- Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
- Dipartimento di Fisica, Università della Calabria, Arcavacata di Rende, Italy
- Laboratori Nazionali di Frascati, INFN (Istituto Nazionale di Fisica Nucleare), Frascati, Italy
| | - Andrea Rossi
- Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
| | | | - Rosita Paladino
- IRA - Istituto di Radioastronomia, INAF (Istituto Nazionale di Astrofisica), Bologna, Italy
| |
Collapse
|
2
|
Ishizaki W, Ioka K. Parametric decay instability of circularly polarized Alfvén waves in magnetically dominated plasma. Phys Rev E 2024; 110:015205. [PMID: 39160913 DOI: 10.1103/physreve.110.015205] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/24/2024] [Accepted: 06/17/2024] [Indexed: 08/21/2024]
Abstract
We investigate parametric decay instability (PDI) of circularly polarized Alfvén wave into daughter acoustic wave and backward Alfvén wave in magnetically dominated plasma, in which the magnetization parameter σ (energy density ratio of background magnetic field to matter) exceeds unity. We analyze relativistic magnetohydrodynamics (MHD), focusing on wave frequencies sufficiently lower than the plasma and cyclotron frequencies. We derive analytical formulas for the dispersion relation and growth rate of the instability as a function of the magnetization σ, wave amplitude η, and plasma temperature θ. We find that PDI persists even in high magnetization σ, albeit with a decreased growth rate up to σ→∞. Our formulas are useful for estimating the decay of Alfvén wave into acoustic wave and heat in high magnetization σ plasma, which is a ubiquitous phenomenon such as in pulsars, magnetars, and fast radio bursts.
Collapse
Affiliation(s)
- Wataru Ishizaki
- Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan
- Frontier Research Institute for Interdisciplinary Sciences, Tohoku University, Sendai 980-8578, Japan
- Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo, Kyoto 606-8502, Japan
| | - Kunihito Ioka
- Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo, Kyoto 606-8502, Japan
| |
Collapse
|
3
|
Ryder SD, Bannister KW, Bhandari S, Deller AT, Ekers RD, Glowacki M, Gordon AC, Gourdji K, James CW, Kilpatrick CD, Lu W, Marnoch L, Moss VA, Prochaska JX, Qiu H, Sadler EM, Simha S, Sammons MW, Scott DR, Tejos N, Shannon RM. A luminous fast radio burst that probes the Universe at redshift 1. Science 2023; 382:294-299. [PMID: 37856596 DOI: 10.1126/science.adf2678] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/12/2022] [Accepted: 09/04/2023] [Indexed: 10/21/2023]
Abstract
Fast radio bursts (FRBs) are millisecond-duration pulses of radio emission originating from extragalactic distances. Radio dispersion is imparted on each burst by intervening plasma, mostly located in the intergalactic medium. In this work, we observe the burst FRB 20220610A and localize it to a morphologically complex host galaxy system at redshift 1.016 ± 0.002. The burst redshift and dispersion measure are consistent with passage through a substantial column of plasma in the intergalactic medium and extend the relationship between those quantities measured at lower redshift. The burst shows evidence for passage through additional turbulent magnetized plasma, potentially associated with the host galaxy. We use the burst energy of 2 × 1042 erg to revise the empirical maximum energy of an FRB.
