Significance of Black Hole Visualization and Its Implication For
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Radio Astronomy & Radio Telescopes
Radio Astronomy & Radio Telescopes Tasso Tzioumis ([email protected]) Australia Telescope National Facility (ATNF) sms2020, Stellenbosch 2-6 March 2020 CSIRO ASTRONOMY AND SPACE SCIENCE Radio Astronomy – ITU definition 1.13 radio astronomy: Astronomy based on the reception of radio waves of cosmic origin. 1.5 radio waves or hertzian waves: Electromagnetic waves of frequencies arbitrarily lower than 3 000 GHz, propagated in space without artificial guide. • Astronomy covers the whole electromagnetic spectrum • Radio astronomy is the “low energy” part of the spectrum é 3 000 GHz Radioastronomy & Radio telescopes | Tasso Tzioumis Radio Astronomy “special” characteristics Technical challenges • Very faint signals – measured in 10-26 W/m2/Hz (-260 dBW) • “Power collected by all radiotelescopes since the start of radio astronomy would light a 1W bulb for less than 1 second” • à Need “sensitivity” i.e. large antennas and/or arrays of many antennas • à Very susceptible to intereference • Celestial structures at all scales: from very large to very small • à Need “spatial resolution” i.e. ability to see the details at all scales • à Need large antennas and/or arrays of many antennas • Astronomical events at all timescales(from < 1ms to > millions years) & and at all spectral resolutions (from < 1 Hz to GHz) • à Need very high time and frequency resolution • à Sensitive telescopes and arrays & extreme technical challenges Radioastronomy & Radio telescopes | Tasso Tzioumis Radio Astronomy “special” characteristics Scientific challenges • Radio -
Quasistellar Objects: Overview ENCYCLOPEDIA of ASTRONOMY and ASTROPHYSICS
eaa.iop.org DOI: 10.1888/0333750888/1585 Quasistellar Objects: Overview Patrick Osmer From Encyclopedia of Astronomy & Astrophysics P. Murdin © IOP Publishing Ltd 2006 ISBN: 0333750888 Institute of Physics Publishing Bristol and Philadelphia Downloaded on Thu Mar 02 22:43:08 GMT 2006 [131.215.103.76] Terms and Conditions Quasistellar Objects: Overview ENCYCLOPEDIA OF ASTRONOMY AND ASTROPHYSICS Quasistellar Objects: Overview Quasistellar objects, or quasars, were defined originally as star-like objects of large redshift. Quasars are believed to be powered by the accretion of matter onto massive black holes at the centers of galaxies, a process that emits more energy than thermonuclear reactions. Today, quasars are considered to be the most luminous members of the general class of objects called active galactic nuclei, or AGNs. Quasars are the most luminous objects in the universe. This article begins with a brief history of the discovery of quasars. Next it describes their main properties and the concepts that have been developed to explain them. It continues with a description of their nature and theoretical models. Then additional properties and topics are considered: absorption lines, host galaxies, Figure 1. Optical image of 3C273. The object looks stellar in and luminosity functions and evolution. this image except that it is accompanied by a jet of radiation extending to the lower right. (Credit National Optical Astronomy Observatories/National Science Foundation. History Copyright Association of Universities for Research in In 1960 Mathews and Sandage identified the radio source Astronomy Inc (AURA), all rights reserved.) 3C 48 (the 48th object in the 3rd Cambridge catalog of radio sources) with a star-like object of 16th magnitude. -
Pos(Westerbork)006 S 4.0 International License (CC BY-NC-ND 4.0)
