AMANDA 2000-06-21 Per Olof Hulth The Wierdest wonder Is it good or is it bad?

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