DOCSLIB.ORG

The Very-High-Energy Gamma-Ray Sky and the CTA Observatory

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Very-High-Energy Gamma-Ray Sky and the CTA Observatory The very-high-energy gamma-ray sky and the CTA Observatory Jürgen Knödlseder (IRAP, Toulouse) Directeur de Recherche (CNRS) The menu Light starter I. Why we do gamma-ray astronomy Assortment of AppeMzers II. What have we learned so far Main Dish III. What comes next Desert IV. Concluding remarks First course I. Why we do gamma-ray astronomy A historical introducMon The discovery of cosmic rays 1910 1920 1930 1940 1950 1960 Viktor Franz Hess (1912) 1970 1980 1990 2000 2010 The nature of cosmic rays 1910 Charged 1920 parMcles! Gamma 1930 rays! 1940 1950 1960 1970 1980 1990 Robert Millikan and Arthur Holly Compton (1931) A hot debate (1932) 2000 2010 Cosmic charged parMcles ! 1910 1920 1930 1940 MS ChrisMan Huygens 1950 Clay and Berlage (1932) 1960 1970 Geiger counter 1980 4 cm gold bar 1990 Geiger counter 2000 Bothe and Kohlhörster (1929) 2010 Cosmic stac 1910 1920 1930 1940 1950 1960 1970 1980 1990 2000 Karl Jansky (1933) 2010 An ambiMous amateur 1910 1920 1930 1940 1950 1960 1970 1980 1990 2000 Grote Reber (1944) 2010 … and the first radio sky map 1910 1920 Cas A 1930 Cygnus X 1940 1950 1960 1970 1980 Galactic centre 1990 2000 2010 Synchrotron radiaon 1910 1920 1930 1940 1950 1960 Langmuir,Elder,Gurevitsch, 1970 Charleton et Pollock (1948) 1980 1990 2000 Discovery of synchrotron radiaon (1947) 2010 Consequences 1910 Cosmic-ray parMcles emit gamma rays! 1920 1930 Hayakawa (1952) 1940 Hutchinson (1952) 1950 1960 Feenberg and Primakoff (1948) 1970 1980 Curvature Radiation 1990 2000 2010 Radhakrishnan and Cooke (1969) Philip Morrison (1958) The dawn of gamma-ray astronomy 1910 or how to observe photons of the highest energies? 1920 1930 1940 Atmosphere barrier Flux barrier 1950 1960 1970 1980 1 photon per cm2/keV per year ! 1990 1 photon per cm2/keV per century ! 2000 2010 Going into space 1910 or how to overcome the atmosphere barrier 1920 1930 1940 1950 Explorer XI (1962) OSO 3 (1967) 1960 Comparison of effecMve 1970 detecMon area (to scale) 1980 COS-B (1975) 1990 EGRET (1991) 2000 2010 Fermi (2008) Observing from ground 1910 or how to overcome the flux barrier (and turn the atmosphere into a detector) 1920 1930 1940 1950 1960 1970 1980 1990 2000 2010 Observing from ground 1910 The Cherenkov technique in a nutshell 1920 1930 1940 1950 1960 1970 1980 1990 2000 2010 Observing from ground 1910 The stereo Cherenkov technique in a nutshell 1920 1930 1940 1950 1960 1970 1980 1990 2000 2010 Observing from ground 1910 1920 1930 1940 1950 1960 1970 1980 1990 2000 Galbraith & Jelley (1953) 2010 Observing from ground 1910 1920 1930 1940 1950 Crimée (1960-1963) Photographie d’une gerbe (1961) 1960 1970 1980 1990 2000 2010 Irlande (1963-1967) Whipple (1968-1990) Observing from ground 1910 1920 1930 1940 1950 1960 HESS (2004-) 1970 1980 1990 2000 2010 MAGIC (2004-) VERITAS (2007-) Observing from ground 1910 1920 1930 1940 1950 MILAGRO (2004-2008) 1960 1970 1980 1990 2000 HAWC (2014-) 2010 Second course II. What have we learned so far In the VHE domain (ground-based gamma-ray astronomy) with a strong focus on GalacMc science A hundred of gamma-ray sources The source zoo SNRs Binaries Starbursts AGN Pulsars/PWN Jets Shocks Shocks Jets Accreon Diffusion Diffusion Cosmic Winds rays GRBs Dark Jets matter Shocks Intergalactic VHE gamma rays probe medium ParMcle acceleraon and propagaon Cosmic rays Highest energy processes in a large variety of objects IntergalacMc medium Dark maer and fundamental physics Significance, in full detail full in Significance, Significance GalacMc populaons H.E.S.S. GalacMc Plane Survey Deil, Chaves+ (H.E.S.S.) 15 VHE source distribution GalacMc populaons GalacMc latude profile of H.E.S.S. GalacMc Plane Survey sources GalacticGalacMc populaons TeV source populations