Download or read book Characterizing the Search for Ultra high Energy Neutrinos with the ARIANNA Detector written by Kamlesh Dookayka and published by . This book was released on 2011 with total page 265 pages. Available in PDF, EPUB and Kindle. Book excerpt: The Antarctic Ross Ice-shelf ANtenna Neutrino Array (ARIANNA) experiment exploits unique properties of the Ross Ice Shelf, namely its radio transparency and reflectivity at the ice-water boundary beneath the shelf, to search for ultra-high energy neutrinos. It consists of an array of detectors embedded just beneath the surface with antennas facing down to listen to characteristic radio Cherenkov pulses generated by neutrino interactions in the ice. A simulation tool has been developed and used for optimization studies and to evaluate ARIANNA's energy-dependent aperture (effective volume & times steradians). This metric can be used to estimate the expected number of neutrinos detected from a given model prediction. The software and its physics, as well as the enhancements and additions to the original version, are described. We have included an improved treatment of the firn layer with an updated parametrization (based on latest measurements) of its graded index which impact signal path and polarization. Tau-neutrino interactions now take into account regeneration from their passage through Earth, and an approximation of the 'double-bang' effect. The antenna response is more accurately represented by averaging the relative gain in both E and H-planes. Studies show that ARIANNA can detect ~ 35 events/year from the GZK mechanism using the ESS model prediction. The high sensitivity results from nearly six months or more of continuous yearly operation, low energy threshold (> 3 x 1017 eV), large volume (513 km3), and a view of slightly more than half the sky (declination +30° to -90°). The rates of background events are consistent with thermal noise fluctuations. A new reconstruction framework has been devised for the energy and direction of a detected neutrino using measured parameters from a single station, such as relative time differences between antenna and signal amplitudes. Using simulated data, the energy and angular resolutions with a single station is calculated as delta E/ E ~ 2.2, sigma (theta) ~ 2.9°, sigma (phi) ~ 2.5° respectively. In addition to ARIANNA's potential for diffuse flux studies, these capabilities bode well for future UHE neutrino point source studies.

Download or read book A Search for Ultra High Energy Neutrinos and Cosmic Rays with ANITA 2 written by Matthew Joseph Mottram and published by Springer Science & Business Media. This book was released on 2012-07-10 with total page 150 pages. Available in PDF, EPUB and Kindle. Book excerpt: The winner of UCL's annual HEP thesis prize, this work describes an analysis of the data from the second flight of the Antarctica Impulsive Transient Antenna (ANITA). ANITA is a balloon-borne experiment that searches for radio signals originating from ultra-high energy neutrinos and cosmic rays interacting with the Antarctic ice or air. The search for ultrahigh energy neutrinos of astrophysical origin is one of the outstanding experimental challenges of the 21st century. The ANITA experiment was designed to be the most sensitive instrument to ultra-high energy neutrinos that originate from the interactions of cosmic rays with the cosmic microwave background. The methodology and results of the neutrino and cosmic ray searches are presented in the thesis.

Download or read book High Energy Neutrinos from Gamma Ray Bursts Theoretical Predictions Experimental Searches and Prospects for Detection written by Oindree Banerjee and published by Oindree Banerjee. This book was released on 2020-10-23 with total page 41 pages. Available in PDF, EPUB and Kindle. Book excerpt: Abstract Gamma-ray bursts (GRBs) are the most luminous transient events in the observed Universe. However, there is no direct observational evidence for what exactly drives a GRB. The most widely accepted model for these cosmic events is the fireball model where it is thought that a substantial fraction of the kinetic energy of the source is converted to gamma-radiation by shock accelerated electrons emitting synchrotron and inverse-Compton radiation. The acceleration of protons in the gamma-ray emitting region of the GRB has been hypothesized as well. In this hadronic acceleration model, it is predicted that protons may interact with gamma-ray photons to produce a burst of neutrinos at energy ∼10^14 eV during prompt emission and energy ∼10^18 eV during afterglow emission. Several experimental searches for these high energy neutrinos have been conducted and no GRB neutrinos have yet been found. The analytical prediction for neutrino flux has been replaced with a more thorough numerical prediction for neutrino flux. The neutron model of GRBs, where only neutrons can escape the GRB and reach Earth as cosmic rays, has been ruled out by the experimental work of IceCube and ANTARES. Upgraded versions of current experiments such as IceCube, ANTARES, ANITA and ARA, as well as new experiments such as KM3NeT, are preparing to probe and further constrain the fireball paradigm of GRB neutrino production. This review includes: Introduction Early theoretical predictions for neutrino fluences due to GRBs Overview of high energy neutrino experiments and related physics Experimental searches for high energy neutrinos from GRBs Prospects for detection of high energy neutrinos from GRBs High Energy Neutrinos from Gamma Ray Bursts: Theoretical Predictions, Experimental Searches, and Prospects for Detection was originally written as a review submitted for my Ph.D. candidacy paper on Nov 23, 2015. It has been edited for a "Short Read" on Amazon Kindle Direct Publishing in Oct 2020. It is a public domain work. Special thanks to the Connolly group at Ohio State University (OSU) and the physics and astronomy departments at OSU. Moreover, I am grateful for the contribution of each and every scientist and author listed in the "References" section of this review. This review would not be possible without their published science and hard work. Please let me know if you find any mistakes or problems, I will fix it. My email is [email protected]. I am happy for this to be a living document. I am anxious to improve it but feel that it needs to be out at this point before that can happen.

