Measurement of the flux of ultra high energy cosmic rays by the stereo technique

Abbasi, Rasha; Abu‐Zayyad, T.; Al-Seady, M.; Allen, M.; Amann, J. F.; Archbold, G.; Belov, K.; Belz, J. W.; Bergman, D. R.; Blake, S. A.; Brusova, O.; Burt, G. W.; Cannon, C.; Cao, Zhen; Deng, W.; Fedorova, Y.; Findlay, J.; Finley, C.; Gray, R.; Hanlon, W.; Hoffman, C. M.; Holzscheiter, M. H.; Hughes, G.; Hüntemeyer, P.; Ivanov, D.; Jones, B. F.; Jui, C.; Kim, K.; Kirn, M.; Loh, E. C.; Maestas, M. M.; Manago, Naohiro; Marek, Lukáš; Martens, K.; Matthews, John; Matthews, J. N.; Moore, Sheva; O’Neill, A.; Painter, C. A.; Perera, L.; Reil, K.; Riehle, R.; Roberts, M.; Rodriguez, D.; Sasaki, M.; Schnetzer, S.; Scott, L. M.; Sinnis, G.; Smith, J. D.; Snow, R.; Sokolsky, P.; Springer, R. W.; Stokes, B. T.; Stratton, S. R.; Thomas, J. R.; Thomas, S. B.; Thomson, G. B.; Tupa, D.; Wiencke, L.; Zech, A.; Zhang, B. K.; Zhang, X.; Zhang, Y.

doi:10.1016/j.astropartphys.2009.06.001

Cited by 94 publications

(76 citation statements)

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“…Theorists and phenomenologists can improve on the model predictions and test them not only with UHECR data but also with a large number of multi-messenger information being collected with photons (from radio to gamma-rays) and neutrinos (e.g., two cosmic neutrinos of PeV energies were recently reported by IceCube [58]). The particle physics effort will certainly gain with LHC data and deeper understanding 02001-p. 9 of the observed shower properties. However, the observational challenge at ultrahigh energies is crucial to solving this puzzle.…”

Section: Uhecr 2012mentioning

confidence: 99%

“…The question of the existence of a GZK feature in the spectrum above tens of EeV (EeV = 10 18 eV) was successfully answered by the most recent generation of UHECR observatories, beginning with the High Resolution Fly's Eye (HiRes) results [7][8][9] followed by a significant jump in statistics by the Pierre Auger Observatory [10,11], and most recently the Telescope Array (TA) [12]. Figure 1 shows a compilation of the cosmic ray spectrum (multiplied by E 2 ) from TeV (= 10 12 eV) to ZeV (ZeV = 10 21 eV) energies.…”

Section: Introductionmentioning

confidence: 99%

“…The existence of the GZK effect had been already challenged by observations in 1963 of a trans-GZK event (and event above 60 EeV) by Linsley [3], but much higher statistics observations by AGASA [4] suggested the need to go beyond known physics to explain the absence of a Figure 1. All particle cosmic ray flux multiplied by E 2 observed by ATIC [13], Proton [14], RUNJOB [15], Tibet AS- [16], KASCADE [17], KASCADE-Grande [18], HiRes-I [9], HiRes-II [8], and Auger [11]. LHC energy reach of p − p collisions (in the frame of a proton) is indicated for comparison.…”

Section: Introductionmentioning

confidence: 99%

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UHECR theory and phenomenology: Summary and outlook

