The internal alignment and position resolution of the AMS-02 silicon tracker determined with cosmic-ray muons

Alpat, B.; Ambrosi, G.; Azzarello, P.; Battiston, R.; Bertucci, B.; Bourquin, M.; Burger, W. J.; Cadoux, F.; Costa, C. F. Da Silva; Choutko, V.; Duranti, M.; Fiandrini, E.; Haas, D.; Haino, S.; Ionica, M.; Ionica, R.; Lechanoine‐Leluc, C.; Menichelli, M.; Natale, Sonia; Oliva, A.; Paniccia, M.; Perrin, E.; Pohl, M.; Rapin, D.; Tomassetti, Nicola; Zuccon, P.; Zurbach, C.

doi:10.1016/j.nima.2009.11.065

Cited by 91 publications

(44 citation statements)

References 8 publications

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“…The tracker [9] has nine layers, the first (L1) at the top of the detector, the second (L2) just above the magnet, six (L3 to L8) within the bore of the magnet, and the last (L9) just above the ECAL. L2 to L8 constitute the inner tracker.…”

Section: Detectormentioning

confidence: 99%

Precision Measurement of the Proton Flux in Primary Cosmic Rays from 1 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station

Choutko¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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Section: Detectormentioning

confidence: 99%

Precision Measurement of the Proton Flux in Primary Cosmic Rays from 1 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station

Choutko¹

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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“…[17,18]. All detector elements are used for particle identification in the present analysis: the silicon tracker [19], the permanent magnet [5,20], the time of flight counters TOF [21], the anticoincidence counters ACC [22], the transition radiation detector TRD [23], the ring imaging Čerenkov detector RICH [24], and the electromagnetic calorimeter ECAL [25].…”

mentioning

confidence: 99%

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

Aguilar¹,

Cavasonza²,

Alpat³

et al. 2016

Phys. Rev. Lett.

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468

560

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International audienceA precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio inprimary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49 × 105antiproton events and 2.42 × 109 proton events. The fluxes and flux ratios of charged elementary particlesin cosmic rays are also presented. In the absolute rigidity range ∼60 to ∼500 GV, the antiproton ¯p, protonp, and positron eþ fluxes are found to have nearly identical rigidity dependence and the electron e− fluxexhibits a different rigidity dependence. Below 60 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios eachreaches a maximum. From ∼60 to ∼500 GV, the ( ¯ p=p), ( ¯ p=eþ), and (p=eþ) flux ratios show no rigiditydependence. These are new observations of the properties of elementary particles in the cosmos

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“…1. It consists of 9 planes of precision silicon tracker with two outer planes, 1 and 9, and the inner tracker, planes 2-8 [5]; a transition radiation detector, TRD [6]; four planes of time of flight counters, TOF [7]; a permanent magnet [8]; an array of anti-coincidence counters, ACC [9], inside the magnet bore; a ring imagingČerenkov detector, RICH [10]; and an electromagnetic calorimeter, ECAL [11]. The figure also shows a high energy positron of 369 GeV recorded by AMS.…”

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confidence: 99%

High Statistics Measurement of the Positron Fraction in Primary Cosmic Rays of 0.5–500 GeV with the Alpha Magnetic Spectrometer on the International Space Station

Accardo¹,

Aguilar²,

Aisa³

et al. 2014

Phys. Rev. Lett.

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520

424

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A precision measurement by AMS of the positron fraction in primary cosmic rays in the energy range from 0.5 to 500 GeV based on 10.9 million positron and electron events is presented. This measurement extends the energy range of our previous observation and increases its precision. The new results show, for the first time, that above ∼200 GeV the positron fraction no longer exhibits an increase with energy. 3Over the last two decades, there has been a strong interest in the cosmic ray positron fraction in both particle physics and astrophysics [1]. The positron fraction is defined as the ratio of the positron flux to the combined flux of positrons and electrons. The first results from the Alpha Magnetic Spectrometer (AMS) on the positron fraction were reported in [2]. They generated widespread interest [3]. In this Letter we report new results based on all the data collected during 30 months of AMS operations on the International Space Station (ISS), from 19 May 2011 to 26 November 2013. Due to the excellent and steady performance of the detector, and an increase of the data sample by a factor of 1.7, the measurement of the positron fraction is extended up to 500 GeV with improved precision.AMS detector.-The layout of the AMS-02 detector [4] is shown in Fig. 1. It consists of 9 planes of precision silicon tracker with two outer planes, 1 and 9, and the inner tracker, planes 2-8 [5]; a transition radiation detector, TRD [6]; four planes of time of flight counters, TOF [7]; a permanent magnet [8]; an array of anti-coincidence counters, ACC [9], inside the magnet bore; a ring imagingČerenkov detector, RICH [10]; and an electromagnetic calorimeter, ECAL [11]. The figure also shows a high energy positron of 369 GeV recorded by AMS. AMS operates without interruption on the ISS and is monitored continuously from the ground.The timing, location and attitude of AMS are determined by a combination of GPS units affixed to AMS and to the ISS. The AMS coordinate system is concentric with the center of the magnet. The x axis is parallel to the main component of the magnetic field and the z axis points vertically. The (y-z ) plane is the bending plane. The maximum detectable rigidity over tracker planes 1-9, a lever arm of 3 m, is ∼2 TV. Detector performance, described in detail in [2,4], is steady over time.Three main detectors provide clean and redundant identification of positrons and electrons with independent suppression of the proton background. These are the TRD (above the magnet), the ECAL (below the magnet) and the tracker. The TRD and the ECAL are separated by the magnet and the tracker. This ensures that most of the secondary particles produced in the TRD and in the upper TOF planes are swept away and do not enter into the ECAL. Events with large angle scattering are also rejected by a quality cut on the measurement of the trajectory using the tracker. The matching of the ECAL energy, E, and the momentum measured with the tracker, p, greatly improves the proton rejection.To differentiate between e ± and prot...

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The internal alignment and position resolution of the AMS-02 silicon tracker determined with cosmic-ray muons

Cited by 91 publications

References 8 publications

Precision Measurement of the Proton Flux in Primary Cosmic Rays from 1 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station

Precision Measurement of the Proton Flux in Primary Cosmic Rays from 1 GV to 1.8 TV with the Alpha Magnetic Spectrometer on the International Space Station

Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station

High Statistics Measurement of the Positron Fraction in Primary Cosmic Rays of 0.5–500 GeV with the Alpha Magnetic Spectrometer on the International Space Station

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