Curriculum Vitae Kazunori (Kazu) Akiyama Contact Information
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Constraints on Black-Hole Charges with the 2017 EHT Observations of M87*
PHYSICAL REVIEW D 103, 104047 (2021) Constraints on black-hole charges with the 2017 EHT observations of M87* – Prashant Kocherlakota ,1 Luciano Rezzolla,1 3 Heino Falcke,4 Christian M. Fromm,5,6,1 Michael Kramer,7 Yosuke Mizuno,8,9 Antonios Nathanail,9,10 H´ector Olivares,4 Ziri Younsi,11,9 Kazunori Akiyama,12,13,5 Antxon Alberdi,14 Walter Alef,7 Juan Carlos Algaba,15 Richard Anantua,5,6,16 Keiichi Asada,17 Rebecca Azulay,18,19,7 Anne-Kathrin Baczko,7 David Ball,20 Mislav Baloković,5,6 John Barrett,12 Bradford A. Benson,21,22 Dan Bintley,23 Lindy Blackburn,5,6 Raymond Blundell,6 Wilfred Boland,24 Katherine L. Bouman,5,6,25 Geoffrey C. Bower,26 Hope Boyce,27,28 – Michael Bremer,29 Christiaan D. Brinkerink,4 Roger Brissenden,5,6 Silke Britzen,7 Avery E. Broderick,30 32 Dominique Broguiere,29 Thomas Bronzwaer,4 Do-Young Byun,33,34 John E. Carlstrom,35,22,36,37 Andrew Chael,38,39 Chi-kwan Chan,20,40 Shami Chatterjee,41 Koushik Chatterjee,42 Ming-Tang Chen,26 Yongjun Chen (陈永军),43,44 Paul M. Chesler,5 Ilje Cho,33,34 Pierre Christian,45 John E. Conway,46 James M. Cordes,41 Thomas M. Crawford,22,35 Geoffrey B. Crew,12 Alejandro Cruz-Osorio,9 Yuzhu Cui,47,48 Jordy Davelaar,49,16,4 Mariafelicia De Laurentis,50,9,51 – Roger Deane,52 54 Jessica Dempsey,23 Gregory Desvignes,55 Sheperd S. Doeleman,5,6 Ralph P. Eatough,56,7 Joseph Farah,6,5,57 Vincent L. -
16Th HEAD Meeting Session Table of Contents
16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113 -
THOMAS M. CRAWFORD University of Chicago
Department of Astronomy and Astrophysics ERC 433 5640 South Ellis Avenue Chicago, IL 60637 Office: 773.702.1564, Home: 773.580.7491 THOMAS M. CRAWFORD [email protected] University of Chicago DEGREES PhD University of Chicago. Astronomy & Astrophysics. 2003. MS University of Chicago. Astronomy & Astrophysics. 1997. BS DePaul University. Physics. 1996. BA Columbia University. German Language & Literature. 1992. DISSERTATION Title: Mapping the Southern Polar Cap with a Balloon-borne Millimeter-wave Telescope. Advisor: Stephan Meyer. HONORS Breakthrough Prize Winner. 2020. National Academy of Sciences Kavli Fellow. 2014. NASA Center of Excellence Award. 2002. NASA Graduate Student Research Fellowship. 1999–2002. B.S. conferred With Highest Honors. B.A. conferred Magna Cum Laude. ACADEMIC POSITIONS University of Chicago: Research Professor, Department of Astronomy & Astrophysics. 2019–Present. University of Chicago: Senior Researcher, Kavli Institute for Cosmological Physics. 2009–Present. University of Chicago: Research Associate Professor, Department of Astronomy & Astrophysics. 2017–2019. University of Chicago: Senior Research Associate, Department of Astronomy & Astrophysics. 2009–2017. University of Chicago: Research Scientist, Department of Astronomy & Astrophysics. 2006–2009. University of Chicago: Associate Fellow, Kavli Institute for Cosmological Physics. 2003–2009. University of Chicago: Research Associate, Department of Astronomy & Astrophysics. 2003–2006. Thomas M. Crawford, page 2 of 11 RECENT SYNERGISTIC ACTIVITIES Chair, Simons Observatory operations review committee, October 2020 Member, CMB-S4 Collaboration Governing Board, 2018 – present Member, NASA Legacy Archive for Microwave Background Data Analysis (LAMBDA) Users’ Group, 2016 – present Referee, Physical Review D, Physical Review Letters, Astrophysical Journal, Nature, Journal of Cosmology and Astroparticle Physics, and others, 2008 – present DOE, NASA, and NSF review panel member, 2013 – present RECENT INVITED COLLOQUIA AND SEMINARS University of Chicago: Astronomy Colloquium. -
Very Long Baseline Interferometry Imaging of the Advancing Ejecta in the first Gamma-Ray Nova V407 Cygni? M
