The wierdest wonder
Download
1 / 40

The Wierdest wonder - PowerPoint PPT Presentation


  • 73 Views
  • Uploaded on

The Wierdest wonder. Is it good or is it bad?. 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.

loader
I am the owner, or an agent authorized to act on behalf of the owner, of the copyrighted work described.
capcha
Download Presentation

PowerPoint Slideshow about 'The Wierdest wonder' - aminia


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.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript
The wierdest wonder
The Wierdest wonder

  • Is it good or is it bad?

Per Olof Hulth


Amanda experience
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

Per Olof Hulth



Amanda data analysis
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

    • n point sources

    • Diffuse n flux

    • Neutrinos from GRB

    • and Supernova, magn. monoples, AMANDA-SPASE etc

Per Olof Hulth


Amanda ii feb 00
AMANDA-II Feb. 00

Per Olof Hulth


Amanda n candidate
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

Per Olof Hulth


Amanda n candidate1
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

Per Olof Hulth


Search strategies for he n s
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.

Per Olof Hulth


Signal background separation
Signal-background Separation

Arb. normalization between signal and BG

Per Olof Hulth


Spase amanda
SPASE-AMANDA

SPASE: South Pole Air Shower Experiment

  • Calibration of absolute pointing

  • Calibration of pointing resolution

  • Calibration of signal efficiency

Per Olof Hulth


Data reduction 1997
Data Reduction 1997

E.g. one of the atmospheric neutrino analysis, 1997.

Per Olof Hulth


Atm n background rejection
Atm. n: 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. n signal

103

1

Per Olof Hulth


Angular distributions
Angular Distributions

Two distinct analysis techniques, but not independent

(a)

(b)

MC

(normalized)

Per Olof Hulth


Atmospheric neutrinos
Atmospheric Neutrinos

  • Stronger selection criteria than point analysis

  • Two distinct analysis methods

  • Expected number of events depends on analysis efficiency

Per Olof Hulth


Search for he n point sources
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

Per Olof Hulth


Sky plot of events
Sky Plot of Events

Equatorial Coordinates

  • 1097 events

  • No obvious clustering

  • Event sample consists of atm. n and atm. muons.

Per Olof Hulth


Significance distribution
Significance distribution

  • Bin sky according to angular resolution

  • Use declination band to estimate background

  • No statistically significant excess

Per Olof Hulth


Flux limit preliminary
Flux Limit (preliminary)

  • AMANDA B10 limits are compared to MACRO limits. SuperK curve is estimated!

  • AMANDA-II will complement sky coverage of SuperK

Per Olof Hulth


Point source fluxes
Point Source Fluxes

Figure adopted from Mannheim & Learned

  • Theoretical predictions are very small

  • AMANDA limit assumes source with E-2 spectrum

Per Olof Hulth


Mk 501 flux limit
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

Per Olof Hulth


Search for diffuse flux
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

Per Olof Hulth


Diffuse flux
Diffuse Flux

  • Generally 103 larger than point fluxes

  • Atm. n backgrounds 103 worse

  • E2Fn < 1.6x10-6 GeVcm-2s-1sr-1

AMANDA

Per Olof Hulth


Wimps from sun earth
WIMPs from Sun/Earth

Per Olof Hulth


Angular spread of wimp signal
Angular Spread of WIMP signal

  • Angular spread decreases as WIMP mass increases, reducing atm. n background

Per Olof Hulth


Cuts for wimp search
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.

Per Olof Hulth


Wimps from the earth
WIMPs from the Earth

Optimized search for vertical neutrinos (1997 data)

  • AMANDA limits comparable to MACRO and Baksan

  • AMANDA sensitivity will increase at low mass due to special string trigger and better optimized analyzes

Per Olof Hulth


Wimp search with ice 3
WIMP search with Ice3

The WIMP search has been tested for two different

geometries and the limits are given for 10 years of running

Per Olof Hulth


Wimps from the earth with ice 3
WIMPs from the Earth with Ice3

Optimized search for vertical neutrinos

  • Ice3 will significantly improve the sensitivity.

Per Olof Hulth


Wimps from the earth with ice 31
WIMPs from the Earth with Ice3

Optimized search for vertical neutrinos

  • Ice3 will completely cover the DAMA area

Per Olof Hulth


Wimps from the sun with ice 3
WIMPs from the Sun with Ice3

  • Ice3 will significantly improve the sensitivity.

Per Olof Hulth



Search for he n from grb
Search for HE n from GRB

Per Olof Hulth


Grb science
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(Ice3)

  • Search for n emission in coincidence with Gamma ray detectors

Per Olof Hulth


He n emission from grb s
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)

Per Olof Hulth


Amanda supernova detection
AMANDA Supernova detection

  • ne + 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

Per Olof Hulth


Amanda sn sensitivity
AMANDA SN sensitivity

  • AMANDA-B10 has a sensitivity for SN up to the centre of our galaxy

  • Aim to connect AMANDA SuperK, MACRO, LVD, SNO,.. in an early warning SN system

Per Olof Hulth


Amanda effective area
AMANDA Effective Area

  • AMANDA-II 30,000-50,000 m2

  • AMANDA-II has nearly uniform response over all zenith angles

Per Olof Hulth


Summary and outlook
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

Per Olof Hulth


Publications
Publications

  • Many conference reports

  • So far X Ph.D. Thesis based on AMANDA

  • First neutrino results in Astroparticle Physics 13 (2000) 1, (AMANDA-B4)

  • Six 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

Per Olof Hulth


Amanda results
AMANDA Results

  • Supermassive Black Holes (AGN)

    • E-2 point source: fn (>10 GeV) <10-7 (cm-2s-1)

    • E-2 diffuse flux : E2fn< 1.6x10-6GeV cm-2s-1sr-1

  • GRB in coincidence with BATSE

    • Cumulative Fluencen< 4x10-4 cm-2TeV

  • Atmospheric neutrinos (138 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

Per Olof Hulth


ad