The cosmic-ray spectrum or the quest for the GalacMc PeVatron ParMcle acceleraon at shocks or the Fermi mechanism ParMcles gain energy by crossing and recrossing the shock The Hillas criterion or what systems can accelerate parMcles Systems below the lines are excluded Supernova remnants as parMcle R. D. Blandford et al. / Nuclearaccelerators Physics B Proceedings Supplement 00 (2014) 1–14 3 Figure 3: Chandra X-ray 4.0 6.0 keV image of the Tycho supernova remnant, showing detailed non-thermal emitting features manifesting the Non-thermal X-ray emission is a clear sign for electron acceleraon to − shock fronts (from [16]). ~ 100 TeV (synchrotron emission of electrons in amplified B fields) are not obviously seen in any other spectral band (eg. [32, 33] and [34] for a review). Figure 5 shows the light curve of the biggest flare in April 2011. The flux doubled within td . 8 hours at the rising edges. The spectral energy distribution for a few flares taken near the peak flux level is shown in Figure 6. The emission process is most likely to be synchrotron, requiring elec- trons/positrons of energy 3 PeV in a 1 mG mag- ⇠ ⇠ netic field. A peak of 400 MeV indicates very effi- ⇠ cient acceleration that goes beyond the classical radia- tion reaction limit in an MHD setting. These flares are not accompanied by changes in the pulsar timing and so presumably originate in the nebula which is many Figure 4: Gamma-ray spectrum of W44 as measured with the Fermi light years in size. The isotropic energy radiated in the LAT, which shows good agreement with pion-decay gamma-ray pro- strongest flare was 1034 J which is equivalent to the ⇠ duction model (from [17]). energy contained within a region about a hundred, not ten, light hours across. Either there is strong relativis- 1.3. Crab Nebula tic beaming or some way must be found to concentrate energy within a small volume (or both). The Crab Nebula has long been our best high energy astrophysics laboratory and many common e↵ects have 1.4. Relativistic Jets first been identified there. It is not disappointing us. Re- cent discoveries include 400 GeV pulsation [28, 29], Fermi and the ACTs have also made dramatic ob- ⇠ rapid secular variation in the total nebular flux [30] and servations of relativistic jets from AGN, GRB and bi- rapid variation of the “inner knot” which may mark the nary sources. Blazars (AGN directed towards us) ex- termination of the wind in the inner nebula [31]. How- hibit variability on timescales that can be as short as few ever the most striking discovery, which may presage a minutes (e.g., [35, 36]). However, we can place a lower new kind of particle acceleration with clear relevance to bound on the radius of emission because the gamma cosmic ray origin, is the discovery of dramatic, 10 hr rays have to avoid pair production as they escape the ⇠ γ-ray flares which are localized around 400 MeV and near infrared photons. The far more luminous quasars, Hadronic and leptonic emission the pion bump as a disMncMve feature Eγ ~ 0.1 Ep R. D. Blandford et al. / Nuclear Physics B Proceedings Supplement 00 (2014) 1–14 3 Figure 3: Chandra X-ray 4.0 6.0 keV image of the Tycho supernova remnant, showing detailed non-thermal emitting features manifesting the − shockIndicaons for a pion bump fronts (from [16]). but not a GalacMc PeVatron are not obviously seen in any other spectral band (eg. [32, 33] and [34] for a review). Figure 5 shows the light curve of the biggest flare in April 2011. The flux doubled within td . 