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1. Galactic Halo size in the light of recent AMS-02 data

Author

Nathanael Weinrich, David Maurin, Pasquale D. Serpico, Mathieu Boudaud, L. Derome, Julien Lavalle, P. Salati, G. Weymann-Despres, Yoann Génolini, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology [2007-2019] (Grenoble INP [2007-2019])-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Instituto de Física Teórica UAM/CSIC (IFT), Universidad Autonoma de Madrid (UAM)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), IFAC, Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), ANR-18-CE31-0006,GADAMA,GALACTIC DARK MATTER(2018), European Project: 674896,H2020,H2020-MSCA-ITN-2015,ELUSIVES(2016), European Project: 690575,H2020,H2020-MSCA-RISE-2015,InvisiblesPlus(2016), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], IN-DIFFUSION MODELS, NEUTRON MONITORS, Dark matter, FOS: Physical sciences, Context (language use), Cosmic ray, MUON DETECTORS, Astrophysics, 01 natural sciences, 7. Clean energy, Galactic halo, COSMIC-RAY PROPAGATION, Positron, SPATIAL ORIGIN, cosmic rays, POSITRON FLUX, 0103 physical sciences, halo [Galaxy], ISOTOPIC COMPOSITION, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, 010308 nuclear & particles physics, astroparticle physicscosmic rayshigh-energy astrophysical phenomena, Astronomy and Astrophysics, GAMMA, Galaxy, Galaxy: halo, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], astroparticle physics, 13. Climate action, Space and Planetary Science, SOLAR MODULATION, ABUNDANCE, Halo, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The vertical diffusive halo size of the Galaxy, $L$, is a key parameter for dark matter indirect searches. It can be better determined thanks to recent AMS-02 data. We set constraints on $L$ from Be/B and $^{10}$Be/Be data, and we performed a consistency check with positron data. We detail the dependence of Be/B and $^{10}$Be/Be on $L$ and forecast on which energy range better data would be helpful for future $L$ improvements. We used USINE v3.5 for the propagation of nuclei, and $e^+$ were calculated with the pinching method of Boudaud et al. (2017). The current AMS-02 Be/B ($\sim3\%$ precision) and ACE-CRIS $^{10}$Be/Be ($\sim 10\%$ precision) data bring similar and consistent constraints on $L$. The AMS-02 Be/B data alone constrain $L=5^{+3}_{-2}$~kpc at a 68\% confidence level (spanning different benchmark transport configurations), a range for which most models do not overproduce positrons. Future experiments need to deliver percent-level accuracy on $^{10}$Be/$^9$Be anywhere below 10 GV to further constrain $L$. Forthcoming AMS-02, HELIX, and PAMELA $^{10}$Be/$^9$Be results will further test and possibly tighten the limits derived here. Elemental ratios involving radioactive species with different lifetimes (e.g. Al/Mg and Cl/Ar) are also awaited to provide complementary and robuster constraints., 15 pages, 10 figures, 6 tables. Additional references and few clarifications (matches A&A accepted version)

Published
2020
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2. ISS-CREAM Flight Operation

Author

Ji Lee, M. Chung, D. Angelaszek, T. Mernik, S. Jeong, J. F. Liang, Jong Moon Park, Y. S. Yoon, J. A. Jeon, O. Ofoha, H.G. Huh, B. Mark, Hun Kuk Park, Ki Chun Kim, M. Nester, I. H. Park, J. R. Smith, L. Derome, M. H. Lee, R.P. Weinmann, P. Walpole, M. Copley, Y. Amare, Hyeyoung Lee, S C. Kang, HyoJung Hyun, Y.S. Hwang, J P. Lundquist, S. Rostsky, Hak Jun Kim, A. Gerrety, Min-Hyeok Kim, A. Mechaca-Rocha, G.H. Choi, Eun-Suk Seo, L. Lutz, N. Picot-Clemente, Z. Yin, H G. Zhang, R. Takeishi, L. Eraud, L. Lu, L. Hagenau, C. Falana, J. H. Han, H. B. Jeon, J. Wu, N. Anthony, C. Lamb, T. Tatoli, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and CREAM

Subjects
Ethernet, 010504 meteorology & atmospheric sciences, business.industry, Computer science, Payload, Cosmic ray, Satellite system, 01 natural sciences, Software, 0103 physical sciences, International Space Station, Telecommunications link, Aerospace engineering, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, 010303 astronomy & astrophysics, Flight computer, 0105 earth and related environmental sciences
Abstract

International audience; The Cosmic Ray Energetics And Mass experiment for the International Space Station (ISS-CREAM) is designed and built to measure the elemental energy spectra of cosmic-ray particles (1 ≤ Z ≤ 26) and electrons. It measures the energy of incident cosmic rays from 10^12 to 10^15 eV. ISS-CREAM was launched and deployed to the ISS in August 2017. The Science Operations Center (SOC) at the University of Maryland has been operating the payload on the Interna-tional Space Station (ISS) in coordination with the Payload Operations Integration Center (POIC) at NASA’s Marshall Space Flight Center. The SOC has been responsible for sending commands to and receiving data from the Science Flight Computer (SFC) on board ISS-CREAM. The ISS-CREAM data taking program interfaces with the POIC using the Telescience Resources Kit through the Software Toolkit for Ethernet Lab-Like Architecture developed by the Boeing Company. The command uplink and data downlink have been through the Track-ing and Data Relay Satellite System. We present the ISS-CREAM flight operations including ISS communications, SFC performance, etc.

Published
2019
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3. Monte Carlo Simulations of the ISS-CREAM Instrument

Author

C. Falana, R. Takeishi, Y.S. Hwang, O. Ofoha, Eun-Suk Seo, J. Wu, M. H. Lee, L. Hagenau, L. Lu, Joowon Lee, J. F. Liang, Arturo Alejandro Menchaca-Rocha, J.A. Jeon, L. Derome, Kwangmoo Kim, Z. Yin, Y. S. Yoon, Hun Kuk Park, L. Lutz, Y. Amare, N. Anthony, M. Nester, L. Eraud, G.H. Choi, H G. Zhang, Hyeyoung Lee, P. Walpole, Inkyu Park, J. H. Han, H. B. Jeon, N. Picot-Clemente, M. Chung, D. Angelaszek, T. Mernik, Jong Moon Park, HyoJung Hyun, A. Gerrety, S. Jeong, J P. Lundquist, J. R. Smith, H.G. Huh, M.H. Kim, R.P. Weinmann, M. Copley, S C. Kang, S. Rostsky, T. Tatoli, C. Lamb, Hak Jun Kim, B. Mark, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and CREAM

Subjects
Physics, Range (particle radiation), Proton, Calorimeter (particle physics), Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Electron, Scintillator, 01 natural sciences, 7. Clean energy, Computational physics, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

International audience; Cosmic Ray Energetics and Mass for the International Space Station (ISS-CREAM) is designed to directly measure the energy spectra of high-energy cosmic rays, encompassing proton to iron nuclei, over the energy range from 1012 to 1015 eV [1]. The capability to measure an extended energy range enables us to probe the origin and acceleration mechanisms of cosmic rays. The ISS-CREAM instrument is configured with the balloon-borne CREAM calorimeter (CAL) for energy measurements and four layers of a finely segmented Silicon Charge Detector (SCD) for charge measurements. In addition, two new compact detectors have been developed for electron/proton separation: Top and Bottom scintillator-based counting detectors (TCD/BCD) and a boronated scintillator detector (BSD). Simulations use the GEANT3 package [2] with the FLUKA hadronic model [3]. An isotropic event generator was developed for the ISS-CREAM geometry with particles incident from the upper hemisphere. We will present simulation results regarding ISS-CREAM performance, including trigger rates, energy resolution, energy response, tracking resolution, charge efficiency, etc.

Published
2019
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4. On-orbit performance of the top and bottom counting detectors for the ISS-CREAM experiment on the international space station

Author

J.A. Jeon, Hyunghoon Kim, N. Picot-Clemente, Inkyu Park, R. Takeishi, R. Quinn, S. L. Nutter, Hyeyoung Lee, J. F. Liang, S. Morton, J.R. Smith, J. T. Link, Kwangmoo Kim, P. Walpole, O. Ofoha, L. Lutz, L. Eraud, S. I. Mognet, L. Hagenau, M. Nester, K. Cheryian, S. Im, G.H. Choi, J P. Lundquist, J. Wu, L. Derome, Y. Amare, Y. S. Yoon, S.C. Kang, M. H. Lee, Eun-Suk Seo, L. Lu, Arturo Alejandro Menchaca-Rocha, H. Park, Joowon Lee, S. Coutu, D. Angelaszek, M.H. Kim, HyoJung Hyun, R.P. Weinmann, N. Anthony, M. Copley, H.G. Huh, S. Jeong, John Mitchell, J. H. Han, H. B. Jeon, Y.S. Hwang, T. Mernik, Jong Moon Park, T. Anderson, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
Atmospheric Science, Astrophysics::High Energy Astrophysical Phenomena, Physics::Medical Physics, Aerospace Engineering, Cosmic ray, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Acceleration, Computer Science::Hardware Architecture, Optics, 0103 physical sciences, International Space Station, 010306 general physics, 010303 astronomy & astrophysics, Cosmic rays, Physics, Elemental composition, Calorimeter (particle physics), business.industry, Detector, TCD/BCD, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, ISS-CREAM, Geophysics, Space and Planetary Science, Orbit (dynamics), General Earth and Planetary Sciences, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CREAM
Abstract

International audience; The Cosmic Ray Energetics And Mass (CREAM) instrument on the International Space Station (ISS) is an experiment to study origin, propagation, acceleration and elemental composition of cosmic rays. The Top Counting Detector (TCD) and Bottom Counting Detector (BCD) are parts of the detector suite of the ISS-CREAM experiment and are designed to separate electrons and protons for studying electron and gamma-ray physics. In addition, the TCD/BCD provide a redundant trigger to that of the calorimeter and a low energy trigger to the ISS-CREAM instrument. After launching, the TCD/BCD trigger was found to be working well. Also, the TCD/BCD have been stable and their hit positions were confirmed to be well matched with other detectors on board. We present the performance and status of the TCD/BCD in flight.

Published
2019
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5. The ISS-CREAM Silicon Charge Detector for identification of the charge of cosmic rays up to Z = 26: Design, fabrication and ground-test performance

Author

G. Hong, S.C. Kang, J. F. Liang, S. Morton, Kwangmoo Kim, J.R. Smith, Y. Amare, O. Ofoha, L. Derome, R. Quinn, N. Picot-Clemente, J. T. Link, L. Eraud, L. Hagenau, S. I. Mognet, John Mitchell, J. H. Han, H. J. Kim, G.H. Choi, T. Mernik, HyoJung Hyun, Inkyu Park, M. Nester, Jong Moon Park, S. L. Nutter, Y.S. Hwang, H. B. Jeon, D. Angelaszek, Hyeyoung Lee, Arturo Alejandro Menchaca-Rocha, T. Anderson, K. Cheryian, S. Im, J. Wu, H. Park, P. Walpole, M. H. Lee, Y. S. Yoon, Joowon Lee, J.A. Jeon, S. Jeong, N. Anthony, M.H. Kim, L. Lutz, R.P. Weinmann, M. Copley, H.G. Huh, Eun-Suk Seo, L. Lu, S. Coutu, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)

Subjects
Silicon, Astrophysics::High Energy Astrophysical Phenomena, chemistry.chemical_element, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, International Space Station, Optics, 0103 physical sciences, Silicon Charge Detector, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Cosmic rays, Physics, Large Hadron Collider, 010308 nuclear & particles physics, business.industry, Detector, Astronomy and Astrophysics, Charge (physics), ISS-CREAM, chemistry, business, Beam (structure), Space environment
Abstract

International audience; The Cosmic Ray Energetics And Mass experiment for the International Space Station (ISS-CREAM) is a space-borne mission designed for the precision measurement of the energy and elemental composition of cosmic rays. The Silicon Charge Detector (SCD), placed at the top of the ISS-CREAM payload, consists of 4 layers. Each layer has 2688 silicon pixels and associated electronics arranged in such a fashion that its active detection area of 78.2 × 73.6 cm 2 is free of dead area. The foremost goal of the SCD is to efficiently and precisely measure the charge of cosmic rays passing through it. The 4-layer configuration was chosen to achieve the best precision in measuring the charge of cosmic rays within the constraints on the mass, volume and power allotted to it. The amount of material used for its support structure was minimized as well to reduce the chance of interactions of the cosmic ray within the structure. Given the placement of the SCD, its 4-layer configuration and the minimal amount of material in the cosmic-ray trajectory, the SCD is designed to measure the charge of cosmic rays ranging from protons to iron nuclei with excellent detection efficiency and charge resolution. We present the design and fabrication of the SCD as well as its performance during space environment tests which it underwent successfully. We also present its performance in charge measurement using heavy ions in a beam test at CERN, the European Organization for Nuclear Research.

