2000-2006 AMANDA-II Point Source Search Results

1. 2000-2006 AMANDA-II Point Source Search Results Jim Braun IceCube Spring 2008 Collaboration Meeting

2. 2000 2001 2002 2003 2004 2005 2006 m-DAQ Point Source Searches AMANDA-II complete Hauschildt, Steele: Phys.Rev.Lett.92:071102 2004 This Analysis Combine all years for best possible sensitivity Final sample will also be utilized by John K. and others Y.-R. Wang: Phys.Rev.D71:077102 2005 M. Ackermann: Phys.Rev.D75:102001 2007 Unblinded in 2007 by J. Braun Unblinded in 2007 by J. Braun m-DAQ decommissioned

3. Data Overview 2000-2004 unified filtering done in Zeuthen by Ackermann et al. 2005-2006 filtered in Madison with a very similar configuration. • Data and neutrino simulation available in Madison

4. Event Selection • 20M events at L3 • Use cuts from 5 year analysis • Smoothness • Paraboloid error • Up/down likelihood ratio • Use an SVM-based cut for d < 1.5o • 6595 total events • Much more information available on analysis web page: http://www.icecube.wisc.edu/~jbraun/combined_point_source

5. Event Selection

6. Search Method • Apply unbinned maximum likelihood search method • Use paraboloid error estimate as a measure of reconstruction uncertainty • Use event energy (Nch) to separate signal from atmospheric neutrinos • Method details described in internal report: http://internal.icecube.wisc.edu/reports/data/icecube/2008/04/001/icecube_200804001_v2.pdf

7. Search Method

8. Sensitivity

9. Unblinded Skymap Short, short summary: We see nothing

10. Analysis What did we do with the data? 1. All-sky search 2. Search based on a list of candidates 3. Milagro stacking search 4. Search for autocorrelation

11. 3yr max significance: 3.73s 1.5s Max Significance d=54o, a=11.4h 3.38s Significance All-Sky Search 5yr max significance: 3.74s 2.8s 95 of 100 data sets randomized in RA have a significance ³ 3.38s

12. Source List Search Selected Sources The Crab: • Significance decreases • Still a minor upward fluctuation • Upward Fluctuations: • LS I +61 303 • Geminga • Downward Fluctuations: • Mrk 421 The probability of obtaining p £ 0.0086 for at least one of the 26 sources is 20%

13. Experimental Limits Energy Range (90%): 1 TeV – 3 PeV

14. Milagro Stacking Search A. Abdo et al. Proc. First Glast Symposium • Apply stacking search to 6 Milagro sources with >5s pretrial significance • Exclude PWN sources (Crab, Geminga) • Use method developed by HiRes* to perform our likelihood search simultaneously for all Milagro source locations • Improves per-source flux sensitivity and discovery potential by a factor of 4 compared to a fixed-point search for any of the six sources * R.U. Abbasi, et al. Astrophys. J., 636 680 (2006)

15. Milagro Stacking Search Halzen, Kappes, O’Murchada [arXiv:0803.0314]

16. Potential IC40 Sensitivity Milagro Stacking Search Halzen, Kappes, O’Murchada [arXiv:0803.0314]

17. Significance Autocorrelation Search • Search for event clustering at angular scales comparable to detector resolution • Signal scenario: A number of small event clusters • Method: Count the number of event pairs given a maximum angular separation and minimum Nch and compare to distributions from data with randomized RA • Max significance: 1.6s • 99 out of 100 sets of randomized data have a max significance of 1.6s or greater

18. Systematics • Systematics will be similar to those from the 5 year analysis • ANIS predicts 8% fewer atmospheric neutrino events compared to NUSIM • Include nt muon contribution? • Systematics of unbinned analysis

19. Publication • Rapidly address systematics and get manuscript to collaboration as soon as possible

20. Conclusions • This analysis is a factor of 2 more sensitive than previous point source analysis • We didn’t see anything • IC22, IC40 will yield substantial improvements