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Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford.

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Presentation on theme: "Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford."— Presentation transcript:

1 Sean Grullon For the IceCube Collaboration Searching for High Energy Diffuse Astrophysical Neutrinos with IceCube TeV Particle Astrophysics 2009 Stanford Linear Accelerator Laboratory

2 Sean Grullon – TeVPA 20092 Overview Astrophysical Neutrinos & Searching for a Diffuse Flux of Muon Neutrinos Muon Energy Estimation 22 String Diffuse Analysis Results Outlook for 40 Strings Questions & Discussion

3 Sean Grullon – TeVPA 20093 Neutrinos as Cosmic Messengers Neutrinos help answer many questions in astrophysics: What are the sources of highest energy cosmic rays? Are there pp and p  interactions at the source? Can neutrino production be linked to TeV  sources, GRBs, AGN? Can a superposition of faint neutrino sources cause a detectable signal?

4 Sean Grullon – TeVPA 20094 IceTop InIce Air shower detector threshold ~ 300 TeV 80-86 Strings, 60 Optical Modules per String 2004-2005 : 1 String 2005-2006: 8 Strings AMANDA 19 Strings 677 Modules first data 2005 upgoing muon 18. July 2005 2006-2007: 13 Strings 2007-2008: 18 Strings

5 Sean Grullon – TeVPA 20095 Astrophysical (signal) Atmospheric Atmospheric  Cosmic ray 

6 Sean Grullon – TeVPA 20096 Downgoing Muon Rejection Apply quality cuts on Data, Corsika MC, and Atmospheric Neutrino MC

7 Sean Grullon – TeVPA 20097 Analysis Strategy Find an excess of extra-terrestrial neutrinos (E -2 ) over atmospheric neutrinos (E -3.7 ) at the high-energy tail of an energy distribution

8 Sean Grullon – TeVPA 20098 Diffuse Analysis Strategy Find an excess of astrophysical neutrinos (E -2 ) over atmospheric neutrinos (E -3.7 ) at the high-energy tail of an energy distribution

9 Sean Grullon – TeVPA 20099 Energy Estimation Convert what is measured, Cherenkov light, to an estimate of the Muon energy. Simplest estimation: Number of Triggered Optical Modules (NCh) More Sophisticated: Muon Energy Loss (dE/dX) e+e-e+e-    pair-creation bremsstrahlung photo-nuclear

10 Sean Grullon – TeVPA 200910 Reconstructing The Muon energy loss Approximate as: dusty clean deep shallow Incorporate Ice Properties: Formulate LLH:

11 Sean Grullon – TeVPA 200911 Muon Energy Correlation – 40 Strings dE/dX reco more linearly correlated with Muon energy dE/dX Reco NChannel

12 Sean Grullon – TeVPA 200912 Energy Resolution – 40 Strings Width 0.27 Width 0.43 dE/dX reco has narrower energy resolution

13 Sean Grullon – TeVPA 200913 Energy Resolution as a Function of Muon Energy – 40 Strings

14 Sean Grullon – TeVPA 200914 The dE/dX distribution of IC22 275.7 days LiveTime Keep Energy Cut > 1.4 Background above cut = 4.1 Events Observed Data above cut = 4.0 Events Sensitivity: 2.5 x10 -7 GeV cm -2 s -1 sr -1 Find cut that minimizes average upper limit

15 Sean Grullon – TeVPA 200915 The dE/dX distribution of IC40 300 days LiveTime - MC Only

16 Sean Grullon – TeVPA 200916 Likelihood Analysis Method Likelihood - product over bin-by-bin Poisson probabilities: Events observed in bin i Events expected in bin i Conventional Atmospheric νAstrophysical νPrompt ν

17 Sean Grullon – TeVPA 200917 Fitting Example: 1 Year IC40 - No Astrophysical or Prompt ν “Data” Poisson sampled from 1 year of Atm. ν MC