8 hours at the rising edges. The spectral energy distribution for a few flares taken near the peak flux level is shown in Figure 6. The emission process is most likely to be synchrotron, requiring elec- trons/positrons of energy 3 PeV in a 1 mG mag- ⇠ ⇠ netic field. A peak of 400 MeV indicates very effi- ⇠ cient acceleration that goes beyond the classical radia- tion reaction limit in an MHD setting. These flares are not accompanied by changes in the pulsar timing and so presumably originate in the nebula which is many Figure 4: Gamma-ray spectrum of W44 as measured with the Fermi light years in size. The isotropic energy radiated in the LAT, which shows good agreement with pion-decay gamma-ray pro- strongest flare was 1034 J which is equivalent to the ⇠ duction model (from [17]). energy contained within a region about a hundred, not ten, light hours across. Either there is strong relativis- 1.3. Crab Nebula tic beaming or some way must be found to concentrate energy within a small volume (or both). The Crab Nebula has long been our best high energy astrophysics laboratory and many common e↵ects have 1.4. Relativistic Jets first been identified there. It is not disappointing us. Re- cent discoveries include 400 GeV pulsation [28, 29], Fermi and the ACTs have also made dramatic ob- ⇠ rapid secular variation in the total nebular flux [30] and servations of relativistic jets from AGN, GRB and bi- rapid variation of the “inner knot” which may mark the nary sources. Blazars (AGN directed towards us) ex- termination of the wind in the inner nebula [31]. How- hibit variability on timescales that can be as short as few ever the most striking discovery, which may presage a minutes (e.g., [35, 36]). However, we can place a lower new kind of particle acceleration with clear relevance to bound on the radius of emission because the gamma cosmic ray origin, is the discovery of dramatic, 10 hr rays have to avoid pair production as they escape the ⇠ γ-ray flares which are localized around 400 MeV and near infrared photons. The far more luminous quasars, EvoluMon of the SNR accelerator HESSHESS Indicaons for a J1641-463: J1641-463: PeVatron HESS J1641-463 p-pleptonic model modelfits data doesn't better fit → well Emax (Klein-Nishina > 100 TeV (99% effect) CL) Assuming a PL for Kelner+06 parameterization primary electron spectrum RX J1713 for Assuming a PL withcomparison Γ = 2.1 Requires electron primary proton spectrum cutoff > 700 TeV (99% CL) to fit measured VHE One of the highest Emax every spectrum inferred from VHE data 4 Hundreds of TeV electrons measured luminosity (d = 11 kpc) 1 34 -1 ) suffer severe losses in L = 4 ¥ 10 erg s .
Load more

Recommended publications
  • CR-/3017S B ORBITING SOLAR OBSERVATORY FINAL REPORT
    4: it W::: 050-7 ~AS ACR-/3017s B ORBITING SOLAR OBSERVATORY FINAL REPORT N C) U2a ~ 0mU 4~~~~~~~~~~~~~~~~~~~~~~~~~~~~~-4' W 10 ~~~~~~ -7 Ol C",.1-a -9- ---- o ' ocl '.-l Q) o QU2i~WL4cO 1-a . ), 3xr N~~~~~~~~~~~~~~~. .~ tjir~ V I ed F7. 3 wUii rH1 _.1- ~~z,~~OULECORD r~ BALBOTESRSERHCRPRTO o~~~~~USDAY FBL OPRTO BOULDER, COLRAD I~ ~..... LDER-'COLOR.DO '-01 OSO-7 ORBITING SOLAR OBSERVATORY PROGRAM FINAL REPORT F72-01 December 31, 1972 PREPARED BY APPROVED BY OSO Program Staff J. O. Simpson Director, OSO Programs BALL BROTHERS RESEARCH CORPORATION SUBSIDIARY OF BALL CORPORATION BOULDER, COLORADO F72-01 PREFACE During the 1950's rapid progress was made in solar physics and in instrument and space hardware technology, using rocket and balloon flights that, although of brief duration, provided a view of the sun free from the obscuring atmosphere. The significance of data from these flights confirmed the often-asserted value of long-term observations from a spacecraft in advancing our knowledge of the sun's behavior. Thus, the first of NASA's space platforms designed for long-term observations of the universe from above the atmosphere was planned, and the Orbiting Solar Observatory program started in 1959. Solar physics data return began with the launch of OSO-1 in March of 1962. OSO-2 and OSO-3 were launched in 1965, OSO-4 and OS0-5 in 1967, OSO-6 in 1969, and the most recent, OSO-7/, was launched on September 29, 1971. All seven OSO's have been highly successful both in scientific data return and in per- formance of the engineering systems.
