Bulletin of the American Physical Society
APS April Meeting 2014
Volume 59, Number 5
Saturday–Tuesday, April 5–8, 2014; Savannah, Georgia
Session S8: Radio in Ice: UHECR Cosmic-rays and Neutrinos |
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Sponsoring Units: DAP Chair: Amy Connolly, Ohio State University Room: 202 |
Monday, April 7, 2014 1:30PM - 1:42PM |
S8.00001: The Askaryan Radio Array: Status and Performance Ryan Maunu, Kara Hoffman, Mike Richman Ultra high energy neutrinos could be most efficiently detected in dense, radio frequency transparent media via the Askaryan effect. The Askaryan Radio Array is a new ultra high energy neutrino detector which will encompass a fiducial area of 100 square kilometers of the deep radio transparent ice near the South Pole. A ``Testbed'' and the first three clusters of antennae (out of 37 planned) have been installed to date. The primary science goal is the discovery of the cosmogenic neutrinos and measurement of the flux. We report on the science, design, and performance of this instrument, along with the prospects for completion of the detector construction. [Preview Abstract] |
(Author Not Attending)
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S8.00002: ARA testbed template based UHE neutrino search Steven Prohira The Askaryan Radio Array (ARA) is an in-ice Antarctic neutrino detector deployed near the South Pole. ARA is designed to detect ultra high energy (UHE) neutrinos in the range of 0.1-10 EeV. Data from the ARA testbed, deployed in the 2010-2011 season, is used for a template based neutrino search. [Preview Abstract] |
Monday, April 7, 2014 1:54PM - 2:06PM |
S8.00003: A cut-based search for ultra-high energy neutrinos with the ARA TestBed Eugene Hong, Amy Connolly, Carl Pfendner The cosmic ray flux cut off above primary energies of 10$^{19.5}$ eV lead us to expect an UHE neutrino flux due to the GZK effect. Askaryan Radio Array (ARA) is an ultra-high energy (UHE) cosmic neutrino detector located at the South Pole that uses the radio Cherenkov technique by deploying radio frequency antennas at a depth of 200m in the Antarctic ice. While there are three complementary ARA neutrino searches in progress, I present the result of the first neutrino search with 2011-2012 ARA TestBed data using a cut-based analysis. For the analysis, I use a Monte Carlo (MC) simulation named AraSim that is calibrated against TestBed calibration pulser data and thermal noise data. We generate custom radio Cherenkov signals in the ice in the time domain for each event with a fully parameterized model. Using timing differences measured at antennas within a single station, we use interferometric techniques to reject thermal noise and continuous wave (CW) backgrounds, and reconstructed directions to search for neutrino candidates in the ice. I will present the UHE neutrino flux constraints from all ARA TestBed analyses. [Preview Abstract] |
Monday, April 7, 2014 2:06PM - 2:18PM |
S8.00004: Time Domain Analysis of ARIANNA Data Acquisition: Distinguishing Askaryan Radiation from Thermal Backgrounds Jordan Hanson The Antarctica Ross Ice Shelf Antenna Neutrino Array (ARIANNA) is a high energy astrophysical neutrino detector, currently under construction near McMurdo Station, Antarctica. The ARIANNA detector design is optimized for detection of Askaryan radio frequency pulses, created in the ice shelf above the Antarctic ocean, that originate from cosmogenic GZK neutrino interactions. A formal analysis of the electromagnetic properties of the ARIANNA detection chain in the time domain is presented, and combined with a theoretical understanding of the Askaryan signal. This combination produces signal templates, used to distinguish thermal backgrounds from true signal in the current ARIANNA data. The results of this data analysis are also presented. [Preview Abstract] |
Monday, April 7, 2014 2:18PM - 2:30PM |
S8.00005: The ExaVolt Antenna Brian Dailey There are strong motivations for a flux of ultra-high energy (UHE) neutrinos that is observable on earth, yet they remain undetected. The proposed ExaVolt Antenna (EVA) uses a novel approach to increase the expected rate of neutrinos in a balloon-borne experiment such as ANITA by 100-fold by turning a 100m-diameter, long-duration, super pressure NASA balloon into an antenna reflector with receivers deployed in the interior of the balloon. EVA would be the world's largest airborne telescope with $\sim$ 1000 $m^{2}$ of collection area. I will present preliminary results from a 1:20 scale EVA prototype test conducted in early 2014 in a hangar at NASA's Wallops Flight Facility. I will conclude with the expected sensitivity of the full EVA experiment to UHE neutrino fluxes. [Preview Abstract] |
Monday, April 7, 2014 2:30PM - 2:42PM |
S8.00006: Radio Frequency Attenuation Length Estimates In Ice from Antarctic and Greenlandic Radar Depth Sounding Data Mark Stockham The balloon-borne Antarctic Impulsive Transient Antenna (ANITA) experiment is designed to detect in-ice neutrino collisions in Antarctica. These collisions produce radio waves that propagate upward to the suite of 32 horn antennas that constitute ANITA. The primary virtue of ANITA is the ability to simultaneously observe 1 million cubic kilometers of ice from its 38 kilometer altitude vantage point. The radio frequency signal strength observed at the balloon, however, depends on the radio frequency attenuation length of the ice through which the neutrino-generated signal must travel. Attenuation length is a location-specific ice property and varies mainly as a function of temperature and chemistry. The Center for Remote Sensing of Ice Sheets (CReSIS) project has data from many locations in Antarctica and Greenland produced by radar depth sounding. Using methods developed by analyzing the continuum signal in radar depth sounding data from Greenland, attenuation length estimates are compared to estimates derived from ice core data. [Preview Abstract] |
Monday, April 7, 2014 2:42PM - 2:54PM |
S8.00007: Optimization of energy reconstruction for ANITA III Viatcheslav Bugaev, Brian Rauch, Robert Binns, Martin Israel, Konstantin Belov, David Urdaneta, Joe Lam, Andrew Romero-Wolf, Stephanie Wissel The third flight of the high-altitude balloon-borne ANtarctic Impulsive Transient Antenna (ANITA III) planned for December 2014 will be optimized for the measurement of impulsive radio signals from the charged component of extensive air showers initiated by Ultra-High Energy Cosmic Rays (UHE CR) in the frequency range $\sim 80-\sim 1200$ MHz (RF), in addition to detection of radio impulses initiated by the high-energy neutrinos, which was the objective of the first two ANITA flights. Based on an extensive set of Monte Carlo simulations of radio emissions from CR with the ZHAireS simulation package, we propose a strategy of utilizing reconstructed RF spectra from individual showers optimized for the energy reconstruction of primary CR particles. The optimization, in particular, takes advantage of an extended sensitive frequency range of ANITA III due to adding a drop-down antenna shifting the lower limit from $\sim 180$ MHz to $\sim 80$ MHz. An idealized model of the detector is used in our study, in which RF spectra can be reconstructed to an arbitrary precision. [Preview Abstract] |
Monday, April 7, 2014 2:54PM - 3:06PM |
S8.00008: Ice surface roughness modeling for effect on radio signals from UHE particle showers Jessica Stockham For radio antenna detectors located in or above the Antarctic ice sheet, the reconstruction of both ultra-high energy (UHE) neutrino and cosmic ray air shower events requires understanding the transmission and reflection properties of the air-ice interface. To this end, surface and volume scattering from granular materials in the microwave frequency range are measured and stereoscopic images of the ice surface, obtained by the Antarctric Geophysics Along the Vostok Expedition (AGAVE), are used to determine the 3D surface structure. This data is implemented to determine an appropriate model for use in simulation and data analysis of the shower events. [Preview Abstract] |
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