Download or read book Performance of Sub array of ARIANNA Detector Stations During First Year of Operation written by Joulien Tatar and published by . This book was released on 2013 with total page 152 pages. Available in PDF, EPUB and Kindle. Book excerpt: The ARIANNA high energy neutrino telescope is designed to search for ultrahigh energy neutrinos produced by the collision of cosmic rays with the cosmic microwave background. ARIANNA exploits the recent development of low noise, low power data acquisition technology to measure the brief radio pulses created by neutrino-induced charged particle showers in the Ross Ice Shelf of Antarctica. Three stations were installed and commissioned in early December 2012 as part of a pilot program to construct a hexagonal array of 7 radio stations. Each station required only 10 Watts of power and operated autonomously using both solar panels and wind generators. In addition, an environmental station was deployed at the ARIANNA site. Data is stored locally and reliably transmitted from Antarctica over high speed wireless internet and Iridium satellite modem during special transmission windows. The wireless internet ceased operation on March 15, corresponding to the fading light condition just before Austral winter. With the aid of wind generation, the stations operated until late May before winter hibernation. Communication was re-established after winter hibernation on September 11, 2013 for three of the four stations. Overall, the stations operated for 65% of the year. The station acquired three types of events: (1) forced, (2) thermal, and (3) signals from an external transmitter, which are called "heartbeat" events. The forced trigger captures the ambient RF conditions at a random snapshot in time. The thermal trigger configuration usually required any 2 of the 4 antenna channels to exceed a voltage level of ~ 6 x V[rms], where V[rms] is the root mean square of the random voltage fluctuations. Individual channel thresholds were adjusted to account for temperature dependences in the electronics. The vast majority of thermal triggers are consistent random gaussian noise expected from thermal processes in the ice and amplifier. Excess power, but no increase is trigger rates, is observed when wind speeds exceed ~ 6 mph. The frequency components of the excess noise are compatible with noise emitted by the wind generator. There are several periods of impulsive noise with durations of minutes to hours in January and narrowband, suggesting an origin from external transmitters. On one occasion, the noise was contemporaneous with rescue operations at McMurdo Station. Heartbeat events were collected in special runs in 4 separate time periods. They indicate that LPDA coupling to ice medium increased over the first few weeks as the pits with the receiver antennas filled in with snow, and then increased slowly as the snow overburden increased on the transmitting antenna, initially placed flat on the snow surface. We conducted a search for neutrino events in the data from Station 3 between December 6, 2012 and March 13, 2013 by cross-correlating observed waveforms in parallel receiver channels with the expected neutrino template in the time domain. The cross-correlation analysis rejects all thermal triggers and retains more than 90% of the simulated neutrino events. It is clear that none of the collected events contain waveforms that match the shape expected for neutrino signals in two parallel channels, but cross-correlation of waveforms with excess power during windy periods are systematically larger than thermal noise events. Thermal triggers with the largest cross-correlation values are clustered in time and, as described in the text, possess unusual characteristics that clearly indicate they are background processes. This analysis indicates that the ARIANNA site is RF quiet, and meets requirements of the ARIANNA project. Using the effective volume per station and measured live-time, a preliminary flux limit was obtained to be E2 0 [zero with line through it] ≤ 10̄̄̄ ̄5 GeV cm ̄2 s ̄1 sr ̄1 assuming a E ̄2 differential energy spectrum. Based on initial experience with station operation and control, data transmission, and event analysis, we conclude that main scientific and technological objectives HRA pilot program are met. Initially, it was planned to complete HRA this upcoming season, but due to the government shutdown and subsequent drawdown of Antarctic operations, HRA completion has been postponed until November 2014. The focus of those efforts will be to reduce the time and manpower to deploy a station, reduce the level of logistical support to transport equipment to field and maintain the field camp, and reduce the cost of station construction and testing.