    [Show full text]
  • Information Summaries
    TIROS 8 12/21/63 Delta-22 TIROS-H (A-53) 17B S National Aeronautics and TIROS 9 1/22/65 Delta-28 TIROS-I (A-54) 17A S Space Administration TIROS Operational 2TIROS 10 7/1/65 Delta-32 OT-1 17B S John F. Kennedy Space Center 2ESSA 1 2/3/66 Delta-36 OT-3 (TOS) 17A S Information Summaries 2 2 ESSA 2 2/28/66 Delta-37 OT-2 (TOS) 17B S 2ESSA 3 10/2/66 2Delta-41 TOS-A 1SLC-2E S PMS 031 (KSC) OSO (Orbiting Solar Observatories) Lunar and Planetary 2ESSA 4 1/26/67 2Delta-45 TOS-B 1SLC-2E S June 1999 OSO 1 3/7/62 Delta-8 OSO-A (S-16) 17A S 2ESSA 5 4/20/67 2Delta-48 TOS-C 1SLC-2E S OSO 2 2/3/65 Delta-29 OSO-B2 (S-17) 17B S Mission Launch Launch Payload Launch 2ESSA 6 11/10/67 2Delta-54 TOS-D 1SLC-2E S OSO 8/25/65 Delta-33 OSO-C 17B U Name Date Vehicle Code Pad Results 2ESSA 7 8/16/68 2Delta-58 TOS-E 1SLC-2E S OSO 3 3/8/67 Delta-46 OSO-E1 17A S 2ESSA 8 12/15/68 2Delta-62 TOS-F 1SLC-2E S OSO 4 10/18/67 Delta-53 OSO-D 17B S PIONEER (Lunar) 2ESSA 9 2/26/69 2Delta-67 TOS-G 17B S OSO 5 1/22/69 Delta-64 OSO-F 17B S Pioneer 1 10/11/58 Thor-Able-1 –– 17A U Major NASA 2 1 OSO 6/PAC 8/9/69 Delta-72 OSO-G/PAC 17A S Pioneer 2 11/8/58 Thor-Able-2 –– 17A U IMPROVED TIROS OPERATIONAL 2 1 OSO 7/TETR 3 9/29/71 Delta-85 OSO-H/TETR-D 17A S Pioneer 3 12/6/58 Juno II AM-11 –– 5 U 3ITOS 1/OSCAR 5 1/23/70 2Delta-76 1TIROS-M/OSCAR 1SLC-2W S 2 OSO 8 6/21/75 Delta-112 OSO-1 17B S Pioneer 4 3/3/59 Juno II AM-14 –– 5 S 3NOAA 1 12/11/70 2Delta-81 ITOS-A 1SLC-2W S Launches Pioneer 11/26/59 Atlas-Able-1 –– 14 U 3ITOS 10/21/71 2Delta-86 ITOS-B 1SLC-2E U OGO (Orbiting Geophysical
    [Show full text]
  • OSO 20M Telescope Handbook
    OSO 20m Telescope Handbook Onsala Space Observatory August 31, 2016 The latest version of this handbook can be found here. Original version by Lars E.B. Johansson. Latest revisions by A.O.H.Olofsson and E. De Beck. Table of Contents Contents2 List of Figures5 List of Tables6 1 Introduction7 1 Quick system overview..........................7 2 Observing.................................8 3 Staff....................................9 4 Communication..............................9 2 Technical description 10 1 The telescope............................... 10 2 Receivers / frontends........................... 10 2.1 3 mm: 85 – 116 GHz........................ 11 2.2 4 mm: 67 – 87 GHz........................ 12 2.3 100 GHz receiver......................... 12 3 Spectrometers / backends........................ 14 4 Telescope and instrument control system................ 15 3 Spectral-line observations 16 1 Observing modes............................. 16 1.1 Beam switching.......................... 16 1.2 Position switching......................... 17 1.3 Frequency switching....................... 17 1.4 Mapping.............................. 17 2 Calibration................................ 18 3 Pointing strategy............................. 18 4 Velocity systems.............................. 18 5 Time estimates.............................. 19 6 Atmospheric transmission........................ 20 4 Data 22 1 Backups, retrieval and transfer...................... 22 2 File names................................. 22 2 OSO 20 m Telescope Handbook Table
    [Show full text]
  • Pokroky Kosmické Astronomie
    Pokroky matematiky, fyziky a astronomie Marcel Grün; Pavel Koubský Pokroky kosmické astronomie Pokroky matematiky, fyziky a astronomie, Vol. 15 (1970), No. 2, 62--76 Persistent URL: http://dml.cz/dmlcz/138230 Terms of use: © Jednota českých matematiků a fyziků, 1970 Institute of Mathematics of the Academy of Sciences of the Czech Republic provides access to digitized documents strictly for personal use. Each copy of any part of this document must contain these Terms of use. This paper has been digitized, optimized for electronic delivery and stamped with digital signature within the project DML-CZ: The Czech Digital Mathematics Library http://project.dml.cz POKROKY KOSMICKÉ ASTRONOMIE MARCEL GRÚN, PAVEL KOUBSKÝ, Praha Astronomická pozorování konaná ze zemského povrchu jsou znesnadňována přítomností atmosféry, která se chová jako filtr se specifickými vlastnostmi: 1. Je nepropustná pro většinu frekvencí elektromagnetických vln přicházejících z vesmíru (obr. I). 2. Omezuje rozlišovací schopnost v těch oborech, které propouští. Vzhledem k difrakci světla je teoretická rozlišovací schopnost přímoúměrná apertuře (průměru objektivu) a nepřímo- úměrná vlnové délce. To však platí pouze pro ideální podmínky, neboť turbulence atmosféry nedovoluje rozlišit ve viditelném oboru více než 0,1". Obvyklé pozorovací podmínky snižují tuto hodnotu nejméně o řád; třiceticentimetrový dalekohled ve vakuu je po stránce praktické rozlišo­ vací schopnosti ekvivalentní největším pozemským přístrojům. 3. Pozorování je rušeno existencí vlastního záření atmosféry a přítomností záření rozptýleného v atmosféře. Rozptýlené záření způsobuje, že dosah největších fotografických dalekohledů je nižší, než by odpovídalo optice a citlivosti detektorů. Záření atmosféry je překážkou též při spektrální analýze slabých objektů. Ve zprávě [1] se předpokládá, že třímetrový reflektor na oběž­ né dráze pointovaný s přesností 0,004" by byl schopen zachytit objekty do 29m, o 2 řády méně jasné než dosud ze Země.