Olinto

2013

EPJ Web of Conferences

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Abstract. Theorists and phenomenologists have contributed significantly to the development of the field of ultrahigh energy cosmic rays (UHECRs). Great progress has been achieved in modeling hadronic interactions, developing precise propagation codes, understanding the role of different backgrounds and magnetic fields in the propagation of ultrahigh energy protons and nuclei, predicting the flux of secondary neutrinos and photons, modeling astrophysical sources and their acceleration mechanisms, developing new techniques to test anisotropies in the sky distribution, proposing new physics phenomena that can be tested at ultrahigh energy, and sharpening the distinction between astrophysical interpretations of unexpected trends (such as the composition at the highest energies) and new physics at play in hadronic interactions at energies well beyond the reach of terrestrial laboratories. Better developed models when combined with recent data have framed current open questions. 1. Is the spectral feature at the highest energies the GZK cutoff or the effect of E max ? 2. Is the composition of primaries changing at the highest energies or are new interactions responsible for the change in behavior of extensive air showers? 3. At what energy and sensitivity will sources be observed? 4. At what energies cosmic rays transition from being Galactic to becoming extragalactic? And the most basic question remains, 5. what are the sources (and the acceleration mechanism) of ultrahigh energy cosmic rays? To answer these questions more observations are needed. Chief among the theorists' wish list is the increase in statistics at the highest energies and the second wish is for full sky coverage. These efforts should lead to the localization of a source (or sources) in the sky which would revolutionize the field. Another avenue for major progress would be the detection of neutrino and photon secondaries, especially at ultrahigh energies. More immediate progress can be reached with a better establishment of an absolute energy scale which has a direct impact on many models. Another fertile area is the ongoing tests of hadronic interaction models with the LHC. More precise measurements of airshower properties may also enable the distinction between primary composition and hadronic physics effects on a wide energy range. Joint anisotropy and composition analysis between the two leading experiments (Auger and TA) would also provide a much needed consistency between the two hemispheres. This meeting marks the beginning of a great effort in this direction.

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Section: Uhecr 2012mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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UHECR theory and phenomenology: Summary and outlook

Olinto

2013

EPJ Web of Conferences

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“…Since at this energy range those losses are the dominant factor in reshaping the proton spectrum and diffusion effects are minimal, we have restricted ourselves to one-dimensional simulations. The spectra (black dots) are compared to observations from Auger [22] (open triangles), HiRes-I [23] (open squares) and Telescope Array [24] (x's). The resulting UHECR spectra, neglecting any energy losses and propagation effects, are plotted for comparison reasons with a dashed line.…”

Section: The Leptohadronic-synchrotron (Lhs) Modelmentioning

confidence: 99%

Time dependent photon and neutrino emission from Mkr 421 in the context of the one-zone leptohadronic model

Mastichiadis

Πετροπούλου

Dimitrakoudis

2013

EPJ Web of Conferences

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Abstract. We apply a recently developed time-dependent one-zone leptohadronic model to study the emission of the blazar Mrk 421. Both processes involving proton-photon interactions, i.e. photopair (Bethe-Heitler) and photopion, have been modeled in great detail using the results of Monte Carlo simulations, like the SOPHIA event generator, in a self-consistent scheme that couples energy losses and secondary injection. We find that TeV gamma-rays can be attributed to synchrotron radiation either from relativistic protons or, alternatively, from secondary leptons produced via photohadronic processes. We also study the variability patterns that each scenario predicts and we find that while the former is more energetically favored, it is the latter that produces, in a more natural way, the usual quadratic behavior between X-rays and TeV gamma-rays. We also use the obtained SEDs to calculate in detail the expected neutron and neutrino fluxes that each model predicts.

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“…One is the HiRes experiment, operating between 1999 and 2004 in stereo mode with two fluorescence detectors (Abbasi et al, 2009a). The other is the southern PAO array which is taking data since 2004 with a hybrid technique of fluorescence telescopes and Cherenkov detectors.…”

Section: Instruments and Data Samplesmentioning

confidence: 99%

Directional correlations between UHECRs and neutrinos observed with IceCube

Lauer¹

2011

Astrophys. Space Sci. Trans.

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Abstract.Ultra-high energy cosmic rays (UHECR) above an energy threshold of tens of EeV might undergo only small deflections due to interstellar magnetic fields. Their arrival directions would then point to regions of possible hadronic acceleration processes, which are likely to be also sources of high energy neutrinos. To search for such cosmic accelerators, we present here the first high statistics analysis of directional correlations between neutrino candidates from the IceCube Observatory and UHECR events. Data taken with IceCube in a configuration of 22 strings provided the basis for using published events from both the Pierre Auger Observatory and the HiRes experiment as reference directions in a search for coincidences with neutrinos. The analysis was optimized according to strict blindness criteria and showed an excess of neutrino candidates close to UHECR directions with a probability of 1% to occur as a random fluctuation, consistent with a background-only hypothesis. An extension of this analysis to include newer IceCube data, taken with 40 strings and using a likelihood analysis, is discussed in the outlook.

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Measurement of the flux of ultra high energy cosmic rays by the stereo technique

Cited by 94 publications

References 20 publications

UHECR theory and phenomenology: Summary and outlook

UHECR theory and phenomenology: Summary and outlook

Time dependent photon and neutrino emission from Mkr 421 in the context of the one-zone leptohadronic model

Directional correlations between UHECRs and neutrinos observed with IceCube

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