SADE ANITA Monte Carlo(SAM) Test Results Amir Javaid University of Delaware

Topics ● Introduction to SADE ANITA MC. ● Test Runs – List of test runs – Phase space for event generation – Event geometry analysis – Events Above analysis threshold – Electric Field at point payload analysis – Correlation of polarization and ray launch angle with Electric Field ● To do list

Introduction to SADE ANITA MC(SAM) ● The goal of SADE ANITA MC is to estimate the sensitivity of ANITA 1 & 2 for neutrinos and cosmic rays. ● For realistic ray tracing SAM uses depth dependent refractive index and attenuation models. ● Ray tracing is done using geocentric and topocentric (local) coordinates. ● AVZ parameterization is used to simulated neutrino and cosmic ray events. Cosmic ray events uses 10% Primary energy approxy parameterization. Electric field parameterization for cosmic rays is under construction. ● Flat ice/air and bedrock surfaces with no roughness are used. Surface slope and roughness implementation is under construction. ● Bedrock is assumed to be perfectly reflective. ● ANITA triggering model is incorporated in the MC but not properly tested yet.

List of Test Runs ● Cosmic rays core shower case 1. – Ice depth 0.5km & surface elevation 0km. ● Cosmic rays core shower case 2. – Ice depth 1.5km & surface elevation 3.5 km. ● Cosmic rays core shower case 3. – Ice depth from the Bedmap and surface elevation from the Ramp data with 100 m resolution. ● Neutrino case 1 – Ice depth 0.5km & surface elevation 0km. ● Neutrino case 2 – Ice depth 1.5km & surface elevation 3.5 km.

Phase Space for Event Generation ● Payload at -89degree latitude and -180 degree longitude. ● Event throw radius was 900 Km ● Simulation kept events for which payload height >100m in event Topocentric coordinates ● Throw Azimuthal Angles were degrees. The zenith angles for neutrinos were degrees and for Cosmic rays degrees. ● The plots on the right show a sample of generated events

Event Geometry Analysis The set of plots shown here are from Cosmic ray case 2 and 3.They present distributions of the following parameters involved in the simulation. ● Launch angle measure from shower axis. ● Arriving angle is the zenith of signal in payload local coordinates. ● Fresnel Factor ● Ray path in ice

Events Above Analysis Threshold To analyze the data from the simulation runs I have applied an Analysis threshold of 10^-5 mV/cm/GHz for Electric field. The easting and northing histograms on the right show the events above this threshold in blue. The histogram at the bottom show these events in dark red.

Electric Field at point payload Analysis The plot on top right show the Electric Field distribution for different cases. The plot on the right bottom shows describes the attenuation model used for the simulation. The Following are the counts of events that passed the analysis threshold

Correlation of polarization and ray launch angle with Electric Field

Effective Area Estimation To get the effevtive area plot shown on top right. I estimated Efield triggering threshold value from a10^19eV icemc run which is Eth =5.5*10^-7 V/m/MHz approx. Utilizing the Efield distribution for events above my analysis threshold for 10^19eV Cosmic ray run I scaled the energy by the following formula. E(scaled)=(Eth/E)*10^19eV Then I weighted the CR histogram events by total number of CR simulated events and then multiplied by total geometric area *10^15 sqcm sr inside the 500km horizon. Ice mc

To do List ● Cosmic ray Electric Field parameterization. ● Test the code with realistic ANITA trigger configuration ● Implement the surface slope and roughness for ice/air and bedrock

Event Geometry Analysis The set of plots shown here are from Cosmic ray case 2 and 3.They present distributions of the following parameters involved in the simulation. ● Launch angle measure from shower axis. ● Arriving angle is the zenith of signal in payload local coordinates. ● Fresnel Factor ● Ray path in ice

Correlation of polarization and ray launch angle with Electric Field

Effective Area Estimation To get the effevtive area plot shown on top right. I estimated Efield triggering threshold value from a10^19eV icemc run which is Eth =5.5*10^-7 V/m/MHz approx. Utilizing the Efield distribution for events above my analysis threshold for 10^19eV Cosmic ray run I scaled the energy by the following formula. E(scaled)=(Eth/E)*10^19eV Then I weighted the CR histogram events by total number of CR simulated events and then multiplied by total geometric area *10^15 sqcm sr inside the 500km horizon. Ice mc