Exploring the time-varying Universe PoS(Westerbork)006 Richard Strom ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] Lodie Voûte ASTRON, Anton Pannekoek Inst. Of Astronomy, University of Amsterdam, Postbus 94249, 1090 GE Amsterdam, The Netherlands E-mail: [email protected] Benjamin Stappers School of Phys. & Astron., Alan Turing Bldg., University of Manchester, Oxford Road, Manchester M13 9PL, UK E-mail: [email protected] Gemma Janssen ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] Jason Hessels ASTRON Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands E-mail: [email protected] 50 Years Westerbork Radio Observatory, A Continuing Journey to Discoveries and Innovations Richard Strom, Arnold van Ardenne, Steve Torchinsky (eds) Published with permission of the Netherlands Institute for Radio Astronomy (ASTRON) under the terms of the Creative CommonsAttribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Exploring the time-varying Universe Chapter 5.1 The earliest start Richard Strom* Introduction The WSRT interferometrically measures Fourier components of the sky bright- ness distribution from a region set by the primary beam of the telescope ele- ments, at a radio frequency determined by the receiver. This information is used to construct a two-dimensional image of radio emission from the piece of sky observed. Because it is an east-west interferometer array, the information obtained at any instant of time can only be used to construct a one-dimensional map (the telescope so synthesized has the response of a fan beam – narrow in one direction, but orthogonally very elongated). -
Interferometry and Aperture Synthesis in Order to Understand the Re
Summer Student Lecture Notes INTERFEROMETRY AND APERTURE SYNTHESIS Bruce Balick July 1973 The following pages are reprinted (with corrections) from Balick, B. 1972, thesis (Cornell University) CHAPTER II INTERFEROMETRY AND APERTURE SYNTHESIS Electromagnetic radiation is a wave phenomena, consequently in- struments used to observe this radiation are subject to diffraction limi- tations on their resolution. The angular limit, A, is given approxi- mately by AS6 D/A, where D is the aperture dimension and X is the obscwrving wavelcngth; for radio work - _____A - 140 B/cm) min -arc [D/feet] Thus the 300-foot telescope has a maximum resolution of 6' .arc at XAll cm, whereas a 10-cm aperture optical telescope has a diffraction limit of 1" are at optical wavelengths. (The same high resolution would require ap- ertures 1-1000 km in diameter at radio wavelengths.) To obtain high resolution at radio wavelengths, partially fill- ed apertures of large diameter can be synthesized. For this, two tele- scopes separated by a baseline B can be used to simulate the response of a nearly circular annulus of diameter IB. The telescope pair is con- figured in such a manner that it is best described as an interferometer in the ordinary optical sense. By moving the telescopes to obtain inter- ferometers of different spacings, annuli of different sizes can be simu- lated. The results obtained on the various spacings can be added appropriately to synthesize the response of a single telescope of very large diameter, and thereby yield maps of high resolution. For example, the interferometer of the National Radio Astronomy Observatory (NRAO) can 10 S. -
Cross-Correlator Implementations Enabling Aperture Synthesis for Geostationary-Based Remote Sensing
THESIS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Cross-Correlator Implementations Enabling Aperture Synthesis for Geostationary-Based Remote Sensing ERIK RYMAN Division of Computer Engineering Department of Computer Science and Engineering CHALMERS UNIVERSITY OF TECHNOLOGY Göteborg, Sweden 2018 Cross-Correlator Implementations Enabling Aperture Synthesis for Geostationary-Based Remote Sensing Erik Ryman ISBN 978-91-7597-751-5 Copyright © Erik Ryman, 2018. Doktorsavhandlingar vid Chalmers tekniska högskola Ny serie Nr 4432 ISSN 0346-718X Technical report No. 156D Department of Computer Science and Engineering VLSI Research Group Department of Computer Science and Engineering Chalmers University of Technology SE-412 96 GÖTEBORG, Sweden Phone: +46 (0)31-772 10 00 Author e-mail: [email protected] Cover: A 64-channel cross-correlator unit, including chip photos of digital correlator and analog-to-digital converter. Printed by Chalmers Reproservice Göteborg, Sweden 2018 Cross-Correlator Implementations Enabling Aperture Synthesis for Geostationary-Based Remote Sensing Erik Ryman Department of Computer Science and Engineering, Chalmers University of Technology ABSTRACT An ever-increasing demand for weather prediction and high climate modelling ac- curacy drives the need for better atmospheric data collection. These