Cosmic Rays at 120,000 feet above Antarctica The Advanced Thin Ionization Calorimeter (ATIC) Experiment
|
|
- Lorraine Scott
- 5 years ago
- Views:
Transcription
1 Cosmic Rays at 120,000 feet above Antarctica The Advanced Thin Ionization Calorimeter (ATIC) Experiment ATIC is a ~4,000 pound experiment, carried to the near-space environment (~23 miles) by a large volume (sufficient to fill a football stadium) helium filled balloon for days over the continent of Antarctica, to measure the charge composition and energy spectra of primary cosmic rays over the energy range from about to ev in order to investigate the relationship between high energy galactic matter and remnant supernova shock waves. Louisiana State University, Marshall Space Flight Center, University of Maryland, Southern University, Moscow State University, Max Plank Institute - Lindau LSU 11/15/05 ATIC Science - McMurdo 1
2 Cosmic Rays were discovered less than a hundred years ago In 1912 Victor Hess became the first cosmic ray balloonist Measured an increase in the background radiation as a function of altitude, but only up to about 17,000 feet Received the 1936 Nobel Prize in Physics for this work Data measured in 2003 by a simple 400 gm student-built sounding balloon payload. LSU 11/15/05 ATIC Science - McMurdo 2
3 Understanding the nature of cosmic rays Initial thoughts (1920 s) were that this mysterious radiation was some form of high energy photon Hence the name Cosmic RAYS In the 1930 s this viewpoint changed with the understanding that cosmic ray are mostly composed of high energy charged particles Effects due to Earth s magnetic field (east-west; latitude) Discovery of positron and muon Birth of elementary particle physics Until the advent of particle accelerators in the mid s, the cosmic ray beam was used to develop the theory of elementary particles. LSU 11/15/05 ATIC Science - McMurdo 3
4 The Space Age provided new tools In the 1960 s space probes began identifying individual cosmic ray components Sources from the Sun as well as outside our Solar System Electrons, protons and other elements were identified Began measuring the energy spectrum Measurements of the energy density gave first clue about the galactic cosmic ray (GCR) source GCR energy density is roughly equivalent to the energy released by a supernova every 50 to 100 years 70 s, 80 s and 90 s pushed the frontiers in both charge and energy Antiprotons, elements up to Uranium, energies to ~10 21 ev LSU 11/15/05 ATIC Science - McMurdo 4
5 Cosmic Rays extend over a large charge and energy range Tevatron, LHC Max Energy LSU 11/15/05 ATIC Science - McMurdo 5
6 Fundamental questions remain unanswered! Where does this galactic matter come from? How does it get accelerated to such high energies? LSU 11/15/05 ATIC Science - McMurdo 6
7 Recent Chandra X-ray observations of Tycho s Supernova Remnant Supernova remnant observed by Tycho Brahe in 1572 Outward moving shock wave indicated by high energy electrons (blue) Hot stellar debris (red & green) keeping pace with outer shock, contrary to standard theory Warren & Hughes et al. (2005) suggest that a large fraction of outward shock energy is accelerating atomic nuclei to speeds approaching the speed of light LSU 11/15/05 ATIC Science - McMurdo 7
8 Standard Model of Cosmic Ray Acceleration Supernova shock waves may accelerate cosmic rays via first order Fermi process Model predicts an upper energy limit of E ~ Z x ev ATIC Energy Range LSU 11/15/05 ATIC Science - McMurdo 8
9 ATIC Program Summary Investigate relationship between Supernova Remnant (SNR) Shocks and high energy galactic cosmic rays (GCR) Multiple flights needed to obtain necessary exposure ATIC-1 test flight during ATIC-2 during days exposure ATIC-3 scheduled for season Scientific Ballooning programs at Universities provides unique education experiences for the future aerospace workforce ATIC involved over 45 LSU & SU students Are SNR the cosmic accelerators for GCR Measure GCR Hydrogen to Nickel from 50 GeV to ~100 TeV total energy Determine spectral differences Study High Energy Electron Spectrum Flight test pixilated Silicon detector LSU 11/15/05 ATIC Science - McMurdo 9
10 ATIC Instrument Summary Measure charge, energy and number Ionization Calorimetry only practical method to measure high energy light elements Silicon Matrix (Si) has 4,480 pixels to measure GCR charge in presence of shower backscatter Graphite Target to interact the primary particle and generate fragments that, in turn, will start an electromagnetic cascade. Also provides some backscatter shielding Plastic scintillator hodoscopes (S1, S2, S3), embedded in Carbon target, provides event trigger plus charge & trajectory information Fully active calorimeter includes 400 Bismuth Germinate (BGO) crystals to foster and measure the nuclear - electromagnetic cascade showers Geometrical factor: 0.24 m 2 sr (S1 S3 BGO6) LSU 11/15/05 ATIC Science - McMurdo 10
