Neutrino Astronomy with AMANDA

Transcription

1 Neutrino Astronomy with AMANDA NeSS 2002 Washington, D.C. Sep 20, 2002 Albrecht Karle University of Wisconsin-Madison

2 The AMANDA Collaboration 7 US, 9 European and 1 South American institutions, ~110 members: Bartol Research Institute, University of Delaware, Newark, USA BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium Universidad Simon Bolivar, Caracas, Venezuela DESY-Zeuthen, Zeuthen, Germany Dept. of Technology, Kalmar University, Kalmar, Sweden Lawrence Berkeley National Laboratory, Berkeley, USA Dept. of Physics, UC Berkeley, USA Institute of Physics, University of Mainz, Mainz, Germany University of Mons-Hainaut, Mons, Belgium University of California, Irvine, CA Dept. of Physics, Pennsylvania State University, University Park, USA Physics Department, University of Wisconsin, River Falls, USA Physics Department, University of Wisconsin, Madison, USA Division of High Energy Physics, Uppsala University, Uppsala, Sweden Fysikum, Stockholm University, Stockholm, Sweden Vrije Universiteit Brussel, Brussel, Belgium

3 South Pole Dark sector Skiway AMANDA Dome IceCube

4 AMANDA 19 strings 677 Optical Modules (OM) 200 m diameter 400 m tall History: AMANDA-B10: 1997, 10 strings, 300 OM AMANDA-II: 2000, 19 strings, 677 OM

5 Optical sensor Deployment

6 AMANDA DATA Event Signatures: Muons CC muon neutrino interactions Æ Muon tracks n m + N Æ m + X

7 AMANDA Event Signatures: Cascades MC, 1 TeV CC electron and tau neutrino interactions: n (e,t) + N Æ (e,t) + X NC neutrino interactions: n x + N Æ n x + X Cascades

8 Atmospheric Muons and Neutrinos Lifetime: 135 days (AMANDA-B10) Triggered Reconstructed upgoing Pass Quality Cuts Observed Data 1,200,000, Predicted Neutrinos

9 AMANDA Neutrino Sky atmospheric neutrinos events Observed Prediction: Atmos. n Observation of atmospheric neutrinos with 10 strings in agreement with prediction. ----> AMANDA is a functioning neutrino telescope! cos(zenith angle) Ref: Andres et al., Nature 2001 Ahrens et al., Phys. Rev. D (astro/ph. )

10 AMANDA II: Atmospheric n s as Test Beam Selection Criteria: (N hit < 50 only) Zenith > 110 o High fit quality Uniform light deposition along track Excellent shape agreement! Less work to obtain than with A-B10 3 cuts only! 4 n/day Data MC a. b. c. d. 290 events Gradual tightening of cuts extracts atm. n signal

11 Point Sources Amanda II (2000) In 6 o 6 o bin, for E -2 spectrum, 10-8 cm -2 s -1 flux: ~2 signal events Data: ~1 background event Sensitivities calculated using background levels as measured from data. Skyplot is scrambled in event time for blind analysis, Plot has been released, and results will be available soon. Examples for a few candidates will be given. Equatorial coordinates: declination vs. right ascension.

12 Point Sources Amanda II (2000) Results for three examples of possible sources: Source candidate looked at Mrk421 Mrk501 SS433 Declination Right ascension F m (E>10GeV,90% c.l.)/10-15 cm -2 s F n (E>10GeV,90% c.l.)/10-8 cm -2 s Number of events (observed) Number of events (background) Muon sensitivity (as F m ) Neutrino sensitivity (as F n ) F m = Limit on integrated E -2 muon flux above 10 GeV [10-15 cm -2 s -1 ] F n = Limit on integrated E -2 neutrino flux [10-8 cm -2 s -1 ]

13 Compare to Mrk 501 gamma rays Field of view: Continuous 2 p sr (northern sky) AMANDA B10 limit 1997 AMANDA II limit 2000, prel. Search for Point Sources of High Energy Neutrinos with AMANDA, (AMANDA B10) to appear in Ap.J., also astro-ph/

14 m cm -2 s -1 Super-Kamiokande astro-ph/

15 Search for diffuse flux of h.e. n m using 1 year of AMANDA B10 Atmospheric neutrino flux (MC) Injected AGN (MC) with 10-5 E -2 GeV -1 cm -2 s -1 sr -1 Energy cut DATA Thin lines: after energy cut Number of OMs with signal E 2 F < GeV -1 cm -2 s -1 sr -1

16 Same analysis for diffuse flux with AMANDA II (20%) Atmospheric neutrino flux Injected AGN with 10-5 E -2 GeV -1 cm -2 s -1 sr -1 DATA Sensitivity for 20% of AMANDA II Data is comparable to 1 year of AMANDA B10 data. PRELIMINARY Number of OM with signal per 100m of track length E 2 F < GeV -1 cm -2 s -1 sr -1

