THE UNIVERSE IS HISSING at US by Locke Patton

Total Page:16

File Type:pdf, Size:1020Kb

THE UNIVERSE IS HISSING at US by Locke Patton TJO Newsletter Summer 2017 THE UNIVERSE IS HISSING AT US By Locke Patton This story doesn’t start with a Big Bang. It starts was in fact an astrophysical phenomenon coming from with an unrelenting hiss from the universe. In 1960, Bell beyond our galaxy in need of an explanation. Labs built a horn antenna, a radio telescope in Holmdel, They called astrophysics theorist Robert Dicke, New Jersey. It was 20 feet long and hypersensitive to who worked nearby at Princeton University. His focus microwave radio signals, on the low-energy side of the was on the newest hot topic in astronomy at the time: the spectrum of light. Scientists kept the detector cooled to Big Bang theory. Recent observations showed that only 4 degrees Kelvin above absolute zero using liquid galaxy clusters – the visible parts of our universe – were nitrogen – the equivalent of cooling your freezer down to flying away from each other. In other words, the fabric of -269 ºC. Working with the incredibly sensitive data, the universe – space itself – was expanding at an Robert Wilson and Arno Penzias discovered a accelerating rate and carrying matter along for the ride! background noise, much like the static you might have This contradicted even Einstein: the universe heard in your car radio, except this signal was persistent was not in fact a static steady-state universe. Instead, as and uniformly coming from all visible portions of the sky. you roll back time, all objects in the universe fly together, Furthermore, the microwave strength was 100 times becoming more compact until all energy, mass, light and more intense than what current theories had anticipated. space are compressed. It is this singularity of unimaginable mass and energy that first exploded as the Big Bang, and eventually formed the universe we see today. Big Bang theory predicted that the initial universe was an expanding plasma soup of light and particles. As the energy budget within our universe began to spread thin, stretched across expanding space, temperatures lowered rapidly. At 5,000°F, the equivalent temperature of the sun, electrons and protons were cool Original Bell Labs Horn Antenna. Credit: Wikipedia What could cause this excess radio signal? Could New York City be the source? Was it coming from the telescope itself because of a poor internal setup of the device? Even after the scientists kicked out a flock of The moment when free electrons and protons formed Hydrogen atoms, freeing light to travel through space pigeons from their telescope – and cleaned away their and time, reach the Bell Lab telescope and confuse leftover droppings – the noise persisted. They were Penzias and Wilson in the form of the Microwave ultimately forced to conclude that this background signal Radiation. Credit: Universe Adventures 3 TJO Newsletter Summer 2017 enough to find partners. This coupling into electron- – the first possible baby photo of the universe. proton pairs – Hydrogen atoms – finally lifted the veil of The evidence of a uniform cosmic microwave free-moving particles that scattered light. 380,000 years background radiation definitively proved the Big Bang after the Big Bang, the universe turned from opaque to theory. Einstein corrected his equations, calling it his transparent. For the first time, light within the universe biggest blunder. The experimentalists Penzias and was free to travel across space and time, eventually Wilson had the significance of their discovery explained landing at the Horn Antenna. This light – the surface of to them by the newspaper the next morning, but last scattering – was set free. nonetheless jointly won the Nobel Prize in 1978 for their When Penzias and Wilson called Robert Dicke at incredible experimental discovery of the CMB. Further his Princeton office, he infamously commented to his observations of the Cosmic Microwave Background have colleagues “well boys, we’ve been scooped!” The since found tiny 0.00001 K fluctuations of temperature, microwave radiation discovered by Penzias and Wilson known as anisotropies, corresponding to slight density was the first detection of the light from the transparent variations in the plasma from the moment of last universe. Because light travels at the cosmic speed limit scattering. Anisotropies laid the foundation that built of 293 million m/s from the most distant visible reaches modern-day large-scale galactic structure. To this day, of the universe, the light arriving is 14 billion years old. scientists study the CMB to probe the formation of Furthermore, as light travels, it is constrained by the structure and matter in the universe, and cosmology. expanding and cooling universe. While the light left at In the words of my favorite intergalactic 5,000°F, it reaches our detectors as the Cosmic hitchhiker, don’t panic. We are on a sometimes