11 Silicon Matrix Detector Si-Matrix: 4480 pixels each 2 cm x 1.5 cm mounted on offset ladders; 0.95 m x 1.05 m area; 16 bit ADC; CR-1 ASIC s; sparsified readout. LSU 11/15/05 ATIC Science - McMurdo 11
12 Plastic Scintillator Hodoscopes Scintillators: 3 x-y layers; 2 cm x 1 cm cross section; Bicron BC-408; Hamamatsu R5611 pmts both ends; two gain ranges; ACE ASIC. S1 336 channels; S2 280 channels; S3 192 channels; First level trigger: S1-S3 LSU 11/15/05 ATIC Science - McMurdo 12
13 BGO Calorimeter Calorimeter: 10 layers ; 2.5 cm x 2.5 cm x 25 cm BGO crystals, 40 per layer, each crystal viewed by R5611 pmt; three gain ranges; ACE ASIC; 1200 channels. LSU 11/15/05 ATIC Science - McMurdo 13
14 On-board Control & Data System Data System: All data recorded on-board; 150 Gbyte disk; LOS data rate 330 kbps; TDRSS data rate 6+ kbps; Underflight capability (not used). Housekeeping: Temperature, Pressure, Voltage, Current, Rates, Software Status, Disk status Command Capability: Power on / off; Trigger type; Thresholds; Pre-scaler; Housekeeping frequency; LOS data rate, Reboot nodes; High Volt settings; Data collection on / off LSU 11/15/05 ATIC Science - McMurdo 14
15 ATIC has been extensively simulated An example of a proton shower in the McMurdo flight configuration Trajectory resolution in S1 calculated from the BGO shower profile for 1 TeV protons. Energy dependence of the proton mean energy deposit and the energy resolution. Energy deposition in 20 cm depth BGO calorimeter for 10 2, 5x10 2, 10 3, 10 4, and 10 5 GeV protons. LSU 11/15/05 ATIC Science - McMurdo 15
16 Particle incident energy determined from shower profile in BGO calorimeter 8 TeV Total Energy Event Shower profiles for protons of indicated energy. Open symbols are simulations & filled symbols are flight data. LSU 11/15/05 ATIC Science - McMurdo 16
17 High altitude winds are circumpolar during summer LSU 11/15/05 ATIC Science - McMurdo 17
18 Assembly of ATIC at Willy Attach the upper support structure Assemble / test detector stack and mount in lower support structure Install Kelar pressure vessel shells Solar arrays provide power & the payload is rolled out the hanger door Attach the thermal protection ATIC is transported to the insulation launch pad LSU 11/15/05 ATIC Science - McMurdo 18
19 Finally everything was ready for launch LSU 11/15/05 ATIC Science - McMurdo 19
20 ATIC Test Flight from McMurdo 43.5 Gbytes Recorded Data 26,100,000 Cosmic Ray triggers 1,300,000 Calibration records 742,000 Housekeeping records 18,300 Rate records Low Energy Trigger > 10 GeV for protons >70% Live-time >90% of channels operating nominally Internal pressure (~8 psi) held constant Internal Temperature: C Altitude: 37 ± 1.5 km Launch: 12/28/00 04:25 UTC Begin Science: 12/29/00 03:54 UTC End Science: 01/12/01 20:33 UTC Termination: 01/13/01 03:56 UTC Recovery: 01/23/01; 01/25/01 LSU 11/15/05 ATIC Science - McMurdo 20
21 First ATIC Science Flight from McMurdo Launch: 12/29/02 04:59 UTC Begin Science: 12/30/02 05:40 UTC End Science: 01/18/03 01:32 UTC Termination: 01/18/03 02:01 UTC Recovery: 01/28/03; 01/30/03 65 Gbytes Recorded Data 16,900,000 Cosmic Ray triggers 1,600,000 Calibration records 184,000 Housekeeping records 26,000 Rate records High Energy Trigger > 75 GeV for protons >96% Live-time >90% of channels operating nominally Internal pressure (~8 psi) decreased slightly (~0.7 psi) for 1 st 10 days then held constant Internal Temperature: C Altitude: 36.5 ± 1.5 km LSU 11/15/05 ATIC Science - McMurdo 21
22 Flight and Recovery Flight path for ATIC-1 (2000) and ATIC-2 (2002) The good ATIC-1 landing on 1/13/01 (left) and the not so good landing of ATIC-2 on 1/18/03 (right) ATIC is designed to be disassembled in the field and recovered with Twin Otters. Two recovery flights are necessary to return all the ATIC components. Pictures show 1 st recovery flight of ATIC-1 LSU 11/15/05 ATIC Science - McMurdo 22
23 Steps in the data analysis Determine incident particle charge and energy Count the number of each species and bin in energies to produce an energy deposit spectrum Deconvolve the instrument response to produce an incident energy spectrum Unfold the transforming effects that occur as the GCR diffuse around the galaxy for millions of years. Use Leaky Box model of cosmic ray confinement Compare with expectations of SNR shock acceleration model LSU 11/15/05 ATIC Science - McMurdo 23
24 An example of event reconstruction Primary (He) Albedo x, cm z, cm y, cm y, cm z, cm x, cm LSU 11/15/05 ATIC Science - McMurdo 24
25 Charge resolution in the p-he group EBGO > 50 GeV EBGO > 500 GeV EBGO > 5 TeV LSU 11/15/05 ATIC Science - McMurdo 25
26 Charge resolution in the CNO-group EBGO > 50 GeV EBGO > 250 GeV EBGO > 1 TeV C O LSU 11/15/05 ATIC Science - McMurdo 26
