Efficiency and sensitivity for the halo detector
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Efficiency and Sensitivity for the HALO Detector. Cara Esposito Saint Joseph’s University Dr. Kate Scholberg Duke University. Outline. Brief background on neutrinos, supernovae, and the HALO detector Efficiency and the important information gained from examining the efficiency

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Efficiency and Sensitivity for the HALO Detector

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Efficiency and Sensitivity for the HALO Detector

Cara Esposito

Saint Joseph’s University

Dr. Kate Scholberg

Duke University


Outline

  • Brief background on neutrinos, supernovae, and the HALO detector

  • Efficiency and the important information gained from examining the efficiency

  • Sensitivity for HALO

  • Summary


Background

  • The Equation above is for the probability of detecting flavor g at L for a two flavor case.

  • Although there are three flavors, the Δm2 remains

  • Normal Mass Hierarchy (NMH) has one heavy and two light mass states, while IMH has two heavy and one light mass state


Background

Before

After

  • Supernovae happen when a massive star can no longer sustain itself and it explodes

  • 99% of the energy of core collapse supernovae is neutrinos


Background

  • SNOLab in Canada

  • 79 tons of lead

  • 128 helium detectors

  • 2 km underground

  • HALO 2 is currently in the developing phase and will most likely use 1 kiloton of lead

Lead

Helium Detectors


Background

  • Visualization of the simulation using Geant4


How HALO Works

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How HALO Works

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How HALO Works

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How HALO Works

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How HALO Works

  • 1n

ν

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How HALO Works

  • 1n

ν

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How HALO Works

  • 1n

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How HALO Works

  • 1n

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Flux

  • The left panel is for inverted mass hierarchy

  • The right panel is for normal mass hierarchy


Energy Spectrum

  • From the energy deposited in the detector we can determine whether it’s a 1N or a 2N event.


Energy Spectrum

1N

2n

  • From the energy deposited in the detector we can determine whether it’s a 1N or a 2N event.


Efficiency

  • Tells us how well the detector works


Sensitivity

  • HALO 1’s sensitivity for 5kpc supernovae

  • Contours in which ninety percent of the number of one-neutron and two-neutron events fall

  • The different colored curves correspond to different spectral parameters


Sensitivity

  • For 10 kpc supernovae HALO 1 can only constrain extreme models


Sensitivity

  • HALO 2 ‘s discriminatory power will increase with a greater number of counts for 10 kpc supernovae.


Summary

  • Simulated neutron events in the HALO Geant4 simulator

  • Efficiency for 1N events is approximately 36%

  • Efficiency for 2N events is approximately 56%

  • HALO 1 has good sensitivity for 5 kpc supernovae, but can only constrain extreme models for 10 kpc supernovae

  • HALO 2 the larger the number of counts, the greater the yield for the discriminatory power


Acknowledgements

  • K.Scholberg, C.Walter, A.Himmel, Duke University High Energy Physics Neutrino Group

  • Triangle Universities Nuclear Laboratory's Research Experience for Undergraduates

  • Halo Collaboration/SNOLab


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