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Measurement of the proton-air cross section with Telescope Array’s Middle Drum detector and surface array in hybrid mode

R. U. Abbasi et al. (Telescope Array Collaboration)
Phys. Rev. D 92, 032007 – Published 25 August 2015; Erratum Phys. Rev. D 92, 079901 (2015)

Abstract

In this work we are reporting on the measurement of the proton-air inelastic cross section σpairinel using the Telescope Array detector. Based on the measurement of the σpairinel, the proton-proton cross section σpp value is also determined at s=958+5TeV. Detecting cosmic ray events at ultrahigh energies with the Telescope Array enables us to study this fundamental parameter that we are otherwise unable to access with particle accelerators. The data used in this report are the hybrid events observed by the Middle Drum fluorescence detector together with the surface array detector collected over five years. The value of the σpairinel is found to be equal to 567.0±70.5[Stat]25+29[Sys]mb. The total proton-proton cross section is subsequently inferred from Glauber formalism and the Block, Halzen and Stanev QCD inspired fit and is found to be equal to 17044+48[Stat]17+19[Sys]mb.

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  • Received 7 May 2015
  • Corrected 14 September 2015

DOI:https://doi.org/10.1103/PhysRevD.92.032007

© 2015 American Physical Society

Corrections

14 September 2015

Erratum

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Vol. 92, Iss. 3 — 1 August 2015

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Images

  • Figure 1
    Figure 1

    The Telescope Array detector configuration. The filled squares are the 507 SD scintillators on a 1.2 km grid. The SD scintillators are enclosed by three fluorescent detectors shown in filled triangles together with their field of view in solid lines. The northernmost fluorescence detector is called Middle Drum while the southern fluorescence detectors are referred to as Black Rock Mesa and Long Ridge. The filled circle in the middle equally spaced from the three fluorescence detectors is the central laser facility used for atmospheric monitoring and detector calibration.

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  • Figure 2
    Figure 2

    The value of K vs the lower edge in the fit range Xi to the tail of the Xmax distribution for several data sets 1018.4, 1018.7, and 1019eV simulated using CONEX with the high-energy model QGSJETII.4. Each data set contains 10 000 simulated events.

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  • Figure 3
    Figure 3

    Λm (g/cm2) vs the lower edge in the fit range Xi to the tail of the Xmax distribution at an energy range of 1018.31019.3eV. The value of Λm is calculated using CONEX with the high-energy model QGSJETII.4 (square markers). These events were not propagated through the detector. In addition, the value of Λm is also calculated using CORSIKA (circle markers). These events successfully survived the pattern recognition cuts after they were successfully detected and reconstructed.

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  • Figure 4
    Figure 4

    The value of K obtained vs energy in Log10(eV) for simulated data sets using CONEX with the high-energy model QGSJETII.4, for the energy range of the data, between 1018.3 and 1019.3eV.

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  • Figure 5
    Figure 5

    The proton-air interaction length λpair in g/cm2 vs energy in Log10(eV) for the simulated data sets using CONEX with the high-energy model QGSJETII.4, for the energy range of the data, between 1018.3 and 1019.3eV. The circle points are the λpair values obtained from the X1 distribution. Triangle points are the ones determined from reconstructing the λpair values using the K-factor method.

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  • Figure 6
    Figure 6

    The number of events per Xmax bin (ΔXmax) vs Xmax g/cm2 for the Telescope Array data with the energy between 1018.3 and 1019.3eV. The line is the exponential fit to the slope.

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  • Figure 7
    Figure 7

    The proton-air cross section result of this work, including the statistical (outer/thinner) and systematic (inner/thicker) error bar. The result of this work is shown in comparison to other experimental results [1, 2, 28, 29, 30, 31, 32, 33, 34]. In addition, the high-energy models (QGSJETII.4, QGSJET01, SIBYLL, EPOS-LHC) cross section predictions are also shown by solid line, fine dashed line, dotted line, and dashed line consecutively.

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  • Figure 8
    Figure 8

    The elastic slope B in ((GeV/c)2) vs σpptotal in mb. The solid and the dotted curves are the relation between B and σpptotal for the constant value of the measured σpairinel by the Telescope Array detector and the statistical error using Glauber Formalism. The dashed line is the BHS QCD inspired fit [8]. While the gray shaded area is the unitarity constraint.

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  • Figure 9
    Figure 9

    The proton-proton cross section vs the center of mass energy result of this work, including the statistical (outer/thinner) and systematic (inner/thicker) error bars. The p¯p and the pp data are shown in smaller darker circles and square symbols consecutively [41]. The recent result from LHC is also shown by the star marker [42]. The result of this work is shown in comparison to previous work by cosmic rays detectors ([1, 2, 29, 32]). The dashed curve is the QCD inspired fit by BHS [7].

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