2000-06-21
AMANDA
Per Olof Hulth
The Wierdest wonder
• Is it good or is it bad?
Seven Wonders of Modern AstronomyThe Sharpest The Biggest The Farthest FlungThe Most Extensive The Swiftest The DeadliestThe Wierdestwww.sciam.com/1999/1299engineering/1299musser.html
2000-06-21
AMANDA
Per Olof Hulth
AMANDA experience
• Bad Calibration of the detector very heavy (“perfect” time constants for
AMANDA-B13 ready first May 2000!) The analysis delayed due to this.
• Good Deployment procedure established. “Easy” to reconstruct neutrinos
2000-06-21
AMANDA
Per Olof Hulth
AMANDA deployment history
Year DetectorNumber
ofdeployed
OM
Totalnumber of
strings
Totalnumber of
OM
1995/1996 AMANDA-B4 86 4 86
1996/1997 AMANDA-B10 218 10 302
1998/1999 AMANDA-B13 125 13 428
1999/2000 AMANDA-II 252 19 680
2000-06-21
AMANDA
Per Olof Hulth
AMANDA data analysis
• The first neutrino candidates published from AMANDA-B4 (data 1996)
• AMANDA-B10 data 1997 analysis in progress for Atmospheric neutrinos Search for WIMP annihilation in the Earth point sources Diffuse flux Neutrinos from GRB and Supernova, magn. monoples, AMANDA-SPASE etc
2000-06-21
AMANDA
Per Olof Hulth
AMANDA data analysis
Atmospheric neutrinos WIMP search from Earth Point sources Diffuse neutrino flux
Neutrinos from GRB Supernova neutrinos Magnetic monopoles AMANDA-SPASE
AMANDA-B10 data is analysed for several different topics with the following in a “final” stage:
2000-06-21
AMANDA
Per Olof Hulth
AMANDA-II Feb. 00
2000-06-21
AMANDA
Per Olof Hulth
AMANDA -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
2000-06-21
AMANDA
Per Olof Hulth
AMANDA -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
2000-06-21
AMANDA
Per Olof Hulth
Event Rate Predictions
Source_______Rate(/km2yr)Eμ > 1 TeV
SNa RemnantA (GN 3C273 )Mk421, Mk501GR B (Γ flu .ct model)
31-1001-10 fr omγ flux~ a few(fro m arar e burst)
SourceRate(/km2yr sr)Eμ > 1 T _eV ____
AGNA GN jetsGRBAt m
400 -8004510100 0
Point Sources Diffuse Sources
2000-06-21
AMANDA
Per Olof Hulth
Search Strategies for HE ’s
• Diffuse flux are most difficult to detect, but largest predicted rates.
• GRBs have least background due to time and position correlations.
SourceRejectionmethod____ Background
Diffuse flux 1. up-down (109/yr)(atm.μ)
Po intSource( . . e g A )GN
1. up-down2. direction3. energy?
(10 9/yr)( .atmμ)x(dΩ/2π)
Bursts( . . e g GRB)
1. up-down2. direction3. ti mestamp4. energy?
(10 9 /yr)( .atmμ)x(dΩ/2π)x( /dt3 10x 7)
2000-06-21
AMANDA
Per Olof Hulth
Signal-background SeparationArb. normalization between signal and BG
2000-06-21
AMANDA
Per Olof Hulth
SPASE-AMANDA
• Calibration of absolute pointing
• Calibration of pointing resolution
• Calibration of signal efficiency
SPASE: South Pole Air Shower Experiment
2000-06-21
AMANDA
Per Olof Hulth
Data Reduction 1997
Observed numberof events
Predicted numberof neutrinos
Triggered 1.2*109 4500
Reconstructed asupgoing track
5.1*104 570
Passing final cuts 193 235
E.g. one of the atmospheric neutrino analysis, 1997.
2000-06-21
AMANDA
Per Olof Hulth
Atm. : background rejection
• Satisfactory agreement at all stages of analysis
• Rejection criteria are progressively improved, leaving fewer down-going events
• Initially data agrees with BG simulation, but then agrees with atm. signal
103
1
2000-06-21
AMANDA
Per Olof Hulth
Angular DistributionsTwo distinct analysis techniques, but not independent
(a)MC (normalized)
(b)
2000-06-21
AMANDA
Per Olof Hulth
Atmospheric Neutrinos
• Stronger selection criteria than point analysis
• Two distinct analysis methods
• Expected number of events depends on analysis efficiency
2000-06-21
AMANDA
Per Olof Hulth
Search for HE 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
2000-06-21
AMANDA
Per Olof Hulth
Sky Plot of Events
• 1097 events
• No obvious clustering
• Event sample consists of atm. and atm. muons.
Equatorial Coordinates
2000-06-21
AMANDA
Per Olof Hulth
Significance distribution
• Bin sky according to angular resolution
• Use declination band to estimate background
• No statistically significant excess
Title: /tmp_mnt/u/tornado1/youngs/data/sigma.coguci.24x48.Creator: HIGZ Version 1.23/09Preview: This EPS picture was not saved with a preview (TIFF or PICT) included in itComment: This EPS picture will print to a postscript printer but not to other types of printers
2000-06-21
AMANDA
Per Olof Hulth
Flux Limit (preliminary)
• AMANDA B10 limits are compared to MACRO limits. SuperK curve is estimated!
