Ultra-Powerful Signals Known As Fast Radio Bursts Are Bombarding Earth
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Fast Radio Bursts May Be Firing Off Every Second 21 September 2017
Fast radio bursts may be firing off every second 21 September 2017 see with our eyes, these flashes come in radio waves." To make their estimate, Fialkov and co-author Avi Loeb assumed that FRB 121102, a fast radio burst located in a galaxy about 3 billion light years away, is representative of all FRBs. Because this FRB has produced repeated bursts since its discovery in 2002, astronomers have been able to study it in much more detail than other FRBs. Using that information, they projected how many FRBs would exist across the entire sky. "In the time it takes you to drink a cup of coffee, hundreds of FRBs may have gone off somewhere This artist's impression shows part of the cosmic web, a in the Universe," said Avi Loeb. "If we can study filamentary structure of galaxies that extends across the even a fraction of those well enough, we should be entire sky. The bright blue, point sources shown here are able to unravel their origin." the signals from Fast Radio Bursts (FRBs) that may accumulate in a radio exposure lasting for a few minutes. The radio signal from an FRB lasts for only a While their exact nature is still unknown, most few thousandths of a second, but they should occur at scientists think FRBs originate in galaxies billions of high rates. Credit: M. Weiss/CfA light years away. One leading idea is that FRBs are the byproducts of young, rapidly spinning neutron stars with extraordinarily strong magnetic fields. When fast radio bursts, or FRBs, were first Fialkov and Loeb point out that FRBs can be used detected in 2001, astronomers had never seen to study the structure and evolution of the Universe anything like them before. -
Atmospheric Interpretation of Anomalous Terrestrial
Atmospheric Interpretation of Anomalous Terrestrial Emission Serendipitously Discovered in Radioastronomy Data at 1 Gigahertz Sarah Burke-Spolaor1, Ron Ekers1, and Jean-Pierre Macquart 2 1 CSIRO Astronomy and Space Sciences, PO Box 76, Epping NSW 1710, Australia [email protected] 2 ICRAR/Curtin Institute of Radio Astronomy, GPO Box U1987, Perth WA 6845, Australia Abstract A publication in the Astrophysical Journal [1] reported the discovery of swept-frequency, terrestrial emission in a search for astrophysical pulses. The emission's origin has yet to be determined; its attributes are atypical of known sources of terrestrial signals. We review the observed properties of the emission and present a simple model for a physical mechanism that could occur in the atmosphere to produce it. If this mechanism is the cause of the emission, its origin may lie in secondary effects of lightning production in the upper atmosphere. 1 Introduction Searches for isolated astronomical radio pulses have grown in popularity following a number of recent discoveries [e.g. 2-3]. The surfeit of Earth-origin (man-made and natural) pulses requires these searches to use techniques that discriminate target signals from terrestrial pulses. A basic feature of astronomical pulses is their frequency-dependent delay, which follows δt / f −2. This is an additive dispersion effect resulting from propagation through interstellar plasma that is negligible in locally-generated emission (see Fig. 1). Recently, sixteen terrestrial pulses with frequency-swept characteristics that mimic an astronomical dis- persion delay were reported [1]. They were found in data taken at sparse intervals over the years 1998{2003, using the multibeam receiver on Parkes Radio Telescope in Australia and a specialized back-end hardware that allows 96 spectral bands to be sampled across a 288 MHz bandwidth centered at f = 1:375 GHz. -
Ionization History of Hydrogen
Signatures of the First Generation of Objects KITP 2004 Ionization History of Hydrogen REDSHIFT 6 1000 TIME Billion Million years years Avi Loeb, Harvard (KITP Galaxy-IGM Conference 10/26/04) 1 Signatures of the First Generation of Objects Emergence of the First Star Clusters molecular hydrogen Yoshida et al. 2003 Hydrogen e- p Ground level excitation rate= (atomic collisions)+(radiative coupling to CMB) Couple T s to T k Couples T s to Tí spin 21cm = (1:4GHz) 1 1s 1=2 p e- 0s 1=2 p e- n 1 g1 0:068K Spin Temperature = expf à g (g1=g0) = 3 n 0 g0 Ts Predicted by Van de Hulst in 1944; Observed by Ewen &Purcell in 1951 at Harvard Avi Loeb, Harvard (KITP Galaxy-IGM Conference 10/26/04) 2 Signatures of the First Generation of Objects 21 cm Absorption by Hydrogen Prior to Structure Formation à 1=2 à T = ü Ts Tí T = 28mK 1+ z Ts Tí b 1+ z b 10 Ts Fluctuations in 21cm brightness are sourced by fluctuations in gas density Loeb & Zaldarriaga, Phys. Rev. Lett., 2004; astro-ph/0312134 Observed wavelength=21cm (1+z) 3D tomography (slicing the universe in redshift ) Largest Data Set on the Sky Number of independent patches: 3 16 lmax É ÷ ø 10 106 ÷ while Silk damping limits the primary CMB anisotropies to only ø 107 Noise due to foreground sky brightness: Loeb & Zaldarriaga, Phys. Rev. Lett., 2004; astro-ph/0312134 Avi Loeb, Harvard (KITP Galaxy-IGM Conference 10/26/04) 3 Signatures of the First Generation of Objects Line-of-Sight Anisotropy of 21cm Flux Fluctuations à T = ü Ts Tí b 1+ z 1 + î n HI = nö(1 + î ) Peculiar velocity changes ü / 1 dvr =dr -