27 Charge resolution in the Ne-Si group EBGO > 50 GeV EBGO > 250 GeV EBGO > 1 TeV Ne Mg Si S LSU 11/15/05 ATIC Science - McMurdo 27
28 Charge resolution in the Fe group EBGO > 50 GeV EBGO > 250 GeV EBGO > 1 TeV Fe S Ca LSU 11/15/05 ATIC Science - McMurdo 28
29 Deconvolution Primary Energy Spectra (E 0 ) Instrument + = Response Measured Energy Deposit Spectra (E d ) (must solve the inverse problem) A(E 0,E d ) = response matrix Obtained from FLUKA model of instrument See K.E. Batkov et al., 29 th ICRC, 2005 LSU 11/15/05 ATIC Science - McMurdo 29
30 Preliminary ATIC-2 Energy spectra for H and He Proton (top) and Helium (bottom) Energy Deposit spectra from the ATIC-2 flight used as the input to the first order de-convolution calculation. De-convolved Proton and Helium spectrum compared with other measurements and propagation calculations using the Leaky Box model (1, 3) and a diffusion model with weak reacceleration (2, 4). LSU 11/15/05 ATIC Science - McMurdo 30
31 Energy spectra of abundant nuclei C C O/10 Mg Mg O Si Si/10 Ne/100 Ne Fe Fe/100 HEAO-3-C2 ATIC-2 CRN LSU 11/15/05 ATIC Science - McMurdo 31
32 Electrons might provide additional information about the GCR source High energy electrons have a high energy loss rate Lifetime of ~10 5 years for >1 TeV electrons Transport of GCR through interstellar space is a diffusive process Implies that source of high energy electrons are < 1 kpc away Know that electrons are accelerated in SNR Only a handful of SNR meet the lifetime & distance criteria Kobayashi et al (2004) calculations show structure in electron spectrum at high energy LSU 11/15/05 ATIC Science - McMurdo 32
33 ATIC is able to identify GCR electrons Possible bump at GeV seen by both Kobayashi and ATIC may be a source signature? Long duration ATIC flight this season will be critical to resolving this issue e LSU 11/15/05 ATIC Science - McMurdo 33
34 Conclusions Deconvolution Algorithm is still preliminary Initial analysis of heavy ions indicate: Simple Leaky Box not good representation Diffusion model in which λ esc hardens with increasing energy gives better fit. For the diffusion model parameterization, the source energy spectral indices for H and He must be different Electrons show a bump in the GeV range Possibly THE most important result from ATIC ATIC has had two flights in Antarctica and is looking for its third Need at least two times around (~30 days) to confirm the electron results and collect the required heavy ion statistics. LSU 11/15/05 ATIC Science - McMurdo 34
35 Our enthusiastic crew is looking forward to another successful ATIC flight! LSU 11/15/05 ATIC Science - McMurdo 35
The Advanced Thin Ionization Calorimeter (ATIC) Long Duration Balloon Experiment
The Advanced Thin Ionization Calorimeter (ATIC) Long Duration Balloon Experiment A ~1,660 kg experiment, carried to the near-space environment (~36 km) by a large volume (sufficient to fill a football
More informationCosmic Rays and the need for heavy payloads
Cosmic Rays and the need for heavy payloads T. Gregory Guzik Department of Physics and Astronomy Louisiana State University Baton Rouge, LA LSU 04/19/07 LCANS 2007 - April 27, 2007 1 Ballooning leads the
More informationCosmic Ray Energetics And Mass (CREAM) Moriond 2005
Cosmic Ray Energetics And Mass (CREAM) Moriond 2005 Eun-Suk Seo Institute for Physical Science and Technology Department of Physics University of Maryland Cosmic Ray Energy Spectra BESS Space & Heliospheric
More informationCosmic Rays in the Galaxy
1, Over View Cosmic Rays in the Galaxy Discovery : Legendary baloon flight of Victor Hess Observation of Cosmic Rays : Satellite, Balloon (Direct), Air shower (Indirect) Energy Spectrum of Cosmic Rays
More informationCosmic Rays - R. A. Mewaldt - California Institute of Technology
Cosmic Rays - R. A. Mewaldt - California Institute of Technology Cosmic rays are high energy charged particles, originating in outer space, that travel at nearly the speed of light and strike the Earth
More informationLomonosov Moscow State University. NUCLEON Chemical Composition and Energy Spectra of Cosmic Rays at TeV
Lomonosov Moscow State University NUCLEON Chemical Composition and Energy Spectra of Cosmic Rays at 1-1000 TeV D. Podorozhny for Sources of Galactic cosmic rays APC, Paris - December 11-14, 2018 NUCLEON
More informationSupernova Remnants as Cosmic Ray Accelerants. By Jamie Overbeek Advised by Prof. J. Finley
Supernova Remnants as Cosmic Ray Accelerants By Jamie Overbeek Advised by Prof. J. Finley Cosmic Rays Discovered by Victor Hess in 1911 during a balloon flight through Austria He used an electroscope to
More informationA detailed FLUKA-2005 Monte-Carlo simulation for the ATIC detector
Available online at www.sciencedirect.com Advances in Space Research (8) 7 www.elsevier.com/locate/asr A detailed FLUKA- Monte-Carlo simulation for the ATIC detector R.M. Gunasingha a, *, A.R. Fazely a,