Collapse
Affiliation(s)
- S D Ryder
- School of Mathematical and Physical Sciences, Macquarie University, Sydney, NSW 2109, Australia
- Astrophysics and Space Technologies Research Centre, Macquarie University, Sydney, NSW 2109, Australia
| | - K W Bannister
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
| | - S Bhandari
- Netherlands Institute for Radio Astronomy (ASTRON), 7991 PD Dwingeloo, Netherlands
- Joint institute for Very Long Baseline Interferometry in Europe, 7991 PD Dwingeloo, Netherlands
| | - A T Deller
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - R D Ekers
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - M Glowacki
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - A C Gordon
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL 60208, USA
| | - K Gourdji
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - C W James
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - C D Kilpatrick
- Center for Interdisciplinary Exploration and Research in Astrophysics, Northwestern University, Evanston, IL 60208, USA
- Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USA
| | - W Lu
- Department of Astronomy University of California, Berkeley, CA 94720, USA
- Theoretical Astrophysics Center, University of California, Berkeley, CA 94720, USA
| | - L Marnoch
- School of Mathematical and Physical Sciences, Macquarie University, Sydney, NSW 2109, Australia
- Astrophysics and Space Technologies Research Centre, Macquarie University, Sydney, NSW 2109, Australia
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Macquarie University, Sydney, NSW 2109, Australia
| | - V A Moss
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
| | - J X Prochaska
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
- Kavli Institute for the Physics and Mathematics of the Universe, Kashiwa, 277-8583, Japan
| | - H Qiu
- Square Kilometre Array Observatory, Jodrell Bank, Lower Withington, Macclesfield SK11 9FT, UK
| | - E M Sadler
- Australia Telescope National Facility, Commonwealth Science and Industrial Research Organisation, Space and Astronomy, Epping, NSW 1710, Australia
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - S Simha
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA
| | - M W Sammons
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - D R Scott
- International Centre for Radio Astronomy Research, Curtin Institute of Radio Astronomy, Curtin University, Perth, WA 6102, Australia
| | - N Tejos
- Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile
| | - R M Shannon
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| |
Collapse
|
4
|
Paragi Z. An origin scenario for a fast radio burst. Science 2023; 380:580. [PMID: 37167378 DOI: 10.1126/science.adh8099] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 05/13/2023]
Abstract
Never-before-observed behavior of a repeating burst suggests its possible origin.
Collapse
Affiliation(s)
- Zsolt Paragi
- Joint Institute for VLBI ERIC (JIVE), 7991 PD Dwingeloo, Netherlands
| |
Collapse
|
5
|
Bailes M. The discovery and scientific potential of fast radio bursts. Science 2022; 378:eabj3043. [DOI: 10.1126/science.abj3043] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
Abstract
Fast radio bursts (FRBs) are millisecond-time-scale bursts of coherent radio emission that are luminous enough to be detectable at cosmological distances. In this Review, I describe the discovery of FRBs, subsequent advances in understanding them, and future prospects. Thousands of potentially observable FRBs reach Earth every day, which likely originate from highly magnetic and/or rapidly rotating neutron stars in the distant Universe. Some FRBs repeat, with this subclass often occurring in highly magnetic environments. Two repeating FRBs exhibit cyclic activity windows, consistent with an orbital period. One nearby FRB was emitted by a Galactic magnetar during an x-ray outburst. The host galaxies of some FRBs have been located, providing information about the host environments and the total baryonic content of the Universe.
Collapse
Affiliation(s)
- Matthew Bailes
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia
| |
Collapse
|
6
|
Constraints on the Helium Abundance from Fast Radio Bursts. UNIVERSE 2022. [DOI: 10.3390/universe8060317] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/04/2022]
Abstract
Through the relationship between dispersion measures (DM) and redshifts, fast radio bursts (FRBs) are considered to be very promising cosmological probes. In this paper, we attempted to use the DM-z relationship of FRBs to study the helium abundance (YHe) in the universe. First, we used 17 current FRBs with known redshifts for our study. Due to their low redshifts and the strong degeneracy between YHe and Ωbh2, however, this catalog could not provide a good constraint on the helium abundance. Then, we simulated 500 low redshift FRB mock data with z∈[0,1.5] to forecast the constraining ability on YHe. In order to break the degeneracy between YHe and Ωbh2 further, we introduced the shift parameters of the Planck measurement (R,lA,Ωbh2) as a prior, where Ωbh2 represents the baryon density parameter, and R and lA correspond to the scaled distance to recombination and the angular scale of the sound horizon at recombination, respectively. We obtained the standard deviation for the helium abundance: σ(YHe)=0.025. Finally, we considered 2000 higher redshift FRB data with the redshift distribution of [0,3] and found that the constraining power for YHe would be improved by more than 2 times, σ(YHe)=0.011, which indicates that the FRB data with high redshift can provide a better constraint on the helium abundance. Hopefully, large FRB samples with high redshift from the Square Kilometre Array can provide high-precision measurements of the helium abundance in the near future.
