The Tianshan Radio Experiment for Neutrino Detectio n. Olivier Martineau-Huynh NAOC G&C lunch talk May 28, 2014. Milky Way over 21CM array ( Gu Junhua ). Physics with UHE cosmic neutrinos. UHE neutrinos as a tool to study violent phenomena in the Universe
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NAOC G&C lunch talk May 28, 2014
MilkyWay over 21CM array (GuJunhua)
(Ke Fang et al., arXiv:1311.2044)
p+gCMB D+p+ + n.
p+ l +nl.
Great tool to studyUHECRs.
Ahlers et al., arxiv:1208.4181
Need for cheap / scalable /easilymaintainabledetector.
requires dense & large target:
Target = Earth
Extensive air shower
Eth ~1017 eV
(sensitivityevaluation TBC by
The GRAND project
- 220 days data subset
- 1.2 1010 triggers recorded
- 1.4 109coincidences
over TREND-50 array
Expected EAS trigger rate:
~100 events/day for E>1017 eV
Reconstrcuted source position
Background rejection is a key issue for EAS radio-detection.
Background sources: HV lines, radio emiters, train, cars, planes, thunderstorms…
Proton showers @ 1017eV
396 candidates in 320 live days.
Standard EAS signal:
focusedgroundpatern & rapid drop of amplitude
n-induced (~horizontal) shower:
no significant variation of amplitude alongshower axis
(but OK in lateral direction)
Linearpolarity, withP Bgeo & P shower direction
(q=66°, j = 354°)
b ~89° on all antennas
h ~7° on all antennas