Published
2019
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6. The boronated scintillator detector of the ISS-CREAM experiment

Author

O. Ofoha, Arturo Alejandro Menchaca-Rocha, M.H. Kim, R.P. Weinmann, J.R. Smith, M. Copley, John Mitchell, N. Picot-Clemente, T. Anderson, Y. Amare, S. L. Nutter, Hyeyoung Lee, J. H. Han, Inkyu Park, S. Jeong, H. J. Kim, K. Cheryian, M. Nester, P. Walpole, H. B. Jeon, Y.S. Hwang, G.H. Choi, H. Park, J.A. Jeon, J. F. Liang, H.G. Huh, S. Morton, L. Eraud, L. Hagenau, Kwangmoo Kim, L. Derome, S. Coutu, J. Wu, HyoJung Hyun, D. Angelaszek, R. Quinn, S. I. Mognet, Y. S. Yoon, Joowon Lee, M. H. Lee, N. Anthony, L. Lutz, Eun-Suk Seo, L. Lu, S.C. Kang, S. Im, J.T. Link, T. Mernik, Jong Moon Park, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
Physics, Nuclear and High Energy Physics, Range (particle radiation), Hydrogen, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, chemistry.chemical_element, Cosmic ray, Electron, Scintillator, 01 natural sciences, 7. Clean energy, Nuclear physics, chemistry, 13. Climate action, 0103 physical sciences, International Space Station, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Boron, 010303 astronomy & astrophysics, Instrumentation
Abstract

The Cosmic Ray Energetics And Mass for the International Space Station (ISS-CREAM) instrument is a next-generation experiment for the direct detection and study of cosmic-ray nuclei and electrons. With a long exposure in low Earth orbit, the experiment will determine the particle fluxes and spectral details of cosmic-ray nuclei from hydrogen to iron, over an energy range of about 1 0 12 eV to > 1 0 15 eV, and of cosmic-ray electrons over an energy range of about 5 × 1 0 10 eV to > 1 0 13 eV. The instrument was deployed to the ISS in August 2017 on the SpaceX CRS-12 mission. We review the design, implementation and performance of one of the ISS-CREAM detector systems: a boron loaded scintillation detector used in discriminating electron-induced events from the much more abundant cosmic-ray nuclei.

Published
2019
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7. A simulation study of Top and Bottom Counting Detectors in ISS-CREAM experiment for cosmic ray electron physics

Author

J.A. Jeon, Joowon Lee, H. B. Jeon, Hyeyoung Lee, S. L. Nutter, Y.S. Hwang, L. Lutz, L. Derome, N. Anthony, I.J. Howley, Eun-Suk Seo, HyoJung Hyun, H.G. Huh, M.H. Kim, J. T. Link, D. Angelaszek, L. Eraud, R.P. Weinmann, S.C. Kang, M. Copley, J.R. Smith, Arturo Alejandro Menchaca-Rocha, Y. Amare, M. H. Lee, D.Y. Kim, H. Park, B. Yon, H. Arnold, N. Picot-Clemente, Hyunghoon Kim, Jong Moon Park, C. Ebongue, I. Faddis, M. Nester, S. Coutu, O. Ofoha, Inkyu Park, G.H. Choi, John Mitchell, P. Walpole, J. H. Han, S. Im, J. Wu, T. Anderson, S. Jeong, P. King, Y. S. Yoon, J. F. Liang, S. Morton, Kwangmoo Kim, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
Atmospheric Science, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Physics::Medical Physics, satellite, cosmic radiation: energy, Aerospace Engineering, Cosmic ray, time-to-digital converter, Electron, 01 natural sciences, 7. Clean energy, Nuclear physics, Time-to-digital converter, Acceleration, TDC/BCD, 0103 physical sciences, International Space Station, propagation, Ultra-high-energy cosmic ray, electron p, 010306 general physics, e/p Separation, Cosmic rays, 0105 earth and related environmental sciences, Physics, energy: high, Detector, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, electron: cosmic radiation, Astronomy and Astrophysics, showers, acceleration, ISS-CREAM, Geophysics, Space and Planetary Science, gamma ray, GEANT, General Earth and Planetary Sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], CREAM
Abstract

International audience; The Cosmic Ray Energetics and Mass experiment at the International Space Station (ISS-CREAM) is developed for studying the origin, acceleration and propagation mechanism of high energy cosmic rays. The Top and Bottom Counting Detectors (TCD/BCD), sub-detectors of the ISS-CREAM instrument, are developed for electron/ γ -ray physics. The TCD/BCD help distinguish electrons from protons by comparing the hit and shower width distributions for electrons and protons. The e/p separation capability of the TCD/BCD is studied by using the GEANT3 simulation package, and optimal parameters for the e/p separation are obtained.

Published
2018
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8. Simulation Status of the Top and Bottom Counting Detectors for the ISS-CREAM Experiment

Author

J. T. Link, L. Derome, L. Hagenau, L. Eraud, T. Mernik, J. F. Liang, S. Morton, J. Wu, Y.S. Hwang, H. B. Jeon, Kwangmoo Kim, J.A. Jeon, M. H. Lee, Jong Moon Park, N Picot Clemente, Y. S. Yoon, S. L. Nutter, S. Coutu, H. Park, K. Cheryian, S. Im, Joowon Lee, HyoJung Hyun, N. Anthony, Eun-Suk Seo, Y. Amare, G.H. Choi, L. Lu, Inkyu Park, S. I. Mognet, P. Walpole, Hyeyoung Lee, John Mitchell, J. H. Han, O. Ofoha, S. Jeong, M.H. Kim, R.P. Weinmann, M. Copley, S.C. Kang, H.G. Huh, L. Lutz, T. Anderson, M. Nester, J.R. Smith, A Mechaca Rocha, H. J. Kim, D. Angelaszek, R. Quinn, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)

Subjects
Physics, 010504 meteorology & atmospheric sciences, Proton, Calorimeter (particle physics), business.industry, Detector, Cosmic ray, Scintillator, 01 natural sciences, 7. Clean energy, Photodiode, law.invention, Optics, law, 0103 physical sciences, International Space Station, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], business, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Space environment
Abstract

International audience; The Cosmic-Ray Energetics And Mass (CREAM) instrument for the International Space Station (ISS) is a detector for studying the origin, acceleration and propagation mechanism of high-energy cosmic rays. The ISS-CREAM instrument is scheduled to launch in 2017 to the ISS. The Top and Bottom Counting Detectors (TCD/BCD) are designed for studying electron and gamma-ray physics. The TCD/BCD are composed of a plastic scintillator and an array of photodiodes The active detection areas of the TCD/BCD are 500 $\times$ 500 mm$^2$ and 600 $\times$ 600 mm$^2$, respectively. The TCD/BCD were completed in 2015 and passed the environmental tests for safety in a space environment. After finishing these tests, the TCD/BCD were integrated with the payload. The TCD is located between the carbon target of the ISS-CREAM instrument and the calorimeter, and the BCD is located below the calorimeter. The TCD/BCD can distinguish between electrons and protons by using the different shapes between electromagnetic and hadronic showers in the high-energy region. We study the TCD/BCD performance in various energy ranges by using GEANT3 simulation data. Here, we present the status of the electron and proton separation study with the TCD/BCD simulation.

Published
2017
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9. The Grenoble Analysis Toolkit (GreAT)—A statistical analysis framework

Author

A. Putze, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, Evolutionary algorithm, Context (language use), 01 natural sciences, Field (computer science), Computational science, symbols.namesake, 0103 physical sciences, Cosmic-ray physics, Markov Chain Monte Carlo, Statistical physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astroparticle physics, Physics, 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, Markov chain Monte Carlo, Modular design, Object (computer science), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Statistical analysis, Space and Planetary Science, symbols, business, Fermi Gamma-ray Space Telescope
Abstract

The field of astroparticle physics is currently the focus of prolific scientific activity. In the last decade, this field has undergone significant developments thanks to several experimental results from CREAM, PAMELA, Fermi, and H.E.S.S. Moreover, the next generation of instruments, such as AMS-02 (launched on 16 May 2011) and CTA, will undoubtedly facilitate more sensitive and precise measurements of the cosmic-ray and γ -ray fluxes. To fully exploit the wealth of high precision data generated by these experiments, robust and efficient statistical tools such as Markov Chain Monte Carlo algorithms or evolutionary algorithms, able to handle the complexity of joint parameter spaces and datasets, are necessary for a phenomenological interpretation. The Grenoble Analysis Toolkit (GreAT) is an user-friendly and modular object orientated framework in C++, which samples the user-defined parameter space with a pre- or user-defined algorithm. The functionality of GreAT is presented in the context of cosmic-ray physics, where the boron-to-carbon (B/C) ratio is used to constrain cosmic-ray propagation models.

Published
2014
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10. Measurement of delayed fluorescence in plastic scintillator from 1 to 10 μs

Author

N. Picot-Clemente, M.H. Kim, R.P. Weinmann, S.C. Kang, M. Copley, H.G. Huh, L. Eraud, L. Hagenau, J. Wu, Inkyu Park, G.H. Choi, H. B. Jeon, S. I. Mognet, Y. S. Yoon, D. Angelaszek, Y.S. Hwang, HyoJung Hyun, S. Coutu, Y. Amare, J.T. Link, Joowon Lee, S. Im, T. Anderson, K. Cheryian, M. H. Lee, N. Anthony, J.R. Smith, O. Ofoha, L. Lutz, L. Derome, S. L. Nutter, Eun-Suk Seo, John Mitchell, J.A. Jeon, T. Mernik, L. Lu, H Y. Lee, Jong Moon Park, J. H. Han, S. Jeong, M. Nester, H. J. Kim, R. Quinn, P. Walpole, J. F. Liang, S. Morton, Kwangmoo Kim, Arturo Alejandro Menchaca-Rocha, H. Park, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)

Subjects
Plastic scintillator, [PHYS]Physics [physics], Physics, Nuclear and High Energy Physics, Muon, 010308 nuclear & particles physics, Scintillator, 01 natural sciences, 7. Clean energy, Fluorescence, Delayed fluorescence, Charged particle, Particle shower, Rise time, 0103 physical sciences, Light emission, Cosmic ray detector, Atomic physics, Nucleus and electron detector, 010303 astronomy & astrophysics, Instrumentation, Excitation
Abstract

The time dependence of the relative light emission of Eljen Technology EJ-200 polyvinyltoluene-based plastic scintillator was measured between 1 and 10 μ s after the passage of a particle shower, a singly charged particle (atmospheric muon), and with a UV LED exciting the fluor. This was compared in magnitude to the integrated response for the prompt light (within 500 ns of excitation). A model with a time-dependent yield consisting of three exponentially decaying components (fast, medium, and slow) was developed to fit the data. Note that the exact time structure of early ( 1 μ s ) light emission was not measured for individual components, only for all three components together This model assumes all three components share the same rise time. The decay time constants of the fast, medium and slow components are, respectively, 7.8 ns, 490 ns, and 2370 ns. The relative total normalized yields for each component are: fast 95.8%, medium 2.2%, and slow 2.0%.

Published
2019
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11. Cosmic ray solar modulation and Forbush decrease analyses based on atmospheric neutron spectrometry at mountain altitude and GEANT4 simulations of extensive air showers

Author

Guillaume Hubert, L. Derome, V. Lacoste, A. Cheminet, and David Maurin

Subjects
Bonner sphere, Physics, Neutron monitor, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics, 01 natural sciences, Nuclear physics, Geophysics, Earth's magnetic field, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Coronal mass ejection, Forbush decrease, Neutron, 010303 astronomy & astrophysics, Zenith, 0105 earth and related environmental sciences
Abstract

[1] A Bonner sphere spectrometer extended to high energies (HERMEIS) was set up at the summit of the Pic du Midi de Bigorre in the French Pyrenees (altitude: +2,885 m; geomagnetic cutoff: 5.6 GV) in May 2011. The spectral fluence rate distribution of the cosmic ray induced neutrons was continuously measured over a broad energy range from meV up to several GeV and with a 1 h time resolution. While the Sun's activity was increasing and reaching its 24th maximum in the 11 year solar cycle, some Forbush decreases were observed in the atmospheric secondary radiation at mountain altitude. We investigated the evolution of the cascade fluence rate (i.e., neutrons with energy greater than 20 MeV) during the March 2012 events with a series of strong coronal mass ejections hitting the Earth's magnetosphere. The amplitude of the greatest Forbush decrease peaked at 10%. Then, a simulation work based on the GEANT4 toolkit was carried out to quantify the solar modulation induced on the galactic cosmic ray transportation during these events. We performed calculations of extensive air showers generated by monoenergetic primaries (Hydrogen and Helium nuclei) for several zenith incidences. Hence, a complete database was built and validated. We derived an analytical model to estimate the atmospheric neutron spectrum at the Pic du Midi according to primary spectra which only depend on the solar modulation potential (force field approximation). We compared the solar modulation potentials obtained in March 2012 with the ones derived by the neutron monitor yield method. Finally, a satisfying agreement was found.

Published
2013
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12. Performance of the BACCUS Transition Radiation Detector

Author

J. Wu, Y. S. Yoon, Arturo Alejandro Menchaca-Rocha, Joowon Lee, Eun-Suk Seo, L. Lu, O. Ofoha, S. I. Mognet, N. Anthony, L. Hagenau, Inkyu Park, J.R. Smith, J. T. Link, Hyeyoung Lee, L. Eraud, K. Cheryian, J.A. Jeon, M. Nester, S. Jeong, S. Coutu, Y. Amare, N. Picot-Clemente, P. Walpole, S. Im, John Mitchell, J. H. Han, R. Quinn, L. Derome, M. H. Lee, G.H. Choi, S. L. Nutter, J. F. Liang, S. Morton, Kwangmoo Kim, H.G. Huh, M.H. Kim, R.P. Weinmann, M. Copley, L. Lutz, T. Anderson, T. Mernik, D. Angelaszek, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
Physics, Large Hadron Collider, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Electron, 01 natural sciences, 7. Clean energy, Nuclear physics, Transition radiation detector, Lorentz factor, symbols.namesake, Pion, 13. Climate action, 0103 physical sciences, symbols, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Detectors and Experimental Techniques, 010303 astronomy & astrophysics, Stratosphere, 0105 earth and related environmental sciences
Abstract

International audience; The Boron And Carbon Cosmic rays in the Upper Stratosphere (BACCUS) balloon-borne exper-iment flew for 30 days over Antarctica in December 2016. It is the successor of the CREAMballoon program in Antarctica which recorded a total cumulative exposure of 161 days. BAC-CUS is primarily aimed to measure cosmic-ray boron and carbon fluxes at the highest energiesreachable with a balloon or satellite experiment, in order to provide essential information for abetter understanding of cosmic-ray propagation in the Galaxy. The payload is made of multipleparticle physics detectors which measure the charge up to Z=26 and energy of incident particlesfrom a few hundred GeV to a few PeV. The newly designed Transition Radiation Detector (TRD)measures signals that are a function of the charge and Lorentz factor. In April 2016, BACCUSwas taken to CERN in its flight configuration to characterize its detectors’ response to beams ofelectrons and pions. The performance of the TRD using beam test data are reported in this paper.