Microwave Background (CMB) at a uniform and cold - incomprehensible but beautiful ride within a universe 450° F, or just 2.7° Kelvin above absolute zero. When sparked by an incredibly massive Big Bang. And we can Penzias and Wilson found their microwave background thank Penzias, Wilson and Dicke for finding and noise, they had stumbled upon a 14-billion-year-old hiss explaining the initial clues that let us know. Thanks to tiny variations in a plasma of particles 14 billion years ago, we now have a hissing universe filled with galactic structure, the Milky Way, Earth, and the curious creatures who call it home. SOURCES CITED Daniel, Lisa. You Can Still Hear the Hiss of the Big Bang. Slate: 2014. Print. Discovery of cosmic microwave background radiation. CMB light is incredibly uniform. Finding variations in Wikipedia, 2017. Print. the 2.7° K temperature is equivalent to finding a Koberlein, Brian. One Universe at a Time: What does the cosmic microwave background tell us? 2015. Print. microbe on a basket ball. But tiny 0.00001 K ripples in The Universe Adventure - Origins of the CMB. temperature of plasma depicted above on a globe are universeadventure.org, 2017. Print. responsible for large scale galactic structure seen Reich, Henry. Picture of the Big Bang (a.k.a. Oldest Light in today. Credit: Brian Koberlein the Universe). minutephysics, 2017. Video. 4 .
Recommended publications
  • What Made Bell Labs Special? Ley in Recent Years, the High Pay and Excellent Working Conditions at Bell Labs Attracted Many Who Might Look Elsewhere Today
    physicsworld.com Christmas books Andrew Gelman What made Bell Labs special? ley in recent years, the high pay and excellent working conditions at Bell Labs attracted many who might look elsewhere today. Second, there was nothing to do at the labs all day but work. I have known lots of middle-aged profes- sors who don’t spend much time teaching but don’t do any research either. At Bell Labs it was harder to be deadwood. Located as it was in the middle of nowhere, the Murray Hill campus was not a place to relax, and if you were going into the lab every weekday anyhow, you might as well work – there was nothing better to do. Several researchers, including Shannon and Shockley, had sharp mid-career productivity declines – but after they left Murray Hill. In my own experience working at Bell Labs for three summers during Bell Laboratories/Alcatel-Lucent USA/AIP Emilio Segrè Visual Archives, Hecht Collection the 1980s, I vividly recall a general feeling of comfort and well-being, Innovation central Bell Labs was a legendary place, an Idea Factory. I say this not at all as a along with the low-level intensity Ali Javan (left) and industrial lab in the outer suburbs of criticism of its author, the journalist that comes from working eight-hour Donald R Herriott New York where thousands of scien- Jon Gertner; rather, there was just so days, week after week after week. work with a helium- tists, working nine to five, changed much going on at Bell that it cannot I did the research underlying my neon optical gas the world’s technological history.
    [Show full text]
  • G.W.A.T.T. (Global 'What If' Analyzer of Network Energy Consumption)
    G.W.A.T.T. New Bell Labs application able to measure the impact of technologies like SDN & NFV on network energy consumption WHITE PAPER Increased energy consumption is a key challenge for the Information and Communications Technologies (ICT) industry. Network energy bills represent more than 10 percent of operators’ operational expenses. With the advent of the Internet of Things era, and the inexorable consumption of video and cloud services promising to drive massively increased traffic across networks, it is even more important for operators to have a complete view of the energy impact of different technology and architectural evolution options. G.W.A.T.T. (Global “What if” Analyzer of NeTwork Energy ConsumpTion) has been built to allow operators and industry stakeholders to better understand these challenges. This application visualizes the current and future communication networks and forecasts key trends in energy consumption, energy efficiency, cost and carbon emissions based on a wide variety of traffic growth scenarios and technology evolution choices. It is intended as a mind-sharing tool to grasp the importance of the energy challenge and how innovation and new technologies can help address these issues in the future. EXECUTIVE SUMMARY The explosion of the Internet traffic volume resulting from both the worldwide broadband subscriber base extension and the increasing number and diversity of available applications and services require a relentless deployment of new technologies and infrastructures to deliver the expected user-experience. At the same time, it also raises the issue of the energy consumption and energy cost of the Internet and more generally of the Information and Communication Technologies (ICT).