    [Show full text]
  • Photographs Written Historical and Descriptive
    CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY HAER FL-8-B BUILDING AE HAER FL-8-B (John F. Kennedy Space Center, Hanger AE) Cape Canaveral Brevard County Florida PHOTOGRAPHS WRITTEN HISTORICAL AND DESCRIPTIVE DATA HISTORIC AMERICAN ENGINEERING RECORD SOUTHEAST REGIONAL OFFICE National Park Service U.S. Department of the Interior 100 Alabama St. NW Atlanta, GA 30303 HISTORIC AMERICAN ENGINEERING RECORD CAPE CANAVERAL AIR FORCE STATION, MISSILE ASSEMBLY BUILDING AE (Hangar AE) HAER NO. FL-8-B Location: Hangar Road, Cape Canaveral Air Force Station (CCAFS), Industrial Area, Brevard County, Florida. USGS Cape Canaveral, Florida, Quadrangle. Universal Transverse Mercator Coordinates: E 540610 N 3151547, Zone 17, NAD 1983. Date of Construction: 1959 Present Owner: National Aeronautics and Space Administration (NASA) Present Use: Home to NASA’s Launch Services Program (LSP) and the Launch Vehicle Data Center (LVDC). The LVDC allows engineers to monitor telemetry data during unmanned rocket launches. Significance: Missile Assembly Building AE, commonly called Hangar AE, is nationally significant as the telemetry station for NASA KSC’s unmanned Expendable Launch Vehicle (ELV) program. Since 1961, the building has been the principal facility for monitoring telemetry communications data during ELV launches and until 1995 it processed scientifically significant ELV satellite payloads. Still in operation, Hangar AE is essential to the continuing mission and success of NASA’s unmanned rocket launch program at KSC. It is eligible for listing on the National Register of Historic Places (NRHP) under Criterion A in the area of Space Exploration as Kennedy Space Center’s (KSC) original Mission Control Center for its program of unmanned launch missions and under Criterion C as a contributing resource in the CCAFS Industrial Area Historic District.
    [Show full text]
  • Observing Photons in Space
    —1— Observing photons in space For the truth of the conclusions of physical science, observation is the supreme court of appeals Sir Arthur Eddington Martin C.E. HuberI, Anuschka PauluhnI and J. Gethyn TimothyII Abstract This first chapter of the book ‘Observing Photons in Space’ serves to illustrate the rewards of observing photons in space, to state our aims, and to introduce the structure and the conventions used. The title of the book reflects the history of space astronomy: it started at the high-energy end of the electromagnetic spectrum, where the photon aspect of the radiation dominates. Nevertheless, both the wave and the photon aspects of this radiation will be considered extensively. In this first chapter we describe the arduous efforts that were needed before observations from pointed, stable platforms, lifted by rocket above the Earth’s atmosphere, became the matter of course they seem to be today. This exemplifies the direct link between technical effort — including proper design, construction, testing and calibration — and some of the early fundamental insights gained from space observations. We further report in some detail the pioneering work of the early space astronomers, who started with the study of γ- and X-rays as well as ultraviolet photons. We also show how efforts to observe from space platforms in the visible, infrared, sub-millimetre and microwave domains developed and led to today’s emphasis on observations at long wavelengths. The aims of this book This book conveys methods and techniques for observing photons1 in space. ‘Observing’ photons implies not only detecting them, but also determining their direction at arrival, their energy, their rate of arrival, and their polarisation.
