lceCube High-energy Neutrino Astrophysics Where we are and where we good a Shigeru Yoshida' Department of Physics - Chiba University lceCube 2007-2008: 18 Strings 2006-2007: 13 Strings 2008 -2009 Data 40 strings 80 lceTop tank 2005-2006: 8 Strings 2009-2010 59 strings 2010-2011 79 strings 1450m 2004-2005 : 1 String 80+6 Strings 60 Optical Modules 17 m between Modules 125 m between Strings 2450m
USA: Bartol Research Institute, Delaware University of California, Berkeley University of California, Irvine Pennsylvania State University Clark-Atlanta University Ohio State University Georgia Tech University of Maryland University of Alabama, Tuscaloosa University of Wisconsin-Madison University of Wisconsin-River Falls Lawrence Berkeley National Lab. University of Kansas Southern University and A&M College, Baton Rouge University of Alaska, Anchorage Sweden: Germany: 33 institutions, ~250 members http://icecube.wisc.edu
“Flasher Board” 13" Glass (hemi)sphere Data Filtering at South Pole PY 2008 season 40 strings ~ a half of the completed IceCube Simple Majority Trigger 8 folds with 5 μ sec ~ 950 Hz Muon Filter selects “up-going” tracks ~20 Hz EHE Filter selects “bright” events Cascade Filter selects “cascade”-like events Many others Min Bias Moon, lceTop ~1.3 Hz ~17 Hz NPE > 630 p.e. To Northern Hemisphere-
Materials to cook μ filtered, EHE filtered and min-bias events Require Quality cuts in multiple stages Common aspects In many other analysis to filter out vastly dominated down-going muons to realize reasonable agreement between MC and data Point source specific to create a sample of events with good angular resolution
All sky search: post-trial p-value 18% Hottest spot:  RA 113.75 Dec 15.15  -log(p)=5.28 Jon Dumm (UW-Madison)
lceCube Preliminary
CygA Pretrial 4.8 % →post-trial  62 % for the source list * Shown here is only a part of the IceCube pre-determined source list Jon Dumm (UW-Madison)
Jon Dumm (UW-Madison)
Milagro Sources (17 sources) 9 TeV SNRs + 8 new associated with Fermi (6 SNRs with Fermi association) Nearby starburst galaxies (127 sources) 33 % Clusters of glaxies (5 sources) 78 % Followed Murase, Inoue, Nagataki (2008) Virgo, Perseus, Centaurus, Coma, Ophiuchus p-value 32 % (a posteriori) 1% Jon Dumm (UW-Madison)
Materials to cook → u base μ filtered and EHE filtered Require Quality cuts in multiple stages Zenith > 85 deg. to filter out vastly dominated down-going muons Common aspects In many other analysis to realize reasonable agreement between MC and data GRB specific use “off-time” data as the BG sample to train the BDT
Unbinned Maximum Likelihood PDF Total PDF Optimize BDT score to maximize the discovery potential
109 GRBs detected by Fermi, Swift, Konus, and WAM Peter Redl (UMD) We are on the way to indicate GRBs are unlikely to be a major UHECR origin. Materials to cook EHE filtered events All v flavor base No strong quality cuts necessary because.. these v’s are more energetic than atmospheric μ BG Unique features in this particular analysis Just increase energy threshold in analysis leads to better S/N GZK analysis specific issues • Earth filters out signal v as well
→ Sensitive to - starting track/ cascade Directly induced events from v → Sensitive to   Ve  Vμ  Vτ og 10 (total NP Experimental verification MC overestimates NPE by ~18% Sys. error ~ 7% in SIG rate ~ 50% in BG rate 0. 0. The detailed description available in Abbasi et al PRD 82 072003 (2010)
Energy → NPE (total # of photoelectrons) Look for luminous (high NPE) horizontal events
Final level 3 cut Selects bright(=high NPE) events penetrating long path from the earth surface
E² φ(E) < 4.2x10 -8 GeV/cm² sec sr   (2PeV < E < 8 EeV)
Now IceCube  : constrained UHECR cosmological luminosity at the comparable level with Fermi, but more direct way A major fraction of the Fermi diffuse γ is NOT responsible for UHECR emissions
This event p-value for the background hypothesis  ~0.2% (posteriori) • Detected in 2008 December 10th • NPE  2.55x105 photo-electrons • Zenith 64.7 deg
The same analysis method/systematics applied on the full IceCube MC