demands in- clude better spatial and temporal coverage of mainly humidity and temperature distributions in the atmosphere. A new type of remote sensing satellite technol- ogy is emerging, originating in the field of radio astronomy where telescope aper- ture upscaling could not keep up with the increasing demand for higher resolution. Aperture synthesis imaging takes an array of receivers and emulates apertures ex- tending way beyond what is possible with any single antenna. In the field of Earth remote sensing, the same idea could be used to construct satellites observing in the microwave region at a high resolution with foldable antenna arrays. -
Book of Abstracts
Dissecting the Universe - Workshop on Results from High-Resolution VLBI Monday 30 November 2015 - Wednesday 02 December 2015 Max-Planck-Institut für Radioastronomie, Bonn, Germany Book of Abstracts Contents GMVA Observations of M87 and Status Report of the GLT Project . 1 Water megamasers at high resolution . 1 Millimeter VLBI Observations of the Twin-Jet-System in NGC1052 . 1 First 3mm-VLBI imaging of the two-sided jet in Cygnus A: zooming into the launching region . 2 New insight into AGN-jets: they are alive! . 2 The connection between the mm VLBI jet and the gamma-ray emission in the blazar CTA102 and the radio galaxy 3C120 . 2 New Developments with the Event Horizon Telescope . 3 Dissecting TeV blazars: Space VLBI study of the BL Lac source Markarian 501 . 3 VLBI Studies of Star Forming Regions using Molecular Masers . 4 The farthest view with overterrestrial baselines . 4 Probing the innermost regions of AGN jets and their magnetic fields with RadioAstron 4 What has VLBI at the highest resolutions taught us about the VLBI "core"? . 5 The most compact H2O maser spots and their locations in W3 IRS5 . 5 A physical model for the radio and GeV emission from the microquasar LS I +61◦303 6 Detection and Implications of Horizon-Scale Polarization in Sgr A* . 7 The Discovery and Implications of Refractive Substructure for VLBI at the Highest Angular Resolutions . 7 Microarcsecond Structure of the Parsec Scale Jet of the Quasar 3C454.3 . 7 Jets from Water-Disk-Megamaser Galaxies . 8 Unlocking the secrets of PKS 1502+106. Synergies between mm-VLBI and single-dish monitoring . -
Aperture Synthesis James Di Francesco National Research Council of Canada North American ALMA Regional Center – Victoria
A Crash Course in ! Radio Astronomy and Interferometry:! 2. Aperture Synthesis James Di Francesco National Research Council of Canada North American ALMA Regional Center – Victoria (thanks to S. Dougherty, C. Chandler, D. Wilner & C. Brogan) Aperture Synthesis Output of a Filled Aperture • Signals at each point in the aperture are brought together in phase at the antenna output (the focus) • Imagine the aperture to be subdivided into N smaller elementary areas; the voltage, V(t), at the output is the sum of the contributions ΔVi(t) from the N individual aperture elements: V(t) = ∑ΔVi (t) € Aperture Synthesis Aperture Synthesis: Basic Concept • The radio power measured by a receiver attached to the telescope is proportional to a running time average of the square of the output voltage: 2 P V V V ∝ (∑Δ i ) = ∑∑ (Δ iΔ k ) 2 = ∑ ΔVi + ∑∑ ΔViΔVk i≠k • Any€ measurement with the large filled-aperture telescope can be written as a sum, in which each term depends on contributions from only two of the N aperture€ elements • Each term 〈ΔViΔVk〉 can be measured with two small antennas, if we place them at locations i and k and measure the average product of their output voltages with a correlation (multiplying) receiver Aperture Synthesis Aperture Synthesis: Basic Concept • If the source emission is unchanging, there is no need to measure all the pairs at one time • One could imagine sequentially combining pairs of signals. For N sub-apertures there will be N(N-1)/2 pairs to combine • Adding together all the terms effectively “synthesizes” one measurement -
H I Observations of Two New Dwarf Galaxies: Pisces a and B with the SKA Pathfinder KAT-7? C