18 Sean Grullon – TeVPA 200918 Allowed Regions, No Astrophysical or Prompt ν : 1 Year of IC40 Preliminary IC40 Diffuse Sensitivity: E 2 < 1.1 x 10 -8 GeV cm -2 s -1 sr -1 No Systematics included

19 Sean Grullon – TeVPA 200919 Models & Limits IC22 IC40 WB

20 Sean Grullon – TeVPA 200920 Models & Limits, cont.

21 Sean Grullon – TeVPA 200921 Summary A reliable log-likelihood reconstruction of the muon energy loss is now available for IceCube analyses. The IC22 sensitivity is E 2 = 1.4 275.7 days of IC22 data were analyzed and compared with the Bartol + naumov RQPM atmospheric neutrino simulation. No data excess over the atmospheric neutrino prediction observed above the dE/dX cut. The IC40 analysis uses a likelihood method giving a preliminary sensitivity of E 2 < 1.1 x 10 -8 GeV cm -2 s -1 sr -1 and the incorporation of systematic errors is currently underway.

22 Sean Grullon – TeVPA 200922 Backup slides

23 Sean Grullon – TeVPA 200923 IC22 Sensitivity Estimator Energy cut Sensitivity x 10 -7 Bartol+Naumov RQPM (Bartol only) 1e-7 E -2 MC data log 10 (dEdX)>=1.4 0.25 (0.21) 4.1 (2.45) 19.84 Data is consistent with the atmospheric neutrino models Simple energy estimators (no energy reconstruction) Estimator Energy cut Sensitivity x 10 -7 Bartol+Naumov RQPM 1e-7 E -2 MC data NCh>=990.229.324.222 log10(NPe)>=3.150.266.622.510 * numbers in parenthesis are calculated without the prompt neutrino model

24 Sean Grullon – TeVPA 200924 Systematics – IC22 Observed data exceeds MC by a factor of 2 in deep ice Deep Ice 40% clearer. AMANDA depth New from IceCube DataAtms. Nu MC Single Mu Coinc. Mu

25 Sean Grullon – TeVPA 200925 DataAtms. Nu MC Systematic Test (low energy, NCh<50) COGZ Data - MC upgoing cos(zenith) horizon COGZ Data excess is observed even with the low energy events (conventional atmospheric neutrinos) Divide the detector in 2 depths : upper half and lower half

26 Sean Grullon – TeVPA 200926 Systematic Test Estimator Energy cut Sensitivity x 10 -7 Bartol+Naumov RQPM 1e-7 E -2 MC data log 10 (dEdX)>=0.970.507.912.25 NCh>=680.417.915.03 log10(NPe)>=2.850.548.011.35 Upper Half Lower Half Estimator Energy cut Sensitivity x 10 -7 Bartol+Naumov RQPM 1e-7 E -2 MC data log 10 (dEdX)>=0.910.5815.514.014 NCh>=800.4712.815.725 log10(NPe)>=3.150.642.46.44

27 Sean Grullon – TeVPA 200927 The dE/dX distribution of IC40 BurnSample (30 Days LiveTime) No systematics are included

28 Sean Grullon – TeVPA 200928 Sensitivities: Likelihood Method Extraterrestrial Only Energy EstimatorMRFLimit MC ν 0.044* 10 -9 MCμ0.0666.6* 10 -9 Photorec0.1011.01* 10 -8 MuE0.1221.22* 10 -8 NChan0.1251.25* 10 -8

29 Sean Grullon – TeVPA 200929 Fitting Example: No Signal

30 Sean Grullon – TeVPA 200930 Fitting Example: No Signal

31 Sean Grullon – TeVPA 200931 Allowed Signal and Prompt Regions

32 Sean Grullon – TeVPA 200932 Fitting Example: Astrophysical+Bg

33 Sean Grullon – TeVPA 200933 Allowed Signal and Prompt Regions

34 Sean Grullon – TeVPA 200934 Fitting Example: Signal + Prompt + Conventional Atmospheric Neutrinos “Data” sampled from Atm Nu backgro und

35 Sean Grullon – TeVPA 200935 Allowed Extraterrestrial and Prompt Regions

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