Published
2017
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13. Non-parametric determination of H and He interstellar fluxes from cosmic-ray data

Author

A. Ghelfi, L. Derome, David Maurin, F. Barao, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astroparticle physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Nonparametric statistics, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Markov chain Monte Carlo, Astrophysics, Approx, 01 natural sciences, Computational physics, High Energy Physics - Phenomenology, symbols.namesake, Flux (metallurgy), High Energy Physics - Phenomenology (hep-ph), 13. Climate action, Space and Planetary Science, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], 0103 physical sciences, symbols, Relative precision, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

Top-of-atmosphere (TOA) cosmic-ray (CR) fluxes from satellites and balloon-borne experiments are snapshots of the solar activity imprinted on the interstellar (IS) fluxes. Given a series of snapshots, the unknown IS flux shape and the level of modulation (for each snapshot) can be recovered. We wish (i) to provide the most accurate determination of the IS H and He fluxes from TOA data alone, (ii) to obtain the associated modulation levels (and uncertainties) while fully accounting for the correlations with the IS flux uncertainties, and (iii) to inspect whether the minimal force-field approximation is sufficient to explain all the data at hand. Using H and He TOA measurements, including the recent high-precision AMS, BESS-Polar, and PAMELA data, we performed a non-parametric fit of the IS fluxes $J^{\rm IS}_{\rm H,~He}$ and modulation level $\phi_i$ for each data-taking period. We relied on a Markov chain Monte Carlo (MCMC) engine to extract the probability density function and correlations (hence the credible intervals) of the sought parameters. Although H and He are the most abundant and best measured CR species, several datasets had to be excluded from the analysis because of inconsistencies with other measurements. From the subset of data passing our consistency cut, we provide ready-to-use best-fit and credible intervals for the H and He IS fluxes from MeV/n to PeV/n energy (with a relative precision in the range [2-10\%] at 1$\sigma$). Given the strong correlation between $J^{\rm IS}$ and $\phi_i$ parameters, the uncertainties on $J^{\rm IS}$ translate into $\Delta\phi\approx \pm 30$~MV (at 1$\sigma$) for all experiments. We also find that the presence of $^3$He in He data biases $\phi$ towards higher $\phi$ values by $\sim 30$~MV. The force-field approximation gives an excellent ($\chi^2/$dof$=1.02$) description of the recent high-precision TOA H and He fluxes., Comment: 10 pages, 5 figures, 3 tables (matches A&A accepted version) + Erratum for Eq. (8) and Table 3 (submitted to A&A)

Published
2016
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14. In-beam aerogel light yield characterization for the AMS RICH detector

Author

Eun-Suk Seo, P. Goncalves, Bruny Baret, Arturo Alejandro Menchaca-Rocha, M. Pimenta, M. Aguilar-Benitez, G. Laurenti, J. Berdugo, G.P. Barreira, I. Cernuda, Rui Miguel Faisca Rodrigues Pereira, Fernando Barão, M. Vargas-Trevino, C. de la Guia, A. Keating, F. Giovacchini, G. Martinez, D. Crespo, C. Delgado, A. Malinine, A. Barrau, L. Derome, M. Buénerd, J. Marín, Luísa Arruda, J. Casaus, C. Maña, Carlos Díaz, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Nuclear and High Energy Physics, Photomultiplier, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Instrumentation and Detectors, Reflector (antenna), 01 natural sciences, Optics, 0103 physical sciences, Aerogel light yield, AMS, 010306 general physics, RICH, Instrumentation, Cherenkov radiation, Aerogel, Physics, Spectrometer, 010308 nuclear & particles physics, business.industry, Detector, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space instrumentation, Cherenkov imaging, Radiator (engine cooling), High Energy Physics::Experiment, business, Charged particle detectors, Beam (structure)
Abstract

The ring imaging Cherenkov (RICH) detector of the AMS-02 spectrometer provides a very precise measurement of the electric charge and velocity. The RICH detector is composed of a conical reflector ended on top by a dual radiator plane made of sodium fluoride and aerogel, and at the bottom by a detector plane made of pixelized photomultipliers. The vast majority of the events ( ∼ 90 % ) that are collected in the RICH cross the aerogel radiator. Therefore, the choice and characterization of the aerogel radiator is essential for reaching the design goals. A prototype of the RICH detector was built for both concept proof and testing of the different elements. Beam tests with the RICH prototype and using several aerogel radiator samples were performed at CERN in 2002 and 2003. This note summarizes the method used and the results obtained for the light yield of different aerogel samples.

Published
2010
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15. UCTM2: An updated User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics

Author

O. Bourrion, B. Boyer, L. Derome, G. Pignol, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, 010308 nuclear & particles physics, 0103 physical sciences, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, 01 natural sciences, Instrumentation
Abstract

We developed a highly integrated and versatile electronic module to equip small nuclear physics experiments and lab teaching classes: the User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics (UCTM). It is configurable through a Graphical User Interface (GUI) and provides a large number of possible trigger conditions without any Hardware Description Language (HDL) required knowledge. This new version significantly enhances the previous capabilities by providing two additional features: signal digitization and time measurements. The design, performances and a typical application are presented., Comment: 14 pages, 9 figures. arXiv admin note: text overlap with arXiv:1110.2917

Published
2016
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16. Improvement in the shot noise of a laser interferometer gravitational wave detector by means of an output mode-cleaner

Author

R. Hermel, R. Flaminio, F Moreau, L. Massonnet, A. Masserot, D. Verkindt, F. Beauville, D. Buskulic, F. Marion, L. Derome, J. Ramonet, A. Dominjon, M. Yvert, E. Tournefier, B. Mours, Olivier Veziant, P Mugnier, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and VIRGO

Subjects
Physics, Atom interferometer, Gravitational-wave observatory, Physics and Astronomy (miscellaneous), 010308 nuclear & particles physics, business.industry, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Shot noise, 01 natural sciences, law.invention, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010309 optics, Interferometry, Optics, law, Optical cavity, 0103 physical sciences, 04.80.Nn, 95.55.Ym, Astronomical interferometer, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], business, Noise (radio)
Abstract

The sensitivity of a gravitational wave detector based on a laser interferometer is limited by photon shot noise for signals with frequencies above a few hundred hertz. The amplitude of this noise depends on the interferometer fringe contrast. By means of a complete simulation, we show that using a short optical cavity placed at the interferometer output port, the contrast can be significantly improved and the optimal sensitivity recovered. Such an output mode-cleaner has been realized and tested. The adopted design and the results of the tests are presented.

Published
2006
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17. Virgo: a laser interferometer to detect gravitational waves