17 Limit to diffuse HE n m -flux Macro Baikal AMANDA B10 Systematic error: ~2 AMANDA-II (3 y) 1 pp core AGN (Nellen) 2 pg core AGN Stecker & Salomon) 3 pg maximum model (Mannheim et al.) 4 pg blazar jets (Mannh) 5 pg AGN (Rachen & Biermann) 6 pp AGN (Mannheim) 7 GRB (Waxman & Bahcall) 8 TD (Sigl) From: Mannheim & Learned, 2000

18 Diffuse flux with cascade events (see slide 7 for def.) 20% Amanda II cascade limit (Y2K) Ref.: Search for Neutrino-Induced Cascades with the AMANDA Detector, subm. To Phys Rev. D., Ahrens et al. (AMANDA coll.), also: astro-ph/ Unique result: Limit on all n flavors First to use full reconstruction of cascade Analysis gets easier and more competitive with muons as detector grows in size, especially at higher energies Astrophysical n s F ne+ne = 10-6 E -2 GeV cm -2 s -1 F nt+nt = 10-6 E -2 GeV cm -2 s -1 Atmospheric n s n e (CC), n e +n m (NC) Prompt charm (RQPM) Predicted events in 100% of 2000 data Predicted events in 100% of 2000 data Search for Neutrino-Induced Cascades with the AMANDA Detector

19 Off source GRB search bin GRB coincidences? GRB Position 16 s 1 hour 1 hour BKG - off time 88 BATSE bursts in 1997 BKG - off time on time GRB burst Background cuts can be loosened considerably Æ high signal efficiency No signal seen in 97 data.

20 A-II Sensitivity to GRB 58 bursts Feb-May 2000 Sensitivity for 2000 data: ~30 x Waxman/Bahcall 99 Figure from: Mannheim & Learned, 2000 AMANDA II 2000 data 90% limit setting potential Waxman/Bahcall 99

21 Dark matter: WIMP Search Limit on F m from WIMP annihilation WIMP annihilation at Earth s center, use directional handle: (Area approximate) Earth n m AMANDA m MSSM/ DarkSUSY Limits to the muon flux from WIMP annihilation in the center of the Earth with the AMANDA detector. To appear in Phys Rev D Also at: astro-ph/ ,

22 Coinicidences between Surface detector and AMANDA SPASE air shower array calibration of AMANDA angular resolution and pointing! 1 km Amanda-B10 (med): ~3.5 Amanda-II (med): ~ 2 2 km absolute pointing < 1.

23 Mass Composition of cosmic rays at the knee preliminary uncertainties.

24 EHE (E ev) Event Search EHE events very bright; many PMTs detect multiple photons vertical Sensitive to non-throughgoing events Main background: muon bundles Comparable N PMT but smaller N g Calibrate with in-situ N 2 laser Still evaluating systematic uncertainties R m 10 km. Note: At EHE energies, expect only ~horizontal events

25 2002 real time analysis June 14 Daily transmission ~ 1 GB via satellite Full data to tape (available next polar summer) Monitoring shifts in home labs From 02/03: Iridium connection for supernova alarm

26 Summary AMANDA-II provides much higher sensitivity than the 10 string array (B10) Diffuse flux: Best limits. Testing models. Diffuse flux in cascade analysis (good sensitivity for ne and nt) Diffuse EHE fluxes: 0.3 km 2 at EeV. A-II testing EeV blazar models. Point sources: Best limits. A-II much better sensitivity, preview on reults. GRB sensitivity 2000: approaching predictions Relativistic Magnetic Monopoles (not shown): Best limits (0.05 x Parker bound) WIMP search: high mass limits ~ Underground limits Monitoring Galaxy for SN bursts Cosmic Ray Composition at knee.

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28 Relativistic Magnetic Monopoles upper limit (cm -2 s -1 sr -1 ) d electrons C - light output µ n = 1.33 (g/e) = 137 / 2 n 2 (g/e) b = v/c 1.00 ª 8300 C.Spiering, n2000

29 Supernova Monitor Amanda B10 has monitored 60% of the Galaxy with 90% detection efficiency for a SN1987A type supernova. IceCube will monitor the full Galaxy.

30 SPASE - AMANDA: Energy resolution of air shower primary Log(E_true) Proton Iron Log(E_reconstructed) Energy resolution of air shower primary for 1<E/PeV<10: s E 7% log(e) (Mass independent; based on MC) Entries 1798 Constant Mean E-01 Sigma E-01 1 PeV - 10 PeV log(e_reconstructed)-log(e_true)

31 Measuring mass and energy of cosmic ray primary particle Unfolding energy and mass using SPASE and AMANDA AMANDA (number of muons) log(e/gev)