    [Show full text]
  • Table of Artificial Satellites Launched Between 1 January and 31 December 1967
    This electronic version (PDF) was scanned by the International Telecommunication Union (ITU) Library & Archives Service from an original paper document in the ITU Library & Archives collections. La présente version électronique (PDF) a été numérisée par le Service de la bibliothèque et des archives de l'Union internationale des télécommunications (UIT) à partir d'un document papier original des collections de ce service. Esta versión electrónica (PDF) ha sido escaneada por el Servicio de Biblioteca y Archivos de la Unión Internacional de Telecomunicaciones (UIT) a partir de un documento impreso original de las colecciones del Servicio de Biblioteca y Archivos de la UIT. (ITU) ﻟﻼﺗﺼﺎﻻﺕ ﺍﻟﺪﻭﻟﻲ ﺍﻻﺗﺤﺎﺩ ﻓﻲ ﻭﺍﻟﻤﺤﻔﻮﻇﺎﺕ ﺍﻟﻤﻜﺘﺒﺔ ﻗﺴﻢ ﺃﺟﺮﺍﻩ ﺍﻟﻀﻮﺋﻲ ﺑﺎﻟﻤﺴﺢ ﺗﺼﻮﻳﺮ ﻧﺘﺎﺝ (PDF) ﺍﻹﻟﻜﺘﺮﻭﻧﻴﺔ ﺍﻟﻨﺴﺨﺔ ﻫﺬﻩ .ﻭﺍﻟﻤﺤﻔﻮﻇﺎﺕ ﺍﻟﻤﻜﺘﺒﺔ ﻗﺴﻢ ﻓﻲ ﺍﻟﻤﺘﻮﻓﺮﺓ ﺍﻟﻮﺛﺎﺋﻖ ﺿﻤﻦ ﺃﺻﻠﻴﺔ ﻭﺭﻗﻴﺔ ﻭﺛﻴﻘﺔ ﻣﻦ ﻧﻘﻼ ً◌ 此电子版（PDF版本）由国际电信联盟（ITU）图书馆和档案室利用存于该处的纸质文件扫描提供。 Настоящий электронный вариант (PDF) был подготовлен в библиотечно-архивной службе Международного союза электросвязи путем сканирования исходного документа в бумажной форме из библиотечно-архивной службы МСЭ. © International Telecommunication Union HIS list of artificial satellites launched in 1967 was prepared from information provided by TTelecommunication Administrations, the Com­ m ittee on Space Research (COSPAR), the Goddard Space Flight Center (GSFC), the United States National Aeronautics and Space Administration (NASA), the International Fre­ quency Registration Board (IFRB), one of the fo ur permanent organs o f the ITU, and from details published in the specialized press. For decayed satellites the data concerning the orbit parameters are those immediately after launching. For the others, still in orbit, the orbit parameters are those reported on 31 De­ cember 1967 by GSFC.
    [Show full text]
  • General Disclaimer One Or More of the Following Statements May Affect
    General Disclaimer One or more of the Following Statements may affect this Document This document has been reproduced from the best copy furnished by the organizational source. It is being released in the interest of making available as much information as possible. This document may contain data, which exceeds the sheet parameters. It was furnished in this condition by the organizational source and is the best copy available. This document may contain tone-on-tone or color graphs, charts and/or pictures, which have been reproduced in black and white. This document is paginated as submitted by the original source. Portions of this document are not fully legible due to the historical nature of some of the material. However, it is the best reproduction available from the original submission. Produced by the NASA Center for Aerospace Information (CASI) • X-523-09-506 r, t It r X-2 EFFECTS OF SPACECRAFT INTERFERENCE ON A 136 MHz PCM TFUMETRY DATA LINK RALPH E. TAYLOR THOMAS J. KARRAS S NOVEMBER 1969 f d FAQ,` ^ ,y^ l O ^ f --- GODDARD SPACE FLIGHT CENTER GREENBELT, MARYLAND N70- 1`1047 Mp • = IACCE^810 Nw^1 UMDERI1 0 ^j L at - J / J~ 'RACE 1 !CODE) UtASA CA OR TIKX Oft Au NUMBER) ICATL3 TI 6 X-523-69r-506 EFFECTS OF SPACECRAFT INTERFERENCE ON A 136 MHz PCM TELEMETRY DAT'k LINK R.Jph E. Taylor Thomas J. Karras Advanced Development Division Information Processing Division Tracking and Data Systems Directorate it November 1969 GODDARD SPACE FLIGHT CENTER Greenbelt, Maryland CONTENTS Page ABSTRACT . iii I. INTRODUCTION .