Author

Tjeerd Ketel, Antonio Eleuteri, M. Parisi, R. Passaquieti, L. Di Fiore, B. Mours, A. Królak, M. Blom, F. Beauville, K. G. Arun, G. A. Prodi, R. DeSalvo, M. Barsuglia, Gianpietro Cagnoli, Gianluca Persichetti, V. Granata, Julien Moreau, B. Mansoux, D. Verkindt, G. Losurdo, Anna Dari, M. Doets, B. Canuel, F. Piergiovanni, G. Ballardin, T Maiani, L. Giacobone, Y. Minenkov, M. Pietka, Patrice Hello, E. Turri, X Grave, R. Morand, L. Bonelli, M. Davier, G. Pagliaroli, I. Maksimovic, J. Marque, R. L. Ward, R. Hermel, G. Hemming, A. Masserot, Marco G. Tarallo, F. Vetrano, M. A. Mazzoni, L. Journet, O Lodygensky, J. P. Zendri, F. Nocera, G. Vedovato, V. Loriette, G. Barrand, P. N. Y. David, István Rácz, D. Boget, Ludovico Carbone, P. Popolizio, C Drezen, D. Passuello, C. Palomba, V Reita, Piotr Jaranowski, J.-M. Mackowski, Antoine Heidmann, Lisa Barsotti, Riccardo Sturani, Shourov Chatterji, Sofiane Aoudia, C. Arnault, Fausto Acernese, Andreas Freise, A. Di Virgilio, A. Giazotto, F. Mul, Alessandra Toncelli, G. Parguez, L. Brocco, Claude Boccara, J-Y. Vinet, I. Ferrante, S. Hamdani, R. Sottile, F. Cleva, M. Mantovani, Samuele Cortese, C Garnier, M. Lorenzini, V. Dattilo, S. D'Antonio, T. Bouedo, F. Travasso, R. Gouaty, Michał Bejger, Alessandra Corsi, L. Giordano, Mauro Tonelli, L. A. Forte, A. Dietz, M. Alshourbagy, M. Granata, L. Derome, L. Fabbroni, E. Genin, G. Cella, R. Bilhaut, L. Taffarello, A. Grado, J. L. Beney, B Dujardin, V. Fafone, R. Del Fabbro, M. Punturo, Andrea Chincarini, G. Gemme, M. Drago, P. Amico, P. Ganau, M. Galimberti, P. La Penna, F. Raffaelli, Eric Hennes, A. Pasqualetti, M. G. Beker, S. Petit, M. Pichot, Enrico Calloni, N. Liguori, L. Salconi, O. Veziant, V. Re, Guido Russo, Mirko Prato, C. Bradaschia, M. Dehamme, G. De Carolis, P. Dominici, L Matone, L. Holloway, F. Antonucci, Saverio Avino, O. Francois, A. Chiummo, Luca Gammaitoni, A. Paoli, F. Moreau, N. Leroy, B. L. Swinkels, F. Marion, F. Ricci, B. Dulach, D. Sentenac, G. Debreczeni, B. Lagrange, P. Puppo, Maurizio Ripepe, R. Paoletti, M. Loupias, F. Fidecaro, G. M. Guidi, E. Chassande-Mottin, S. Kreckelbergh, M. E. Gáspár, B. Lieunard, V. Moscatelli, K. Yamamoto, A. Brillet, M. Del Prete, Igor Neri, N. Letendre, L. Bosi, B. Bouhou, L. Pinard, C. Girard, T. Accadia, L. Naticchioni, Salvatore Vitale, M Laval, H Voet, F. Richard, P. Astone, M. Perciballi, Tania Regimbau, S. Frasca, M. Branchesi, R. Cavalieri, H. J. Bulten, L. Massonnet, L. Palladino, R. De Rosa, V. Malvezzi, A. Colla, A. Morgia, F. Frasconi, A. Basti, J. F. J. van den Brand, R. Flaminio, S. Birindelli, Tenglin Li, Archana Pai, F. Paoletti, P. Ruggi, S. Mancini, M. Iannarelli, S. Braccini, M. Tacca, D. Babusci, J.-P. Coulon, D. Jehanno, B. Sassolas, J. C. Lacotte, A Dominjon, L. Sperandio, A. C. Clapson, G. Conforto, F. Garufi, A. Viceré, H Groenstege, Andrea Gaddi, J.-D. Fournier, L. Rolland, Fabrizio Barone, C. Buy, I. Kowalska, Marie-Anne Bizouard, M. Bebronne, J. Franc, C. Michel, N. Morgado, J. C. Le Marec, V Sannibale, J. Colas, Ettore Majorana, G. Gennaro, P. Marin, M. Yvert, A. Rocchi, C. Eder, E. Campagna, P. Roudier, Fabio Marchesoni, R. Taddei, N. Arnaud, G. Daguin, J. L. Montorio, I. Fiori, R Pignard, R. Day, V. Boschi, Luisa Bracci, Roberto Cecchi, Tristan Briant, P. Rapagnani, M. Mohan, N. Man, S. Hebri, Nelson Christensen, A Remilleux, E. Tournefier, F. Cavalier, Matthew Evans, Stefano Bigotta, Ketevan Qipiani, C. Magazzù, Silvio Pardi, O. Torre, O. Rabaste, Leopoldo Milano, C. Tremola, M. Bitossi, A. Di Lieto, A. Reboux, E. Cuoco, S. Rapisarda, T. Pradier, D. Rosińska, M. Vasúth, Salvatore Solimeno, D. Enard, Elena Cesarini, B. Lopez, J. F. Hayau, E. Coccia, F. Robinet, G. Calamai, C. N. Colacino, Joseph M. Kovalik, V. Brisson, G. Matone, C. Van Den Broeck, B. Perniola, M. Was, Ruggero Stanga, S Tissot, Maria Grazia Bernardini, Ph Heusse, D. Buskulic, Zhenyu Zhang, C. Greverie, Rosa Poggiani, R. Chiche, H. Vocca, S. Karkar, A. Gennai, P. Mugnier, Simona Mosca, M. Vavoulidis, S. Vilalte, S. Van Der Putten, Tomasz Bulik, L. Fournier, Th. S. Bauer, François Bondu, G. Giordano, M. Colombini, Francesco Cottone, F. Bellachia, G. Vajente, D. Forest, A. Belletoile, W. Del Pozzo, P. F. Cohadon, H. Heitmann, D. S. Rabeling, Rocco Romano, M. Dialinas, F. Menzinger, Iolanda Ricciardi, F. Carbognani, M. Di Paolo Emilio, A. Bozzi, D. Huet, H Fang, R. Bonnand, E Pacaud, F. Martelli, S Mitra, Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, T., Accadia, F., Acernese, M., Alshourbagy, P., Amico, F., Antonucci, S., Aoudia, N., Arnaud, C., Arnault, K. G., Arun, P., Astone, S., Avino, D., Babusci, G., Ballardin, F., Barone, G., Barrand, L., Barsotti, M., Barsuglia, A., Basti, Th S., Bauer, F., Beauville, M., Bebronne, M., Bejger, M. G., Beker, F., Bellachia, A., Belletoile, J. L., Beney, M., Bernardini, S., Bigotta, R., Bilhaut, S., Birindelli, M., Bitossi, M. A., Bizouard, M., Blom, C., Boccara, D., Boget, F., Bondu, L., Bonelli, R., Bonnand, V., Boschi, L., Bosi, T., Bouedo, B., Bouhou, A., Bozzi, L., Bracci, S., Braccini, C., Bradaschia, M., Branchesi, T., Briant, A., Brillet, V., Brisson, L., Brocco, T., Bulik, H. J., Bulten, D., Buskulic, C., Buy, G., Cagnoli, G., Calamai, Calloni, Enrico, E., Campagna, B., Canuel, F., Carbognani, L., Carbone, F., Cavalier, R., Cavalieri, R., Cecchi, G., Cella, E., Cesarini, E., Chassande Mottin, S., Chatterji, R., Chiche, A., Chincarini, A., Chiummo, N., Christensen, A. C., Clapson, F., Cleva, E., Coccia, P. F., Cohadon, C. N., Colacino, J., Cola, A., Colla, M., Colombini, G., Conforto, A., Corsi, S., Cortese, F., Cottone, J. P., Coulon, E., Cuoco, S., D'Antonio, G., Daguin, A., Dari, V., Dattilo, P. Y., David, M., Davier, R., Day, G., Debreczeni, G., De Caroli, M., Dehamme, R., Del Fabbro, W., Del Pozzo, M., del Prete, L., Derome, DE ROSA, Rosario, R., Desalvo, M., Dialina, L., Di Fiore, A., Di Lieto, M., Di Paolo Emilio, A., Di Virgilio, A., Dietz, M., Doet, P., Dominici, A., Dominjon, M., Drago, C., Drezen, B., Dujardin, B., Dulach, C., Eder, A., Eleuteri, D., Enard, M., Evan, L., Fabbroni, V., Fafone, H., Fang, I., Ferrante, F., Fidecaro, I., Fiori, R., Flaminio, D., Forest, Forte, LUCA ANTONIO, J. D., Fournier, L., Fournier, J., Franc, O., Francoi, S., Frasca, F., Frasconi, A., Freise, A., Gaddi, M., Galimberti, L., Gammaitoni, P., Ganau, C., Garnier, Garufi, Fabio, M. E., Gáspár, G., Gemme, E., Genin, A., Gennai, G., Gennaro, L., Giacobone, A., Giazotto, G., Giordano, L., Giordano, C., Girard, R., Gouaty, A., Grado, M., Granata, V., Granata, X., Grave, C., Greverie, H., Groenstege, G. M., Guidi, S., Hamdani, J. F., Hayau, S., Hebri, A., Heidmann, H., Heitmann, P., Hello, G., Hemming, E., Henne, R., Hermel, P., Heusse, L., Holloway, D., Huet, M., Iannarelli, P., Jaranowski, D., Jehanno, L., Journet, S., Karkar, T., Ketel, H., Voet, J., Kovalik, I., Kowalska, S., Kreckelbergh, A., Krolak, J. C., Lacotte, B., Lagrange, P., La Penna, M., Laval, J. C., Le Marec, N., Leroy, N., Letendre, T. G. F., Li, B., Lieunard, N., Liguori, O., Lodygensky, B., Lopez, M., Lorenzini, V., Loriette, G., Losurdo, M., Loupia, J. M., Mackowski, T., Maiani, E., Majorana, C., Magazzù, I., Maksimovic, V., Malvezzi, N., Man, S., Mancini, B., Mansoux, M., Mantovani, F., Marchesoni, F., Marion, P., Marin, J., Marque, F., Martelli, A., Masserot, L., Massonnet, G., Matone, L., Matone, M., Mazzoni, F., Menzinger, C., Michel, Milano, Leopoldo, Y., Minenkov, S., Mitra, M., Mohan, J. L., Montorio, R., Morand, F., Moreau, J., Moreau, N., Morgado, A., Morgia, S., Mosca, V., Moscatelli, B., Mour, P., Mugnier, F. A., Mul, L., Naticchioni, I., Neri, F., Nocera, E., Pacaud, G., Pagliaroli, A., Pai, L., Palladino, C., Palomba, F., Paoletti, R., Paoletti, A., Paoli, S., Pardi, G., Parguez, M., Parisi, A., Pasqualetti, R., Passaquieti, D., Passuello, M., Perciballi, B., Perniola, G., Persichetti, S., Petit, M., Pichot, F., Piergiovanni, M., Pietka, R., Pignard, L., Pinard, R., Poggiani, P., Popolizio, T., Pradier, M., Prato, G. A., Prodi, M., Punturo, P., Puppo, K., Qipiani, O., Rabaste, D. S., Rabeling, I., Rácz, F., Raffaelli, P., Rapagnani, S., Rapisarda, V., Re, A., Reboux, T., Regimbau, V., Reita, A., Remilleux, F., Ricci, I., Ricciardi, F., Richard, M., Ripepe, F., Robinet, A., Rocchi, L., Rolland, R., Romano, D., Rosińska, P., Roudier, P., Ruggi, Russo, Guido, L., Salconi, V., Sannibale, B., Sassola, D., Sentenac, S., Solimeno, R., Sottile, L., Sperandio, R., Stanga, R., Sturani, B., Swinkel, M., Tacca, R., Taddei, L., Taffarello, M., Tarallo, S., Tissot, A., Toncelli, M., Tonelli, O., Torre, E., Tournefier, F., Travasso, C., Tremola, E., Turri, G., Vajente, J. F. J., van den Brand, C., Van Den Broeck, S., van der Putten, M., Vasuth, M., Vavoulidi, G., Vedovato, D., Verkindt, F., Vetrano, O., Véziant, A., Viceré, J. Y., Vinet, S., Vilalte, S., Vitale, H., Vocca, R. L., Ward, M., Wa, K., Yamamoto, M., Yvert, J. P., Zendri, Z., Zhang, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), (Astro)-Particles Physics, Mathematical Analysis, Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Max-Planck-Gesellschaft-Max-Planck-Gesellschaft

Subjects
Gravitational-wave observatory, PROTOTYPE, 01 natural sciences, SCATTERED-LIGHT NOISE, law.invention, Detection of gravitational wave, interferometers, law, Instrumentation, gravitational wave, Mathematical Physics, ComputingMilieux_MISCELLANEOUS, Physics, SEISMIC NOISE, Detector, SUPER ATTENUATOR, Settore FIS/01 - Fisica Sperimentale, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Interferometry, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 1ST, SUSPENSION, Gravitational waves, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Optics, Suspensions, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Detection theory, Gravitational Waves, Interferometric Detector, Electronics, 010306 general physics, 010308 nuclear & particles physics, business.industry, Gravitational wave, Lasers, Michelson interferometer, PERFORMANCE, Antennas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Sensitivity (electronics), SHOT-NOISE, SYSTEM, PENDULUM
Abstract

This paper presents a complete description of Virgo, the French-Italian gravitational wave detector. The detector, built at Cascina, near Pisa (Italy), is a very large Michelson interferometer, with 3 km-long arms. In this paper, following a presentation of the physics requirements, leading to the specifications for the construction of the detector, a detailed description of all its different elements is given. These include civil engineering infrastructures, a huge ultra-high vacuum (UHV) chamber (about 6000 cubic metres), all of the optical components, including high quality mirrors and their seismic isolating suspensions, all of the electronics required to control the interferometer and for signal detection. The expected performances of these different elements are given, leading to an overall sensitivity curve as a function of the incoming gravitational wave frequency. This description represents the detector as built and used in the first data-taking runs. Improvements in different parts have been and continue to be performed, leading to better sensitivities. These will be detailed in a forthcoming paper. © 2012 IOP Publishing Ltd and Sissa Medialab srl.

Published
2012
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18. Simulation of cosmic Be isotopes detected by the RICH in AMS on the ISS

Author

A. Bouchet, L. Derome, M. Buenerd, T. Thuillier, Arturo Alejandro Menchaca-Rocha, bibliotheque, LPSC, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics, Nuclear and High Energy Physics, COSMIC cancer database, Isotope, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, 0103 physical sciences, 010306 general physics, 01 natural sciences, Astrobiology
Published
2001
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19. Constraining Galactic cosmic-ray parameters with Z<=2 nuclei

Author

A. Putze, L. Derome, B. Coste, David Maurin, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astroparticle physics, Physics, High energy, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astronomy and Astrophysics, Markov chain Monte Carlo, Probability density function, Cosmic ray, Astrophysics, 01 natural sciences, 7. Clean energy, Astrophysics - Astrophysics of Galaxies, Interstellar medium, symbols.namesake, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Simulated data, 0103 physical sciences, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Diffusion (business), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

The secondary-to-primary B/C ratio is widely used to study Galactic cosmic-ray propagation processes. The 2H/4He and 3He/4He ratios probe a different Z/A regime, therefore testing the `universality' of propagation. We revisit the constraints on diffusion-model parameters set by the quartet (1H, 2H, 3He, 4He), using the most recent data as well as updated formulae for the inelastic and production cross-sections. The analysis relies on the USINE propagation package and a Markov Chain Monte Carlo technique to estimate the probability density functions of the parameters. Simulated data are also used to validate analysis strategies. The fragmentation of CNO cosmic rays (resp. NeMgSiFe) on the ISM during their propagation contributes to 20% (resp. 20%) of the 2H and 15% (resp. 10%) of the 3He flux at high energy. The C to Fe elements are also responsible for up to 10% of the 4He flux measured at 1 GeV/n. The analysis of 3He/4He (and to a less extent 2H/4He) data shows that the transport parameters are consistent with those from the B/C analysis: the diffusion model with delta~0.7 (diffusion slope), Vc~20 km/s (galactic wind), Va~40 km/s (reacceleration) is favoured, but the combination delta~0.2, Vc~0, and Va~80 km/s is a close second. The confidence intervals on the parameters show that the constraints set by the quartet data are competitive with those brought by the B/C data. These constraints are tighter when adding the 3He (or 2H) flux measurements, and the tightest when further adding the He flux. For the latter, the analysis of simulated and real data show an increased sensitivity to biases. Using secondary-to-primary ratio along with a loose prior on the source parameters is recommended to get the most robust constraints on the transport parameters., Comment: 17 pages, 7 tables, 20 figures (submitted to A&A)

Published
2011
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20. Design and construction of a Cherenkov imager for charge measurement of nuclear cosmic rays

Author

M. Marton, M. Brinet, D. Grondin, J.-P. Scordilis, Y. Sallaz-Damaz, B. Boyer, L. Lutz, Antje Putze, D. Fombaron, L. Derome, O. Bourrion, Y. S. Yoon, M. Buenerd, Jerome Bouvier, J.N. Périé, L. Eraud, J. L. Bouly, Eun-Suk Seo, A. Pelissier, Moo Hyun Lee, D. Bondoux, R. Foglio, A. Menchaca-Rocha, Ch. Bernard, S. Roudier, G. Damieux, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Institut Clément Ader (ICA), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-IMT École nationale supérieure des Mines d'Albi-Carmaux (IMT Mines Albi), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), CREAM, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-IMT École nationale supérieure des Mines d'Albi-Carmaux (IMT Mines Albi), and Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO)

Subjects
Photomultiplier, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, 01 natural sciences, Effective nuclear charge, Optics, 0103 physical sciences, CHERCAM, 010303 astronomy & astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), RICH, Mathematical Physics, Cherenkov radiation, Physics, Range (particle radiation), 010308 nuclear & particles physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Charge (physics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Radiator (engine cooling), business, Astrophysics - Instrumentation and Methods for Astrophysics, CREAM
Abstract

A proximity focusing Cherenkov imager called CHERCAM, has been built for the charge measurement of nuclear cosmic rays with the CREAM instrument. It consists of a silica aerogel radiator plane across from a detector plane equipped with 1,600 1" diameter photomultipliers. The two planes are separated by a ring expansion gap. The Cherenkov light yield is proportional to the charge squared of the incident particle. The expected relative light collection accuracy is in the few percents range. It leads to an expected single element separation over the range of nuclear charge Z of main interest 1 < Z < 26. CHERCAM is designed to fly with the CREAM balloon experiment. The design of the instrument and the implemented technical solutions allowing its safe operation in high altitude conditions (radiations, low pressure, cold) are presented., 24 pages, 19 figures

Published
2011
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21. UCTM: A User friendly Configurable Trigger, scaler and delay Module for nuclear and particle physics