• AMANDA-II will complement sky coverage of SuperK
Title: /export/cascade1/youngs/mc_signal_new/nusim_50100/rCreator: HIGZ Version 1.23/09Preview: This EPS picture was not saved with a preview (TIFF or PICT) included in itComment: This EPS picture will print to a postscript printer but not to other types of printers
2000-06-21
AMANDA
Per Olof Hulth
Point Source Fluxes
• Theoretical predictions are very small
• AMANDA limit assumes source with E-2 spectrum
Figure adopted from Mannheim & Learned
2000-06-21
AMANDA
Per Olof Hulth
Mk 501 Flux Limit
• Recent diffuse IR measurements imply strong attenuation of TeV photons
• AMANDA can rule out similar neutrino spectrum.
AMANDA
Figure adapted from Protheroe and Meyer, astro-ph/0005349
2000-06-21
AMANDA
Per Olof Hulth
Search for Diffuse Flux
• OM multiplicity distribution is (weakly) related to energy deposition.
• Distribution is consistent with atm
• New energy estimators will lead to improved limits
2000-06-21
AMANDA
Per Olof Hulth
Diffuse Flux
• Generally 103 larger than point fluxes
• Atm backgrounds 103 worse
• E2 < 1.6x10-6 GeVcm-2s-1sr-1
AMANDA
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from Sun/Earth
2000-06-21
AMANDA
Per Olof Hulth
Angular Spread of WIMP signal
• Angular spread decreases as WIMP mass increases, reducing atm. background
2000-06-21
AMANDA
Per Olof Hulth
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.
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from the Earth
• AMANDA limits comparable to MACRO and Baksan
• AMANDA sensitivity will increase at low mass due to special string trigger and better optimized analyzes
Optimized search for vertical neutrinos (1997 data)
2000-06-21
AMANDA
Per Olof Hulth
WIMP search with Ice3
The WIMP search has been tested for two different geometries and the limits are given for 10 years of running
2000-06-21
AMANDA
Per Olof Hulth
Simulation of WIMPs in Ice3
• Signal neutrinos from WIMP annihilations are simulated with Pythia
• No background simulated, but PMT noise is included
• At least 5 remaining hits after cleaning
• Reconstructed muon angle within 5 degrees of simulated
• This is the best-case limits since since efficiency of future cuts to remove background has not been included.
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from the Earth with Ice3
• Ice3 will significantly improve the sensitivity.
Optimized search for vertical neutrinos
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from the Earth with Ice3
• Ice3 will completely cover the DAMA area
Optimized search for vertical neutrinos
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from the Sun with Ice3
• Ice3 will significantly improve the sensitivity.
2000-06-21
AMANDA
Per Olof Hulth
WIMPs from the SUN with Ice3
2000-06-21
AMANDA
Per Olof Hulth
Search for HE from GRB
Off source
GRB search bin
GRB Position
1 hour 1 hour16 s
BKG - off time BKG - off timeon time
GRB burst
2000-06-21
AMANDA
Per Olof Hulth
GRB Science
• Verify fireball model• GRBs may be sources of highest energy cosmic
rays• Test of special relativity
• Search for appearance at m2> 10-17 eV2(Ice3)
• Search for emission in coincidence with Gamma ray detectors
2000-06-21
AMANDA
Per Olof Hulth
HE emission from GRB’s ?
10-1
10-6
1 100Burst Duration (s)
Waxman and Bahcall
Combined Limit (90% CL)
Flu
ence
(T
eVcm
-2)
- Not so far
2000-06-21
AMANDA
Per Olof Hulth
AMANDA Supernova detection
• e + p n + e+
• PMT noise increase due to the positrons
• AMANDA records noise on the PMTs over 0.5 sec and summing up total rate over 10 sec intervals
2000-06-21
AMANDA
Per Olof Hulth
AMANDA SN sensitivity
• AMANDA-B10 is monitoring 60% of the Galaxy with 90% detection efficiency for a SN1987 type.
• AMANDA is going to join SNEWS in 2001
2000-06-21
AMANDA
Per Olof Hulth
Magnetic Monopole detection
2000-06-21
AMANDA
Per Olof Hulth
AMANDA Effective Area
• AMANDA-II 30,000-50,000 m2
• AMANDA-II has nearly uniform response over all zenith angles
2000-06-21
AMANDA
Per Olof Hulth
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 , background studies, and Spase-AMANDA coincidence events
• AMANDA-II is taking data
2000-06-21
AMANDA
Per Olof Hulth
Publications
• Many conference reports and so far X Ph.D. Thesis.
• First neutrino results in Astroparticle Physics 13 (2000) 1, (AMANDA-B4)
• Eight drafts in preparation for submission in autumn 2000 (AMANDA-B10, 1997 data) Atmospheric neutrinos WIMP search Neutrino limits from GRB Point sources Diffuse limit AMANDA-SPASE Supernova Magnetic Monoples
2000-06-21
AMANDA
Per Olof Hulth
AMANDA Results
• Supermassive Black Holes (AGN) E-2 point source: (>10 GeV) <10-7 (cm-2s-1)
E-2 diffuse flux : E2< 1x10 GeV cm-2s-1sr-1
• GRB in coincidence with BATSE Cumulative Fluence< 4x10-4 TeVcm-2
• Atmospheric neutrinos (135 live days) ~170 events from 1997, depends on analysis Calibration of sensitivity within factor 2
• WIMPs from the earthAlso, see ICRC99 for limits on relativistic monopoles, search for SNa, ice properties