    [Show full text]
  • Design Studies for a Multi-Tev Γ-Ray Telescope Array : Pex (Pev Explorer)
    Design studies for a multi-TeV γ-ray telescope array : PeX (PeV eXplorer) Jarrad Denman B.Sc (Hons), Physics Submitted in total fulfilment of the requirements of the degree of Doctor of Philosophy arXiv:1408.0931v1 [astro-ph.IM] 5 Aug 2014 July 16, 2012 School of Chemistry & Physics The University of Adelaide ii Contents Contents iii Abstract vii Declaration of Originality ix Acknowledgements xi Public Display of Results xiii 1 TeV Gamma-Ray Astronomy and its Motivation 1 1.1 TeV γ-ray Production Mechanisms . 4 1.2 Established sources of relativistic particles . 6 1.3 Motivation for a Multi-TeV ( > 10 TeV) γ-ray detector . 13 1.3.1 Astrophysical Motivations . 13 1.3.2 Technical Motivations . 17 1.3.3 Proposed concept : TenTen / PeX . 20 2 Ground-Based Detection of Gamma-rays 23 2.1 Brief overview of γ-ray detectors . 23 2.2 Electromagnetic EAS . 25 2.3 Electromagnetic and Hadronic EAS comparisons . 28 2.4 Cherenkov Light Production . 29 2.5 Imaging Atmospheric Cherenkov Technique . 34 3 The PeV eXplorer (PeX) Five Telescope Cell: Standard Configuration 39 3.1 Monte Carlo EAS Simulations . 41 3.2 Night sky background (NSB) contributions . 42 3.3 Telescope and Camera Specifications . 45 3.4 Image Cleaning . 48 3.5 Image Parameter Reconstruction . 49 3.6 Event Direction Reconstruction . 51 3.7 Stereoscopic Image Shape Reconstruction . 58 iii 3.8 Angular and Core Resolution . 64 3.9 Energy Resolution . 66 3.10 Effective Area . 67 3.11 Flux Sensitivity . 68 4 Low Altitude PeX cell optimisation 73 4.1 Telescope Separation .
    [Show full text]
  • Business Name D/B/A Name #1A LIFESAFER of COLORADO LLC
    Business Name D/B/A Name #1A LIFESAFER OF COLORADO LLC 101 PARK AVENUE PARTNERS INC 1-800 CONTACTS INC 3 DAY BLINDS LLC 303 FURNITURE INC 303 TACTICAL LLC 303 TACTICAL 360 RAIL SERVICES LLC 3BB INC GREAT CLIPS 3D AUTOGLASS 3D STAINLESS LLC 3FORM LLC 3R Technology Solutions Inc 3SI SECURITY SYSTEMS INC 3T CULINARY INC THREE TOMATOES CATERING 4 FRONT ENGINEERED SOL INC 4283929 DELAWARE LLC ROCKY MTN PET CREMATION SERVICES 48FORTY SOLUTIONS LLC PALLET COMPANIES LLC 4imprint, Inc. 4LIFE RESEARCH CSA LLC 4LIFE RESEARCH USA LLC 50 IN 52 JOURNEY INC THE JOURNEY INSTITUTE 5071 INC 50-80 MASSAGE 5280 Contract Flooring 5280 HEATING COOLING & REFRIGERATION 5280 MAINTENANCE INC 5280 Stone Company, LLC 5280 Stone Company, LLC 5280 Telecom, LLC 5280 TOWING LLC 52Eighty Customs 5850 EAST 58TH AVENUE LLC 5850 EAST 58TH AVENUE LLC 6 ITALIAN WOLF SECURITY LLC 6171 LLC THE HIDEAWAY TAVERN 7-ELEVEN INC 7-ELEVEN STORE #38170 7-ELEVEN INC 7-ELEVEN STORE 37570 7-ELEVEN INC / JC INC 35828A 7-ELEVEN STORE 35828A 7-ELEVEN INC 23829 7-ELEVEN STORE 23829 7-ELEVEN INC 23829B 7-ELEVEN STORE 23829B 7-ELEVEN INC 34087 7-ELEVEN STORE 34087 7-ELEVEN INC 35828 7-ELEVEN STORE 35828 7-ELEVEN INC 35864 7-ELEVEN STORE 35864 7-ELEVEN INC 36013 7-ELEVEN STORE 36013 7-ELEVEN INC 36013 7-ELEVEN STORE 36013 7-ELEVEN INC 36464 7-ELEVEN STORE 36464 7-ELEVEN INC 36775 7-ELEVEN STORE 36775 7-ELEVEN INC 37291 7-ELEVEN STORE 37291 7-ELEVEN STORE 34087A 7-ELEVEN INC / S&As STORE INC 34087A 7-ELEVEN STORE 36013A EMHT INC & 7-ELEVEN INC 800-FLOWERS INC 8X8 INC A & A QUALITY APPLIANCE A & B Engineering Services LLC A CUSTOM COACH A CUT ABOVE LANDSCAPE LLC A GOOD LIL TRANNY SHOP LLC A GOOD SHOP INC A HOLE IN THE WALL CONSTRUCTIO AHW CONSTRUCTION A MAN WITH A VAN INC A SIMPLEE GORGEOUS BOUTIQUE A TO Z RENTAL CENTER, INC.