Collapse
|
7
|
Abstract
Fast radio bursts (FRBs) have a story which has been told and retold many times over the past few years as they have sparked excitement and controversy since their pioneering discovery in 2007. The FRB class encompasses a number of microsecond- to millisecond-duration pulses occurring at Galactic to cosmological distances with energies spanning about 8 orders of magnitude. While most FRBs have been observed as singular events, a small fraction of them have been observed to repeat over various timescales leading to an apparent dichotomy in the population. ∼50 unique progenitor theories have been proposed, but no consensus has emerged for their origin(s). However, with the discovery of an FRB-like pulse from the Galactic magnetar SGR J1935+2154, magnetar engine models are the current leading theory. Overall, FRB pulses exhibit unique characteristics allowing us to probe line-of-sight magnetic field strengths, inhomogeneities in the intergalactic/interstellar media, and plasma turbulence through an assortment of extragalactic and cosmological propagation effects. Consequently, they are formidable tools to study the Universe. This review follows the progress of the field between 2007 and 2020 and presents the science highlights of the radio observations.
Collapse
|
8
|
Qu K, Meuren S, Fisch NJ. Signature of Collective Plasma Effects in Beam-Driven QED Cascades. PHYSICAL REVIEW LETTERS 2021; 127:095001. [PMID: 34506208 DOI: 10.1103/physrevlett.127.095001] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/21/2020] [Revised: 07/21/2021] [Accepted: 08/02/2021] [Indexed: 06/13/2023]
Abstract
QED cascades play an important role in extreme astrophysical environments like magnetars. They can also be produced by passing a relativistic electron beam through an intense laser field. Signatures of collective pair plasma effects in these QED cascades are shown to appear, in exquisite detail, through plasma-induced frequency upshifts in the laser spectrum. Remarkably, these signatures can be detected even in small plasma volumes moving at relativistic speeds. Strong-field quantum and collective pair plasma effects can thus be explored with existing technology, provided that ultradense electron beams are colocated with multipetawatt lasers.
Collapse
Affiliation(s)
- Kenan Qu
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
| | - Sebastian Meuren
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
- Stanford PULSE Institute, SLAC National Accelerator Laboratory, Menlo Park, California 94025, USA
| | - Nathaniel J Fisch
- Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA
| |
Collapse
|
9
|
Abstract
Fast Radio Bursts (FRBs) represent a novel tool for probing the properties of the universe at cosmological distances. The dispersion measures of FRBs, combined with the redshifts of their host galaxies, has very recently yielded a direct measurement of the baryon content of the universe, and has the potential to directly constrain the location of the “missing baryons”. The first results are consistent with the expectations of ΛCDM for the cosmic density of baryons, and have provided the first constraints on the properties of the very diffuse intergalactic medium (IGM) and circumgalactic medium (CGM) around galaxies. FRBs are the only known extragalactic sources that are compact enough to exhibit diffractive scintillation in addition to showing exponential tails which are typical of scattering in turbulent media. This will allow us to probe the turbulent properties of the circumburst medium, the host galaxy ISM/halo, and intervening halos along the path, as well as the IGM. Measurement of the Hubble constant and the dark energy parameter w can be made with FRBs, but require very large samples of localised FRBs (>103) to be effective on their own—they are best combined with other independent surveys to improve the constraints. Ionisation events, such as for He ii, leave a signature in the dispersion measure—redshift relation, and if FRBs exist prior to these times, they can be used to probe the reionisation era, although more than 103 localised FRBs are required.
