1 / 50

AMANDA Supernova detection

AMANDA Supernova detection. n e + p n + e + PMT noise increase due to the positrons AMANDA samples noise on each PMT over 0.5 sec and summing up total rate over 10 sec intervals. AMANDA SN sensitivity. Test. Kalmar University Staffan Carius, Sr.Lecturer Pär Lindahl, grad.student

yoshi
Download Presentation

AMANDA Supernova detection

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. AMANDA Supernova detection • ne + p n + e+ • PMT noise increase due to the positrons • AMANDA samples noise on each PMT over 0.5 sec and summing up total rate over 10 sec intervals

  2. AMANDA SN sensitivity • Test

  3. Kalmar University Staffan Carius, Sr.Lecturer Pär Lindahl, grad.student Arvid Pohl, grad. student Stockholm University, experiment Patrik Ekström, grad.student Per Olof Hulth, Professor Yulia Minaeva, grad.student Julio Rodrıguez Martino, grad.student Christian Walck, Sr.Lecturer Stockholm University, theory Lars Bergström, Professor Joakim Edsjö, post doc Hector Rubinstein, Professor Uppsala Universitet Olga Botner, Professor Allan Hallgren, Sr. Lecturer Pia Loaiza, lic. Pawel Marciniewski, grad. Student Carlos Perez de los Heros, NFR-Researcher Jan Conrad, grad.student AMANDA people in Sweden

  4. Multi-messenger Astronomy • Take advantage of complete suite of information carriers • Particle Probes ( HE n and EHE cosmic rays) • Gravity Wave Detectors • Multi-wavelength photon studies • Coincidence studies are planned, and may offer a powerful tool to understand the most cataclysmic objects in the Universe

  5. Messengers of Astronomy • The neutrino window begins at energies above 106 eV • Era of multi-messenger astronomy

  6. AMANDA Science Goals-1 • EHE cosmic rays: a compelling mystery • What are they? • Where do they come from? • How are they produced? • Origin of Galactic Cosmic Rays

  7. AMANDA Science Goals-2 • Particle Physics and Cosmology • Dark Matter (WIMPs from sun and earth) • Relativistic Monopoles • Charm production • Neutrino mass • EHE n’s from topological defects • Interdisciplinary Science • Optical, mechanical, and thermal properties of Antarctic ice

  8. Cosmic Neutrino Factories • Most models assume a central black-hole and accretion disk. • Particle acceleration occurs either near the black hole or in the jet • AGNs

  9. Detection Method for nm • Cherenkov photons are detected by array of PMTs • Tracks are reconstructed by maximum likelihood method using photon arrival times.

  10. AMANDA-IIFeb. 00

  11. AMANDA n-candidate • Early photons are red, late photons are blue. More photons are larger circles • Bottom of array is toward center of Earth • The muon is clearly traveling in the upward direction

  12. AMANDA n-candidate • Early photons are red, late photons are blue. More photons are larger circles • Bottom of array is toward center of Earth • The muon is clearly traveling in the upward direction

  13. Event Rate Predictions Point Sources Diffuse Sources

  14. Search Strategies for HE n’s • Diffuse flux are most difficult to detect, but largest predicted rates. • GRBs have least background due to time and position correlations.

  15. Atmospheric Neutrinos • Stronger selection criteria than point analysis • Two distinct analysis methods • Expected rate depends on analysis efficiency

  16. Data Reduction 1997 E.g. one of the atmospheric neutrino analysis, 1997.

  17. AMANDA Effective Area • AMANDA-II 30,000-50,000 m2 • AMANDA-II has nearly uniform response over all zenith angles

  18. Diffuse Flux • Generally 103 larger than point fluxes • Atm. n backgrounds 103 worse • E2Fn < 1.6*10-6 GeVcm-2s-1sr-1 AMANDA

  19. Search for HE n Point Sources • Concentrate on continuous emission from sources with hard spectra (~E-2) • Optimize search on Signal to Noise Ratio • Aeff depends on rejection requirements • Iterative procedure defined a priori • Background for this search • Poorly reconstructed atmospheric muons • Atmospheric neutrinos

  20. Sky Plot of Events Equatorial Coordinates • 1097 events • No obvious clustering • Event sample consists of atm. n and atm. muons.

  21. Significance distribution • Bin sky according to angular resolution • Use declination band to estimate background • No statistically significant excess

  22. Flux Limit (preliminary) • AMANDA B10 limits are compared to MACRO limits. SuperK curve is estimated! • AMANDA-II will complement sky coverage of SuperK

  23. SPASE-AMANDA SPASE: South Pole Air Shower Experiment • Calibration of absolute pointing • Calibration of pointing resolution • Calibration of signal efficiency

  24. Angular Distributions Two distinct analysis techniques, but not independent (a) (b) MC (normalized)

  25. Signal-background Separation Arb. normalization between signal and BG

  26. Search for Diffuse Flux • OM multiplicity distribution is (weakly) related to energy deposition. • Distribution is consistent with atm n • New energy estimators will lead to improved limits

  27. WIMPs from Sun/Earth

  28. Angular Spread of WIMP signal • Angular spread decreases as WIMP mass increases, reducing atm. n background

  29. Cuts for WIMP search • Optimized cuts for almost vertical upward moving muons. • The simulated WIMP signal is reduced to 30% after reducing background by 108.

