Performance of drift chambers in a magnetic rigidity spectrometer for measuring the cosmic radiation

Hof, M.; Bremerich, M.; Menn, W.; Pfeifer, C.; Reimer, O.; Simon, M.; Mitchell, J. W.; Barbier, L.; Christian, E. R.; Ormes, J. F.; Streitmatter, R. E.; Golden, R. L.; Stochaj, S. J.

doi:10.1016/0168-9002(94)90516-9

Cited by 26 publications

(4 citation statements)

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“…Figure 8 shows the positron fraction measured in the two CAPRICE experiments along with other experimental results and theoretical predictions (Protheroe, 1982, Moskalenko andStrong, 1998) for positron secondary production. CAPRICE data do not confirm the possible indication of a primary component near 10 GeV claimed by Coutu et al (1999).…”

Section: Discussionmentioning

confidence: 92%

“…The balloon floated at an average atmospheric depth of 3.9 g/ cm2 for nearly 23 hours at a mean vertical cutoff rigidity of about 0.5 GV/c. The instrument (Figure 1) included from top to bottom a Ring Imaging Cherenkov (RICH) detector with a solid NaF radiator having a threshold Lorentz factor of 1.5 (Carlson et al, 1994), a time-of-flight system (ToF), a superconducting magnet spectrometer with a tracking system made by a stack of multiwire proportional chambers (MWPC) (G o Id en et al, 1991) and two drift chambers (Hof et al, 1994), and a 7-radiation-length silicon-tungsten imaging calorimeter (Bocciolini et al, 1996). The average maximum detectable rigidity (MDR) of this spectrometer was 175 GV/c.…”

Section: Introductionmentioning

confidence: 99%

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Measurements of cosmic-ray electrons and positrons by the Wizard/CAPRICE collaboration

Boezio

Barbiellini

Bonvicini

et al. 2001

Advances in Space Research

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Section: Discussionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Measurements of cosmic-ray electrons and positrons by the Wizard/CAPRICE collaboration

Boezio

Barbiellini

Bonvicini

et al. 2001

Advances in Space Research

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“…The MASS91 instrument, shown in Figure 1, is composed of a magnet spectrometer, a plastic scintillator time-of-flight (TOF) system, a gas Cerenkov counter, and an imaging calorimeter. The spectrometer consists of a single-coil superconducting magnet with a system of drift chambers (DCs) (Hof et al 1994) and multiwire proportional chambers (MWPCs) (Golden et al 1991). These were used to determine the particle's trajectory in the magnetic field.…”

Section: Instrumentmentioning

confidence: 99%

Measurement of Cosmic-Ray Antiprotons from 3.7 to 19 GeV

Hof

Menn

Pfeifer

et al. 1996

The Astrophysical Journal

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The antiproton-to-proton ratio, p/p, in cosmic rays has been measured in the energy range 3.7-19 GeV. This measurement was carried out using a balloon-borne superconducting magnetic spectrometer along with a gas Cerenkov counter, an imaging calorimeter, and a time-of-flight scintillator system. The measured p/p ratio was determined to be 1.24 Ϫ0.51 ϩ0.68 ϫ 10 Ϫ4. The present result, along with other recent observations, shows that the observed abundances of antiprotons are consistent with models in which antiprotons are produced as secondaries during the propagation of cosmic rays in the Galaxy.

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“…Results from 5.32 3 10 4 s are reported here. The IMAX magnetic spectrometer used a single-coil superconducting magnet [14] with drift chambers (DC) [15] and multiwire proportional chambers (MWPC) [14] giving 20 position measurements (12 DC,8 MWPC) in the bending direction and 12 (8 DC, 4 MWPC) in the nonbending direction. The most probable maximumdetectable rigidity (MDR), determined by the path integral of the magnetic field and the trajectory resolution, was 200 GV͞c for Z 1 particles.…”

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Measurement of 0.25–3.2 GeV Antiprotons in the Cosmic Radiation

et al. 1996

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The balloon-borne Isotope Matter-Antimatter Experiment (IMAX) was flown from Lynn Lake, Manitoba, Canada on 16 -17 July 1992. Using velocity and magnetic rigidity to determine mass, we have directly measured the abundances of cosmic ray antiprotons and protons in the energy range from 0.25 to 3.2 GeV. Both the absolute flux of antiprotons and the antiproton͞proton ratio are consistent with recent theoretical work in which antiprotons are produced as secondary products of cosmic ray interactions with the interstellar medium. This consistency implies a lower limit to the antiproton lifetime of ϳ10 7 yr.PACS numbers: 98.70. Sa, 14.20.Dh, 95.85.Ry Measurement of the antiproton abundance in the cosmic radiation bears strongly on questions ranging from the possibility of a baryon symmetric universe to characterizing the origin and transport of the cosmic rays. However, the interpretation of cosmic ray antiproton measurements has been very uncertain ever since their discovery by Golden et al. [1]. While antiprotons in the cosmic radiation are expected as "secondary" products of interactions of the primary cosmic radiation, principally protons, with the ambient interstellar medium (ISM) [2][3][4], the first positive measurements [1,5,6] reported higher antiproton fluxes than predicted by contemporary models of cosmic ray transport. Of the numerous explanations proposed (reviewed in Stephens and Golden [7]), one class assumed that secondary antiprotons are produced by cosmic ray protons and helium which have passed through more matter than implied by measured secondary͞primary ratios of heavier elements (e.g., boron͞carbon). Others considered "exotic" sources such as the evaporation of primordial black holes, the decay of dark matter, or acceleration in relativistic plasmas. It was also suggested that the excess could be a manifestation of a baryon symmetric cosmology [8]. The largest discrepancy was at ϳ200 MeV [6], where antiproton production in p-p interactions is heavily suppressed [7,9]; however, later measurements gave corresponding upper limits which were significantly lower [10,11]. The Isotope Matter-Antimatter Experiment (IMAX) [12] and other recent experiments [13] were designed to clarify these issues.The fluxes of antiprotons and protons from ϳ0.2 to 3.2 GeV were measured by IMAX using magnetic rigidity, ionization energy loss, and velocity measurements to determine the charge (from energy loss and b) and mass (from Z, b, and rigidity) of incident particles. Data were taken for ϳ16 h at an average altitude of 36 km C2 and C3) [17] with n 1.043 silica-aerogel radiators (giving b Ck ). A third Cherenkov counter (C1) was not used in the current analysis. For Z 1, b 1 particles, the TOF resolution (s) was 122 ps and the yields from C2 and C3 were 11 and 13 photoelectrons. The sum of the signals expected from C2 and C3 for a Z 1, b 1 particle was normalized to 1. Energy loss was measured by the TOF and scintillators S1 and S2. Agreement was required among the four resulting charge measurements.Tracking quali...

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Performance of drift chambers in a magnetic rigidity spectrometer for measuring the cosmic radiation

Cited by 26 publications

References 10 publications

Measurements of cosmic-ray electrons and positrons by the Wizard/CAPRICE collaboration

Measurements of cosmic-ray electrons and positrons by the Wizard/CAPRICE collaboration

Measurement of Cosmic-Ray Antiprotons from 3.7 to 19 GeV

Measurement of 0.25–3.2 GeV Antiprotons in the Cosmic Radiation

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