    [Show full text]
  • DTMF Control System
    P a g e | 38 Vol. 10 Issue 11 (Ver. 1.0) October 2010 Global Journal of Computer Science and Technology A2Z Control System- DTMF Control System Er. Zatin Gupta1, Payal Jain2 , Monika3 GJCST Classification (FOR) H.4.3 Abstract-Dual Tone Multi Frequency (DTMF) technique for c) Microcontroller (At89s52) controlling the domestic and industrial appliances is being presented in this paper. A simple mobile phone which works on Microcontroller is the control unit of this system. We have DTMF tone, used to control the domestic as well as industrial used AT89S52. It is low power, high performance CMOS 8- electrical appliances which with the control system which we Bit controller with 4K bytes of ROM and 128 bytes of RAM. have designed here for experimental study. In recent state of affairs, domestic, military and industrial applications use this d) Dtmf Signal technique because it can be operated from remote location. Radio frequency (RF) is also used for wireless communication but DTMF is most widely known method of Multi Frequency DTMF is an alternate for RF. Mobile phone is used to send the Shift Keying (MSFK) data transmission technique. DTMF DTMF code from remote location to the control system. The was developed by Bell Labs to be used in the telephone blocks of system are mobile phone, Microcontroller (AT89S52), system. Most telephones today uses DTMF dialing (or “tone” DTMF Decoder (MT8870D), Relays and power supply. This dialing). paper shows the working areas where the system is applicable and how it has advantages over RF. 1209 1336 1477 1633 Hz Hz Hz Hz I.
    [Show full text]
  • The Merlin - Phase 2
    Radio Interferometry: Theory, Techniques and Applications, 381 IAU Coll. 131, ASP Conference Series, Vol. 19, 1991, T.J. Comwell and R.A. Perley (eds.) THE MERLIN - PHASE 2 P.N. WILKINSON University of Manchester, Nuffield Radio Astronomy Laboratories, Jodrell Bank, Macclesfield, Cheshire, SKll 9DL, United Kingdom ABSTRACT The Jodrell Bank MERLIN is currently being upgraded to produce higher sensitivity and higher resolving power. The major capital item has been a new 32m telescope located at MRAO Cambridge which will operate to at least 50 GHz. A brief outline of the upgraded MERLIN and its performance is given. INTRODUCTION The MERLIN (Multi-Element Radio-Linked Interferometer Network), based at Jodrell Bank, was conceived in the mid-1970s and first became operational in 1980. It was a bold concept; no one had made a real-time long-baseline interferometer array with phase-stable local oscillator links before. Six remotely operated telescopes, controlled via telephone lines, are linked to a control computer at Jodrell Bank. The rf signals are transmitted to Jodrell via commercial multi-hop microwave links operating at 7.5 GHz. The local oscillators are coherently slaved to a master oscillator via go-and- return links operating at L-band, the change in the link path-length being taken out in software. This single-frequency L-band link can transfer phase to the equivalent of < 1 picosec (< 0.3 mm of path length) on timescales longer than a few seconds. A detailed description of the MERLIN system has been given by Thomasson (1986). The MERLIN has provided the UK with a unique astronomical facility, one which has made important contributions to extragalactic radio source and OH maser studies.