  30. WIMPs from the Earth Optimized search for vertical neutrinos • AMANDA limits comparable to MACRO and Baksan • AMANDA sensitivity will increase at low mass due to special string trigger

  31. WIMPs from the Earth with Ice3 Optimized search for vertical neutrinos • Ice3 will improve the sensitivity several orders of magnitude

  32. WIMPs from the Earth with Ice3 Optimized search for vertical neutrinos • Ice3 will completely cover the DAMA area

  33. WIMPs from the Sun with Ice3 • Ice3 will improve the sensitivity several orders of magnitude.

  34. WIMPs from the SUN with Ice3 • Ice3 will improve the sensitivity several orders of magnitude

  35. WIMP search with Ice3 The WIMP search has been tested for two different geometries

  36. Search for HE n from GRB

  37. GRB Science • Verify fireball model • GRBs may be sources of highest energy cosmic rays • Test of special relativity • Search for nt appearance at Dm2> 10-17 eV2 • Search for n emission in coincidence with BATSE or MILAGRO

  38. HE n emission from GRB’s ? - Not so far 10-1 Combined Limit (90% CL) Fluence (TeVcm-2) 10-6 Waxman and Bahcall 1 100 Burst Duration (s)

  39. Future : Ice3 !! • Neutrino astronomy needs a detector size of about 1 km3 in effective volume! • AMANDA collaboration plus new groups have applied (Nov. 99) to NSF for a 80 string detector with about 5000 optical modules. • Project reviewed by the SAGENAP committee (March 00). • NSF has appointed a committee chaired by Don Hartellwhich will review the project 21-23 of June 2000 in Madison. • The Swedish AMANDA groups (experimentalists) have applied to FRN for 36 MSEK over 6 years.

  40. Ice3 Muon Event (simulated) • OMs that detect Cherenkov photons are colored circles • Earliest photons are red, latest photons are blue.

  41. Ice3 Electron neutrino Event • Color circles indicate OMs that detect Cherenkov photons. • Earliest photons are red, latest photons are blue.

  42. Ice3 Tau Event (double-bang) • Color circles indicate OMs that detect Cherenkov photons. • Earliest photons are red, latest photons are blue.

  43. AMANDA Results • Supermassive Black Holes (AGN) • E-2 point source: fn (>10 GeV) <10-7 (cm-2s-1) • E-2 diffuse flux : E2fn< 1.6*10-6GeV cm-2s-1sr-1 • GRB in coincidence with BATSE • Fn< 5x1010 km-2yr-1 • Atmospheric neutrinos (135 live days) • ~170 events from 1997, depends on analysis • Calibration of sensitivity within factor 2 • WIMPs from the earth Also, see ICRC99 for limits on relativistic monopoles, search for SNa, ice properties

  44. Publications • Many conference reports • In Sweden 2 Ph.D. Thesis and 4 Lic. • First neutrino results in Astroparticle Physics 13 (2000) 1, (AMANDA-B4) • Six drafts in preparation for submission in September 2000 (AMANDA-B10, 1997 data) • Atmospheric neutrinos • WIMP search • Neutrino limits from GRB • Point sources • Diffuse limit • AMANDA-SPASE

  45. Summary and Outlook • No point sources (AGN, GRB or WIMPS) detected, but • more data on tape with bigger array (1998, 1999) • ~170 atmospheric neutrinos candidates • Number depends on efficiency of analysis • Sensitivity and performance confirmed (to within factor of 2) by atm n, background studies, and Spase-AMANDA coincidence events • AMANDA-II is taking data

  46. Swedish activities in AMANDA • The AMANDA-trigger and discriminator has been designed and built by the Uppsala group. • The signal pre-amplifiers have been designed and built by the Stockholm group. • 50% of the optical modules in AMANDA-B4 were built and tested in Sweden. • A TV-camera was constructed and built by the Stockholm group and deployed to 2350 m depth • Collaboration with Swedish industry on development of signal transmission cables • Swedish drillers have contributed essentially for commision of AMANDA

  47. Swedish activities in AMANDA cont. • The Swedish groups have access to all data without any restriction. • The Swedish groups have been heavily involved in the ice analysis as well as the calibration analysis of the detector constants. • The WIMP search has been done by the Swedish groups. • The first neutrino events in the AMANDA-B4 detector were reconstructed by the Swedish groups using the Swedish reconstruction program. • The groups are also involved in the search for low energy neutrinos from GRB as well as sensitivity investigation of neutrino oscillations.

  48. Optical Absorption Length • ~200m for blue light • Varies with depth, correlated with ice ages

  49. Optical Scattering Length • Variation with depth only recently included in detector simulation

  50. Mk 501 Flux Limit • Recent diffuse IR measurements imply strong attenuation of TeV photons • AMANDA can rule out similar neutrino spectrum. Figure adapted from Protheroe and Meyer, astro-ph/0005349 AMANDA

More Related