Collapse
|
10
|
Abstract
The origin and phenomenology of the Fast Radio Burst (FRB) remains unknown despite more than a decade of efforts. Though several models have been proposed to explain the observed data, none is able to explain alone the variety of events so far recorded. The leading models consider magnetars as potential FRB sources. The recent detection of FRBs from the galactic magnetar SGR J1935+2154 seems to support them. Still, emission duration and energetic budget challenge all these models. Like for other classes of objects initially detected in a single band, it appeared clear that any solution to the FRB enigma could only come from a coordinated observational and theoretical effort in an as wide as possible energy band. In particular, the detection and localisation of optical/NIR or/and high-energy counterparts seemed an unavoidable starting point that could shed light on the FRB physics. Multiwavelength (MWL) search campaigns were conducted for several FRBs, in particular for repeaters. Here we summarize the observational and theoretical results and the perspectives in view of the several new sources accurately localised that will likely be identified by various radio facilities worldwide. We conclude that more dedicated MWL campaigns sensitive to the millisecond–minute timescale transients are needed to address the various aspects involved in the identification of FRB counterparts. Dedicated instrumentation could be one of the key points in this respect. In the optical/NIR band, fast photometry looks to be the only viable strategy. Additionally, small/medium size radiotelescopes co-pointing higher energies telescopes look a very interesting and cheap complementary observational strategy.
Collapse
|
11
|
Abstract
Fast radio bursts are mysterious millisecond-duration transients prevalent in the radio sky. Rapid accumulation of data in recent years has facilitated an understanding of the underlying physical mechanisms of these events. Knowledge gained from the neighbouring fields of gamma-ray bursts and radio pulsars has also offered insights. Here I review developments in this fast-moving field. Two generic categories of radiation model invoking either magnetospheres of compact objects (neutron stars or black holes) or relativistic shocks launched from such objects have been much debated. The recent detection of a Galactic fast radio burst in association with a soft gamma-ray repeater suggests that magnetar engines can produce at least some, and probably all, fast radio bursts. Other engines that could produce fast radio bursts are not required, but are also not impossible.
Collapse
|
12
|
Bochenek CD, Ravi V, Belov KV, Hallinan G, Kocz J, Kulkarni SR, McKenna DL. A fast radio burst associated with a Galactic magnetar. Nature 2020; 587:59-62. [DOI: 10.1038/s41586-020-2872-x] [Citation(s) in RCA: 229] [Impact Index Per Article: 57.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/12/2020] [Accepted: 09/21/2020] [Indexed: 11/09/2022]
|
13
|
A bright millisecond-duration radio burst from a Galactic magnetar. Nature 2020; 587:54-58. [DOI: 10.1038/s41586-020-2863-y] [Citation(s) in RCA: 230] [Impact Index Per Article: 57.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/19/2020] [Accepted: 09/01/2020] [Indexed: 11/08/2022]
|
14
|
Abstract
The Square Kilometre Array (SKA) will answer fundamental questions about the origin, evolution, properties, and influence of magnetic fields throughout the Universe. Magnetic fields can illuminate and influence phenomena as diverse as star formation, galactic dynamics, fast radio bursts, active galactic nuclei, large-scale structure, and dark matter annihilation. Preparations for the SKA are swiftly continuing worldwide, and the community is making tremendous observational progress in the field of cosmic magnetism using data from a powerful international suite of SKA pathfinder and precursor telescopes. In this contribution, we revisit community plans for magnetism research using the SKA, in light of these recent rapid developments. We focus in particular on the impact that new radio telescope instrumentation is generating, thus advancing our understanding of key SKA magnetism science areas, as well as the new techniques that are required for processing and interpreting the data. We discuss these recent developments in the context of the ultimate scientific goals for the SKA era.