    [Show full text]
  • Measurement of the Cosmic Microwave Background Radiation at 19 Ghz
    Measurement of the Cosmic Microwave Background Radiation at 19 GHz 1 Introduction Measurements of the Cosmic Microwave Background (CMB) radiation dominate modern experimental cosmology: there is no greater source of information about the early universe, and no other single discovery has had a greater impact on the theories of the formation of the cosmos. Observation of the CMB confirmed the Big Bang model of the origin of our universe and gave us a look into the distant past, long before the formation of the very first stars and galaxies. In this lab, we seek to recreate this founding pillar of modern physics. The experiment consists of a temperature measurement of the CMB, which is actually “light” left over from the Big Bang. A radiometer is used to measure the intensity of the sky signal at 19 GHz from the roof of the physics building. A specially designed horn antenna allows you to observe microwave noise from isolated patches of sky, without interference from the relatively hot (and high noise) ground. The radiometer amplifies the power from the horn by a factor of a billion. You will calibrate the radiometer to reduce systematic effects: a cryogenically cooled reference load is periodically measured to catch changes in the gain of the amplifier circuit over time. 2 Overview 2.1 History The first observation of the CMB occurred at the Crawford Hill NJ location of Bell Labs in 1965. Arno Penzias and Robert Wilson, intending to do research in radio astronomy at 21 cm wavelength using a special horn antenna designed for satellite communications, noticed a background noise signal in all of their radiometric measurements.
    [Show full text]
  • Dynamics of the Arecibo Radio Telescope
    DYNAMICS OF THE ARECIBO RADIO TELESCOPE Ramy Rashad 110030106 Department of Mechanical Engineering McGill University Montreal, Quebec, Canada February 2005 Under the supervision of Professor Meyer Nahon Abstract The following thesis presents a computer and mathematical model of the dynamics of the tethered subsystem of the Arecibo Radio Telescope. The computer and mathematical model for this part of the Arecibo Radio Telescope involves the study of the dynamic equations governing the motion of the system. It is developed in its various components; the cables, towers, and platform are each modeled in succession. The cable, wind, and numerical integration models stem from an earlier version of a dynamics model created for a different radio telescope; the Large Adaptive Reflector (LAR) system. The study begins by converting the cable model of the LAR system to the configuration required for the Arecibo Radio Telescope. The cable model uses a lumped mass approach in which the cables are discretized into a number of cable elements. The tower motion is modeled by evaluating the combined effective stiffness of the towers and their supporting backstay cables. A drag model of the triangular truss platform is then introduced and the rotational equations of motion of the platform as a rigid body are considered. The translational and rotational governing equations of motion, once developed, present a set of coupled non-linear differential equations of motion which are integrated numerically using a fourth-order Runge-Kutta integration scheme. In this manner, the motion of the system is observed over time. A set of performance metrics of the Arecibo Radio Telescope is defined and these metrics are evaluated under a variety of wind speeds, directions, and turbulent conditions.
    [Show full text]
  • The Meerkat Radio Telescope Rhodes University SKA South Africa E-Mail: a B Pos(Meerkat2016)001 Justin L
    The MeerKAT Radio Telescope PoS(MeerKAT2016)001 Justin L. Jonas∗ab and the MeerKAT Teamb aRhodes University bSKA South Africa E-mail: [email protected] This paper is a high-level description of the development, implementation and initial testing of the MeerKAT radio telescope and its subsystems. The rationale for the design and technology choices is presented in the context of the requirements of the MeerKAT Large-scale Survey Projects. A technical overview is provided for each of the major telescope elements, and key specifications for these components and the overall system are introduced. The results of selected receptor qual- ification tests are presented to illustrate that the MeerKAT receptor exceeds the original design goals by a significant margin. MeerKAT Science: On the Pathway to the SKA, 25-27 May, 2016, Stellenbosch, South Africa ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/ MeerKAT Justin L. Jonas 1. Introduction The MeerKAT radio telescope is a precursor for the Square Kilometre Array (SKA) mid- frequency telescope, located in the arid Karoo region of the Northern Cape Province in South Africa. It will be the most sensitive decimetre-wavelength radio interferometer array in the world before the advent of SKA1-mid. The telescope and its associated infrastructure is funded by the government of South Africa through the National Research Foundation (NRF), an agency of the Department of Science and Technology (DST). Construction and commissioning of the telescope has been the responsibility of the SKA South Africa Project Office, which is a business unit of the PoS(MeerKAT2016)001 NRF.