Author

O. Bourrion, Guillaume Pignol, B. Boyer, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Particle physics, Physics - Instrumentation and Detectors, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], FOS: Physical sciences, 01 natural sciences, [PHYS.PHYS.PHYS-ED-PH]Physics [physics]/Physics [physics]/Physics Education [physics.ed-ph], Physics Education (physics.ed-ph), 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Digitization, computer.programming_language, Graphical user interface, Physics, User Friendly, 010308 nuclear & particles physics, business.industry, Hardware description language, SIGNAL (programming language), Physics - Physics Education, Instrumentation and Detectors (physics.ins-det), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, business, computer
Abstract

A configurable trigger scaler and delay NIM module has been designed to equip nuclear physics experiments and lab teaching classes. It is configurable through a Graphical User Interface (GUI) and provides a large number of possible trigger conditions without any Hardware Description Language (HDL) required knowledge. The design, performances and typical applications are presented., Comment: 11 pages, 10 figures

Published
2011
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22. Characterization study of silica aerogel for Cherenkov imaging

Author

C. Matteuzzi, M. Mangin-Brinet, A. Ortiz-Velàsquez, T. Bellunato, M. Vargas-Trevino, H. Léon-Vargas, L. Derome, A. Putze, M. Loth, O. Veziant, D. L. Perego, M. Buénerd, Y. Sallaz-Damaz, E. Belmont, A. Malinine, K.V. Protasov, M. Vargas-Magaña, Rui Miguel Faisca Rodrigues Pereira, Fernando Barão, Arturo Alejandro Menchaca-Rocha, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Accuracy and precision, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 01 natural sciences, Optics, Deflection (engineering), 0103 physical sciences, 010306 general physics, Instrumentation, Cherenkov radiation, Physics, 010308 nuclear & particles physics, business.industry, Detector, Cherenkov detectors, Ring imaging, Metrology, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Refractive index uniformity, Transverse plane, Silica aerogels, visual_art, visual_art.visual_art_medium, Tile, business, Refractive index
Abstract

Different methods to measure the characteristics of silica aerogel tiles used as Cherenkov radiator in the CREAM and AMS experiments have been investigated to optimize the detector performances. The measurement accuracy dictated by the physics objectives on the velocity and charge resolutions set stringent requirements on the aerogel refractive index determination, namely Δ n ∼ 1.5 × 10 − 4 and Δ n ∼ 5 × 10 − 4 for the AMS and CREAM imagers, respectively. The matching of such accuracies for this material turned out to be a metrological challenge, and finally led to a full R&D program, to develop an appropriate characterization procedure. Preliminary studies performed with a standard refractive index measurement technique (laser beam deviation by a prism) have revealed a significant systematic index nonuniformity for the AMS tiles at a level ( 10 − 3 ) , not acceptable considering the aimed accuracy. These large variations were confirmed in a beam test. A second method, mapping the transverse index gradient by deflection of a laser beam entering normally to the tile has then been developed. It is shown that this procedure is suitable to reach the required accuracy, at the price of using both methods combined. The several hundreds of tiles of the radiator plane of the CREAM and AMS Cherenkov imagers were characterized using a simplified procedure, however, appropriate for each case, compromising between the amount of work and the time available. The experimental procedures and set-ups used are described in the text, and the obtained results are reported.

Published
2010
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23. CREAM: 70 days of flight from 2 launches in Antarctica

Author

S. L. Nutter, Arturo Alejandro Menchaca-Rocha, L. Lutz, N. B. Conklin, A. Malinin, P. S. Marrocchesi, Michael DuVernois, K. C. Kim, Gabriele Bigongiari, P. Walpole, J. J. Beatty, R. Bazer-Bachi, Eun-Suk Seo, L. M. Barbier, H. S. Ahn, J. A. Jeon, M. Buenerd, S. Coutu, S. Y. Zinn, S. P. Wakely, S. P. Swordy, A. Barrau, M. Mangin-Brinet, J. Wu, M. H. Lee, J. H. Han, R. Sina, T. J. Brandt, J. T. Childers, J. Yang, Y. S. Yoon, O. Ganel, L. Derome, N. H. Park, Inkyu Park, S. Minnick, Riccardo Zei, S. I. Mognet, Paolo Maestro, Patrick Allison, Antje Putze, S. W. Nam, Maria Grazia Bagliesi, P. J. Boyle, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and CREAM

Subjects
Physics, Atmospheric Science, Meteorology, 010308 nuclear & particles physics, Payload, Antarctica, Balloon experiment, Cosmic rays, CREAM, ULDB, Aerospace Engineering, Astronomy and Astrophysics, 01 natural sciences, 7. Clean energy, Preliminary analysis, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Flight duration, Geophysics, Space and Planetary Science, 0103 physical sciences, General Earth and Planetary Sciences, Support system, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics
Abstract

The Cosmic-Ray Energetics And Mass balloon-borne experiment has been launched twice in Antarctica, first in December 2004 and again in December 2005. It circumnavigated the South Pole three times during the first flight, which set a flight duration record of 42 days. A cumulative duration of 70 days within 13 months was achieved when the second flight completed 28 days during two circumnavigations of the Pole on 13 January 2006. Both the science instrument and support systems functioned extremely well, and a total 117 GB of data including 67 million science events were collected during these two flights. Preliminary analysis indicates that the data extend well above 100 TeV and follow reasonable power laws. The payload recovered from the first flight has been refurbished for the third flight in 2007, whereas the payload from the second flight is being refurbished to be ready for the fourth flight in 2008. Each flight will extend the reach of precise cosmic-ray composition measurements to energies not previously possible.

Published
2008
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24. CHERCAM: the Cherenkov imager of CREAM experiment

Author

B. Boyer, R. Bazer-Bachi, J. H. Han, O. Bourrion, Eun-Suk Seo, J.-P. Scordilis, L. Lutz, Y. Sallaz-Damaz, L. Eraud, M. Buénerd, L. Derome, J. Bouvier, M. Mangin-Brinet, R. Foglio, Y. S. Yoon, O. Ganel, S. Y. Zinn, A. Putze, A. Malinine, K. C. Kim, A. Barrau, M. H. Lee, L. Gallin-Martel, J. H. Yoo, Arturo Alejandro Menchaca-Rocha, P. Walpole, J.N. Périé, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), A. Bressan, S. Dalla Torre, B. Gobbo, F. Tessarotto, CREAM, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées

Subjects
Nuclear and High Energy Physics, Photomultiplier, Proton, Cherenkov detector, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, 01 natural sciences, 7. Clean energy, law.invention, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, law, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation, Cherenkov radiation, Physics, Range (particle radiation), Large Hadron Collider, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, business.industry, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, business, Beam (structure)
Abstract

International audience; A Cherenkov imager, CHERCAM (CHERenkov CAMera), has been designed and built for the CREAM (Cosmic-Ray Energetic and Mass) balloon-borne experiment. The instrument will perform charge measurements of nuclear cosmic-ray over a range extending from proton to iron. It will achieve individual charge separation of the elements over this range [M. Buénerd, et al., in: 28th ICRC, Tsukuba, Japan, OG 1.5, 2003, p. 2157. [2]] (0:25 charge unit rms), allowing measurements of the energy spectra of individual elements by the CREAM instrument in the energy range from 1010 to 1015 eV. CHERCAM is a proximity focused imager, based on a dedicated mechanical structure, equipped with an n ¼ 1:05 silica aerogel radiator plane, separated by a 12 cm ring expansion gap from a photon detector plane consisting of a 1600 photomultiplier array, backed with dedicated front-end readout electronics. A prototype of the detector has been recently tested with 100 and 300 GeV/c Z ¼ 1 particle beams at CERN. The contribution reports on both the beam test results of the prototype, and of the counter performance in ground operation.

Published
2007
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25. Approaching the knee with direct measurements

Author

S. Coutu, S. Y. Zinn, Paolo Maestro, T. T. Brandt, Maria Grazia Bagliesi, A. Putze, S. P. Wakely, S. Minnick, Patrick Allison, Arturo Alejandro Menchaca-Rocha, P. J. Boyle, S. L. Nutter, Riccardo Zei, P. S. Marrocchesi, Eun-Suk Seo, N. B. Conklin, J. Wu, S. I. Mognet, Y. S. Yoon, O. Ganel, Michael DuVernois, Jeon Jin A, M. Buenerd, L. M. Barbier, S. W. Nam, A. Malinin, L. Derome, P. Walpole, S. P. Swordy, N. H. Park, M. Mangin-Brinet, J. H. Han, Gabriele Bigongiari, A. Barrau, Kwangmoo Kim, R. Bazer-Bachi, M. H. Lee, R. Sina, H. S. Ahn, L. Lutz, J. T. Childers, J. Yang, Y. Sallaz-Damaz, J. J. Beatty, Inkyu Park, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, K.S. Cheng, R. Engel, Y.Q. Ma, B. Pattison, Z.G. Yao and Q.Q. Zhu, and CREAM

Subjects
Physics, Nuclear and High Energy Physics, Range (particle radiation), 010308 nuclear & particles physics, Payload, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Balloon, 7. Clean energy, 01 natural sciences, Atomic and Molecular Physics, and Optics, Atmosphere, Particle acceleration, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Optics, 0103 physical sciences, Particle, business, 010303 astronomy & astrophysics
Abstract

International audience; The Cosmic Ray Energetics And Mass (CREAM) experiment was designed and constructed to push spectral measurements of individual cosmic-ray nuclei from H to Fe to energies approaching the “knee” in a series of balloon flights. A cumulative exposure of 70 days was achieved during two circumpolar flights in Antarctica in 2005 and 2006. Direct measurements at the top of the atmosphere allow event-by-event determination of the incident cosmic-ray particle charge and energy. The objective is to investigate whether and how the knee structure is related to the mechanisms of particle acceleration, propagation, and confinement. The recovered payload is being refurbished for its third flight, which is scheduled for launch in December 2007. The combination of sophisticated particle detectors and long duration balloon flight capabilities now promise high quality measurements over an energy range that was not previously accessible.

Published
2006
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26. Prototype study of the Cherenkov imager of the AMS experiment

Author

Paulo J. S. Gonçalves, F. Giovacchini, A. Barrau, P. Aguayo, L. Eraud, C. Palomares, Carlos Díaz, Arturo Alejandro Menchaca-Rocha, A. Torrento, O. Veziant, L. Derome, C. Delgado, D. Casadei, G. Martinez, J. Casaus, Rui Miguel Faisca Rodrigues Pereira, Eun-Suk Seo, E. Lanciotti, Fernando Barão, M. Aguilar-Benitez, Gaelle Boudoul, G. Laurenti, E. Belmont, M. Pimenta, A. Malinine, K. Protasov, J. Berdugo, Luísa Arruda, E. J. Sanchez, J. Marín, J. Borges, Bruny Baret, I. Sevilla, L. Gallin-Martel, C. Maña, G.P. Barreira, M. Vargas-Trevino, M. Buénerd, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Physics, Nuclear and High Energy Physics, Large Hadron Collider, Ion beam, 010308 nuclear & particles physics, Physics::Instrumentation and Detectors, Detector, Cosmic ray, 01 natural sciences, 7. Clean energy, Charged particle, charge measurement, Ion, Nuclear physics, charged particle detectors, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space instrumentation, Cherenkov imaging, 0103 physical sciences, High Energy Physics::Experiment, 010306 general physics, Nucleon, Instrumentation, Cherenkov radiation, 07.87.+v, 07.77.Ka, 29.40.Ka
Abstract

The AMS experiment includes a Cherenkov imager for mass and charge identification of charged cosmic rays. A second generation prototype has been constructed and its performances evaluated both with cosmic ray particles and with beam ions. In-beam tests have been performed using secondary nuclei from the fragmentation of 20 GeV/c per nucleon Pb ions and 158 GeV/c per nucleon In from the CERN SPS in 2002 and 2003. Partial results are reported. The performances of the prototype for the velocity and the charge measurements have been studied over the range of ion charge Z less, approximate 30. A sample of candidate silica aerogel radiators for the flight model of the detector has been tested. The measured velocity resolution of the detector was found to scale with $Z^{-1}$ as expected, with a value σ(β)/β≈0.7–110^{-3} for singly charged particles and an asymptotic limit in Z of 0.4–0.6×10^{-4}. The measured charge resolution obtained for the n=1.05 aerogel radiator material selected for the flight model of the detector is σ(Z)=0.18 (statistical) circle plus operator 0.015 (systematic), ensuring a good charge separation up to the iron element, for the prototype in the reported experimental conditions.

