T.-C. Liu

Performance of two Askaryan Radio Array stations and first results in the search for ultrahigh energy neutrinos

Ultrahigh energy neutrinos are interesting messenger particles since, if detected, they can transmit exclusive information about ultrahigh energy processes in the Universe. These particles, with energies above 1016 eV, interact very rarely. Therefore, detectors that instrument several gigatons of matter are needed to discover them. The ARA detector is currently being constructed at the South Pole. It is designed to use the Askaryan effect, the emission of radio waves from neutrino-induced cascades in the South Pole ice, to detect neutrino interactions at very high energies. With antennas distributed among 37 widely separated stations in the ice, such interactions can be observed in a volume of several hundred cubic kilometers. Currently three deep ARA stations are deployed in the ice, of which two have been taking data since the beginning of 2013. In this article, the ARA detector “as built” and calibrations are described. Data reduction methods used to distinguish the rare radio signals from overwhelming backgrounds of thermal and anthropogenic origin are presented. Using data from only two stations over a short exposure time of 10 months, a neutrino flux limit of 1.5 × 10−6 GeV=cm2=s=sr is calculated for a particle energy of 1018 eV, which offers promise for the full ARA detector.

Determination of the neutrino flavor ratio at the astrophysical source

We discuss the reconstruction of neutrino flavor ratios at astrophysical sources through the future neutrino-telescope measurements. Taking the ranges of neutrino mixing parameters

Simulating neutron propagations with FLUKA, GEANT4 and MCNP

{\ensuremath{\theta}}_{ij}

Design and Fabrication of Detector Module for UFFO Burst Alert & Trigger Telescope

as those given by the current global fit, we demonstrate by a statistical method that the accuracies in the measurements of energy-independent ratios

Design and implementation of the UFFO burst alert and trigger telescope

R\ensuremath{\equiv}\ensuremath{\phi}({\ensuremath{\nu}}_{\ensuremath{\mu}})/(\ensuremath{\phi}({\ensuremath{\nu}}_{e})+\ensuremath{\phi}({\ensuremath{\nu}}_{\ensuremath{\tau}}))

Antarctic Surface Reflectivity Measurements from the ANITA-3 and HiCal-1 Experiments

and

THE UFFO SLEWING MIRROR TELESCOPE FOR EARLY OPTICAL OBSERVATION FROM GAMMA RAY BURSTS

S\ensuremath{\equiv}\ensuremath{\phi}({\ensuremath{\nu}}_{e})/\ensuremath{\phi}({\ensuremath{\nu}}_{\ensuremath{\tau}})

Flavor transition mechanisms of propagating astrophysical neutrinos: A model independent parametrization

among integrated neutrino flux should both be better than 10% in order to distinguish between the pion source and the muon-damped source at the

Probing Neutrino Mass Hierarchy by Comparing the Charged-Current and Neutral-Current Interaction Rates of Supernova Neutrinos

3\ensuremath{\sigma}

Readout of the UFFO Slewing Mirror Telescope to detect UV/optical photons from Gamma-Ray Bursts

level. The 10% accuracy needed for measuring