More informationCosmic Rays: A Way to Introduce Modern Physics Concepts. Steve Schnetzer
Cosmic Rays: A Way to Introduce Modern Physics Concepts Steve Schnetzer Rutgers CR Workshop May 19, 2007 Concepts Astrophysics Particle Physics Radiation Relativity (time dilation) Solar Physics Particle
More informationMeasurements of Heavy Nuclei with the CALET Experiment
Measurements of Heavy Nuclei with the CALET Experiment for the CALET Collaboration University of Maryland, Baltimore County and NASA Goddard Space Flight Center 8 Greenbelt Rd. Greenbelt, MD 771, USA E-mail:
More informationPayload for Antimatter Matter Exploration and Light-nuclei Astrophysics. PAMELA MissioN 17 December 2010 Prepared by FatiH KAYA
Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics PAMELA MissioN 17 December 2010 Prepared by FatiH KAYA Astropartical Physics İssue To inform. What Powered the Big Bang? Inflation
More informationReview of direct measurements of cosmic rays. Sources of Galactic cosmic rays APC, Paris - December 7-9, 2016
Review of direct measurements of cosmic rays Sources of Galactic cosmic rays APC, Paris - December 7-9, 2016 CR astrophуsics main problems Sources? - Accelerators? The basic paradigm of CR acceleration
More informationPreliminary Results From The First Flight of Atic: The Silicon Matrix
Preliminary Results From The First Flight of Atic: The Silicon Matrix J. H. Adams, Jr. (1) for the ATIC Collaboration (1) NASA Marshall Space Flight Center, Huntsville, AL 35812, USA james.h.adams@msfc.nasa.gov,
More informationSUPPLEMENTARY INFORMATION
1. Selecting electrons in ATIC ATIC is a calorimetric instrument and, as such, relies upon the difference in the development of the cascades (showers) initiated by protons and electrons. Moreover, the
More informationThe Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission
The Large Area Telescope on-board of the Fermi Gamma-Ray Space Telescope Mission 1 Outline Mainly from 2009 ApJ 697 1071 The Pair Conversion Telescope The Large Area Telescope Charged Background and Events
More informationCurrent and Future balloon and space experiments L. Derome (LPSC Grenoble) Tango, May 4-6th, 2009
Current and Future balloon and space experiments L. Derome (LPSC Grenoble) Tango, May 4-6th, 2009 L. Derome, Tango, May 4-6th 2009 1 Plan I will focus on: Future experiments which are going to measure
More informationJustin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration
Measurement of the cosmic ray positron spectrum with the Fermi LAT using the Earth s magnetic field Justin Vandenbroucke (KIPAC, Stanford / SLAC) for the Fermi LAT collaboration International Cosmic Ray
More informationQuestions 1pc = 3 ly = km
Cosmic Rays Historical hints Primary Cosmic Rays: - Cosmic Ray Energy Spectrum - Composition - Origin and Propagation - The knee region and the ankle Secondary CRs: -shower development - interactions Detection:
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More informationCosmic Rays. Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon
Cosmic Rays Discovered in 1912 by Viktor Hess using electroscopes to measure ionization at altitudes via balloon Nobel Prize in 1936 Origin of high energy cosmic rays is still not completely understood
More informationTemperature Dependence Calibration and Correction of the DAMPE BGO Electromagnetic Calorimeter
Temperature Dependence Calibration and Correction of the DAMPE BGO Electromagnetic Calorimeter Yifeng Wei, Zhiyong Zhang, Yunlong Zhang*, Sicheng Wen, Chi Wang, Zhiying Li, Changqing Feng, Xiaolian Wang,
More informationCosmic Ray Composition
+ = Cosmic Ray Composition Stéphane Coutu The Pennsylvania State University 3 rd rd School on Cosmic Rays and Astrophysics Arequipa,, Peru August 28-29, 29, 2008 1/ 30 Outline Cosmic Rays: Origin and Propagation;
More informationPreliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET)
Preliminary results from gamma-ray observations with the CALorimeteric Electron Telescope (CALET) Y.Asaoka for the CALET Collaboration RISE, Waseda University 2016/12/15 CTA-Japan Workshop The extreme
More informationThe Physics of Cosmic Rays
The Physics of Cosmic Rays QuarkNet summer workshop July 23-27, 2012 1 Recent History Most natural phenomena can be explained by a small number of simple rules. You can determine what these rules are by
More informationCosmic Ray panorama. Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1
1912 1932 Cosmic Ray panorama http::// Pamela.roma2.infn.it PAMELA (2012) Experimental challenges : e + /p ~ 10-3 e + /e - ~ 10-1 Pamela : < 0.1 evt year/gev Flux E α α 2.7 / 3.3 Statistical precision
More informationCosmic Rays. This showed that the energy of cosmic rays was many times that of any other natural or artificial radiation known at that time.