A&A 587, L3 (2016) Astronomy DOI: 10.1051/0004-6361/201527910 & c ESO 2016 Astrophysics Letter to the Editor H I observations of two new dwarf galaxies: Pisces A and B with the SKA Pathfinder KAT-7? C. Carignan1;2, Y. Libert1, D. M. Lucero1;4, T. H. Randriamampandry1, T. H. Jarrett1, T. A. Oosterloo3;4, and E. J. Tollerud5 1 Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa e-mail: [email protected] 2 Observatoire d’Astrophysique de l’Université de Ouagadougou, BP 7021, Ouagadougou 03, Burkina Faso 3 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands 4 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands 5 Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA Received 7 December 2015 / Accepted 3 January 2016 ABSTRACT Context. Pisces A and Pisces B are the only two galaxies found via optical imaging and spectroscopy out of 22 Hi clouds identified in the GALFAHI survey as dwarf galaxy candidates. Aims. We derive the Hi content and kinematics of Pisces A and B. Methods. Our aperture synthesis Hi observations used the seven-dish Karoo Array Telescope (KAT-7), which is a pathfinder instru- ment for MeerKAT, the South African precursor to the mid-frequency Square Kilometre Array (SKA-MID). Results. The low rotation velocities of ∼5 km s−1 and ∼10 km s−1 in Pisces A and B, respectively, and their Hi content show that they are really dwarf irregular galaxies (dIrr). -
First Results from the Event Horizon Telescope
First results from the Event Horizon Telescope Dom Pesce On behalf of the Event Horizon Telescope collaboration March 10, 2020 EDSU conference The goal (ca. 2017) The goal is to take a picture of a black hole The goal (ca. 2017) Subrahmanyan Chandrasekhar The goal is to take a picture of a black hole • General relativity makes a prediction for the apparent shape of a black hole “It is conceptually interesting, if not astrophysically very important, to calculate the precise apparent shape of the black hole… Unfortunately, there seems to be no hope of observing this effect.” - James Bardeen, 1973 James Bardeen Photon ring and black hole shadow The warped spacetime around a black hole causes photon trajectories to bend event horizon b photon orbit Photon ring and black hole shadow The warped spacetime around a black hole causes photon trajectories to bend The closer these trajectories get to a critical impact parameter, the more tightly wound they become Photon ring and black hole shadow The warped spacetime around a black hole causes photon trajectories to bend The closer these trajectories get to a critical impact parameter, the more tightly wound they become Photon ring and black hole shadow The warped spacetime around a black hole causes photon trajectories to bend The closer these trajectories get to a critical impact parameter, the more tightly wound they become The trajectories interior to this critical impact parameter intersect the horizon, and these collectively form the black hole “shadow” (Falcke, Melia, & Agol 2000) while the bright surrounding region constitutes the “photon ring” Adapted from: Asada et al. -
Understanding the Bizarre Shapes of Radio Supernova Remnants
Barrels, jets and smoke-rings: Understanding the bizarre shapes of radio supernova remnants Bryan Malcolm Gaensler A thesis submitted for the degree of Doctor of Philosophy at the University of Sydney February 1999 To Dr Michael Bishop, For showing me where to start 1 Abstract This thesis considers the various morphologies of radio supernova remnants (SNRs), and attempts to determine whether their appearance results from the properties of the progenitor star and its supernova explosion, or from the structure of the inter- stellar medium (ISM) and ambient magnetic field into which a SNR consequently expands. High-resolution observations of Supernova 1987A show a young remnant whose appearance and evolution are completely dominated by the structure of its progenitor wind. A statistical study of the Galactic population of bilateral SNRs demonstrates that the symmetry axes of these remnants run parallel to the Galac- tic Plane. This result can be explained by the interaction of main sequence stellar wind-bubbles with the ambient magnetic field; expansion of SNRs into the resulting elongated cavities results in a bilateral appearance with the observed alignment. Radio observations of SNR G296.8{00.3 show a double-ringed morphology which is best explained by expansion either into an anisotropic main-sequence progenitor wind or into multiple cavities in the ISM. Data on SNRs G309.2{00.6 and G320.4{ 01.2 (MSH 15{52) make a strong case that the appearance of both remnants is significantly affected by collimated outflows from a central source; for G309.2{00.6 the source itself is not detected, but for G320.4{01.2 there is now compelling evi- dence that the remnant is associated with and is interacting with the young pulsar PSR B1509{58. -