Published
2006
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27. Flux of light antimatter nuclei near Earth, induced by cosmic rays in the Galaxy and in the atmosphere

Author

A. Barrau, Bruny Baret, L. Derome, K. Protasov, M. Buénerd, Gaelle Boudoul, R. P. Duperray, David Maurin, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Coalescence (physics), Nuclear and High Energy Physics, Antiparticle, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Cosmic ray, Astrophysics, Inelastic scattering, 7. Clean energy, 01 natural sciences, Galaxy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Interstellar medium, Antiproton, Antimatter, 0103 physical sciences, 98.35.Pr, 96.40.-z, 98.70.Sa, 95.30.Cq, 13.75.-n, 13.85.-t, 010306 general physics
Abstract

The fluxes of light antinuclei A, 22 pages, 18 figures, 3 tables. Accepted for publication in Phys. Rev. D

Published
2005
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28. A test bench for the AMS-RICH photodetector modules

Author

L. Eraud, M. Vargas-Trevino, M. Buenerd, J.-P. Scordilis, O. Veziant, L. Derome, G. Boudoul, A. Barrau, L. Gallin-Martel, J. Ballon, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Photomultiplier, Test bench, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Physics::Instrumentation and Detectors, Photodetector, Cosmic ray, 02 engineering and technology, International Space Station, 01 natural sciences, 7. Clean energy, 010309 optics, Optics, Nuclear electronics, 0103 physical sciences, Alpha Magnetic Spectrometer, Prototypes, Focusing, Spectroscopy, Physics, business.industry, Detector, Photodetectors, Astrophysics::Instrumentation and Methods for Astrophysics, Detectors, Electronic equipment testing, 021001 nanoscience & nanotechnology, Particle beams, Ion beams, Performance evaluation, 0210 nano-technology, business
Abstract

International audience; The Alpha Magnetic Spectrometer experiment to be installed on the International Space Station will be equipped with a Proximity Focusing Ring Imaging Cerenkov detector for ion identification. A prototype (2nd generation) has been constructed, which performances have been evaluated both with Cosmic Ray particles and beam ions. A test bench (PMT and Front End Electronics selection) was developed for the testing of the photodetector modules of the flight model. It is described in this contribution

Published
2004
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29. Secondary antiproton flux induced by cosmic ray interactions with the atmosphere

Author

L. Derome, M. Buénerd, C. Y. Huang, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Nuclear and High Energy Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Flux, Cosmic ray, Astrophysics, Atmospheric sciences, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Atmosphere, Antiproton, Physics::Space Physics, 0103 physical sciences, Satellite, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Sea level
Abstract

The atmospheric secondary antiproton flux is studied for detection altitudes extending from sea level up to about 3 earth radii, by means of a 3-dimensional Monte-Carlo simulation, successfully applied previously on other satellite and balloon data. The calculated antiproton flux at mountain altitude is found in fair agreement with the recent BESS measurements. The flux at balloon altitude is also in agreement with calculations performed in previous studies and used for the analysis of balloon data. The flux at sea level is found to be significant. The antineutron flux is also evaluated. The antiproton flux is prospectively explored at large distance from earth up to around 2 10$^4$ km. The results are discussed in the context of the forthcoming measurements by large acceptance experiments., 12 pages, 9 figures, 1 table, submitted to Phys. Rev. D

Published
2003
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30. Secondary proton flux induced by cosmic ray interactions with the atmosphere

Author

Bruny Baret, L. Derome, C. Y. Huang, M. Buénerd, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Nuclear and High Energy Physics, 94.30.Hn, 13.85.-t, 95.85.Ry, 96.40.-z, FOS: Physical sciences, Flux, Cosmic ray, Context (language use), Astrophysics, Antineutron, 7. Clean energy, 01 natural sciences, Earth radius, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, Atmosphere, Altitude, cosmic ray protons, 0103 physical sciences, cosmic ray interactions, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, proton production, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Monte Carlo methods, 13. Climate action, Antiproton, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, Atomic physics
Abstract

The atmospheric secondary proton flux is studied for altitudes extending from sea level up to the top of atmosphere by means of a 3-dimensional Monte-Carlo simulation procedure successfully used previously to account for flux measurements of protons, light nuclei, and electrons-positrons below the geomagnetic cutoff (satellite data), and of muons and antiprotons (balloon data). The calculated flux are compared with the experimental measurements from sea level uo to high float ballon altitudes. The agreement between data and simulation results are very good at all altitudes, including the lowest ones, where the calculations become extremely sensitive to the proton production cross section. The results are discussed in this context. The calculations are extended to the study of quasi trapped particles above the atmosphere to about 5 Earth radii, for prospective purpose., Comment: 7 pages, 5 figures, submitted to Phys. Rev. D

Published
2003
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31. Atmospheric muon and neutrino flux from 3-dimensional simulation

Author

L. Derome, M. Buénerd, Yong Liu, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Physics, Nuclear and High Energy Physics, Muon, Proton, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Flux, Cosmic ray, Electron, 01 natural sciences, 7. Clean energy, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, Positron, 0103 physical sciences, Orbit (dynamics), High Energy Physics::Experiment, Neutrino, 010306 general physics
Abstract

The atmospheric muon and neutrino flux have been simulated using the same approach which successfully accounted for the recent secondary proton, electron and positron flux measurements in orbit by the AMS experiment. For the muon flux, a good agreement is obtained with the CAPRICE and HEAT data for altitudes ranging from sea level up to about 38 km. The general features of the calculated atmospheric neutrino flux are reported and discussed. The flux obtained at the Super-Kamiokande experiment location are reported and compared with other calculations. For low neutrino energies the flux obtained is significantly smaller than that used in the data analysis of underground experiment. The simulation results for the SOUDAN experiment site are also reported.

Published
2003
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32. Secondary electrons and positrons in near earth orbit

Author

L. Derome, Yong Liu, M. Buénerd, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Nuclear and High Energy Physics, Earth's orbit, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, Flux ratio, Secondary electrons, Physics::Geophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear physics, Positron, Earth's magnetic field, 0103 physical sciences, Physics::Space Physics, Cutoff, Orbit (control theory), 010306 general physics, Earth (classical element), Physics::Atmospheric and Oceanic Physics
Abstract

The secondary e+ and e- populations in near earth's orbit have been calculated by simulation. The results are in very good agreement with the recent AMS measurements. The e$^+$ over e$^-$ flux ratio for particles below the geomagnetic cutoff appears to be due to the geomagnetic East-West effect., Comment: Final version for Phys. Lett. B: Title changed, new references added, minor changes in text

Published
2001
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33. Origin of light nuclei in near earth orbit

Author

M. Buenerd, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Nuclear and High Energy Physics, Nuclear Theory, FOS: Physical sciences, chemistry.chemical_element, Astrophysics, 7. Clean energy, 01 natural sciences, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Helium-3, 0103 physical sciences, Physics::Atomic and Molecular Clusters, Physics::Atomic Physics, Nuclear Experiment (nucl-ex), 010306 general physics, Nuclear Experiment, Helium, Coalescence (physics), Physics, Earth's orbit, COSMIC cancer database, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Earth's magnetic field, Deuterium, chemistry, 13. Climate action, Tritium
Abstract

The possible sources of light nuclei populations observed recently below the geomagnetic cutoff by the AMS experiment are discussed in terms of nuclear processes: fragmentation of the incoming flux of cosmic helium on atmospheric nuclei, and nuclear coalescence from proton and helium induced reactions. Results of simulations for deuterium, tritium, helium 3 and 4, are presented., 11 pages, 4 figures

Published
2001
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34. Simulation of the proton component below the geomagnetic cutoff detected by the AMS experiment

Author

M. Buénerd, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and bibliotheque, LPSC

Subjects
Physics, Nuclear and High Energy Physics, Proton, 010308 nuclear & particles physics, Component (thermodynamics), 01 natural sciences, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear magnetic resonance, Earth's magnetic field, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Cutoff, 010306 general physics
Published
2000

35. Origin of the high energy proton component below the geomagnetic cutoff in near earth orbit

Author

T. Thuillier, A. Bouchet, Arturo Alejandro Menchaca-Rocha, A. Barrau, M. Buenerd, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), and AMS

Subjects
Nuclear and High Energy Physics, Proton, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, portal of watch, FOS: Physical sciences, Cosmic ray, Astrophysics, 01 natural sciences, Atmosphere, personalization, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High energy proton, 0103 physical sciences, Cutoff, 010306 general physics, Nuclear Experiment, infomediary, Physics, Earth's orbit, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Component (thermodynamics), Astrophysics (astro-ph), user model, tool of watch, Earth's magnetic field, economic intelligence
Abstract

The high flux proton component observed by AMS below the geomagnetic cutoff can be well accounted for by assuming these particles to be secondaries originating from the interaction of Cosmic Ray protons with the atmosphere. Simulation results are reported, 7 pages, Latex, 4 Postscript figures. Final version (minor corrections) for Physics Letters. B

Published
2000

36. Monitoring and adaptive removal of the power supply harmonics applied to the Virgo read-out noise

Author

Frédérique Marion, D. Buskulic, L. Derome, L. Massonnet, R. Morand, P. Puppo, A. Masserot, R. Hermel, D. Verkindt, B. Mours, R. Flaminio, M. Yvert, J. C. Lacotte, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), VIRGO, and BOMBAR, Claudine

Subjects
Physics, Noise temperature, Power supply rejection ratio, 010308 nuclear & particles physics, Noise (signal processing), business.industry, Electrical engineering, Astronomy and Astrophysics, 01 natural sciences, Signal, Noise floor, Line (electrical engineering), Power (physics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Harmonics, 0103 physical sciences, 010306 general physics, business, Mathematical Physics
Abstract

The VIRGO signal read-out system is based on a sixteen channels architecture. The system is now installed at the site and the noise of eight of the channels has been measured. The noise at 50 Hz and all its harmonics is coherent with a simultaneous measurement of the power supply. The power supply measurement has been used to remove the 50 Hz line and all its harmonics from the signal read-out noise.

Published
1999

37. VEGA an environment for gravitational waves data analysis

Author

M. Yvert, R. Morand, F. Marion, R. Flaminio, B. Mours, D. Buskulic, D. Verkindt, L. Massonet, L. Derome, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), VIRGO, and BOMBAR, Claudine

Subjects
Scale (ratio), AS-Interface, Astrophysics, 01 natural sciences, Computational science, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Unified Modeling Language, 0103 physical sciences, 010306 general physics, Mathematical Physics, computer.programming_language, Physics, Point of view, 010308 nuclear & particles physics, Gravitational wave, Detector, Frame (networking), Vega, Mechanism of filtering, Astronomy and Astrophysics, UML, Data access, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], learning System, computer
Abstract

The objective of this paper is to present an approach that allows modeling and implementing thereafter an E-learning system with different points of view. The norm defined by the UML language obliges to formulate our solution according to its notation. However, the visibility offered by the UML is insufficient to support the dynamic aspect of points of view. To composite for this problem we defined a mechanism of filtering based on the UML and that permits to filter services offered by a class of a system according to its points of view. Such an addition will permit to complete the UML visibility and implement codes of a complex system by the majority of oriented objects languages of the market as JAVA, C++,...

Published
1999

38. SIESTA, a time domain, general purpose simulation program for the VIRGO experiment

Author

R. Flaminio, F. Marion, B. Caron, B. Mours, F. Cavalier, X. Grave, L. Derome, A. Viceré, D. Verkindt, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), VIRGO, and BOMBAR, Claudine

Subjects
Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, 01 natural sciences, Computational science, Theoretical physics, General purpose, 0103 physical sciences, Program Design Language, Time domain, Detectors and Experimental Techniques, SIESTA (computer program), 010303 astronomy & astrophysics
Abstract

In this paper we present the simulation program that has been developed for the VIRGO gravitational wave detection experiment. Although this program — SIESTA — is still evolving, it has reached a stage where the design requirements have been largely fulfilled. We first remind the needs and the choices which have steered the program design and led to the present structure. The contents of the program is then reviewed, the performances are discussed, and some typical applications are briefly described.

Published
1999

39. A VME based CCD imaging system for the VIRGO interferometer control

Author

D. Verkindt, R. Flaminio, B. Mours, D Castelazzi, F Bellachia, L. Massonnet, R Morand, C. Drezen, V. Sannibale, J.C. Lacotte, X. Grave, L. Derome, D Boget, F. Marion, T Carron, G Daguin, Laboratoire d'Annecy de Physique des Particules (LAPP), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, business.industry, Gravitational wave, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Michelson interferometer, Virgo interferometer, 01 natural sciences, law.invention, Interferometry, Optics, law, 0103 physical sciences, Physics::Accelerator Physics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], business, 010303 astronomy & astrophysics, Instrumentation, Sensitivity (electronics), Beam (structure), Fabry–Pérot interferometer
Abstract

Large interferometric detectors, like VIRGO, are planned to detect gravitational waves, by observing the motions of the suspended mirrors of a Michelson interferometer with kilometric Fabry Perot cavity arms. Due to the large sensitivity needed, the set-up requires a real time monitoring of its mirrors positions, and the analysis of beam shape during the alignment. In this paper, we present the development and the performance of a beam imaging system which uses a CCD camera interfaced to a VME board.