Cosmic Rays 1. Discovery As long ago as 1900, C. T. R. Wilson and others found that the charge on an electroscope always 'leaked' away in time, and this could never be prevented, no matter how good the
More informationCosmic Ray Physics with the Alpha Magnetic Spectrometer
Cosmic Ray Physics with the Alpha Magnetic Spectrometer Università di Roma La Sapienza, INFN on behalf of AMS Collaboration Outline Introduction AMS02 Spectrometer Cosmic Rays: origin & propagations: Dominant
More informationThe NUCLEON Space Experiment Preliminary Results. Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, , Russia
The NUCLEON Space Experiment Preliminary Results A. Turundaevskiy a1, E.Atkin a, V.Bulatov c, V.Dorokhov c, N.Gorbunov d, S.Filippov c, V.Grebenyuk d, D.Karmanov a, I.Kovalev a, I.Kudryashov a, M.Merkin
More informationDark Matter Particle Explorer: The First Chinese Cosmic Ray and Hard γ-ray Detector in Space
SPACE SCIENCE ACTIVITIES IN CHINA Dark Matter Particle Explorer: The First Chinese Cosmic Ray and Hard γ-ray Detector in Space AUTHORS CHANG Jin Key Laboratory of Dark Matter and Space Astronomy, Purple
More informationThe PAMELA Satellite Experiment: An Observatory in Space for Particles, Antiparticles and Nuclei in the Cosmic Rays
: An Observatory in Space for Particles, Antiparticles and Nuclei in the Cosmic Rays M. Ricci 1 on behalf of the PAMELA Collaboration INFN, Laboratori Nazionali di Frascati, Via Enrico Fermi 40, I-00044
More informationCOSMIC RAYS DAY INTRODUCTION TO COSMIC RAYS WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII
COSMIC RAYS DAY WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII INTRODUCTION TO COSMIC RAYS MAJOR QUESTIONS: Are there forms of matter in the Universe that do not
More informationDr. John Kelley Radboud Universiteit, Nijmegen
arly impressive. An ultrahighoton triggers a cascade of particles mulation of the Auger array. The Many Mysteries of Cosmic Rays Dr. John Kelley Radboud Universiteit, Nijmegen Questions What are cosmic
More informationGalactic cosmic rays from NUCLEON to HERO. (in Moscow State University) Lomonosov Moscow State University
Lomonosov Moscow State University Galactic cosmic rays from NUCLEON to HERO (in Moscow State University) D. Podorozhny for Sources of Galactic cosmic rays APC, Paris - December 7-9, 2016 Ionization Calorimeter
More informationFrom the Knee to the toes: The challenge of cosmic-ray composition
New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg New Views of
More informationDark Matter Searches with AMS-02. AMS: Alpha Magnetic Spectrometer
Dark Matter Searches with AMS-02 AMS: Alpha Magnetic Spectrometer 2007/2008 Wim de Boer on behalf of the AMS collaboration University of Karlsruhe July, 20. 2004 COSPAR, Paris, W. de Boer, Univ. Karlsruhe
More informationCosmic rays in the local interstellar medium
Cosmic rays in the local interstellar medium Igor V. Moskalenko Igor V. Moskalenko/NASA-GSFC 1 LMC (Magellanic Cloud Emission Nuclear Data-2004/09/28, Line Survey: Smith, Points) Santa Fe R - H G - [S
More informationPrecision measurements of nuclear CR energy spectra and composition with the AMS-02 experiment
Journal of Physics: Conference Series PAPER OPEN ACCESS Precision measurements of nuclear CR energy spectra and composition with the AMS-02 experiment To cite this article: E Fiandrini 2016 J. Phys.: Conf.
More information99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park
99 Years from Discovery : What is our current picture on Cosmic Rays? #6 How cosmic rays travel to Earth? Presented by Nahee Park #5 How do Cosmic Rays gain their energy? I. Acceleration mechanism of CR
More informationNew results from the AMS experiment on the International Space Station. Henning Gast RWTH Aachen
New results from the AMS experiment on the International Space Station Henning Gast RWTH Aachen 1 Questions to AMS-02: Are there galaxies made of anti-matter in the Universe? What is the nature of Dark
More informationTopic 7. Relevance to the course
Topic 7 Cosmic Rays Relevance to the course Need to go back to the elemental abundance curve Isotopes of certain low A elements such as Li, Be and B have larger abundances on Earth than you would expect
More informationThe Silicon-Tungsten Tracker of the DAMPE Mission
The Silicon-Tungsten Tracker of the DAMPE Mission Philipp Azzarello, DPNC, University of Geneva for the DAMPE-STK collaboration 10th International Hiroshima Symposium on the Development and Application
More informationExperimental review of high-energy e e + and p p spectra
Experimental review of high-energy e e + and p p spectra Luca Baldini INFN Pisa luca.baldini@pi.infn.it TeV Particle Astrophysics, July 15 2009 Outline Measurement of the singly charged component of the
More informationLecture 14 Cosmic Rays
Lecture 14 Cosmic Rays 1. Introduction and history 2. Locally observed properties 3. Interactions 4. Demodulation and ionization rate 5. Midplane interstellar pressure General Reference MS Longair, High
More informationN U C L E O N. Satellite Mission. Present status.
N U C L E O N Satellite Mission. Present status. a) Skobeltsyn Institute of Nuclear Physics, Moscow State University b) DB ARSENAL, Sankt-Peterburg, Russia c) Joint Institute for Nuclear Research, Dubna,
More informationPAMELA: a Satellite Experiment for Antiparticles Measurement in Cosmic Rays
PAMELA: a Satellite Experiment for Antiparticles Measurement in Cosmic Rays PAMELA scientific objectives Detector s overview Subsystems description PAMELA status Massimo Bongi Universita degli Studi di
More informationTHE AMS RICH COUNTER
THE AMS RICH COUNTER G. BOUDOUL ISN Grenoble ISN-GRENOBLE 1 The AMS RICH collaboration: Bologna, Grenoble, Lisbon, Madrid, Maryland, Mexico 2 The AMS collaboration UNAM S.C.C. TING (MIT), PI 3 AMS Scientific
More informationISAPP Gran Sasso June 28-July 9, Observations of Cosmic Rays
ISAPP 2004 Gran Sasso June 28-July 9, 2003 Observations of Cosmic Rays Tiina Suomijärvi Institut de Physique Nucléaire Université Paris XI-Orsay, IN2P3/CNRS France Why to Study Cosmic Rays? Cosmic rays
More informationA Guide for ACCESS Design Considerations
A Guide for ACCESS Design Considerations Opher Ganel, Eun-Suk Seo, Jian-Zhong Wang, Jayoung Wu Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, USA Abstract.
More informationAstronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused
More informationSTUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE
STUDY OF EXTENSIVE AIR SHOWERS IN THE EARTH S ATMOSPHERE I. BACIOIU * Institute of Space Science, P.O. Box MG-23, RO-077125 Bucharest-Magurele, Romania, E-mail: iuliana.bacioiu@spacescience.ro Abstract.
More informationCosmic Rays. M. Swartz. Tuesday, August 2, 2011
Cosmic Rays M. Swartz 1 History Cosmic rays were discovered in 1912 by Victor Hess: he discovered that a charged electroscope discharged more rapidly as he flew higher in a balloon hypothesized they were
More informationCosmic-ray energy spectrum around the knee
Cosmic-ray energy spectrum around the knee M. SHIBATA Department of Physics, Yokohama National University, Yokohama, 240-8501, Japan Interesting global and fine structures of cosmic-ray energy spectrum
More informationPoS(ICRC2015)432. Simulation Study On High Energy Electron and Gamma-ray Detection With the Newly Upgraded Tibet ASgamma Experiment
Simulation Study On High Energy Electron and Gamma-ray Detection With the Newly Upgraded Tibet ASgamma Experiment Xu Chen a, D. Chen b, J. Huang a, H. B. Jin b, L. M. Zhai a,b, M. Shibata c, Y. Katayose
More information> News < AMS-02 will be launched onboard the Shuttle Endeavour On May 2nd 2:33 P.M. from NASA Kennedy space center!
> News < Anti-matter, dark matter measurement By measuring the cosmic rays (Mainly electron, positron, proton, anti-proton and light nuclei) AMS-02 will be launched onboard the Shuttle Endeavour On May
More informationStellar Explosions (ch. 21)
Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least
More informationDETAILED elemental spectra of cosmic rays in the energy
IEEE TRANSACTIONS ON NUCLEAR SCIENCE, VOL. 54, NO. 5, OCTOBER 2007 1743 Performance of a Dual Layer Silicon Charge Detector During CREAM Balloon Flight S. Nam, H. S. Ahn, P. Allison, M. G. Bagliesi, L.
More informationThe Fermi Gamma-ray Space Telescope
Abstract The Fermi Gamma-ray Space Telescope Tova Yoast-Hull May 2011 The primary instrument on the Fermi Gamma-ray Space Telescope is the Large Area Telescope (LAT) which detects gamma-rays in the energy
More informationA NEW GENERATION OF GAMMA-RAY TELESCOPE
A NEW GENERATION OF GAMMA-RAY TELESCOPE Aleksandar GOSTOJIĆ CSNSM, Orsay, France 11 th Russbach School on Nuclear Astrophysics, March 2014. Introduction: Gamma-ray instruments GROUND BASED: ENERGY HIGHER
More informationIntroduction History of Cosmic Ray Studies: Origin, Propagation, Spectrum, Composition
Etat actuel et Perspectives de la Physique d'astro-particule Daniel Haas DPNC Geneva Introduction History of Cosmic Ray Studies: Origin, Propagation, Spectrum, Composition Selected Experiments & Results
More informationGAMMA-RAY ASTRONOMY: IMAGING ATMOSPHERIC CHERENKOV TECHNIQUE FABIO ZANDANEL - SESIONES CCD
GAMMA-RAY ASTRONOMY: IMAGING ATMOSPHERIC CHERENKOV TECHNIQUE COSMIC RAYS Discovered in 1912 by Victor Hess (Nobel Prize) Messengers from the non-thermal part of the Universe E < 15 ev: galactic E > 17
More informationMeasurement of Cosmic-Ray Nuclei with the Third Flight of the CREAM Balloon- Borne Experiment
Measurement of Cosmic-Ray Nuclei with the Third Flight of the CREAM Balloon- Borne Experiment ICRC 2017 Dr. Jacob Smith Inst. For Phys. Sci. & Tech. University of Maryland Y. Amare 1, T. Anderson 2, D.
More informationMoonCal An electromagnetic calorimeter on the lunar surface. R.Battiston, M.T.Brunetti, F. Cervelli, C.Fidani, F.Pilo
MoonCal An electromagnetic calorimeter on the lunar surface R.Battiston, M.T.Brunetti, F. Cervelli, C.Fidani, F.Pilo Why the Moon for astroparticle physics? The Moon does not have atmosphere nor water.