    [Show full text]
  • High-Resolution Radio Observations of Submillimetre Galaxies
    Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 7 November 2018 (MN LATEX style file v2.2) High-resolution radio observations of submillimetre galaxies A. D. Biggs1⋆ and R.J. Ivison1,2 1UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ 2Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ Accepted 2007 December 17. Received 2007 December 14; in original form 2007 September 11 ABSTRACT We have produced sensitive, high-resolution radio maps of 12 submillimetre (submm) galax- ies (SMGs) in the Lockman Hole using combined Multi-Element Radio-Linked Interferom- eter Network (MERLIN) and Very Large Array (VLA) data at a frequency of 1.4GHz. Inte- grating for 350hr yielded an r.m.s. noise of 6.0 µJybeam−1 and a resolution of 0.2–0.5arcsec. For the first time, wide-field data from the two arrays have been combined in the (u, v) plane and the bandwidthsmearing response of the VLA data has been removed.All of the SMGs are detected in our maps as well as sources comprising a non-submm luminous control sample. We find evidence that SMGs are more extended than the general µJy radio population and that therefore, unlike in local ultraluminous infrared galaxies (ULIRGs), the starburst compo- nent of the radio emission is extended and not confined to the galactic nucleus. For the eight sources with redshifts we measure linear sizes between 1 and 8kpc with a median of 5kpc. Therefore, they are in general larger than local ULIRGs which may support an early-stage merger scenario for the starburst trigger.
    [Show full text]
  • High Resolution Radio Astronomy Using Very Long Baseline Interferometry
    IOP PUBLISHING REPORTS ON PROGRESS IN PHYSICS Rep. Prog. Phys. 71 (2008) 066901 (32pp) doi:10.1088/0034-4885/71/6/066901 High resolution radio astronomy using very long baseline interferometry Enno Middelberg1 and Uwe Bach2 1 Astronomisches Institut, Universitat¨ Bochum, 44801 Bochum, Germany 2 Max-Planck-Institut fur¨ Radioastronomie, Auf dem Hugel¨ 69, 53121 Bonn, Germany E-mail: [email protected] and [email protected] Received 3 December 2007, in final form 11 March 2008 Published 2 May 2008 Online at stacks.iop.org/RoPP/71/066901 Abstract Very long baseline interferometry, or VLBI, is the observing technique yielding the highest-resolution images today. Whilst a traditionally large fraction of VLBI observations is concentrating on active galactic nuclei, the number of observations concerned with other astronomical objects such as stars and masers, and with astrometric applications, is significant. In the last decade, much progress has been made in all of these fields. We give a brief introduction to the technique of radio interferometry, focusing on the particularities of VLBI observations, and review recent results which would not have been possible without VLBI observations. This article was invited by Professor J Silk. Contents 1. Introduction 1 2.9. The future of VLBI: eVLBI, VLBI in space and 2. The theory of interferometry and aperture the SKA 10 synthesis 2 2.10. VLBI arrays around the world and their 2.1. Fundamentals 2 capabilities 10 2.2. Sources of error in VLBI observations 7 3. Astrophysical applications 11 2.3. The problem of phase calibration: 3.1. Active galactic nuclei and their jets 12 self-calibration 7 2.4.