Published
1998

40. A Markov Chain Monte Carlo technique to sample transport and source parameters of Galactic cosmic rays

Author

Antje Putze, David Maurin, L. Derome, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Convection, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Series (mathematics), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Probability density function, Cosmic ray, Markov chain Monte Carlo, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Computational physics, symbols.namesake, Space and Planetary Science, 0103 physical sciences, symbols, Halo, Diffusion (business), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

On-going measurements of the cosmic radiation (nuclear, electronic, and gamma-ray) are shedding new light on cosmic-ray physics. A comprehensive picture of these data relies on an accurate determination of the transport and source parameters of propagation models. A Markov Chain Monte Carlo is used to obtain these parameters in a diffusion model. From the measurement of the B/C ratio and radioactive cosmic-ray clocks, we calculate their probability density functions, with a special emphasis on the halo size L of the Galaxy and the local underdense bubble of size r_h. The analysis relies on the USINE code for propagation and on a Markov Chain Monte Carlo technique (Putze et al. 2009, paper I of this series) for the parameter determination. As found in previous studies, the B/C best-fit model favours diffusion/convection/reacceleration (Model III) over diffusion/reacceleration (Model II). A combined fit on B/C and the isotopic ratios (10Be/9Be, 26Al/27Al, 36Cl/Cl) leads to L ~ 8 kpc and r_h ~ 120 pc for the best-fit Model III. This value for r_h is consistent with direct measurements of the local interstallar medium. For Model II, L ~ 4 kpc and r_h is consistent with zero. We showed the potential and usefulness of the Markov Chain Monte Carlo technique in the analysis of cosmic-ray measurements in diffusion models. The size of the diffusive halo depends crucially on the value of the diffusion slope delta, and also on the presence/absence of the local underdensity damping effect on radioactive nuclei. More precise data from on-going experiments are expected to clarify this issue., Comment: 20 pages, 14 figures, minor language corrections to match the A&A accepted version

Published
2010
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41. Cosmic ray energetics and mass for the international space station (ISS-CREAM)

Author

H. B. Jeon, L. Lu, L. Lutz, M. Nester, L. Hagenau, Jong Moon Park, M. Chung, J P. Lundquist, M.H. Kim, HyoJung Hyun, S. Jeong, D. Angelaszek, J. Wu, A. Gerrety, Y. S. Yoon, R.P. Weinmann, M. Copley, S C. Kang, L. Eraud, S. Rostsky, J. F. Liang, J. R. Smith, Y.S. Hwang, A. Mechaca-Rocha, H. J. Kim, N. Picot-Clemente, Kwangmoo Kim, T. Mernik, P. Walpole, L. Derome, H. Park, Inkyu Park, C. Falana, H.G. Huh, J. H. Han, Z. Yin, Joowon Lee, H Y. Lee, Y. Amare, J A. Jeon, H G. Zhang, Eun-Suk Seo, R. Takeishi, G.H. Choi, O. Ofoha, M. H. Lee, N. Anthony, B. Mark, T. Tatoli, C. Lamb, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), and CREAM

Subjects
Physics, Range (particle radiation), Calorimeter (particle physics), 010308 nuclear & particles physics, Payload, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic ray, Electron, Scintillator, 7. Clean energy, 01 natural sciences, Nuclear physics, Ionization, 0103 physical sciences, International Space Station, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

International audience; The ISS-CREAM payload was launched on the SpaceX-12 Commercial Resupply Service mission to the International Space Station (ISS) from NASA’s Kennedy Space Center on August 14, 2017. It was successfully installed and activated on the ISS Japanese Experiment Module Exposed Facility as an attached payload on August 22, 2017. The ISS-CREAM instrument is configured with complementary particle detectors capable of measuring elemental spectra for Z = 1 - 26 nuclei in the energy range ~10^12 – 10^15 eV; as well as electrons at multi-TeV energies. The four layers of its finely segmented Silicon Charge Detectors provide precise charge measurements, and its ionization Calorimeter provides energy measurements. In addition, scintillator-based Top and Bottom Counting Detectors and a Boronated Scintillator Detector distinguish electrons from nuclei. The goal is to understand cosmic ray origin, acceleration and propagation by extending direct measurements of cosmic rays to the highest practical energy. On-orbit performance of the instrument and preliminary results from the ongoing analysis are presented.

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42. Boron and carbon cosmic rays in the upper stratosphere (BACCUS)

Author

Kevin Cheryian, J. Wu, Moo Hyun Lee, L. Hagenau, Jik Lee, L. Eraud, Y. S. Yoon, H.G. Huh, Lucy Lu, Gwangho Choi, R.P. Weinmann, S. L. Nutter, Michael Copley, Y. Amare, Hyeyoung Lee, Ryan Quinn, S. I. Mognet, J.R. Smith, John Mitchell, P. Walpole, J. H. Han, S. Im, Jason Link, J. F. Liang, Michael Nester, O. Ofoha, Mun Hwa Kim, Ki Chun Kim, David Angelaszek, L. Derome, Nathan Anthony, T. Mernik, L. Lutz, I. H. Park, Eun-Suk Seo, Steven Morton, N. Picot-Clemente, S. Coutu, Tyler Anderson, Soomin Jeong, Jin A Jeon, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)

Subjects
Physics, Range (particle radiation), Calorimeter (particle physics), Cherenkov detector, Physics::Instrumentation and Detectors, Detector, Cosmic ray, Scintillator, 7. Clean energy, 01 natural sciences, 010305 fluids & plasmas, law.invention, Nuclear physics, Lorentz factor, symbols.namesake, Transition radiation detector, law, 0103 physical sciences, symbols, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics
Abstract

International audience; The balloon-borne BACCUS experiment measures directly the elemental spectra of cosmic-ray nuclei from protons to Fe over the energy range ~10^12 to 10^15 eV. It focuses on the energy dependence of secondary to primary ratios (e.g. B/C) to investigate cosmic-ray propagation history. BACCUS consists of redundant and complementary particle detectors including the Timing Charge Detector (TCD), Transition Radiation Detector (TRD), Cherenkov Detector (CD), Silicon Charge Detector (SCD), and Calorimeter (CAL). The TCD measures the light yield produced by the particle in plastic scintillator. The TRD provides energy measurements of incident 3 ≤ Z ≤ 26 nuclei in the 102 – 105 Lorentz factor range. The CD responds only to particles with velocity exceeding the velocity of light in the plastic. It allows BACCUS to reject the abundant low energy cosmic rays present in the polar region. The CAL is used to determine the particle’s energy for all nuclei for 1 ≤ Z ≤ 26. With the SCD based on pixellation, in addition to the TCD based on timing, and the CD, the BACCUS instrument implements virtually all possible techniques to minimize the effect of backscatter on charge measurements in the presence of a large particle shower in the CAL. The 30 day flight was carried out successfully over Antarctica in 2016 from Nov. 28 to Dec. 28. The integration test, and performance of instruments will be presented.

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43. First Result from the Alpha Magnetic Spectrometer on the International Space Station: Precision Measurement of the Positron Fraction in Primary Cosmic Rays of 0.5–350 GeV