Download or read book A Search for Ultra High Energy Neutrinos and Cosmic Rays with Anita 2 written by Springer and published by . This book was released on 2012-08-31 with total page 160 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book High Energy Astrophysical Neutrinos written by Debanjan Bose and published by Springer Nature. This book was released on 2021-12-07 with total page 75 pages. Available in PDF, EPUB and Kindle. Book excerpt: This book provides a pedagogical introduction to the likely sources of these neutrinos, their propagation and detection mechanisms. Detection of high energy neutrinos of extragalactic origin has led to an interdisciplinary field of research, involving astronomy, astrophysics and particle physics. An extensive review of various detectors and the observations is provided that consolidates the latest findings. Above a few tens of TeVs, neutrinos are conceived as more reliable messengers for astronomy than photons as these photons get absorbed in the background photon field. Determining the neutrino spectrum not only helps in exploring astrophysical objects like AGN, GRB, etc. but also allows us to study particle physics at unprecedented energies. This introductory book is intended to help advanced undergraduate and graduate students to get into the subject with ease, and it simultaneously caters to practicing theoretical or experimental physicists as a reference book.

Download or read book A Prototype Station for ARIANNA written by and published by . This book was released on 2010 with total page 15 pages. Available in PDF, EPUB and Kindle. Book excerpt: The Antarctic Ross Iceshelf Antenna Neutrino Array (ARIANNA) is a proposed detector for ultra-high energy astrophysical neutrinos. It will detect coherent radio Cherenkov emission from the particle showers produced by neutrinos with energies above about 1017 eV. ARIANNA will be built on the Ross Ice Shelf just off the coast of Antarctica, where it will eventually cover about 900 km2 in surface area. There, the ice-water interface below the shelf reflects radio waves, giving ARIANNA sensitivity to downward going neutrinos and improving its sensitivity to horizontally incident neutrinos. ARIANNA detector stations will each contain 4-8 antennas which search for brief pulses of 50 MHz to 1 GHz radio emission from neutrino interactions. We describe a prototype station for ARIANNA which was deployed in Moore's Bay on the Ross Ice Shelf in December 2009, discuss the design and deployment, and present some initial figures on performance. The ice shelf thickness was measured to be 572 +- 6 m at the deployment site.