More informationHAWC Observation of Supernova Remnants and Pulsar Wind Nebulae
HAWC Observation of Supernova Remnants and Pulsar Wind Nebulae a, and H. Zhou a for the HAWC Collaboration b a Department of Physics, Michigan Technological University 1400 Townsend Drive, Houghton, MI,
More informationIAC-08-A MONTE CARLO SIMULATIONS OF ENERGY LOSSES BY SPACE PROTONS IN THE CRATER DETECTOR
IAC-08-A1.4.06 MONTE CARLO SIMULATIONS OF ENERGY LOSSES BY SPACE PROTONS IN THE CRATER DETECTOR Lawrence W. Townsend The University of Tennessee, Knoxville, Tennessee, United States of America ltownsen@tennessee.edu
More informationHigh-energy neutrino detection with the ANTARES underwater erenkov telescope. Manuela Vecchi Supervisor: Prof. Antonio Capone
High-energy neutrino detection with the ANTARES underwater erenkov telescope Supervisor: Prof. Antonio Capone 1 Outline Neutrinos: a short introduction Multimessenger astronomy: the new frontier Neutrino
More informationPAMELA satellite: fragmentation in the instrument
PAMELA satellite: fragmentation in the instrument Alessandro Bruno INFN, Bari (Italy) for the PAMELA collaboration Nuclear Physics for Galactic CRs in the AMS-02 era 3-4 Dec 2012 LPSC, Grenoble The PAMELA
More informationThe CALorimetric Electron Telescope (CALET): High Energy Astroparticle Physics Observatory on the International Space Station
The CALorimetric Electron Telescope (CALET): High Energy Astroparticle Physics Observatory on the International Space Station for the CALET collaboration Research Institute for Science and Engineering
More informationNon-thermal emission from pulsars experimental status and prospects
Non-thermal emission from pulsars experimental status and prospects # γ!"# $%&'() TeV γ-ray astrophysics with VERITAS ( $γ" *$%&'() The charged cosmic radiation - how it all began... Discovery: Victor
More informationPrimary Cosmic Rays : what are we learning from AMS
Primary Cosmic Rays : what are we learning from AMS Roberto Battiston University and INFN-TIFPA of Trento HERD Workshop IHEP-Beijing December 2-3 2013 1 Agile Fermi PAMELA AMS Direct study of the HESS
More informationCRaTER Science Requirements
CRaTER Science Requirements Lunar Reconnaissance Orbiter CRaTER Preliminary Design Review Justin Kasper (CRaTER Proj. Sci.) Outline Energy deposition Classical ionizing radiation Nuclear fragmentation
More informationDeep Space Test Bed. POC Deep Space Test Bed (DSTB)
Deep Space Test Bed Workshop for Radiation Monitoring on the International Space Station September 3-5, 2003 Berkeley, California Presented by Eric Benton POC Mark.J.Christl@NASA.GOV http://sd.msfc.nasa.gov/cosmicray/dstb/dstb.htm
More informationDevelopment of a 3D-Imaging Calorimeter in LaBr 3 for Gamma-Ray Space Astronomy
Development of a 3D-Imaging Calorimeter in LaBr 3 for Gamma-Ray Space Astronomy Aleksandar GOSTOJIĆ CSNSM, Orsay, France 7 th New Developmeants In Photodetection, Tours, France, 2014 Introduction: Gamma-ray
More informationEun-Suk Seo Inst. for Phys. Sci. & Tech. and Department of Physics University of Maryland. Cosmic Rays Eun-Suk Seo
Eun-Suk Seo Inst. for Phys. Sci. & Tech. and Department of Physics University of Maryland Cosmic Rays Eun-Suk Seo 1 Cosmic Rays Eun-Suk Seo 2 How do cosmic accelerators work? BESS ATIC CREAM, TRACER Elemental
More informationChapter 6.2: space based cosmic ray experiments. A. Zech, Instrumentation in High Energy Astrophysics
Chapter 6.2: space based cosmic ray experiments 1 A bit of history... space based experiments 1912-1950: first observations of the cosmic ray flux with detectors onboard balloons and air-planes. 1950s/60s:
More informationThe LHAASO-KM2A detector array and physical expectations. Reporter:Sha Wu Mentor: Huihai He and Songzhan Chen
The LHAASO-KM2A detector array and physical expectations Reporter:Sha Wu Mentor: Huihai He and Songzhan Chen Outline 1. Introduction 2. The KM2A Detector Array 3. Physical Expectations 3.1 Sensitivity
More informationGamma Ray Physics in the Fermi era. F.Longo University of Trieste and INFN
Gamma Ray Physics in the Fermi era F.Longo University of Trieste and INFN Vulcano, May 22, 2018 F.Longo et al. -- 1 Gamma-ray astrophysics above 100 MeV AGILE Fermi 2 Picture of the day, Feb. 28, 2011,
More informationParticle Physics Beyond Laboratory Energies
Particle Physics Beyond Laboratory Energies Francis Halzen Wisconsin IceCube Particle Astrophysics Center Nature s accelerators have delivered the highest energy protons, photons and neutrinos closing
More informationPoS(ICRC2017)1076. Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment
Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment,, Jing-Jing Zang,Tie-Kuang Dong, Antonio Surdo,, Stefania Vitillo 5, on behalf of the DAMPE collaboration Key Laboratory of Dark Matter and Space
More information1 Introduction STATUS OF THE GLAST LARGE AREA TELESCOPE. SLAC-PUB December Richard Dubois. Abstract
SLAC-PUB-10261 December 2003 STATUS OF THE GLAST LARGE AREA TELESCOPE Richard Dubois Stanford Linear Accelerator Center, Stanford University, PO Box 20750, Stanford, CA, USA Abstract The GLAST Large Area
More informationRelative abundance of elements at Earth
Relative abundance of elements at Earth cosmic rays - solar system ~ 1 GeV/n Si = 100 JRH, Adv. Space Res. 41 (2008) 442 TRACER Energy Spectra for individual elements D. Müller et al., ICRC 2007 Energy
More informationInterstellar gamma rays. New insights from Fermi. Andy Strong. on behalf of Fermi-LAT collaboration. COSPAR Scientific Assembly, Bremen, July 2010
