The High-Energy Antimatter Telescope (HEAT): An instrument for the study of cosmic-ray positrons

We present a new measurement of the antiproton to proton abundance ratio, p/p, in the cosmic radiation. The HEAT-pbar instrument, a balloon borne magnet spectrometer with precise rigidity and multiple energy loss measurement capability, was flown successfully in Spring 2000, at an average atmospheric depth of 7.2 g/cm 2 . A total of 71 antiprotons were identified above the vertical geomagnetic cut-off rigidity of 4.2 GV. The highest measured proton energy was 81 GeV. We find that the p/p abundance ratio agrees with that expected from a purely secondary origin of antiprotons produced by primary protons with a standard soft energy spectrum.

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“…The spectrometer has been described in detail [12]. It consists of 479 drift tubes in twenty four layers.…”

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confidence: 99%

Measurement of the Cosmic-Ray Antiproton-to-Proton Abundance Ratio between 4 and 50 GeV

et al. 2001

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“…The development of modern particle space borne detectors (both for charged particles and photons) has been preceded/accompanied by decades of development of particle detectors for ground based nuclear and particle physics detectors, followed by extended use on stratospheric balloons [29][30][31][32][33][34][35][36][37][38].…”

Section: Space Borne Particle Detectorsmentioning

confidence: 99%

Spaceborne Experiments

Battiston¹

2020

Particle Physics Reference Library

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The Universe is the ultimate laboratory to understand the laws of nature. Under the action of the fundamental forces, lasting infinitesimal times or billion of years, matter and energy reach most extreme conditions. Using sophisticated instruments capable to select the signals reaching us from the depths of space and of time, we are able to extract information otherwise not obtainable with the most sophisticated ground based experiments. The results of these observations deeply influence the way we today look at the Universe and try to understand it. During hundreds of thousands of years we have observed the sky only using our eyes, accessing in this way only the very small part of the electromagnetic radiation which is able to traverse the atmosphere, the visible light. The first telescope observations by Galileo in 1609, which dramatically changed our understanding of the solar system, yet were based only on the visible part of the electromagnetic spectrum. Only during the second half of the twentieth century we started to access wider parts of the spectrum. After the end of the war, using the new radar related technology, the scientists developed the radio telescopes to record the first radio images of the galaxy. But only in the 60's, with the advent of the first man made satellites, we began to access the much wider e.m. spectrum, including infrared, UV, X-ray and γ-ray radiation. A similar situation happened with the charged cosmic radiation. Cosmic Rays, discovered by Hess in 1912 [1] using electrometers operated on atmospheric balloons, for about 40 years were the subject of very intense studies. The discovery of a realm of new particles using CR experiments, gave birth to particle physics

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“…Precisely measuring the timing information of a particle in an experiment would allow one to successfully reconstruct physical events. Time of Flight (TOF) methods have been developed and used in many fields such as high energy physics experiments [1,2], astroparticle detectors [3,4], TOF cameras [5,6], TOF-PET detectors [7,8] for identifying the particle species, determining the direction of the particles and energy measurements. The counter telescope is useful in researches which is a relatively a few number of desired particles has to be counted in a major unwanted background.…”

Section: Introductionmentioning

confidence: 99%

“…The counter telescope is useful in researches which is a relatively a few number of desired particles has to be counted in a major unwanted background. The analyzing the coincidence time, passing through the counters telescopes, (1) arXiv:1908.10812v1 [physics.ins-det] 28 Aug 2019 is practical to remove the spurious counts registered because of the accidental coincidence of counts in the each detectors. While comparing the Silicon PhotoMultipliers (SiPMs) with traditional PhotoMultiplier Tubes (PMTs), which have been widely used in the past experiments for decades, SiPMs have some advantages such as advanced photon detection efficiency, compactness, excellent single photon time resolution, insensitive to magnetic fields and inexpensive price.…”

Section: Introductionmentioning

confidence: 99%

Performance Study of a Time-of-Flight Method Used for Cosmic Ray Detection

Yilmaz¹

2019

Acta Phys. Pol. B

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Time of Flight methods have been rapidly developed and used in many experiments recently for determination of particle direction, identification of particles and energy resolutions. This paper describes a method of timemark determination on the reconstruction algorithm, based on the sampled signal, used for time-of-flight measurements. This method was developed for distinguishing the signals by fitting to pulse shape which were received from scintillator detector with a silicon photomultiplier readout have been developed for a cosmic ray counter telescope. The method was verified using experimental data taken in the location 40°54 52 N and 38°19 26 E with the elevation of 30 m above the sea level. The data samples were acquired by the counters which have a scintillator with dimensions of 20×20×1.4 cm 3 , optically coupled from one side to silicon photomultiplier, then the signals readout by fast sampling digitizer board Domino Ring Sampler Board version 4. The method can reconstruct each pulse even for multiple events without losing the count within the small time window. Using this method 4.969 ns time-of-flight value were established and the rise times for scintillation counters, named Tile 1 and Tile 2, were measured about 6.27 ± 0.16 ns and 4.979 ± 0.165 ns, respectively.

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The High-Energy Antimatter Telescope (HEAT): An instrument for the study of cosmic-ray positrons

Cited by 39 publications

References 11 publications

Measurement of the Cosmic-Ray Antiproton-to-Proton Abundance Ratio between 4 and 50 GeV

Measurement of the Cosmic-Ray Antiproton-to-Proton Abundance Ratio between 4 and 50 GeV

Spaceborne Experiments

Performance Study of a Time-of-Flight Method Used for Cosmic Ray Detection

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