A&A 638, A130 (2020) Astronomy https://doi.org/10.1051/0004-6361/202038142 & c ESO 2020 Astrophysics Very long baseline interferometry imaging of the advancing ejecta in the first gamma-ray nova V407 Cygni? M. Giroletti1, U. Munari2, E. Körding3, A. Mioduszewski4, J. Sokoloski5,6, C. C. Cheung7, S. Corbel8,9, F. Schinzel10;??, K. Sokolovsky11,12,13 , and T. J. O’Brien14 1 INAF Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 INAF Astronomical Observatory of Padova, 36012 Asiago (VI), Italy 3 Department of Astrophysics/IMAPP, Radboud University Nijmegen, 6500 GL Nijmegen, The Netherlands 4 National Radio Astronomy Observatory, Array Operations Center, 1003 Lopezville Road, Socorro, NM 87801, USA 5 Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA 6 LSST Corproation, 933 North Cherry Avenue, Tucson, AZ 85721, USA 7 Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA 8 Laboratoire AIM (CEA/IRFU – CNRS/INSU – Université Paris Diderot), CEA DSM/IRFU/SAp, 91191 Gif-sur-Yvette, France 9 Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU, USR 704 – Univ. Orléans, OSUC, 18330 Nançay, France 10 National Radio Astronomy Observatory, PO Box O, Socorro, NM 87801, USA 11 Department of Physics and Astronomy, Michigan State University, 567 Wilson Rd, East Lansing, MI 48824, USA 12 Astro Space Center, Lebedev Physical Inst. RAS, Profsoyuznaya 84/32, 117997 Moscow, Russia 13 Sternberg Astronomical Institute, Moscow University, Universitetsky 13, 119991 Moscow, Russia 14 Jodrell Bank Centre for Astrophysics, Alan Turing Building, University of Manchester, Manchester M13 9PL, UK Received 10 April 2020 / Accepted 11 May 2020 ABSTRACT Context. -
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. -
The Giant Flares of the Microquasar Cygnus X-3: X-Raysstates and Jets
galaxies Article The Giant Flares of the Microquasar Cygnus X-3: X-RaysStates and Jets Sergei Trushkin 1,2,*,† ID , Michael McCollough 3,†, Nikolaj Nizhelskij 1,† and Peter Tsybulev 1,† 1 The Special Astrophysical Observatory of the Russian Academy of Sciences, Niznij Arkhyz 369167, Russia; [email protected] (N.N.); [email protected] (P.T.) 2 Institute of Physics, Kazan Federal University, Kazan 420008, Russia 3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] * Correspondence: [email protected] or [email protected]; Tel.: +7-928-396-3178 † These authors contributed equally to this work. Received: 18 September 2017; Accepted: 21 November 2017; Published: 27 November 2017 Abstract: We report on two giant radio flares of the X-ray binary microquasar Cyg X-3, consisting of a Wolf–Rayet star and probably a black hole. The first flare occurred on 13 September 2016, 2000 days after a previous giant flare in February 2011, as the RATAN-600 radio telescope daily monitoring showed. After 200 days on 1 April 2017, we detected a second giant flare. Both flares are characterized by the increase of the fluxes by almost 2000-times (from 5–10 to 17,000 mJy at 4–11 GHz) during 2–7 days, indicating relativistic bulk motions from the central region of the accretion disk around a black hole. The flaring light curves and spectral evolution of the synchrotron radiation indicate the formation of two relativistic collimated jets from the binaries. Both flares occurred when the source went from hypersoft X-ray states to soft ones, i.e. -
Separating Accretion and Mergers in the Cosmic Growth of Black Holes with X-Ray and Gravitational Wave Observations
Draft version May 4, 2020 Typeset using LATEX twocolumn style in AASTeX61 SEPARATING ACCRETION AND MERGERS IN THE COSMIC GROWTH OF BLACK HOLES WITH X-RAY AND GRAVITATIONAL WAVE OBSERVATIONS Fabio Pacucci1, 2 and Abraham Loeb1, 2 1Black Hole Initiative, Harvard University, Cambridge, MA 02138, USA 2Center for Astrophysics j Harvard & Smithsonian, Cambridge, MA 02138, USA ABSTRACT Black holes across a broad range of masses play a key role in the evolution of galaxies. The initial seeds of black holes formed at z ∼ 30 and grew over cosmic time by gas accretion and mergers. Using observational data for quasars and theoretical models for the hierarchical assembly of dark matter halos, we study the relative importance of gas accretion and mergers for black hole growth, as a function of redshift (0 < z < 10) and black hole mass 3 10 (10 M < M• < 10 M ). We find that (i) growth by accretion is dominant in a large fraction of the parameter 8 5 space, especially at M• > 10 M and z > 6; and (ii) growth by mergers is dominant at M• < 10 M and z > 5:5, 8 and at M• > 10 M and z < 2. As the growth channel has direct implications for the black hole spin (with gas accretion leading to higher spin values), we test our model against ∼ 20 robust spin measurements available thus far. As expected, the spin tends to decline toward the merger-dominated regime, thereby supporting our model. The next generation of X-ray and gravitational-wave observatories (e.g. Lynx, AXIS, Athena and LISA) will map out populations of black holes up to very high redshift (z ∼ 20), covering the parameter space investigated here in almost its entirety. -