Interstellar gamma rays New insights from Fermi Andy Strong on behalf of Fermi-LAT collaboration COSPAR Scientific Assembly, Bremen, July 2010 Session E110: ' The next generation of ground-based Cerenkov
More informationThe High-Energy Interstellar Medium
The High-Energy Interstellar Medium Andy Strong MPE Garching on behalf of Fermi-LAT collaboration Cosmic Ray Interactions: Bridging High and Low Energy Astrophysics Lorentz Centre Workshop March 14-18
More informationThe Cosmic Ray Energetics and Mass (CREAM) Experiment Timing Charge Detector
The Cosmic Ray Energetics and Mass (CREAM) Experiment Timing Charge Detector J. J. Beatty a*, H. S. Ahn b, P. S. Allison a, M. J. Choi c, N. Conklin a, S. Coutu a, M. A. DuVernois d, O. Ganel b, S. Jaminion
More informationA gas-filled calorimeter for high intensity beam environments
Available online at www.sciencedirect.com Physics Procedia 37 (212 ) 364 371 TIPP 211 - Technology and Instrumentation in Particle Physics 211 A gas-filled calorimeter for high intensity beam environments
More informationLow-Energy Cosmic Rays
Low-Energy Cosmic Rays Cosmic rays, broadly defined, are charged particles from outside the solar system. These can be electrons, protons, or ions; the latter two dominate the number observed. They are
More informationA-Exam: e + e Cosmic Rays and the Fermi Large Array Telescope
A-Exam: e + e Cosmic Rays and the Fermi Large Array Telescope Walter Hopkins Physics Department, Cornell University. The Fermi Large Area Telescope is a particle detector in space with an effective collecting
More informationInteraction of particles in matter
Interaction of particles in matter Particle lifetime : N(t) = e -t/ Particles we detect ( > 10-10 s, c > 0.03m) Charged particles e ± (stable m=0.511 MeV) μ ± (c = 659m m=0.102 GeV) ± (c = 7.8m m=0.139
More informationLimits on Antiprotons in Space from the Shadowing of Cosmic Rays by the Moon
Limits on Antiprotons in Space from the Shadowing of Cosmic Rays by the Moon Presented by: Yupeng Xu ( ETH Zürich / L3+C collaboration) PhD Students Seminar, PSI, October 1-2, 2003 The L3+C Experiment
More informationSep. 13, JPS meeting
Recent Results on Cosmic-Rays by Fermi-LAT Sep. 13, 2010 @ JPS meeting Tsunefumi Mizuno (Hiroshima Univ.) On behalf of the Fermi-LAT collaboration 1 Outline Introduction Direct measurement of CRs CRs in
More informationWhere do they originate? How do they gain their enourmous energies? What happens to them in transit from sources to us?
What do cosmic rays tell us about : Where do they originate? How do they gain their enourmous energies? What happens to them in transit from sources to us? Energies of cosmic ray particles: 1 watt of power
More informationHigh-energy Gamma Rays detection with the AMS-02 electromagnetic calorimeter. F. Pilo for the AMS-02 ECAL Group INFN Sezione di Pisa, Italy
Frascati Physics Series Vol. 58 (2014) Frontier Objects in Astrophysics and Particle Physics May 18-24, 2014 High-energy Gamma Rays detection with the AMS-02 electromagnetic calorimeter F. Pilo for the
More informationMeasurement of the CR e+/e- ratio with ground-based instruments
Measurement of the CR e+/e- ratio with ground-based instruments Pierre Colin Max-Planck-Institut für Physik CR Moon shadow MPP retreat - 21 January 2014 Cosmic ray electrons Observation: Above the atmosphere:
More informationSupernova remnants: X-ray observations with XMM-Newton
Supernova remnants: X-ray observations with XMM-Newton Anne DECOURCHELLE, Service d Astrophysique, IRFU, DSM, CEA Supernova remnants: key ingredients to understand our Universe Chemical enrichment, heating
More informationATLAS EXPERIMENT : HOW THE DATA FLOWS. (Trigger, Computing, and Data Analysis)
ATLAS EXPERIMENT : HOW THE DATA FLOWS (Trigger, Computing, and Data Analysis) In order to process large volumes of data within nanosecond timescales, the trigger system is designed to select interesting
More informationThe summer before my junior year, I went to attend the Secondary Student Training
Personal Section The summer before my junior year, I went to attend the Secondary Student Training Program at the University of Iowa. There, I interned for Professor Ugur Akgun to simulate the unfolding
More informationBeam Tests of the Balloon-Borne ATIC Experiment
Beam Tests of the Balloon-Borne ATIC Experiment O. Ganel a*, J.H. Adams Jr b1, H.S. Ahn a, J. Ampe b, G. Bashindzhagyan c, G. Case d, J. Chang e,h, S. Ellison d, A. Fazely f, R. Gould d, D. Granger d,
More informationarxiv: v1 [astro-ph.he] 2 Jul 2009
PROCEEDINGS OF THE 31 st ICRC, ŁÓDŹ 2009 1 First results on Cosmic Ray electron spectrum below 20 GeV from the Fermi LAT. M.Pesce-Rollins on behalf of the Fermi LAT Collaboration Istituto Nazionale di
More informationDetecting. Particles
Detecting Experimental Elementary Particle Physics Group at the University of Arizona + Searching for Quark Compositeness at the LHC Particles Michael Shupe Department of Physics M. Shupe - ATLAS Collaboration
More informationEvolution of High Mass Stars
Luminosity (L sun ) Evolution of High Mass Stars High Mass Stars O & B Stars (M > 4 M sun ): Burn Hot Live Fast Die Young Main Sequence Phase: Burn H to He in core Build up a He core, like low-mass stars
More informationParticle acceleration in Supernova Remnants
Particle acceleration in Supernova Remnants Anne Decourchelle Service d Astrophysique, CEA Saclay Collaborators: J. Ballet, G. Cassam-Chenai, D. Ellison I- Efficiency of particle acceleration at the forward
More information