Collapse
|
15
|
A census of baryons in the Universe from localized fast radio bursts. Nature 2020; 581:391-395. [PMID: 32461651 DOI: 10.1038/s41586-020-2300-2] [Citation(s) in RCA: 213] [Impact Index Per Article: 53.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/27/2019] [Accepted: 03/13/2020] [Indexed: 11/08/2022]
Abstract
More than three-quarters of the baryonic content of the Universe resides in a highly diffuse state that is difficult to detect, with only a small fraction directly observed in galaxies and galaxy clusters1,2. Censuses of the nearby Universe have used absorption line spectroscopy3,4 to observe the 'invisible' baryons, but these measurements rely on large and uncertain corrections and are insensitive to most of the Universe's volume and probably most of its mass. In particular, quasar spectroscopy is sensitive either to the very small amounts of hydrogen that exist in the atomic state, or to highly ionized and enriched gas4-6 in denser regions near galaxies7. Other techniques to observe these invisible baryons also have limitations; Sunyaev-Zel'dovich analyses8,9 can provide evidence from gas within filamentary structures, and studies of X-ray emission are most sensitive to gas near galaxy clusters9,10. Here we report a measurement of the baryon content of the Universe using the dispersion of a sample of localized fast radio bursts; this technique determines the electron column density along each line of sight and accounts for every ionized baryon11-13. We augment the sample of reported arcsecond-localized14-18 fast radio bursts with four new localizations in host galaxies that have measured redshifts of 0.291, 0.118, 0.378 and 0.522. This completes a sample sufficiently large to account for dispersion variations along the lines of sight and in the host-galaxy environments11, and we derive a cosmic baryon density of [Formula: see text] (95 per cent confidence; h70 = H0/(70 km s-1 Mpc-1) and H0 is Hubble's constant). This independent measurement is consistent with values derived from the cosmic microwave background and from Big Bang nucleosynthesis19,20.
Collapse
|
16
|
|
17
|
A repeating fast radio burst source localized to a nearby spiral galaxy. Nature 2020; 577:190-194. [PMID: 31907402 DOI: 10.1038/s41586-019-1866-z] [Citation(s) in RCA: 212] [Impact Index Per Article: 53.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/17/2019] [Accepted: 11/08/2019] [Indexed: 11/08/2022]
Abstract
Fast radio bursts (FRBs) are brief, bright, extragalactic radio flashes1,2. Their physical origin remains unknown, but dozens of possible models have been postulated3. Some FRB sources exhibit repeat bursts4-7. Although over a hundred FRB sources have been discovered8, only four have been localized and associated with a host galaxy9-12, and just one of these four is known to emit repeating FRBs9. The properties of the host galaxies, and the local environments of FRBs, could provide important clues about their physical origins. The first known repeating FRB, however, was localized to a low-metallicity, irregular dwarf galaxy, and the apparently non-repeating sources were localized to higher-metallicity, massive elliptical or star-forming galaxies, suggesting that perhaps the repeating and apparently non-repeating sources could have distinct physical origins. Here we report the precise localization of a second repeating FRB source6, FRB 180916.J0158+65, to a star-forming region in a nearby (redshift 0.0337 ± 0.0002) massive spiral galaxy, whose properties and proximity distinguish it from all known hosts. The lack of both a comparably luminous persistent radio counterpart and a high Faraday rotation measure6 further distinguish the local environment of FRB 180916.J0158+65 from that of the single previously localized repeating FRB source, FRB 121102. This suggests that repeating FRBs may have a wide range of luminosities, and originate from diverse host galaxies and local environments.
Collapse
|
18
|
Oyanguren A. Real-time data analysis model at LHC and connections to other experiments and fields. EPJ WEB OF CONFERENCES 2020. [DOI: 10.1051/epjconf/202024511005] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
With the upcoming increase of proton-proton collision rates at the Large Hadron Collider (LHC) experiments, and the corresponding increase of data volumes, real-time analysis becomes a key ingredient to be able to analyse and select the interesting data within the available computing resources. In this talk I will review the main features of the techniques followed by the ATLAS, CMS and LHCb experiments. Similar challenges have to be faced in other fields, such as astronomy and cosmology, and I will comment about them.
Collapse
|
19
|
Oguri M. Strong gravitational lensing of explosive transients. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2019; 82:126901. [PMID: 31634885 DOI: 10.1088/1361-6633/ab4fc5] [Citation(s) in RCA: 10] [Impact Index Per Article: 2.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/10/2023]
Abstract
Recent rapid progress in time domain surveys makes it possible to detect various types of explosive transients in the Universe in large numbers, some of which will be gravitationally lensed into multiple images. Although a large number of strongly lensed distant galaxies and quasars have already been discovered, strong lensing of explosive transients opens up new applications, including improved measurements of cosmological parameters, powerful probes of small scale structure of the Universe, and new observational tests of dark matter scenarios, thanks to their rapidly evolving light curves as well as their compact sizes. In particular, compact sizes of emitting regions of these transient events indicate that wave optics effects play an important role in some cases, which can lead to totally new applications of these lensing events. Recently we have witnessed first discoveries of strongly lensed supernovae, and strong lensing events of other types of explosive transients such as gamma-ray bursts, fast radio bursts, and gravitational waves from compact binary mergers are expected to be observed soon. In this review article, we summarize the current state of research on strong gravitational lensing of explosive transients and discuss future prospects.