Quantifying Satellites' Constellations Damages
S. Gallozzi et al., 2020 Concerns about Ground Based Astronomical Observations: Quantifying Satellites’ Constellations Damages in Astronomy 1 Concerns about ground-based astronomical observations: QUANTIFYING SATELLITES’CONSTELLATIONS DAMAGES STEFANO GALLOZZI1,D IEGO PARIS1,M ARCO SCARDIA2, AND DAVID DUBOIS3 [email protected], [email protected], INAF-Osservatorio Astronomico di Roma (INAF-OARm), v. Frascati 33, 00078 Monte Porzio Catone (RM), IT [email protected], INAF-Osservatorio Astronomico di Brera (INAF-OABr), Via Brera, 28, 20121 Milano (Mi), IT [email protected], National Aeronautics and Space Administration (NASA), M/S 245-6 and Bay Area Environmental Research Institute, Moffett Field, 94035 CA, USA Compiled March 26, 2020 Abstract: This article is a second analysis step from the descriptive arXiv:2001.10952 ([1]) preprint. This work is aimed to raise awareness to the scientific astronomical community about the negative impact of satellites’ mega-constellations and estimate the loss of scientific contents expected for ground-based astro- nomical observations when all 50,000 satellites (and more) will be placed in LEO orbit. The first analysis regards the impact on professional astronomical images in optical windows. Then the study is expanded to other wavelengths and astronomical ground-based facilities (in radio and higher frequencies) to bet- ter understand which kind of effects are expected. Authors also try to perform a quantitative economic estimation related to the loss of value for public finances committed to the ground -based astronomical facilities harmed by satellites’ constellations. These evaluations are intended for general purposes and can be improved and better estimated; but in this first phase, they could be useful as evidentiary material to quantify the damage in subsequent legal actions against further satellite deployments. -
Introduction
1 Introduction Are there exotic sources of radio impulses in other galaxies? Do undiscovered planets exist in our solar system? What happens to supermassive black holes when two galaxies collide? How correct was Einstein’s theory of relativity? Strangely enough, all of these questions can be addressed through the study of stars that extend no larger than a few tens of kilometres across. This thesis deals with a wide range of topics—all, however, are endeavours motivated by the broad area of research commonly termed “Pulsar Astronomy”. This introduction and the following chapters aim to communicate the rich body of scientific research related to pulsar astronomy and its related technical requirements, even if studying pulsars is not always the central aim of the research. In this chapter we provide a context to understand the advances made in this thesis. The first section introduces pulsars and relevant properties of the stars themselves. The second section gives an introduction to using pulsars as tools to study other physical phenomena, and the third outlines the relationship that pulsar studies have to the exploration of gravitational wave sources, in particular binary supermassive black hole systems. The fourth section reviews the specialised technical systems designed to study pulsars, and how they are being used to search the vast frontier of undiscovered celestial transient radio emitters. 1.1 Pulsars Pulsars have only been the subject of observation since late 1967, when highly periodic pulses were recorded and recognised as a celestial phenomenon by Hewish et al. (1968). The prediction of Baade & Zwicky (1934) stated that compact objects should exist at the 1 2 Chapter 1. -
Interstellar Interlopers Two Recently Sighted Space Rocks That Came from Beyond the Solar System Have Puzzled Astronomers
A S T R O N O MY InterstellarInterstellar Interlopers Two recently sighted space rocks that came from beyond the solar system have puzzled astronomers 42 Scientific American, October 2020 © 2020 Scientific American 1I/‘OUMUAMUA, the frst interstellar object ever observed in the solar system, passed close to Earth in 2017. InterstellarInterlopers Interlopers Two recently sighted space rocks that came from beyond the solar system have puzzled astronomers By David Jewitt and Amaya Moro-Martín Illustrations by Ron Miller October 2020, ScientificAmerican.com 43 © 2020 Scientific American David Jewitt is an astronomer at the University of California, Los Angeles, where he studies the primitive bodies of the solar system and beyond. Amaya Moro-Martín is an astronomer at the Space Telescope Science Institute in Baltimore. She investigates planetary systems and extrasolar comets. ATE IN THE EVENING OF OCTOBER 24, 2017, AN E-MAIL ARRIVED CONTAINING tantalizing news of the heavens. Astronomer Davide Farnocchia of NASA’s Jet Propulsion Laboratory was writing to one of us (Jewitt) about a new object in the sky with a very strange trajectory. Discovered six days earli- er by University of Hawaii astronomer Robert Weryk, the object, initially dubbed P10Ee5V, was traveling so fast that the sun could not keep it in orbit. Instead of its predicted path being a closed ellipse, its orbit was open, indicating that it would never return. “We still need more data,” Farnocchia wrote, “but the orbit appears to be hyperbolic.” Within a few hours, Jewitt wrote to Jane Luu, a long-time collaborator with Norwegian connections, about observing the new object with the Nordic Optical Telescope in LSpain. -