Download or read book Advanced Pattern matching Trigger System Design for the ARIANNA High Energy Neutrino Detector written by Mahshid Roumi and published by . This book was released on 2014 with total page 105 pages. Available in PDF, EPUB and Kindle. Book excerpt: A neutrino is one of the universe's essential ingredients. Neutrinos are very hard to detect because they have no electrical charges and interact little with other particles. Thus, extremely large and sensitive detectors are required to detect neutrinos. The Antarctic Ross Ice shelf ANtenna Neutrino Array (ARIANNA) is a proposed detector for Ultra High Energy (UHE) astrophysical neutrinos. It consists of a surface array of radio receivers and can observe 1 ns radio pulses generated by UHE neutrino interactions with oxygen and hydrogen nuclei in the ice of the Ross Ice Shelf. Each ARIANNA station has four radio frequency antennas, four amplifiers, and a data acquisition system (DAQ). The DAQ of each station has four acquisition channels consisting of four daughter cards and a motherboard. Each daughter card has a custom CMOS digitization and real-time triggering circuitry (ATWD chip), and a field programmable gate array (FPGA) device. The Motherboard has four slots to connect with acquisition cards, another FGPA device for trigger control and data buffering, an embedded CPU with solid-state data storage, and interfaces to an Iridium satellite short burst data transceiver and a long-range wireless communications module. Each acquisition card includes an Advanced Transient Waveform Digitizer (ATWD) chip; a high speed analog sampling, real time pattern matching triggering and digitizing integrated circuit. It has the ability to acquire the incoming waveforms at 2 GHz with over 11-bits of dynamic range. In each station, the acquisition cards receive detected amplified RF signals simultaneously and store them into 128 samples. In addition, the ATWD has the ability to compensate for the fixed pattern noise (FPN) of the sampling and trigger circuitry, which are generated by variations in the gate to drain capacitance in the chip, or variations in the input offsets of the trigger comparators. If left uncorrected, FPN causes variations in trigger thresholds, effectively adding noise in the trigger. Calibration and cancellation of FPN is accomplished by programming per-comparator digital to analog converters to null the FPN at each comparator. After calibration, the RMS trigger noise is reduced by a factor of 3 to 4. The data acquisition system is capable of accepting three types of triggers: external, forced, and thermal. An external trigger acts upon an external electrical input signal much like an oscilloscope's trigger and is used in the laboratory or in the field during experimental studies. A forced trigger is one that is caused by the acquisition system's CPU, and is typically used to force the periodic collection of data that is unbiased by the system's thermal trigger. These "thermal" triggers are the most interesting: they are generated by the signals that the data acquisition system is collecting. Noise - or the rare neutrino events ARIANNA is searching for - will at times cause input signals to exceed trigger thresholds. To allow for low thresholds while keeping trigger rates from being swamped by noise, the thermal trigger system is set up to accept only signal-like events rather than mere noise. This includes requiring bipolar triggers on a per-channel basis over a very brief (~4 ns) time period, plus a requirement that a majority of data acquisition channels (e.g., any 3 out of 4 channels) must all trigger within a brief time window (e.g., 64 ns). These more stringent requirements are expected to capture the vast majority of neutrino events while limiting the rate of "events" due solely to noise. After any triggering event, the sampling of incoming signal is halted, digitized data is read out from the acquisition cards and is stored locally in a solid-state memory card, and then it is transmitted to UC Irvine for further processing over Iridium satellite modem or long-distance wireless communication. This dissertation focuses on the data acquisition system for ARIANNA, most particularly on the design and performance of its trigger system, including FPN calibration and correction and trigger efficiency.

Download or read book Search for Ultra High Energy Neutrinos with AMANDA II written by and published by . This book was released on 2007 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: A search for diffuse neutrinos with energies in excess of 105 GeV is conducted with AMANDA-II data recorded between 2000 and 2002. Above 107 GeV, the Earth is essentially opaque to neutrinos. This fact, combined with the limited overburden of the AMANDA-II detector (roughly 1.5 km), concentrates these ultra high-energy neutrinos at the horizon. The primary background for this analysis is bundles of downgoing, high-energy muons from the interaction of cosmic rays in the atmosphere. No statistically significant excess above the expected background is seen in the data, and an upper limit is set on the diffuse all-flavor neutrino flux of E2 [Phi]{sub 90%CL}

Download or read book Searching for Ultra high Energy Neutrinos in Water written by Ariana Cooper and published by . This book was released on 2005 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book The Performance and Initial Results of the ARIANNA Prototype written by Jordan Christian Hanson and published by . This book was released on 2013 with total page 294 pages. Available in PDF, EPUB and Kindle. Book excerpt: The Antarctic Ross Ice-shelf Antenna Neutrino Array (ARIANNA) experiment exploits serendipitous properties of the Ross Ice Shelf in Western Antarctica. The ice shelf forms the fiducial volume of an ultra-high energy (UHE) neutrino detector capable of observing cosmogenic neutrinos with energies in excess of 10^17 eV. The clarity of the shelf ice and the reflectivity of the ocean-ice interface enhance the detection of radio-frequency (RF) elec- tromagnetic pulses created by neutrino interactions via the Askaryan effect. An array of autonomous electronics stations outfitted with radio antennas listen for these pulses. A prototype station was designed in 2009, using sustainable power and RF trigger and dig- itization electronics. It was deployed in Moore's Bay in December 2009 during the Austral summer, and additional data was collected in two subsequent seasons after the system re- booted automatically during Austral spring. This data located and helped to remove local anthropogenic noise. A total of 90.4 days of live-time was achieved, with thermal noise as the single background. Additionally, data characterizing the environment of Moore's Bay was collected and used in the development of future power systems and RF electronics. The depth and dielectric properties of the ice beneath the detectors were calculated using data taken during the expeditions. The linear fit to the frequency-dependent, temperature- averaged attenuation length of radio waves is L = (500 ± 30 - (0.18 ± 0.05)f[MHz]) m, and the reflection coefficient at the oceanic interface is 0.70

