Chiba, July 29, 2003Tom Gaisser Comments on atmospheric muon and neutrino backgrounds in neutrino telescopes Use semi-analytic estimates to display some systematic features of atmospheric muons and neutrinos deep underground

Chiba, July 29, 2003Tom Gaisser Muons at depth From report of the Neutrino Facilities Assessment Committee

Chiba, July 29, 2003Tom Gaisser Muons at depth (P. Desiati et al., ICRC2003) From report of the Neutrino Facilities Assessment Committee

Chiba, July 29, 2003Tom Gaisser  energy spectra at depth See D Chirkin et al. for application to calibrating N hit in AMANDA

Chiba, July 29, 2003Tom Gaisser Response functions for  at depth Fraction of multi-  :.08,.05,..03,.02,.01, decreases as depth increases

Chiba, July 29, 2003Tom Gaisser Muon multipliclity in coincident events Area--solid-angle ~ 1/3 km 2 sr (including angular dependence of EAS trigger)

Chiba, July 29, 2003Tom Gaisser Neutrino response Neutrino energy Primary energy / nucleon

Chiba, July 29, 2003Tom Gaisser K/  bigger for than for  Flavor-dependence of horizontal/vertical

Chiba, July 29, 2003Tom Gaisser Compare primary response of -induced  to atmospheric  Response for atmospheric

Chiba, July 29, 2003Tom Gaisser Primary spectrum  muons

Chiba, July 29, 2003Tom Gaisser Global atmospheric spectrum Prompt  ee Solar  Plot shows sum of neutrinos + antineutrinos Slope = 3.7 Slope = 2.7

Chiba, July 29, 2003Tom Gaisser Summary Characteristic E  ~ GeV gives tag for energy calibration of neutrino telescope Response functions allow analysis of uncertainty from primary spectrum – -induced muon reponse independent of depth – response of atmospheric  depends on depth –<10% multiple muons when triggering on deep detector, but air shower trigger  multi-mu