RADIO STARS and THEIR LIVES in the GALAXY Lynn D
Accepted to PASP A Preprint typeset using LTEX style emulateapj v. 12/16/11 RADIO STARS AND THEIR LIVES IN THE GALAXY Lynn D. Matthews1 Accepted to PASP ABSTRACT This paper summarizes the three-day international workshop Radio Stars and Their Lives in the Galaxy, held at the Massachusetts Institute of Technology Haystack Observatory on 2012 October 3-5. The workshop was organized to provide a forum for the presentation and discussion of advances in stellar and solar astrophysics recently (or soon to be) enabled by the latest generation of state-of-the- art observational facilities operating from meter to submillimeter wavelengths. The meeting brought together both observers and theorists to discuss how radio wavelength observations are providing new and unique insights into the workings of stars and their role in the Galactic ecosystem. Topics covered included radio emission from hot and cool stars (from the pre- to post-main-sequence), the Sun as a radio star, circumstellar chemistry, planetary nebulae, white dwarf binaries and novae, supernova progenitors, and radio stars as probes of the Galaxy. Subject headings: meeting summary, Stars — stars: AGB and post-AGB – stars: winds, outflows – circumstellar matter – radio lines: stars 1. BACKGROUND AND MOTIVATION FOR THE precision astrometry, and the routine study of sources at WORKSHOP a level of a few tens of µJy. We also heard how develop- Radio emission has now been detected from stars ments in theory, modeling, and laboratory astrophysics across the entire Hertzsprung-Russell (H-R) diagram, are improving our ability to interpret results. This paper spanning virtually every stage of stellar evolution. -
D.A. Frail CV Page 1 CURRICULUM VITAE DALE ANDREW FRAIL
CURRICULUM VITAE DALE ANDREW FRAIL National Radio Astronomy Observatory Socorro, NM 87801 (575) 835-7338 [email protected] Education: 1989 – Ph.D. in Astronomy, University of Toronto 1985 – M.Sc. in Astronomy, University of Toronto Current Position: NRAO Astronomer (tenured) Research Interests: - electromagnetic counterparts of gravitational waves - the origin of gamma ray bursts and soft gamma ray repeaters - time-domain astronomy with an emphasis on the dynamic radio sky - pulsars, supernova remnant associations and pulsar wind nebulae - the 1720 MHz OH maser line toward supernova remnants - HI absorption and interstellar scattering Professional Experience: 1999-Present: Astronomer, NRAO 2019-2020: Interim Assistant Director, Science Support and ResearcH (12 mo) 2016 Visiting Associate in Astronomy, Caltech 2011-2015: Assistant Director, New MeXico Operations, VLA and VLBA 2011: Visiting Scientist, Harvard Smithsonian Center for AstropHysics (CfA) 2010: Visiting Scientist, Weizmann Institute of Science 2006-2009: Assistant Director, Science and Academic Affairs, NRAO 2001-2002: Visiting Associate in Astronomy, CaltecH 1995-1999: Associate Astronomer, NRAO 1993-1995: Assistant Astronomer, NRAO 1990–1993: Jansky Fellow, NRAO 1989-1991: NSERC Postdoctoral Fellow Professional and NRAO Service (since 2010): 2020 TIFR-NCRA Visiting Committee (February 2020) Reviewer for the MeerKAT Large Science Proposal reports 2019 Red Team for Fermi NASA Senior Review Proposal review for GMRT, MeerKAT, German-Israel Foundation Referee for ApJ, PASP Astronomer Performance Review Committee (APRC; ad hoc) Member of Jansky Postdoc Selection Committee (last year) 2018 Chandra User’s Committee (CUC; ends Oct. 2018) Promotion Cases (Michigan, CaltecH, TIFR/NCRA) Referee for MNRAS, A&A, ApJ & Nature External eXaminer for K. AleXander PHD at Harvard D.A.