Download or read book Searching for High Energy Neutrinos with AMANDA II Detector written by Jodi Ann Cooley-Sekula and published by . This book was released on 2003 with total page 164 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book A Search for Ultra high Energy Neutrinos and Cosmic Rays with ANITA 3 written by Ben Strutt and published by . This book was released on 2017 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book Searching for Ultra high Energy Neutrinos with Data from a Prototype Station of the Askaryan Radio Array written by Eugene S. Hong and published by . This book was released on 2014 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: The observed GZK cutoff in the cosmic ray spectrum has led to a strongly motivated expectation of an ultra-high energy (UHE) neutrino flux arising from the interactions between the highest energy cosmic rays and cosmic microwave background photons. Aside from these diffuse neutrinos, UHE neutrinos are also expected to be produced in the same astrophysics sources producing the UHE cosmic rays such as Gamma-Ray Bursts (GRB) and AGNs. Here, we discuss two UHE neutrino searches using data from the Askaryan Radio Array (ARA) prototype Testbed station: one search for a diffuse neutrino flux and another for neutrinos from GRBs. Testbed data from 2011 to 2012 are used for the searches in the thesis. We discuss how we define the analysis cuts, optimize the analysis cut parameters for maximum sensitivity to UHE neutrinos, estimate the number of background and neutrino events, and set neutrino flux constraints in the UHE region (>10^17eV). We use an optimistic flux model from Kotera et. al. 2010 as our baseline model and optimize our analysis cuts for this model. The GRB neutrino search follows the same analysis technique as the diffuse neutrino flux search with some modifications. A timing constraint for each GRB reduces the estimated background dramatically and therefore we can loosen some of our analysis cuts for the GRB neutrino search. We also present detailed descriptions about tools that are used for the searches such as AraSim, a Monte-Carlo simulation that we developed, and RaySolver, a code to carry out ray tracing in ice with a depth-dependent index of refraction model. We present constraints on the neutrino flux from the ARA Testbed for diffuse neutrinos and GRB neutrinos separately. These neutrino flux constraints and analysis techniques from the Testbed will provide a benchmark for the future deep ARA stations' analyses which are expected to improve neutrino flux constraints by a factor of three or more due to differences in the design of the stations.

Download or read book A Search for Ultra High Energy Neutrinos in Highly Inclined Events at the Pierre Auger Observatory written by and published by . This book was released on 2011 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavors above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associated systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E-2 differential energy spectrum the limit on the single-flavor neutrino is E2dN/dE 1.74 x 10sup-7/sup GeV cmsup-2/supssup-1/supsrsup-1/sup at 90% C.L. in the energy range 1 x 10sup17/supeV E

Download or read book A Search for Ultra high Energy Neutrinos and Cosmic Rays with ANITA 3 written by B. A. F. Strutt and published by . This book was released on 2017 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt:

Download or read book Acoustic Detection of Ultra high Energy Neutrinos written by Naoko Kurahashi and published by . This book was released on 2010 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt: Understanding the origin and evolution of cosmic accelerators by measuring ultra-high energy cosmic rays is one of the main goals of astroparticle physics. UHE neutrinos are thought to be better indicators of cosmic accelerators since they travel from their source undeflected by magnetic fields and unimpeded by interactions with the cosmic microwave background. Both cosmic rays and neutrinos have extremely low fluxes at these energies, which makes measurements difficult. Neutrino measurements have the added challenge of a longer interaction length that makes the atmosphere not suitable as a target. Here, we present the Study of Acoustic Ultra-high energy Neutrino Detection (SAUND) which uses an underwater acoustic sensor array spanning 1500 cubic kilometers to search for UHE neutrinos interacting in the ocean. A description of the data acquisition system, results of the background noise study, and an analysis based on an integrated 130 days of data are presented here. Two events are found to have properties compatible with UHE-neutrino-induced particle showers. Since our understanding of transient backgrounds is limited, a flux upper limit is set providing the most sensitive limit to date on UHE neutrinos using the acoustic technique.