    [Show full text]
  • <> CRONOLOGIA DE LOS SATÉLITES ARTIFICIALES DE LA
    1 SATELITES ARTIFICIALES. Capítulo 5º Subcap. 10 <> CRONOLOGIA DE LOS SATÉLITES ARTIFICIALES DE LA TIERRA. Esta es una relación cronológica de todos los lanzamientos de satélites artificiales de nuestro planeta, con independencia de su éxito o fracaso, tanto en el disparo como en órbita. Significa pues que muchos de ellos no han alcanzado el espacio y fueron destruidos. Se señala en primer lugar (a la izquierda) su nombre, seguido de la fecha del lanzamiento, el país al que pertenece el satélite (que puede ser otro distinto al que lo lanza) y el tipo de satélite; este último aspecto podría no corresponderse en exactitud dado que algunos son de finalidad múltiple. En los lanzamientos múltiples, cada satélite figura separado (salvo en los casos de fracaso, en que no llegan a separarse) pero naturalmente en la misma fecha y juntos. NO ESTÁN incluidos los llevados en vuelos tripulados, si bien se citan en el programa de satélites correspondiente y en el capítulo de “Cronología general de lanzamientos”. .SATÉLITE Fecha País Tipo SPUTNIK F1 15.05.1957 URSS Experimental o tecnológico SPUTNIK F2 21.08.1957 URSS Experimental o tecnológico SPUTNIK 01 04.10.1957 URSS Experimental o tecnológico SPUTNIK 02 03.11.1957 URSS Científico VANGUARD-1A 06.12.1957 USA Experimental o tecnológico EXPLORER 01 31.01.1958 USA Científico VANGUARD-1B 05.02.1958 USA Experimental o tecnológico EXPLORER 02 05.03.1958 USA Científico VANGUARD-1 17.03.1958 USA Experimental o tecnológico EXPLORER 03 26.03.1958 USA Científico SPUTNIK D1 27.04.1958 URSS Geodésico VANGUARD-2A
    [Show full text]
  • Index of Astronomia Nova
    Index of Astronomia Nova Index of Astronomia Nova. M. Capderou, Handbook of Satellite Orbits: From Kepler to GPS, 883 DOI 10.1007/978-3-319-03416-4, © Springer International Publishing Switzerland 2014 Bibliography Books are classified in sections according to the main themes covered in this work, and arranged chronologically within each section. General Mechanics and Geodesy 1. H. Goldstein. Classical Mechanics, Addison-Wesley, Cambridge, Mass., 1956 2. L. Landau & E. Lifchitz. Mechanics (Course of Theoretical Physics),Vol.1, Mir, Moscow, 1966, Butterworth–Heinemann 3rd edn., 1976 3. W.M. Kaula. Theory of Satellite Geodesy, Blaisdell Publ., Waltham, Mass., 1966 4. J.-J. Levallois. G´eod´esie g´en´erale, Vols. 1, 2, 3, Eyrolles, Paris, 1969, 1970 5. J.-J. Levallois & J. Kovalevsky. G´eod´esie g´en´erale,Vol.4:G´eod´esie spatiale, Eyrolles, Paris, 1970 6. G. Bomford. Geodesy, 4th edn., Clarendon Press, Oxford, 1980 7. J.-C. Husson, A. Cazenave, J.-F. Minster (Eds.). Internal Geophysics and Space, CNES/Cepadues-Editions, Toulouse, 1985 8. V.I. Arnold. Mathematical Methods of Classical Mechanics, Graduate Texts in Mathematics (60), Springer-Verlag, Berlin, 1989 9. W. Torge. Geodesy, Walter de Gruyter, Berlin, 1991 10. G. Seeber. Satellite Geodesy, Walter de Gruyter, Berlin, 1993 11. E.W. Grafarend, F.W. Krumm, V.S. Schwarze (Eds.). Geodesy: The Challenge of the 3rd Millennium, Springer, Berlin, 2003 12. H. Stephani. Relativity: An Introduction to Special and General Relativity,Cam- bridge University Press, Cambridge, 2004 13. G. Schubert (Ed.). Treatise on Geodephysics,Vol.3:Geodesy, Elsevier, Oxford, 2007 14. D.D. McCarthy, P.K.
    [Show full text]