• Pawan Kumar Outline† Fast Radio Burst Physics & Cosmology
Fast Radio Burst Physics & Cosmology Pawan Kumar Outline† • A brief summary of observations • FRB physics – general constraints & a specific model • FRBs as probe of cosmology †Wenbin Lu, Paz Beniamini (FRB physics) M. Bhattacharya, E. Linder, X. Ma, Eliot Quataert (FRB-cosmology) Paris, May 27, 2021 Fast Radio Bursts (FRBs) * * * * Dispersion relation for EM waves in plasma: # =#+ + - $ ; #+ : plasma frequency "# V = ; signal at # is delayed, wrt # = ∞, by ∝ #)* EM "$ 67489 -3 The magnitude of the delay is ∝ ./ = ∫1234-5 ": ;5 (unit: pc cm ) The first FRB was discovered in 2007 – Parkes 64m radio telescope at 1.4 GHz Lorimer et al. (2007) Lorimer et al. (2007) Duration (δt) = 5ms DM = 375 pc cm-3 (DM from the Galaxy 25 cm-3pc –– high galactic latitude) Estimated distance ~ 500 Mpc (from mean IGM density) ∴ Luminosity = 1043 erg s-1 (1010 times brighter than the Sun) A Brief history (8 years of confusion and then a breakthrough) • 16 more bursts detected (2010) in Parkes archival data by Bailes & Burke-Spolaor These bursts were detected in all 13 beams of the telescope, i.e. most likely terrestrial in origin. Many people suspected that the Lorimer burst was also not cosmological. These bursts were dubbed Peryton – after the mythical winged stag. • Clever detective work by Emily Petroff et al. (2015) established the origin of Perytons (microwave oven!) Arecibo detects a burst in 2012; repeat activity found in 2015 (Spitler et al. 2016). Accurate localization led to distance measurement & confirmation that this event was cosmological and not catastrophic. FRB in our Galaxy! FRB200428 It is associated with a well known magnetar (neutron star with super-strong magnetic field) with 14 B=2.2x10 G; P=3.2s 2 - and spin-down age of 2020) al. -
ASTRONET ERTRC Report
Radio Astronomy in Europe: Up to, and beyond, 2025 A report by ASTRONET’s European Radio Telescope Review Committee ! 1!! ! ! ! ERTRC report: Final version – June 2015 ! ! ! ! ! ! 2!! ! ! ! Table of Contents List%of%figures%...................................................................................................................................................%7! List%of%tables%....................................................................................................................................................%8! Chapter%1:%Executive%Summary%...............................................................................................................%10! Chapter%2:%Introduction%.............................................................................................................................%13! 2.1%–%Background%and%method%............................................................................................................%13! 2.2%–%New%horizons%in%radio%astronomy%...........................................................................................%13! 2.3%–%Approach%and%mode%of%operation%...........................................................................................%14! 2.4%–%Organization%of%this%report%........................................................................................................%15! Chapter%3:%Review%of%major%European%radio%telescopes%................................................................%16! 3.1%–%Introduction%...................................................................................................................................%16! -
Geometry of the Universe ______By Avi Loeb on July 8, 2020
Geometry of the Universe _______ By Avi Loeb on July 8, 2020 At ancient times, wise people like Aristotle thought that heavy objects fall faster than lightweight objects under the influence of gravity. About four and a half centuries ago, Galileo Galilei decided to test this assumption experimentally. He dropped objects of different masses from the Leaning Tower of Pisa and found that they all fall the same way under the influence of Earth’s gravity. Three-and-a-quarter centuries later, Albert Einstein was struck by Galileo’s finding and realized that if all objects follow the same trajectory under gravity, then gravity might not be a force but rather a property of spacetime, the fabric which all objects share the same way (establishing the so-called “equivalence principle”). More importantly, Einstein recognized that when spacetime is curved objects