Difference between revisions of "Data Rates"

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= Solar =
 
= Solar =
 
== References ==
 
== References ==
* 6212
+
* {{DocDB|6212|DocDB 6212}} - M.Smy's slides from 2012 (LBNE solar studies  potential)
 +
 
 
== Muon and Neutron Backgrounds ({{Cl40}}) ==
 
== Muon and Neutron Backgrounds ({{Cl40}}) ==
 
[[File:Solar_bkg_1.png|500px]]
 
[[File:Solar_bkg_1.png|500px]]

Revision as of 22:20, 10 March 2015

Disclaimer

This page is in initial stages of construction.

Overview

According to the physics goals of the experiment, we need to consider the following main sources of signal:

  • The "beam neutrino" signal
  • The Supernova Burst (SNB) signal
  • Proton Decay
  • Solar neutrinos

All these signals have distinct energy scales, topologies and other characteristics. In terms of buffering and processing data in real or near time, they pose different requirements.

Beam Neutrinos

Because of the energy scale (~GeV range) neutrino interactions will be characterized by TPC signals well above radiological background. Zero-suppression will lead to significant reduction of data volume and rates (the detector will appear "empty" for the most part).

SNB

Reactions

νe+40Ar ⇒ e-+40K*

ν e+40Ar ⇒ e++40Cl*

νx+40Ar ⇒ νx+40Ar*

νe,x+e- ⇒ νe,x+e-

References

  • DocDB 6977 - Software for low-energy signals
  • DocDB 8481 - Summary of SNB Working Group Progress (February 2014)

Some reference curves from DocDB 6977:

SNB spectrum 1.png

In a nutshell:

  • approximately 100 events per kiloton, spread over ~30 seconds, ~½ in first second
  • all flavors, few tens of MeV

Solar

References

  • DocDB 6212 - M.Smy's slides from 2012 (LBNE solar studies potential)

Muon and Neutron Backgrounds (40Cl)

Solar bkg 1.png

Background Sources

References

Important radiologicals

  • 39Ar 1.01 Bq/kg β- End-point: 0.565MeV
  • 85Kr 0.1-0.3 Bq/kg β- End-point: 0.687MeV