Background Estimation in MXGS Apparatus on International Space Station

Alpat, B.; Menichelli, M.; Caraffini, Diego; Petasecca, Marco; Renzi, Francesca

doi:10.1109/tns.2010.2042070

Cited by 4 publications

(3 citation statements)

References 7 publications

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“…14 we have reported a parametrization of SEP energy differential fluxes above 100 MeV/n during the whole evolution of the solar events dated 23 February 1956, 13 Finally, we report here the SEP spatial distribution during the evolution of the event dated 23 February 1956: the most intense event occurred since neutron monitors were operating. Shea and Smart 21 estimated for this event an integral intensity of 10 9 protons/cm 2 above 30 MeV.…”

Section: Introductionmentioning

confidence: 93%

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Grimani

2013

Int. J. Mod. Phys. D

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Test-mass charging due to galactic cosmic rays (GCRs) and solar energetic particles (SEPs) represents one of the major sources of noise for missions devoted to gravitational wave detection in space. Particle detectors on board future space interferometers will help in monitoring the test-mass charging process. Variations and fluctuations of GCRs and evolution of SEP events of different intensities are discussed here for the correlation of SEP radiation monitor observations and particle fluxes charging the test masses. We consider the performance of the radiation monitors designed for the LISA Pathfinder mission for the results presented in this work. We point out that in addition to the primary use of test-mass charging monitoring, particle detectors on board space interferometers will naturally provide SEP observations at different intervals in heliolongitude and distances from Earth for space weather applications. PACS Number(s): 96.50.sb, 96.50.sh, 96.50.Vg, 94.05.Sd, 04.80.Nn, 95.55.Ym 1341006-1 Int. J. Mod. Phys. D 2013.22. Downloaded from www.worldscientific.com by QUEEN'S UNIVERSITY on 02/04/15. For personal use only. 1341006-2 Int. J. Mod. Phys. D 2013.22. Downloaded from www.worldscientific.com by QUEEN'S UNIVERSITY on 02/04/15. For personal use only.

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Section: Introductionmentioning

confidence: 93%

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Grimani

2013

Int. J. Mod. Phys. D

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“…Even if these results should be corrected by taking into account the geometrical acceptance of the radiation monitors, it will be quite difficult to associate the actual overall particle flux reaching the LISA-PF test masses during SEP events on the basis of radiation monitor measurements only. However, at the time of LISA-PF data taking, the AMS [56] and, hopefully, the PAMELA experiments will be in the orbit. These experiments are mainly devoted to the detection of antimatter in cosmic rays.…”

Section: Sep Monitoring With the Lisa-pf Particle Detectormentioning

confidence: 99%

On the role of radiation monitors on board LISA Pathfinder and future space interferometers

Grimani

Boatella

Chmeissani

et al. 2012

Class. Quantum Grav.

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LISA (Laser Interferometer Space Antenna) and its precursor mission LISA Pathfinder (LISA-PF) will carry particle monitors for noise diagnostics. It was proposed to build and place radiation detectors on board the ASTROD missions as well. We present here a study of the solar energetic particle (SEP) events that the LISA-PF radiation monitors are able to detect above the galactic cosmic-ray (GCR) background predicted at the time of the mission data taking in 2015. In order to optimize the correlation between radiation monitor measurements and gravitational sensor test-mass charging, the energy threshold for particles traversing both detectors should be approximately the same. In LISA-PF, the radiation monitor particle energy cut-off was conservatively set at 75 MeV per nucleon (MeV/n) for protons and ion normal incidence, while the minimum energy of the same particles reaching the test masses is 100 MeV/n. We find that SEP events detectable on LISA-PF are characterized by peak fluxes and fluences at energies >75 MeV/n larger than about 45%, on average, with respect to those at energies >100 MeV/n. We conclude that for an accurate correlation between radiation monitor count rates and test-mass charging, it is mandatory to benefit from absolute flux measurements of both galactic and high-energy solar particles provided by experiments carrying magnetic spectrometers in space at the time of LISA-PF (PAMELA, AMS). On the other hand, the role of the radiation detectors on board LISA-PF is crucial allowing for SEP event onset and dynamics monitoring.

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“…It is designed to measure cosmic ray particles in the rigidity (defined as R = p/Z in natural units, where R is rigidity, p is particle momentum and Z is charge) range from 1 GV to a few TV. The detector consists of the following subsystems: a nine-layer silicon tracker [2], seven of which are surrounded by a permanent magnet [3]; a transition radiation detector (TRD) [4]; four planes of time of flight scintillator counters (TOF) [5]; an array of anticoincidence counters (ACC) [6]; a ring imaging Cherenkov detector (RICH) [7]; and an electromagnetic calorimeter (ECAL) [8].…”

Section: Introductionmentioning

confidence: 99%

Antiproton identification below threshold with the AMS-02 RICH detector

Mendez

Giovacchini

et al. 2017

Chinese Phys. C

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The Alpha Magnetic Spectrometer (AMS-02) was installed on the International Space Station (ISS) and it has been collecting data successfully since May 2011. The main goals of AMS-02 are the search for cosmic anti-matter, dark matter and the precise measurement of the relative abundance of elements and isotopes in galactic cosmic rays. In order to identify particle properties, AMS-02 includes several specialized sub-detectors. Among them, the AMS-02 Ring Imaging Cherenkov detector (RICH) is designed to provide a very precise measurement of the velocity and electric charge of particles. We describe a method to reject the dominant electron background in antiproton identification with the use of the AMS-02 RICH detector as a veto for rigidities below 3 GV. Ray tracing integration method is used to maximize the statistics ofp with the lowest possible e − background, providing 4 times rejection power gain for e − background with respect to only 3% ofp signal efficiency loss. By using the collected cosmic-rays data, e − contamination can be well suppressed within 3% with β ≈ 1, while keeping 76% efficiency forp below the threshold.

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Background Estimation in MXGS Apparatus on International Space Station

Cited by 4 publications

References 7 publications

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

Implications of Galactic and Solar Particle Measurements on Board Interferometers for Gravitational Wave Detection in Space

On the role of radiation monitors on board LISA Pathfinder and future space interferometers

Antiproton identification below threshold with the AMS-02 RICH detector

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