Collapse
Affiliation(s)
- Masamune Oguri
- Research Center for the Early Universe, University of Tokyo, Tokyo 113-0033, Japan. Department of Physics, University of Tokyo, Tokyo 113-0033, Japan. Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), University of Tokyo, Chiba 277-8582, Japan
| |
Collapse
|
20
|
Prochaska JX, Macquart JP, McQuinn M, Simha S, Shannon RM, Day CK, Marnoch L, Ryder S, Deller A, Bannister KW, Bhandari S, Bordoloi R, Bunton J, Cho H, Flynn C, Mahony EK, Phillips C, Qiu H, Tejos N. The low density and magnetization of a massive galaxy halo exposed by a fast radio burst. Science 2019; 366:231-234. [PMID: 31558577 DOI: 10.1126/science.aay0073] [Citation(s) in RCA: 150] [Impact Index Per Article: 30.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/20/2019] [Accepted: 09/17/2019] [Indexed: 11/02/2022]
Abstract
Present-day galaxies are surrounded by cool and enriched halo gas extending for hundreds of kiloparsecs. This halo gas is thought to be the dominant reservoir of material available to fuel future star formation, but direct constraints on its mass and physical properties have been difficult to obtain. We report the detection of a fast radio burst (FRB 181112), localized with arcsecond precision, that passes through the halo of a foreground galaxy. Analysis of the burst shows that the halo gas has low net magnetization and turbulence. Our results imply predominantly diffuse gas in massive galactic halos, even those hosting active supermassive black holes, contrary to some previous results.
Collapse
Affiliation(s)
- J Xavier Prochaska
- University of California Observatories-Lick Observatory, University of California, Santa Cruz, CA 95064, USA. .,Kavli Institute for the Physics and Mathematics of the Universe, 5-1-5 Kashiwanoha, Kashiwa, 277-8583, Japan
| | - Jean-Pierre Macquart
- International Centre for Radio Astronomy Research, Curtin University, Bentley, WA 6102, Australia
| | - Matthew McQuinn
- Department of Astronomy, University of Washington, Seattle, WA 98195, USA
| | - Sunil Simha
- University of California Observatories-Lick Observatory, University of California, Santa Cruz, CA 95064, USA
| | - Ryan M Shannon
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - Cherie K Day
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia.,Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Lachlan Marnoch
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia.,Department of Physics and Astronomy, Macquarie University, North Ryde, NSW 2109, Australia
| | - Stuart Ryder
- Department of Physics and Astronomy, Macquarie University, North Ryde, NSW 2109, Australia
| | - Adam Deller
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - Keith W Bannister
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Shivani Bhandari
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Rongmon Bordoloi
- Department of Physics, North Carolina State University, Raleigh, NC 27695, USA
| | - John Bunton
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Hyerin Cho
- School of Physics and Chemistry, Gwangju Institute of Science and Technology, Gwangju 61005, Korea
| | - Chris Flynn
- Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia
| | - Elizabeth K Mahony
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Chris Phillips
- Commonwealth Science and Industrial Research Organisation, Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia
| | - Hao Qiu
- Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, NSW 2006, Australia
| | - Nicolas Tejos
- Instituto de Física, Pontificia Universidad Católica de Valparaíso, Casilla 4059, Valparaíso, Chile
| |
Collapse
|
21
|
Petroff E. Finding the location of a fast radio burst. Science 2019; 365:546-547. [PMID: 31395772 DOI: 10.1126/science.aay4330] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Emily Petroff
- Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, Netherlands.
| |
Collapse
|
22
|
|