LUNASKA neutrino search with the Parkes and ATCA telescopes

Bray, J. D.; Ekers, R. D.; Protheroe, R. J.; James, C. W.; Phillips, Chris; Roberts, P.; Brown, A. M.; Reynolds, John E.; McFadden, R.; Aartsen, M. G.

doi:10.1063/1.4807514

Cited by 9 publications

(9 citation statements)

References 26 publications

(43 reference statements)

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“…At EeV energies, relevant for the detection of cosmogenic neutrinos produced in the interactions of cosmic rays with background microwave photons, this is no longer the case and saturation effects must be included in evaluating the sensitivity of ARA [24], ANITA [25], ARIANNA [26], JEM-EUSO [27], and LUNASKA [28]. Our formalism provides a prediction of the EeV-neutrino cross section that, although relying on a (dipole) parameterization, is directly supported by a wealth of data.…”

Section: Introductionmentioning

confidence: 99%

High-energy behavior of photon, neutrino, and proton cross sections

et al. 2015

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By combining the color dipole model of the nucleon with the assumption that cross sections behave asymptotically as ln 2 (s), we are able to describe the data for photon, neutrino and hadron interactions with protons at all energies; s is the center-of-mass energy of the interacting particles. Specifically, we extrapolate the perturbative QCD calculations into the regime of small fractional parton momenta x using a color dipole description of the proton target that guarantees an asymptotic ln 2 (s) behavior of all cross sections. The ambiguity of introducing a parametrization associated with the dipole approximation is mitigated by the requirement that the saturation of the small-x structure functions produces ln 2 (s)-behaved asymptotic cross sections, in agreement with the data. The same formalism allows us to calculate the cross section for the hadronic pair production of charm particles. The results, in particular those for the high-energy neutrino and charm cross sections, are relevant for evaluating the sensitivity as well as the background in neutrino telescopes.

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Section: Introductionmentioning

confidence: 99%

High-energy behavior of photon, neutrino, and proton cross sections

et al. 2015

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“…For example, our 120-hour observations using the Kalyazin 64-m radio telescope (Russia) in the 1.4 GHz and 2.3 GHz frequency ranges [24] showed that the rate of the radio pulses resulting in interactions of neutrinos with energy above 10 20 eV with atoms of the lunar regolith does not exceed (200 hrs) −1 or 1.4 10 −6 sec −1 . In subsequent years many more attempts were undertaken to register the bursts of Cherenkov radio emission from the Moon using the Westerbork synthesis radio telescopes (The Netherlands), some part of the VLA antennae (USA), again the Parks 64-m radio telescope, and other radio astronomy tools [25][26][27][28][29]. The new essentially stronger upper limit to the EHE neutrino flux was obtained from these experiments.…”

Section: Ramhand: the Past And The Prospectsmentioning

confidence: 99%

Development of the radio astronomical method of cosmic particle detection for extremely high-energy cosmic ray physics and neutrino astronomy

et al. 2017

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Abstract. The proposal to use ground based radio telescopes for detection of Askaryan radio pulses from particle cascades arising when extremely high-energy (EHE > 10 20 eV) cosmic rays (including neutrinos) interact with the lunar regolith of multi gigaton mass was made at the end of 1980s in the framework of the Russian (Soviet) DUMAND Program. During more than a quarter of century a number of lunar experiments were carried out mainly in the 1-3 GHz frequency range using the large radio telescopes of Australia, USA, Russia and other countries but these experiments only put upper limits to the EHE cosmic rays fluxes. For this reason, it would be of great interest to search for nanosecond radio pulses from the Moon in a wider interval of frequencies (including lower ones of 100-350 MHz) with larger radio detectors -for example the giant radio telescope SKA (Square Kilometer Array) which is constructed in Australia, New Zealand and South Africa. In this paper possibilities are discussed to use one of the most sensitive meter-wavelength (∼ 110 MHz) Large Phased Array (LPA) of 187 × 384 m 2 and the wide field of view meter-wavelength array of the Pushchino Radio Astronomy Observatory as prototypes of low frequency radio detectors for lunar experiments. The new scheme for fast simulation of ultrahigh and extremely high-energy cascades in dense media is also suggested. This scheme will be used later for calculations of radio emission of cascades in the lunar regolith with energies up to 10 20 eV and higher in the wide frequency band of 0.1− a few GHz.

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“…In particular, Singh et al [40] have proposed lunar radio observations with LOFAR, an aperture array telescope currently in its commissioning phase, and Bray et al [41] have proposed continued use of the Parkes radio telescope used in this experiment, using one of the Phased Array Feed (PAF) receivers recently developed for ASKAP [42]. Both of these proposed experiments would utilise multiple beams pointing on the Moon with a real-time anticoincidence filtering scheme to identify lunarorigin Askaryan pulses.…”

Section: Considerations For Future Experimentsmentioning

confidence: 99%

A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

Bray

Ekers

Roberts

et al. 2015

Astroparticle Physics

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We describe an experiment using the Parkes radio telescope in the 1.2-1.5 GHz frequency range as part of the LUNASKA project, to search for nanosecond-scale pulses from particle cascades in the Moon, which may be triggered by ultra-highenergy astroparticles. Through the combination of a highly sensitive multi-beam radio receiver, a purpose-built backend and sophisticated signal-processing techniques, we achieve sensitivity to radio pulses with a threshold electric field strength of 0.0053 µV/m/MHz, lower than previous experiments by a factor of three. We observe no pulses in excess of this threshold in observations with an effective duration of 127 hours. The techniques we employ, including compensating for the phase, dispersion and spectrum of the expected pulse, are relevant for future lunar radio experiments.

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LUNASKA neutrino search with the Parkes and ATCA telescopes

Cited by 9 publications

References 26 publications

High-energy behavior of photon, neutrino, and proton cross sections

High-energy behavior of photon, neutrino, and proton cross sections

Development of the radio astronomical method of cosmic particle detection for extremely high-energy cosmic ray physics and neutrino astronomy

A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

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