do not follow straight lines. He reckoned that the Earth moves around the Sun because the Sun curves spacetime in its vicinity. The Earth’s orbit follows a circle, similarly to a ball on the rubber surface of a trampoline whose center is pulled down by the weight of a person. In November 1915, Einstein formulated his insight through mathematical equations that established the foundation for his General Theory of Relativity. One side of Einstein’s equations includes all masses that source gravity (like the person standing on the trampoline) and the other side quantifies the curvature of spacetime. In the words of John Wheeler: “Spacetime tells matter how to move and matter tells spacetime how to curve”. The first solution of Einstein’s equations was derived by Karl Schwarzschild a few months later, while serving on the German front during World War II. -
Pos(11Th EVN Symposium)109 Erse (6Cm) and Imply Bright- ⊕ D ⊕ D Ce
RadioAstron Early Science Program Space-VLBI AGN survey: strategy and first results PoS(11th EVN Symposium)109 Kirill V. Sokolovsky∗ Astro Space Center, Lebedev Physical Inst. RAS, Profsoyuznaya 84/32, 117997 Moscow, Russia Sternberg Astronomical Institute, Moscow University, Universitetsky 13, 119991 Moscow, Russia E-mail: [email protected] for the RadioAstron AGN Early Science Working Group RadioAstron is a project to use the 10m antenna on board the dedicated SPEKTR-R spacecraft, launched on 2011 July 18, to perform Very Long Baseline Interferometry from space – Space- VLBI. We describe the strategy and highlight the first results of a 92/18/6/1.35cm fringe survey of some of the brighter radio-loud Active Galactic Nuclei (AGN) at baselines up to 25 Earth diam- eters (D⊕). The survey goals include a search for extreme brightness temperatures to resolve the Doppler factor crisis and to constrain possible mechanisms of AGN radio emission, studying the observed size distribution of the most compact features in AGN radio jets (with implications for their intrinsic structure and the properties of the scattering interstellar medium in our Galaxy) and selecting promising objects for detailed follow-up observations, including Space-VLBI imaging. Our survey target selection is based on the results of correlated visibility measurements at the longest ground-ground baselines from previous VLBI surveys. The current long-baseline fringe detections with RadioAstron include OJ 287 at 10 D⊕ (18cm), BL Lac at 10 D⊕ (6cm) and B0748+126 at 4.3 D⊕ (1.3cm). The 18 and 6cm-band fringe detections at 10 D⊕ imply bright- 13 ness temperatures of Tb ∼ 10 K, about two orders of magnitude above the equipartition inverse Compton limit. -
Fast Radio Bursts
UvA-DARE (Digital Academic Repository) Fast radio bursts Petroff, E.; Hessels, J.W.T.; Lorimer, D.R. DOI 10.1007/s00159-019-0116-6 Publication date 2019 Document Version Final published version Published in Astronomy and Astrophysics Review License CC BY Link to publication Citation for published version (APA): Petroff, E., Hessels, J. W. T., & Lorimer, D. R. (2019). Fast radio bursts. Astronomy and Astrophysics Review, 27(1), [4]. https://doi.org/10.1007/s00159-019-0116-6 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:03 Oct 2021 The Astronomy and Astrophysics Review (2019) 27:4 https://doi.org/10.1007/s00159-019-0116-6 REVIEW ARTICLE Fast radio bursts E. Petroff1,2 · J. -
Astro2010: the Astronomy and Astrophysics Decadal Survey
Astro2010: The Astronomy and Astrophysics Decadal Survey Notices of Interest 1. 4 m space telescope for terrestrial planet imaging and wide field astrophysics Point of Contact: Roger Angel, University of Arizona Summary Description: The proposed 4 m telescope combines capabilities for imaging terrestrial exoplanets and for general astrophysics without compromising either. Extremely high contrast imaging at very close inner working angle, as needed for terrestrial planet imaging, is accomplished by the powerful phase induced amplitude apodization method (PIAA) developed by Olivier Guyon. This method promises 10-10 contrast at 2.0 l/D angular separation, i.e. 50 mas for a 4 m telescope at 500 nm wavelength. The telescope primary mirror is unobscured with off-axis figure, as needed to achieve such high contrast. Despite the off-axis primary, the telescope nevertheless provides also a very wide field for general astrophysics. A 3 mirror anastigmat design by Jim Burge delivers a 6 by 24 arcminute field whose mean wavefront error of 12 nm rms, i.e.diffraction limited at 360 nm wavelength. Over the best 10 square arcminutes the rms error is 7 nm, for diffraction limited imaging at 200 nm wavelength. Any of the instruments can be fed by part or all of the field, by means of a flat steering mirror at the exit pupil. To allow for this, the field is curved with a radius equal to the distance from the exit pupil. The entire optical system fits in a 4 m diameter cylinder, 8 m long. Many have considered that only by using two spacecraft, a conventional on-axis telescope and a remote occulter, could high contrast and wide field imaging goals be reconciled.