Anchored in Shadows: Tying the Celestial Reference Frame Directly to Black Hole Event Horizons
URSI GASS 2020, Rome, Italy, 29 August - 5 September 2020 Anchored in Shadows: Tying the Celestial Reference Frame Directly to Black Hole Event Horizons T. M. Eubanks Space Initiatives Inc Palm Bay, Florida, USA [email protected] Abstract the micro arc second level, and showing that natural radio sources can exhibit brightness temperatures > 1013 K[5]. Both the radio International Celestial Reference Frame This work clearly needs to be continued and extended with (ICRF) and the optical Gaia Celestial Reference Frame larger space radio telescopes at even higher frequencies. (Gaia-CRF2) are derived from observations of jets pro- Further impetus to a new space VLBI mission has been re- duced by the Super Massive Black Holes (SMBH) power- cently provided by the successful imaging of the shadow of ing active galactic nuclei and quasars. These jets are inher- M87 by Event Horizon Telescope (EHT) [6]. ently subject to change and will appear different at differ- ent observing frequencies, leading to instabilities and sys- The EHT is pushing the limits of what is possible with tematic errors in the resulting Celestial Reference Frames purely terrestrial VLBI, due to the limitations caused at- (CRFs). Recently, the Event Horizon Telescope (EHT), a mospheric absorption in the mm and sub-mm bands, which mm-wave Very Long Baseline Interferometry (VLBI) array, limits both the frequencies used and which limits the EHT has observed the 40 μas diameter shadow of the SMBH in to using mostly very dry and high-altitude sites, limiting M87 at 1.3 mm, showing that the emitting region is smaller the (u,v) plane imaging coverage. -
A Conceptual Overview of Single-Dish Absolute Amplitude Calibration
Event Horizon Telescope Memo Series EHT Memo 2017-CE-02 Calibration & Error Analysis WG A conceptual overview of single-dish absolute amplitude calibration S. Issaoun1, T. W. Folkers2, L. Blackburn3, D. P. Marrone2, T. Krichbaum4, M. Janssen1, I. Mart´ı-Vidal5 and H. Falcke1 Sept 15, 2017 – Version 1.0 1Department of Astrophysics/IMAPP, Radboud University Nijmegen, 6500 GL Nijmegen, the Netherlands 2Arizona Radio Observatory, Steward Observatory, University of Arizona, AZ 85721 Tucson, USA 3Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4Max Planck Institut f¨urRadioastronomie (MPIfR), Auf dem H¨ugel 69, 53121 Bonn, Germany 5Onsala Space Observatory, Chalmers University of Technology, Observatoriev¨agen 90, 43992 Onsala, Sweden Abstract This document presents an outline of common single-dish calibration techniques and key differences be- tween centimeter-wave and millimeter-wave observatories in naming schemes and measured quantities. It serves as a conceptual overview of the complete single-dish amplitude calibration procedure for the Event Horizon Telescope, using the Submillimeter Telescope (SMT) as the model station. Note: This document is not meant to be used as a general telescope guide or manual from an engineering perspective. It contains a number of common approximations used at observatories as an attempt to reason through the methods used and the specific calibration information needed to calibrate VLBI amplitudes from Event Horizon Telescope observing runs. This document can be used in conjunction with similar calibration outlines from other stations for procedural comparisons. Contents 1 Introduction to standard single-dish Tsys calibration techniques 4 1.1 The antenna-based system-equivalent flux densities (SEFDs) . -
Seeing Black Holes: from the Computer to the Telescope
universe Review Seeing Black Holes: From the Computer to the Telescope Jean-Pierre Luminet 1,2,3 1 Aix Marseille University, CNRS, LAM, 13013 Marseille, France; [email protected] or [email protected] 2 Aix Marseille University, CNRS, CPT, 13009 Marseille, France 3 Observatoire de Paris, CNRS, LUTH, 92195 Meudon, France Received: 7 July 2018; Accepted: 6 August 2018; Published: 9 August 2018 Abstract: Astronomical observations are about to deliver the very first telescopic image of the massive black hole lurking at the Galactic Center. The mass of data collected in one night by the Event Horizon Telescope network, exceeding everything that has ever been done in any