Author

Aguilar, M, Alberti, G, Alpat, B, Alvino, A, Ambrosi, G, Andeen, K, Anderhub, H, Arruda, L, Azzarello, P, Bachlechner, A, Barao, F, Baret, B, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Basili, A, Batalha, L, Bates, J, Battiston, R, Bazo, J, Becker, R, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Berges, P, Bertucci, B, Bigongiari, G, Biland, A, Bindi, V, Bizzaglia, S, de Boer, W, Bollweg, K, Bolmont, J, Borgia, B. Borsini, S, Boschini, MJ, Boudoul, G, Bourquin, M, Brun, P, Buenerd, M, Burger, J, Burger, W, Cadoux, F, Cai, XD, Capell, M, Casadei, D, Casaus, J, Cascioli, V, Castellini, G, Cernuda, I, Cervelli, F, Chae, MJ, Chang, YH, Chen, AI, Chen, CR, Chen, H, Cheng, GM, Chen, HS, Cheng, L, Chernoplyiokov, N, Chikanian, A, Choumilov, E, Choutko, V, Chung, CH, Clark, C, Clavero, R, Coignet, G, Commichau, V, Consolandi, C, Contin, A, Corti, C, Dios, MT, Costado Coste, B, Crespo, D, Cui, Z, Dai, M, Delgado, C, Della Torre, S, Demirkoz, B, Dennett, P, Derome, L, Di Falco, S, Diao, XH, Diago, A, Djambazov, L, Diaz, C, von Doetinchem, P, Du, WJ, Dubois, JM, Duperay, R, Duranti, M, D'Urso, D, Egorov, A, Eline, A, Eppling, FJ, Eronen, T, van Es, J, Esser, H, Falvard, A, Fiandrini, E, Fiasson, A, Finch, E, Fisher, P, Flood, K, Foglio, R, Fohey, M, Fopp, S, Fouque, N, Galaktionov, Y, Gallilee, M, Gallin Martel, L, Gallucci, G, Garcia, B, Garcia, J, Garcia Lopez, R, Garcia Tabares, L, Gargiulo, C, Gast, H, Gebauer, I, Gentile, S, Gillard, W, Giovacchini, F, Girard, L, Goglov, P, Gong, J, Goy Henningsen, C, Grandi, D, Graziani, M, Grechko, A, Gross, A, Guerri, I, de la Guia, C, Guo, KH, Habiby, M, Haino, S, Hauler, F, He, ZH, Heil, M, Heilig, J, Hermel, R, Hofer, H, Huang, ZC, Hungerford, W, Incagli, M, Ionica, M, Jacholkowska, A, Jang, WY, Jinchi, H, Jongmanns, M, Journet, L, Jungermann, L, Karpinski, W, Kim, GN, Kim, KS, Kirn, Th, Kossakowski, R, Koulemzine, A, Kounina, O, Kounine, A, Koutsenko, V, Krafczyk, MS, Laudi, E, Laurenti, G, Lauritzen, C, Lebedev, A, Lee, MW, Lee, SC, Leluc, C, Vargas, HL, Lepareur, V, Li, JQ, Li, Q, Li, TX, Li, W, Li, ZH, Lipari, P, Lin, CH, Liu, D, Liu, H, Lomtadze, T, Lu, YS, Lucidi, S, Luebelsmeyer, K, Luo, JZ, Lustermann, W, Lv, S, Madsen, J, Majka, R, Malinin, A, Mana, C, Marin, J, Martin, T, Martinez, G, Masciocchi, F, Masi, N, Maurin, D, McInturff, A, McIntyre, P, Menchaca Rocha, A, Meng, Q, Menichelli, M, Mereu, I, Millinger, M, Mo, DC, Molina, M, Mott, P, Mujunen, A, Natale, S, Nemeth, P, Ni, JQ, Nikonov, N, Nozzoli, F, Nunes, P, Obermeier, A, Oh, S, Oliva, A, Palmonari, F, Palomares, C, Paniccia, M, Papi, A, Park, WH, Pauluzzi, M, Pauss, F, Pauw, A, Pedreschi, E, Pereira, R, Perrin, E, Pierschel, G, Pilo, F, Piluso, A, Pizzolotto, C, Plyaskin, V, Pochon, J, Pohl, M, Poireau, V, Porter, S, Pouxe, J, Putze, A, Quadrani, L, Qi, XN, Rancoita, PG, Rapin, D, Ren, ZL, Ricol, JS, Riihonen, E, Rodriguez, I, Roeser, U, Rosier Lees, S, Rossi, L, Rozhkov, A, ROZZA, DAVIDE, Sabellek, A, Sagdeev, R, Sandweiss, J, Santos, B, Saouter, P, Sarchioni, M, Schael, S, Schinzel, D, Schmanau, M, Schwering, G, von Dratzig, AS, Scolieri, G, Seo, ES, Shan, BS, Shi, JY, Shi, YM, Siedenburg, T, Siedling, R, Son, D, Spada, F, Spinella, F, Steuer, M, Stiff, K, Sun, W, Sun, WH, Sun, XH, Tang, CP, Tang, XW, Tang, ZC, Tao, L, Tassan Viol, J, Ting, Samuel CC, Ting, SM, Titus, C, Tomassetti, N, Toral, F, Torsti, J, Tsai, JR, Tutt, JC, Ulbricht, J, Urban, T, Vagelli, V, Valente, E, Vannini, C, Valtonen, E, Trevino, MV, Vaurynovich, S, Vecchi, M, Vergain, M, Verlaat, B, Vescovi, C, Vialle, JP, Viertel, G, Volpini, G, Wang, D, Wang, NH, Wang, QL, Wang, RS, Wang, X, Wang, ZX, Wallraff, W, Weng, ZL, Willenbrock, M, Wlochal, M, Wu, H, Wu, KY, Wu, ZS, Xiao, WJ, Xie, S, Xiong, RQ, Xin, GM, Xu, NS, Xu, W, Yan, Q, Yang, J, Yang, M, Ye, QH, Yi, H, Yu, YJ, Yu, ZQ, Zeissler, S, Zhang, JG, Zhang, Z, Zhang, MM, Zheng, ZM, Zhuang, HL, Zhukov, V, Zichichi, A, Zuccon, P, Zurbach, C., BOELLA, GIULIANO FILIPPO, GERVASI, MASSIMO, PENSOTTI, SIMONETTA, PESSINA, GIANLUIGI EZIO, TACCONI, MAURO, M. Aguilar, G. Alberti, B. Alpat, A. Alvino, G. Ambrosi, K. Andeen, H. Anderhub, L. Arruda, P. Azzarello, A. Bachlechner, F. Barao, B. Baret, A. Barrau, L. Barrin, A. Bartoloni, L. Basara, A. Basili, L. Batalha, J. Bate, R. Battiston, J. Bazo, R. Becker, U. Becker, M. Behlmann, B. Beischer, J. Berdugo, P. Berge, B. Bertucci, G. Bigongiari, A. Biland, V. Bindi, S. Bizzaglia, G. Boella, W. de Boer, K. Bollweg, J. Bolmont, B. Borgia, S. Borsini, M. J. Boschini, G. Boudoul, M. Bourquin, P. Brun, M. Buénerd, J. Burger, W. Burger, F. Cadoux, X. D. Cai, M. Capell, D. Casadei, J. Casau, V. Cascioli, G. Castellini, I. Cernuda, F. Cervelli, M. J. Chae, Y. H. Chang, A. I. Chen, C. R. Chen, H. Chen, G. M. Cheng, H. S. Chen, L. Cheng, N. Chernoplyiokov, A. Chikanian, E. Choumilov, V. Choutko, C. H. Chung, C. Clark, R. Clavero, G. Coignet, V. Commichau, C. Consolandi, A. Contin, C. Corti, M. T. Costado Dio, B. Coste, D. Crespo, Z. Cui, M. Dai, C. Delgado, S. Della Torre, B. Demirkoz, P. Dennett, L. Derome, S. Di Falco, X. H. Diao, A. Diago, L. Djambazov, C. Díaz, P. von Doetinchem, W. J. Du, J. M. Duboi, R. Duperay, M. Duranti, D. D’Urso, A. Egorov, A. Eline, F. J. Eppling, T. Eronen, J. van E, H. Esser, A. Falvard, E. Fiandrini, A. Fiasson, E. Finch, P. Fisher, K. Flood, R. Foglio, M. Fohey, S. Fopp, N. Fouque, Y. Galaktionov, M. Gallilee, L. Gallin-Martel, G. Gallucci, B. García, J. García, R. García-López, L. García-Tabare, C. Gargiulo, H. Gast, I. Gebauer, S. Gentile, M. Gervasi, W. Gillard, F. Giovacchini, L. Girard, P. Goglov, J. Gong, C. Goy-Henningsen, D. Grandi, M. Graziani, A. Grechko, A. Gro, I. Guerri, C. de la Guía, K. H. Guo, M. Habiby, S. Haino, F. Hauler, Z. H. He, M. Heil, J. Heilig, R. Hermel, H. Hofer, Z. C. Huang, W. Hungerford, M. Incagli, M. Ionica, A. Jacholkowska, W. Y. Jang, H. Jinchi, M. Jongmann, L. Journet, L. Jungermann, W. Karpinski, G. N. Kim, K. S. Kim, Th. Kirn, R. Kossakowski, A. Koulemzine, O. Kounina, A. Kounine, V. Koutsenko, M. S. Krafczyk, E. Laudi, G. Laurenti, C. Lauritzen, A. Lebedev, M. W. Lee, S. C. Lee, C. Leluc, H. León Varga, V. Lepareur, J. Q. Li, Q. Li, T. X. Li, W. Li, Z. H. Li, P. Lipari, C. H. Lin, D. Liu, H. Liu, T. Lomtadze, Y. S. Lu, S. Lucidi, K. Lübelsmeyer, J. Z. Luo, W. Lustermann, S. Lv, J. Madsen, R. Majka, A. Malinin, C. Mañá, J. Marín, T. Martin, G. Martínez, F. Masciocchi, N. Masi, D. Maurin, A. McInturff, P. McIntyre, A. Menchaca-Rocha, Q. Meng, M. Menichelli, I. Mereu, M. Millinger, D. C. Mo, M. Molina, P. Mott, A. Mujunen, S. Natale, P. Nemeth, J. Q. Ni, N. Nikonov, F. Nozzoli, P. Nune, A. Obermeier, S. Oh, A. Oliva, F. Palmonari, C. Palomare, M. Paniccia, A. Papi, W. H. Park, M. Pauluzzi, F. Pau, A. Pauw, E. Pedreschi, S. Pensotti, R. Pereira, E. Perrin, G. Pessina, G. Pierschel, F. Pilo, A. Piluso, C. Pizzolotto, V. Plyaskin, J. Pochon, M. Pohl, V. Poireau, S. Porter, J. Pouxe, A. Putze, L. Quadrani, X. N. Qi, P. G. Rancoita, D. Rapin, Z. L. Ren, J. S. Ricol, E. Riihonen, I. Rodríguez, U. Roeser, S. Rosier-Lee, L. Rossi, A. Rozhkov, D. Rozza, A. Sabellek, R. Sagdeev, J. Sandwei, B. Santo, P. Saouter, M. Sarchioni, S. Schael, D. Schinzel, M. Schmanau, G. Schwering, A. Schulz von Dratzig, G. Scolieri, E. S. Seo, B. S. Shan, J. Y. Shi, Y. M. Shi, T. Siedenburg, R. Siedling, D. Son, F. Spada, F. Spinella, M. Steuer, K. Stiff, W. Sun, W. H. Sun, X. H. Sun, M. Tacconi, C. P. Tang, X. W. Tang, Z. C. Tang, L. Tao, J. Tassan-Viol, Samuel C. C. Ting, S. M. Ting, C. Titu, N. Tomassetti, F. Toral, J. Torsti, J. R. Tsai, J. C. Tutt, J. Ulbricht, T. Urban, V. Vagelli, E. Valente, C. Vannini, E. Valtonen, M. Vargas Trevino, S. Vaurynovich, M. Vecchi, M. Vergain, B. Verlaat, C. Vescovi, J. P. Vialle, G. Viertel, G. Volpini, D. Wang, N. H. Wang, Q. L. Wang, R. S. Wang, X. Wang, Z. X. Wang, W. Wallraff, Z. L. Weng, M. Willenbrock, M. Wlochal, H. Wu, K. Y. Wu, Z. S. Wu, W. J. Xiao, S. Xie, R. Q. Xiong, G. M. Xin, N. S. Xu, W. Xu, Q. Yan, J. Yang, M. Yang, Q. H. Ye, H. Yi, Y. J. Yu, Z. Q. Yu, S. Zeissler, J. G. Zhang, Z. Zhang, M. M. Zhang, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, P. Zuccon, C. Zurbach, Azzarello, Philipp, Bourquin, Maurice, Cadoux, Franck, Habiby Alaoui, Marion, Leluc, Catherine, Masciocchi, Florian, Paniccia, Mercedes, Perrin, Eric, Pohl, Martin, Rapin, Divic Jean, Saouter, Pierre, Metsähovi Radio Observatory, Aalto-yliopisto, Aalto University, OpenMETU, CERN [Genève], Centro de Investigaciones Energéticas Medioambientales y Tecnológicas [Madrid] (CIEMAT), Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Istituto Nazionale di Fisica Nucleare (INFN), Karlsruhe Institute of Technology (KIT), Institute for Theoretical Physics [ETH Zürich] (ITP), Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), RWTH Aachen University, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Massachusetts Institute of Technology (MIT), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Département de Physique Nucléaire et Corpusculaire [Genève] (DPNC), Université de Genève (UNIGE), Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Instituto de Astrofisica de Canarias (IAC), Instituto de Matematicas (UNAM), Universidad Nacional Autónoma de México (UNAM), Istituto Nazionale di Fisica Nucleare [Sezione di Roma 1] (INFN), Istituto Nazionale di Fisica Nucleare, INFN Sezione di Pisa (INFN Sezione di Pisa), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), AMS, Aguilar, M, Alberti, G, Alpat, B, Alvino, A, Ambrosi, G, Andeen, K, Anderhub, H, Arruda, L, Azzarello, P, Bachlechner, A, Barao, F, Baret, B, Barrau, A, Barrin, L, Bartoloni, A, Basara, L, Basili, A, Batalha, L, Bates, J, Battiston, R, Bazo, J, Becker, R, Becker, U, Behlmann, M, Beischer, B, Berdugo, J, Berges, P, Bertucci, B, Bigongiari, G, Biland, A, Bindi, V, Bizzaglia, S, Boella, G, de Boer, W, Bollweg, K, Bolmont, J, Borgia, B., B, S, Boschini, M, Boudoul, G, Bourquin, M, Brun, P, Buenerd, M, Burger, J, Burger, W, Cadoux, F, Cai, X, Capell, M, Casadei, D, Casaus, J, Cascioli, V, Castellini, G, Cernuda, I, Cervelli, F, Chae, M, Chang, Y, Chen, A, Chen, C, Chen, H, Cheng, G, Cheng, L, Chernoplyiokov, N, Chikanian, A, Choumilov, E, Choutko, V, Chung, C, Clark, C, Clavero, R, Coignet, G, Commichau, V, Consolandi, C, Contin, A, Corti, C, Dios, M, Costado Coste, B, Crespo, D, Cui, Z, Dai, M, Delgado, C, Della Torre, S, Demirkoz, B, Dennett, P, Derome, L, Di Falco, S, Diao, X, Diago, A, Djambazov, L, Diaz, C, von Doetinchem, P, Du, W, Dubois, J, Duperay, R, Duranti, M, D'Urso, D, Egorov, A, Eline, A, Eppling, F, Eronen, T, van Es, J, Esser, H, Falvard, A, Fiandrini, E, Fiasson, A, Finch, E, Fisher, P, Flood, K, Foglio, R, Fohey, M, Fopp, S, Fouque, N, Galaktionov, Y, Gallilee, M, Gallin Martel, L, Gallucci, G, Garcia, B, Garcia, J, Garcia Lopez, R, Garcia Tabares, L, Gargiulo, C, Gast, H, Gebauer, I, Gentile, S, Gervasi, M, Gillard, W, Giovacchini, F, Girard, L, Goglov, P, Gong, J, Goy Henningsen, C, Grandi, D, Graziani, M, Grechko, A, Gross, A, Guerri, I, de la Guia, C, Guo, K, Habiby, M, Haino, S, Hauler, F, He, Z, Heil, M, Heilig, J, Hermel, R, Hofer, H, Huang, Z, Hungerford, W, Incagli, M, Ionica, M, Jacholkowska, A, Jang, W, Jinchi, H, Jongmanns, M, Journet, L, Jungermann, L, Karpinski, W, Kim, G, Kim, K, Kirn, T, Kossakowski, R, Koulemzine, A, Kounina, O, Kounine, A, Koutsenko, V, Krafczyk, M, Laudi, E, Laurenti, G, Lauritzen, C, Lebedev, A, Lee, M, Lee, S, Leluc, C, Vargas, H, Lepareur, V, Li, J, Li, Q, Li, T, Li, W, Li, Z, Lipari, P, Lin, C, Liu, D, Liu, H, Lomtadze, T, Lu, Y, Lucidi, S, Luebelsmeyer, K, Luo, J, Lustermann, W, Lv, S, Madsen, J, Majka, R, Malinin, A, Mana, C, Marin, J, Martin, T, Martinez, G, Masciocchi, F, Masi, N, Maurin, D, Mcinturff, A, Mcintyre, P, Menchaca Rocha, A, Meng, Q, Menichelli, M, Mereu, I, Millinger, M, Mo, D, Molina, M, Mott, P, Mujunen, A, Natale, S, Nemeth, P, Ni, J, Nikonov, N, Nozzoli, F, Nunes, P, Obermeier, A, Oh, S, Oliva, A, Palmonari, F, Palomares, C, Paniccia, M, Papi, A, Park, W, Pauluzzi, M, Pauss, F, Pauw, A, Pedreschi, E, Pensotti, S, Pereira, R, Perrin, E, Pessina, G, Pierschel, G, Pilo, F, Piluso, A, Pizzolotto, C, Plyaskin, V, Pochon, J, Pohl, M, Poireau, V, Porter, S, Pouxe, J, Putze, A, Quadrani, L, Qi, X, Rancoita, P, Rapin, D, Ren, Z, Ricol, J, Riihonen, E, Rodriguez, I, Roeser, U, Rosier Lees, S, Rossi, L, Rozhkov, A, Rozza, D, Sabellek, A, Sagdeev, R, Sandweiss, J, Santos, B, Saouter, P, Sarchioni, M, Schael, S, Schinzel, D, Schmanau, M, Schwering, G, von Dratzig, A, Scolieri, G, Seo, E, Shan, B, Shi, J, Shi, Y, Siedenburg, T, Siedling, R, Son, D, Spada, F, Spinella, F, Steuer, M, Stiff, K, Sun, W, Sun, X, Tacconi, M, Tang, C, Tang, X, Tang, Z, Tao, L, Tassan Viol, J, Ting, S, Titus, C, Tomassetti, N, Toral, F, Torsti, J, Tsai, J, Tutt, J, Ulbricht, J, Urban, T, Vagelli, V, Valente, E, Vannini, C, Valtonen, E, Trevino, M, Vaurynovich, S, Vecchi, M, Vergain, M, Verlaat, B, Vescovi, C, Vialle, J, Viertel, G, Volpini, G, Wang, D, Wang, N, Wang, Q, Wang, R, Wang, X, Wang, Z, Wallraff, W, Weng, Z, Willenbrock, M, Wlochal, M, Wu, H, Wu, K, Wu, Z, Xiao, W, Xie, S, Xiong, R, Xin, G, Xu, N, Xu, W, Yan, Q, Yang, J, Yang, M, Ye, Q, Yi, H, Yu, Y, Yu, Z, Zeissler, S, Zhang, J, Zhang, Z, Zhang, M, Zheng, Z, Zhuang, H, Zhukov, V, Zichichi, A, Zuccon, P, and Zurbach, C

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, education, Dark matter, General Physics and Astronomy, Electrons, Cosmic ray, ddc:500.2, Electron, 01 natural sciences, and other elementary particle detectors, cosmic ray detectors, Nuclear physics, Physics and Astronomy (all), Positron, cosmic rays, muon, Neutrino, 0103 physical sciences, Alpha Magnetic Spectrometer, 010306 general physics, Anisotropy, Physics, Range (particle radiation), ta115, ta213, ta114, Cosmic rays, positron fraction, space experiments, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], pion, Observable, energy spectra and interactions, pion, and other elementary particle detectors, ELECTRONS, cosmic rays, dark matter, Physics::Accelerator Physics, High Energy Physics::Experiment, Composition
Abstract

A precision measurement by the Alpha Magnetic Spectrometer on the International Space Station of the positron fraction in primary cosmic rays in the energy range from 0.5 to 350 GeV based on 6.8 x 10(6) positron and electron events is presented. The very accurate data show that the positron fraction is steadily increasing from 10 to similar to 250 GeV, but, from 20 to 250 GeV, the slope decreases by an order of magnitude. The positron fraction spectrum shows no fine structure, and the positron to electron ratio shows no observable anisotropy. Together, these features show the existence of new physical phenomena. DOI: 10.1103/PhysRevLett.110.141102

Published
2013
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