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Summary Report of JEM-EUSO Workshop at KICP in Chicago
Instrumentation and Methods for Astrophysics · Submitted 15 Mar 2012
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The goal of the workshop was to discuss the physics reach of the JEM-EUSO mission and how best to implement a global ground based calibration system for the instrument to realize the physics goal of unveiling the origin of the highest energy cosmic rays.
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This document contains a summary of the workshop which took place on 22 - 24 February 2012 at the Kavli Institute of Cosmological Physics in the University of Chicago. The goal of the workshop was to discuss the physics reach of the JEM-EUSO mission and how best to implement a global ground based calibration system for the instrument to realize the physics goal of unveiling the origin of the highest energy cosmic rays.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
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| s0 | This document contains a summary of the workshop which took place on 22 - 24 February 2012 at the Kavli Institute of Cosmological Physics in the University of Chicago. | background 0.86 | 0.20 | 0.02 | asserted 1.00 |
| s1 | The goal of the workshop was to discuss the physics reach of the JEM-EUSO mission and how best to implement a global ground based calibration system for the instrument to realize the physics goal of unveiling the origin of the highest energy cosmic rays. | background 0.60 | 0.07 | 0.10 | asserted 0.97 |
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The paper
Original abstract
This document contains a summary of the workshop which took place on 22 - 24 February 2012 at the Kavli Institute of Cosmological Physics in the University of Chicago. The goal of the workshop was to discuss the physics reach of the JEM-EUSO mission and how best to implement a global ground based calibration system for the instrument to realize the physics goal of unveiling the origin of the highest energy cosmic rays.
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How the literature uses it
10 arXiv papers cite this in 12 sentences
Papers citing it · 6 sentences without a confident label
Uses its data or values 2 papers
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In Table 2, the results for the PAO FD real data [ref] , and the estimated number of UHECRs ($E>55$ EeV) to be detected using JEM-EUSO during 5 years of orbiting the earth onboard the ISS [ref] are shown.
A method to search for correlations of ultra-high energy cosmic ray masses with the large scale structures in the local galaxy density field · A method based on the measurement of the depth of EAS maximum · 0.99
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This innovative pathfinder mission will observe approximately $6 ×10^4 km^2 sr yr$ annually [ref] , a factor of 10 above Auger.
Ensemble Fluctuations of the Flux and Nuclear Composition of Ultra-High Energy Cosmic Ray Nuclei · Introduction · 0.89
Cites it as background 4 papers
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The Extreme Universe Space Observatory on the Japanese Experiment Module (JEM-EUSO) will be placed into orbit aboard the International Space Station (ISS) [ref] .
Sensitivity of JEM-EUSO to Ensemble Fluctuations in the Ultra-High Energy Cosmic Ray Flux · Introduction · 0.82
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This enhanced the prospects for detecting UHE neutrinos of cosmic origin, launched a number of related studies [ref] , and has fundamental implications for the design of experimental cosmic neutrino searches such as the past searches (AMANDA [ref] , ANITA [ref] , FORTE [ref] , GLUE [ref] , RICE [ref] ), those searches presently underway (ICECUBE [ref] , Baikal [ref] , ANTARES [ref] , HiRes [ref] , AUGER [ref] ), and those experiments under development (ARA [ref] , ARIANNA [ref] ) or proposed (JEM-EUSO [ref] ).
Implications of a Froissart bound saturation of $\gamma^*$-$p$ deep inelastic scattering. Part II. Ultra-high energy neutrino interactions · Introduction · 0.88
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The results depend on the behavior of structure functions at ultra-small $x$, down to $x∼10^-12$ for the neutrino energies $E_ν∼10^16$ GeV that will potentially be accessible at cosmic ray neutrino detectors now operating (ICECUBE [ref] , Baikal [ref] , ANTARES [ref] , HiRes [ref] , AUGER [ref] ), or under development (ARA [ref] , ARIANNA [ref] ) or proposed (JEM-EUSO [ref] ).
Connection of the virtual $\gamma^*p$ cross section of $ep$ deep inelastic scattering to real $\gamma p$ scattering, and the implications for $\nu N$ and $ep$ total cross sections · Neutrino-nucleon cross sections · 0.96
What it cites · 86 sentences without a confident label
Uses the method or tool of 2 papers
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This calculation is performed using a dedicated detector simulation package [ref] , together with a fast shower simulation allowing for large statistics.
ESAF: Full Simulation of Space-Based Extensive Air Showers Detectors · JEM-EUSO Mission · 1.00
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This calculation is performed using a dedicated detector simulation package [ref] , together with a fast shower simulation allowing for large statistics.
The JEM-EUSO Mission: Status and Prospects in 2011 · JEM-EUSO Mission · 1.00
Uses data or values from 16 papers
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JEM-EUSO will observe over $4 ×10^4$ km$^2$ sr yr at $E_GZK$ and reaches 100% exposure around $10^20$ eV where it observes $6 ×10^4$ km$^2$ sr yr annually [ref] , a factor of 10 above Auger.
The JEM-EUSO Mission: Status and Prospects in 2011 · Introduction · 0.80
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The exposure growth per unit time is given by [equation] In Fig. [ref] we show the annual exposure (growth in exposure by one year of operation) together with expected event rate on the basis of the energy spectrum reported by the Pierre Auger Collaboration [ref] .
The Pierre Auger Observatory I: The Cosmic Ray Energy Spectrum and Related Measurements · JEM-EUSO Mission · 0.96
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The discovery of the suppression has been confirmed by the Pierre Auger Collaboration, measuring $γ= 2.69 ±0.2 (stat) ±0.06 (syst)$ and $γ= 4.2 ±0.4 (stat) ±0.06 (syst)$ below and above $E = 4.0 ×10^19 eV$, respectively (the systematic uncertainty in the energy determination is estimated as 22%) [ref] .
Observation of the suppression of the flux of cosmic rays above 4x10^19eV · Introduction · 0.92
Cites as support 1 paper
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As a result, the most promising neutrino signal are quasi-horizontal showers initiated deep in the atmosphere [ref] .
On the detection of Ultra High Energy Neutrinos with the Auger Observatory · Neutrino Sensitivity · 0.96
Cites as background 6 papers
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Despite the fact that the existence of particles with energies reaching $10^20$ eV has been known for over 50 years [ref] , their origin continues to be an intriguing puzzle [ref] .
Astrophysical Origins of Ultrahigh Energy Cosmic Rays · Introduction · 0.91
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Despite the fact that the existence of particles with energies reaching $10^20$ eV has been known for over 50 years [ref] , their origin continues to be an intriguing puzzle [ref] .
The Astrophysics of Ultrahigh Energy Cosmic Rays · Introduction · 0.91
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Despite the fact that the existence of particles with energies reaching $10^20$ eV has been known for over 50 years [ref] , their origin continues to be an intriguing puzzle [ref] .
Ultrahigh Energy Cosmic Rays · Introduction · 0.91
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