scientific field, should provide a recomposed image in 2018. All this, forty years after the first numerical simulations performed by the present author. Keywords: black hole; numerical simulation; observation; general relativity 1. Introduction According to the laws of general relativity (for recent overviews at the turn of its centennial, see, e.g., [1,2]), black holes are, by definition, invisible. Contrary to uncollapsed stars, their surface is neither a solid nor a gas; it is an intangible frontier known as the event horizon. Beyond this horizon, gravity is so strong that nothing escapes, not even light. Seen projected onto the background of the sky, the event horizon would probably resemble a perfectly black disk if the black hole is static (Schwarzschild black hole) or a slightly flattened disk if it is rotating (Kerr black hole). A black hole however, be it small and of stellar mass or giant and supermassive, is rarely “bare”; in typical astrophysical conditions it is usually surrounded by gaseous matter. -
Press Kit Draft(1)
B L A C K H O L E S -------------- T H E E D G E O F A L L W E K N O W A film by Peter Galison Contact: Director/Producer: Peter Galison, [email protected] Editor/Co-Producer: Chyld King, [email protected] Distribution: Submarine Entertainment, [email protected] Media: [email protected] Online: www.blackholefilm.com Runtime: 98 min www.blackholefilm.com 1 About the Film Logline Black holes stand at the edge of the knowable universe. The Event Horizon Telescope pursues the first picture of a black hole; Stephen Hawking and collaborators attack the black hole paradox at the heart of physics. Black Holes | The Edge of All We Know follows observers, theorists, and philosophers hunting these most mysterious objects. Synopsis What can black holes teach us about the boundaries of knowledge? These holes in spacetime are the darkest objects and the brightest—the simplest and the most complex. With unprecedented access, Black Holes | The Edge of All We Know follows two powerhouse collaborations. Stephen Hawking anchors one, striving to show that black holes do not annihilate the past. Another group, working in the world’s highest altitude observatories, creates an earth-sized telescope to capture the first-ever image of a black hole. Interwoven with other dimensions of exploring black holes, these stories bring us to the pinnacle of humanity’s quest to understand the universe. www.blackholefilm.com 2 www.blackholefilm.com 3 Director’s Statement I began filming Black Holes | The Edge of All We Know in the spring of 2016, when five colleagues and I launched the Black Hole Initiative, an interdisciplinary center for the study of black holes. -
The European Vlbi Network: a Sensitive and State-Of- The-Art Instrument for High-Resolution Science
THE EUROPEAN VLBI NETWORK: A SENSITIVE AND STATE-OF- THE-ART INSTRUMENT FOR HIGH-RESOLUTION SCIENCE P. CHARLOT Observatoire de Bordeaux (OASU) – CNRS/UMR 5804 BP 89, 33270 Floirac, France e-mail: [email protected] ABSTRACT. The European VLBI Network (EVN) is an array of 18 radio telescopes located throughout Europe and beyond that carry out synchronized very-long-baseline-interferometric (VLBI) observations of radio-emitting sources. The data are processed at a central facility located at the Joint Institute for VLBI in Europe (JIVE) in the Netherlands. The EVN is freely open to any scientist in the world based on peer-reviewed proposals. This paper outlines the current capabilities of the EVN and procedures for observing, highlights some recent results that have been obtained, and puts emphasis on the future development of the array. 1. INTRODUCTION The European VLBI Network (EVN)1 was formed in 1980 by a consortium of five of the major radio astronomy institutes in Europe (the European Consortium for VLBI). Since then, the EVN and the Consortium has grown to include 12 institutes in Spain, UK, the Netherlands, Germany, Sweden, Italy, Finland, Poland and China (Table 1). In addition, the Hartebeesthoek Radio Astronomy Observatory in South Africa and the Arecibo Observatory in Puerto Rico are active Associate Members of the EVN. The EVN members operate 18 individual antennae, which include some of the world’s largest and most sensitive telescopes (Fig. 1). Together, these telescopes form a large scale facility, a continent-wide radio interferometer with baselines ranging from 200 km to 9000 km.