    [Show full text]
  • Table of Contents - 1 - - 2
    Table of contents - 1 - - 2 - Table of Contents Foreword 5 1. The European Consortium for VLBI 7 2. Scientific highlights on EVN research 9 3. Network Operations 35 4. VLBI technical developments and EVN operations support at member institutes 47 5. Joint Institute for VLBI in Europe (JIVE) 83 6. EVN meetings 105 7. EVN publications in 2007-2008 109 - 3 - - 4 - Foreword by the Chairman of the Consortium The European VLBI Network (EVN) is the result of a collaboration among most major radio observatories in Europe, China, Puerto Rico and South Africa. The large radio telescopes hosted by these observatories are operated in a coordinated way to perform very high angular observations of cosmic radio sources. The data are then correlated by using the EVN correlator at the Joint Institute for VLBI in Europe (JIVE). The EVN, when operating as a single astronomical instrument, is the most sensitive VLBI array and constitutes one of the major scientific facilities in the world. The EVN also co-observes with the Very Long Baseline Array (VLBA) and other radio telescopes in the U.S., Australia, Japan, Russia, and with stations of the NASA Deep Space Network to form a truly global array. In the past, the EVN also operated jointly with the Japanese space antenna HALCA in the frame of the VLBI Space Observatory Programme (VSOP). The EVN plans now to co-observe with the Japanese space 10-m antenna ASTRO-G, to be launched by 2012, within the frame of the VSOP-2 project. With baselines in excess of 25.000 km, the space VLBI observations provide the highest angular resolution ever achieved in Astronomy.
    [Show full text]
  • I : the Discovery of the Cosmic Microwave Background
    Class 19 : The cosmic microwave background and the “Hot Big Bang” theory Discovery of the cosmic microwave background Basic idea of the Hot Big Bang I : The discovery of the cosmic microwave background Penzias & Wilson (Bell-Labs) 1 Arno Penzias & Robert Wilson (1964) Were attempting to study radio emissions from our Galaxy using sensitive antenna built at Bell-Labs Needed to characterize and eliminate all sources of noise They never could get rid of a certain noise source… noise had a characteristic temperature of about 3 K. They figured out that the noise was coming from the sky, and was approximately the same in all directions… The COBE mission Built by NASA-Goddard Space Flight Center Launched Nov. 1989 Purpose was to survey infra-red and microwave emission across the whole sky. Primary purpose – to characterize the CMB. Had a number of instruments on it: FIRAS (Far infra-red absolute spectrophotometer) DMR (Differential Microwave Radiometer) DIRBE (Diffuse Infrared background Experiment) 2 Our Galaxy observed by the DIRBE instrument on COBE 3 Almost uniform intensity of microwaves in all directions (isotropic 2.7K black body radiation) 4 Subtracting off the mean level leaves with a “dipole” pattern… what is this?? Subtracting off the dipole finally reveals the emission from the Galaxy that Penzias and Wilson were looking for! 5 Subtracting contribution from Galaxy reveals fluctuations in the CMB WMAP (2004) 6 II : The hot big bang model Penzias & Wilson had discovered radiation left over from the early universe… The hot big bang model… Independently developed by James Peebles and George Gamov They suggested that the universe started off in an extremely hot state.
    [Show full text]
  • Overview of Motion Control on the KAT-7 and Meerkat Radio Telescopes Lance Williams Photo: SKA South Africa
    Overview of Motion Control on the KAT-7 and MeerKAT Radio Telescopes Lance Williams Photo: SKA South Africa KAT-7 Radio Telescope KAT-7 • Prototype/pathfinder for MeerKAT • 7 antennas with approx. 15m main reflector diameter • Elevation over azimuth movement • Azimuth movement via motor driving gear in pedestal • Elevation movement via jack screw Photo: SKA South Africa Technical Challenges • Adapting drives designed for CNC machines. Issues with encoder startup reference caused by position slip during shut down. • The synchronization to NTP required special development. • Adapting controllers for continuous operation. Issues with unexpected controller reboots caused by buffer overflows. • Composite reflector accuracy. Lessons learned • Time spent re -coding or changing development • Better simulators for smoother integration • ICD and requirements for concurrent development Photo: SKA South Africa Photo: SKA South Africa MeerKAT Radio Telescope Motion Control on Radio Telescope • Moving yoke structure on static pedestal • Elevation over azimuth movement • Multiple receivers mounted on rotating platform (receiver indexer) • Precision target tracking • Fast slewing between targets • Continuous operation Photo: SKA South Africa Technical Challenges • EMI measurement - defining new test methods • EMI mitigation • Maintaining EMI performance through manufacture • Unit testing (e.g. gearbox control) • Modification to standard software (e.g. Servo Computer) • Concurrent development Lessons Learned • Testing improvements • Effect of installed
    [Show full text]