Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003.

Slides:



Advertisements
Similar presentations
ICECUBE & Limits on neutrino emission from gamma-ray bursts IceCube collaboration Journal Club talk Alex Fry.
Advertisements

London Collaboration Meeting September 29, 2005 Search for a Diffuse Flux of Muon Neutrinos using AMANDA-II Data from Jessica Hodges University.
AMANDA Lessons Antarctic Muon And Neutrino Detector Array.
AJ Heroux with Teresa Montaruli. Playing in the Snow!! Outline –What is IceCube? History Deployment DOMS IceTop –Shadow of the moon Motivation Methods.
Searching for the footprint of prompt atmospheric neutrino flux and beyond Guey-Lin Lin National Chiao-Tung U. Taiwan With N. Tung and F.-F. Lee KEKPH.
Reso Shanidze 1 Theoretical Bounds and Current Experimental Limits on the Diffuse Neutrino Flux Rezo Shanidze 17/06/2004 Seminar zu aktuellen.
EUSO: Extreme Universe Space Observatory Jessica Cerny Bancroft-Rosalie School.
IceCube By:Nicole Baker ~Waterloo What is IceCube? IceCube is a one-cubic-kilometer international high- energy neutrino observatory being built and installed.
Calorimetry and Showers Learning Objectives Understand the basic operation of a calorimeter (Measure the energy of a particle, and in the process, destroy.
An accelerator beam of muon neutrinos is manufactured at the Fermi Laboratory in Illinois, USA. The neutrino beam spectrum is sampled by two detectors:
Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford.
M. Kowalski Search for Neutrino-Induced Cascades in AMANDA II Marek Kowalski DESY-Zeuthen Workshop on Ultra High Energy Neutrino Telescopes Chiba,
A Search for Point Sources of High Energy Neutrinos with AMANDA-B10 Scott Young, for the AMANDA collaboration UC-Irvine PhD Thesis:
SUSY06, June 14th, The IceCube Neutrino Telescope and its capability to search for EHE neutrinos Shigeru Yoshida The Chiba University (for the IceCube.
Gary C. Hill, CCAPP Symposium 2009, Ohio State University, October 12th, 2009 Photograph: Forest Banks Gary C. Hill University of Wisconsin, Madison for.
GLAST Simulations Theodore E. Hierath Louisiana State University August 20, 2001.
The ANTARES Neutrino Telescope Mieke Bouwhuis 27/03/2006.
LHC ~E -2.7 ~E -3 ankle 1 part km -2 yr -1 knee 1 part m -2 yr -1 T. Gaisser 2005 Nature accelerates particles 10 7 times the energy of LHC! where?how?
Special Issues on Neutrino Telescopy Apostolos G. Tsirigotis Hellenic Open University School of Science & Technology Particle and Astroparticle Physics.
Atmospheric Variations as observed by IceCube HE Serap Tilav 1, Paolo Desiati 2, Takao Kuwabara 1, Dominick Rocco 2, Florian Rothmaier 3, Matt.
EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara for the IceCube collaboration Chiba University.
Petten 29/10/99 ANTARES an underwater neutrino observatory Contents: – Introduction – Neutrino Astronomy and Physics the cosmic ray spectrum sources of.
Special Issues on Neutrino Telescopy Apostolos G. Tsirigotis Hellenic Open University School of Science & Technology Particle and Astroparticle Physics.
Frontiers in Contemporary Physics: May 23, 2005 Recent Results From AMANDA and IceCube Jessica Hodges University of Wisconsin – Madison for the IceCube.
AMANDA Results from the AMANDA neutrino telescope Carlos P. de los Heros Department of High Energy Physics Uppsala University.
CIPANP 2006K. Filimonov, UC Berkeley From AMANDA to IceCube: Neutrino Astronomy at the South Pole Kirill Filimonov University of California, Berkeley.
Why Neutrino ? High energy photons are absorbed beyond ~ 150Mpc   HE  LE  e - e + HE s are unique to probe HE processes in the vicinity of cosmic.
8 th Jan, NuHoRIzons, HRI, Allahabad Atsushi Watanabe (Harish-Chandra Research Institute) In collaboration with Raj Gandhi (HRI) Abhijit Samanta.
Cosmic Rays GNEP Teacher Workshop Steve Shropshire, July 2007.
The ANTARES neutrino telescope is located on the bottom of the Mediterranean Sea, 40 km off the French coast. The detector is installed at a depth of 2.5.
AMANDA. Latest Results of AMANDA Wolfgang Rhode Universität Dortmund Universität Wuppertal for the AMANDA Collaboration.
AMANDA Per Olof Hulth The Wierdest wonder Is it good or is it bad?
Data collected during the year 2006 by the first 9 strings of IceCube can be used to measure the energy spectrum of the atmospheric muon neutrino flux.
Mumbai, August 1, 2005 Tom Gaisser Atmospheric neutrinos Primary spectrum Hadronic interactions Fluxes of muons and neutrinos Emphasis on high energy.
The AMANDA-II Telescope - Status and First Results - Ralf Wischnewski / DESY-Zeuthen for the AMANDA Collaboration TAUP2001, September.
Status and Results Elisa Bernardini DESY Zeuthen, Germany VLVnT Workshop Amsterdam, Oct (
Searching for a Diffuse Flux of Neutrinos with AMANDA-II Jessica Hodges November 5, 2004 Prelim Exam.
Atmospheric Variations as observed by IceCube HE Serap Tilav 1, Paolo Desiati 2, Takao Kuwabara 1, Dominick Rocco 2, Florian Rothmaier 3, Matt.
QuarkNet and Cosmic Ray Muon Flux Experiments Florida Academy of Sciences Spring Conference 2009 Alfred Menendez and Michael Abercrombie with Dr. Marcus.
1 Raghunath Ganugapati(Newt) Preliminary Exam 08/27/04 Strategies for the search for prompt muons in the downgoing atmospheric muon flux with the AMANDA.
Study of the Atmospheric Muon and Neutrinos for the IceCube Observatory Ryan Birdsall Paolo Desiati, Patrick Berghaus,
Nucleon Decay Search in the Detector on the Earth’s Surface. Background Estimation. J.Stepaniak Institute for Nuclear Studies Warsaw, Poland FLARE Workshop.
High-energy gammas from the giant flare of SGR of December 2004 in AMANDA Juande D. Zornoza on behalf of the IceCube.
STUDY OF HIGH ENERY HADRONIC INTERACTION MODELS USING CORSIKA SIMULATION Raghunath Ganugapati (Newt), John Kelley, Teresa Montaruli, and Albrecht Karle.
Atmospheric Neutrinos Phenomenology and Detection p 00 ++  e+e+ e-e- ++  Michelangelo D’Agostino Physics C228 October 18, 2004.
Search for diffuse cosmic neutrino fluxes with the ANTARES detector Vladimir Kulikovskiy The ANTARES Collaboration 3-9 August 2014ANTARES diffuse flux.
Search for a Diffuse Flux of TeV to PeV Muon Neutrinos with AMANDA-II Detecting Neutrinos with AMANDA / IceCube Backgrounds for the Diffuse Analysis Why.
1 slide Brennan Hughey University of Wisconsin – Madison for the AMANDA Collaboration Recent Results From the AMANDA Experiment Rencontres du Vietnam August.
Search for UHE Neutrinos with AMANDA Stephan Hundertmark University of California, Irvine Methodical Aspects of Underwater/Ice Neutrino Telescopes Hamburg,
AMANDA Per Olof Hulth The Wierdest wonder Is it good or is it bad?
Barometric effect Atmospheric pressure is considered as the total mass of the air over the detector. Increase in pressure means that secondary particles.
Search for Ultra-High Energy Tau Neutrinos in IceCube Dawn Williams University of Alabama For the IceCube Collaboration The 12 th International Workshop.
EHE Search for EHE neutrinos with the IceCube detector Aya Ishihara Chiba University.
First All-Sky Measurement of Muon Flux with IceCube IceCube REU Summer 2008 Kristin Rosenau Advisor: Teresa Montaruli.
Imaging the Neutrino Universe with AMANDA and IceCube
Atmospheric neutrinos with Deep Core
Muons in IceCube PRELIMINARY
High Energy and Prompt Neutrino Production in the Atmosphere
The Antares Neutrino Telescope
Recent Results of Point Source Searches with the IceCube Neutrino Telescope Lake Louise Winter Institute 2009 Erik Strahler University of Wisconsin-Madison.
Comparison Of High Energy Hadronic Interaction Models
08/27/04 Strategies for the search for prompt muons in the downgoing
Brennan Hughey for the IceCube Collaboration
Comparison Of High Energy Hadronic Interaction Models
Karen Andeena, Katherine Rawlinsb, Chihwa Song*a
AMANDA-II Experiment Located at the Geographic South Pole
Brennan Hughey for the IceCube Collaboration
Hadronic Interaction Model Analysis Air Shower Development
Amanda Heffner-Wong Wichita State University Wichita, KS
University of Wisconsin-Madison
Presentation transcript:

Muon Vertical Depth Intensity Distribution at the South Pole with AMANDA-II Kimberly Moody 1 August 2003

Meet AMANDA-II Antarctic Muon And Neutrino Detector Array Located at the Geographic South Pole 677 Optical Modules (OMs) arranged on 19 strings 1500 to 2000m below the surface AMANDA is a neutrino telescope...

The Beauty of Neutrinos Protons deflected... Photons interacting with cosmic background... The neutrino remains unaffected! Black Hole, Gamma Ray Burst

What kind of signal does AMANDA receive? Diffuse Cosmic Rays (well-modeled) interact with atmosphere to produce, among other things, low energy muons.

What kind of signal does AMANDA receive? Diffuse Cosmic Rays Prompt Muons (different models suggest different fluxes; the subject of my research)

What kinds of signals does AMANDA receive? Diffuse Cosmic Rays Prompt Muons High-Energy Neutrinos-bingo!-the tell- tale particles AMANDA is looking for.

Atmosphere High Energy Extraterrestrial Neutrino High Energy Prompt Muon (from charmed meson decay) Low Energy Conventional Muons (from kaon and pion decay) Convention Muons (absorbed by Earth) Signals Atmospheric Neutrino This way up.

Data versus Monte Carlo and Quality Criteria

Data versus Monte Carlo and Quality Criteria

Slant Depth 1730m 8650m Slant Depth Binning Bin=1730/cos θ

Prompt Muons RQPM, QGSM: Most Optimistic Models Graph: Gelmini, Gondolo, Varieschi Measuring the prompt atmospheric neutrino flux with down-going muons in neutrinos telescopes (2002) hep-ph/

The Results of Our Prompt Muon Search

Prompt Contamination in First Bins R=N pm /N mc R (2) = % R (1) = % Bin 1 Bin 2

Prompt Muon Contamination in Last Bins R=N pm /N mc Bin Seven Bin Eight R (8) =1.55 % R (7) =0.982 %

cos θ Intensity by bin, cm -2 s -1 sr -1 Bin 1 Bin 2 Bin 3 Bin 4

Intensity by bin, cm -2 s -1 sr -1 cos θ Bin 5Bin 6

Many Thanks To: National Science Foundation The AMANDA Collaboration Fellow Charlie's Angels Dr. Bob Benjamin Dr. Paolo Desiati