AMANDA people in Sweden

Transcript AMANDA people in Sweden

AMANDA

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 2000-06-18

AMANDA

AMANDA SN sensitivity

• Test 2000-06-18

AMANDA

AMANDA people in Sweden

• • Kalmar University  

Staffan Carius, Sr.Lecturer

Pär Lindahl, grad.student



Arvid Pohl, grad. student

Stockholm University, experiment 

Patrik Ekström, grad.student

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Per Olof Hulth, Professor

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Yulia Minaeva, grad.student

Julio Rodrıguez Martino, grad.student

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Christian Walck, Sr.Lecturer

• • Stockholm University, theory  

Lars Bergström, Professor Joakim Edsjö, post doc

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Hector Rubinstein, Professor

Uppsala Universitet 

Olga Botner, Professor

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Allan Hallgren, Sr. Lecturer Pia Loaiza, lic.

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Pawel Marciniewski, grad. Student

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Carlos Perez de los Heros, NFR Researcher



Jan Conrad, grad.student

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AMANDA

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 2000-06-18

AMANDA

Messengers of Astronomy

• The neutrino window begins at energies above 10 6 eV • Era of multi messenger astronomy 2000-06-18

AMANDA

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 2000-06-18

AMANDA

AMANDA Science Goals-2

2000-06-18 • 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

AMANDA

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 2000-06-18

AMANDA

Detection Method for

n m • Cherenkov photons are detected by array of PMTs • Tracks are reconstructed by maximum likelihood method using photon arrival times.

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AMANDA AMANDA-II Feb. 00 2000-06-18

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 2000-06-18

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 2000-06-18

AMANDA

Event Rate Predictions

Point Sources Source_______ SNa Remnant AGN (3C273) Mk421, Mk501 GRB (  fluct. model ) Rate(/km 2 yr) E m > 1 TeV 3 1-100 1-10 from  flux ~ a few (from a rare burst) Source AGN AGN jets GRB Atm n Diffuse Sources Rate(/km 2 yr sr) E m > 1 TeV_____ 400-800 45 10 1000 2000-06-18

AMANDA

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.

Source Rejection method____ Diffuse flux 1. up-down Background (10 9 /yr)(atm.

m ) Point Source (e.g. AGN) 1. up-down 2. direction 3. energy?

(10 x(d 9 /yr)(atm.

 /2  ) m ) Bursts (e.g. GRB) 1. up-down 2. direction 3. time stamp 4. energy?

(10 9 /yr)(atm.

m ) x(d  /2  ) x(dt/3x10 7 ) 2000-06-18

AMANDA

Atmospheric Neutrinos

• Stronger selection criteria than point analysis • Two distinct analysis methods • Expected rate depends on analysis efficiency 2000-06-18

AMANDA

Data Reduction 1997

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

Triggered Observed number of events

1.2*10 9

Predicted number of neutrinos

4500

Reconst.

Upgoing Passing final cuts

5.1*10 4 193 570 235

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AMANDA

AMANDA Effective Area

• AMANDA-II 30,000-50,000 m 2 • AMANDA-II has nearly uniform response over all zenith angles 2000-06-18

AMANDA • Generally 10 3 larger than point fluxes • Atm .n 10 3 backgrounds worse • E 2 F n < 1.6*10 -6 GeVcm -2 s -1 sr -1 2000-06-18

Diffuse Flux

AMANDA

Search for HE

Point Sources

• Concentrate on continuous emission from sources with hard spectra (~E -2 ) • Optimize search on Signal to Noise Ratio   A eff depends on rejection requirements Iterative procedure defined

a priori

• Background for this search   Poorly reconstructed atmospheric muons Atmospheric neutrinos 2000-06-18

AMANDA • 1097 events • No obvious clustering

Sky Plot of Events

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

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AMANDA

Significance distribution

• Bin sky according to angular resolution Title: /tmp_mnt/u/tornado1/youngs/data/sigma.coguci.24x48. Creator: HIGZ Version 1.23/09 Preview: This EPS picture was not saved with a preview (TIFF or PICT) included in it Comment: This EPS picture will print to a postscript printer but not to other types of printers • Use declination band to estimate background • No statistically significant excess 2000-06-18

AMANDA

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/r Creator: HIGZ Version 1.23/09 Preview: This EPS picture was not saved with a preview (TIFF or PICT) included in it Comment: This EPS picture will print to a postscript printer but not to other types of printers 2000-06-18

AMANDA

SPASE-AMANDA

SPASE: South Pole Air Shower Experiment • Calibration of absolute pointing • Calibration of pointing resolution • Calibration of signal efficiency 2000-06-18

AMANDA

Angular Distributions

Two distinct analysis techniques, but not independent (a) MC (normalized) (b) 2000-06-18

AMANDA

Signal-background Separation

Arb. normalization between signal and BG 2000-06-18

AMANDA

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 2000-06-18

AMANDA

WIMPs from Sun/Earth

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AMANDA

Angular Spread of WIMP signal

• Angular spread decreases as WIMP mass increases, reducing atm. n background 2000-06-18

AMANDA

Cuts for WIMP search

• Optimized cuts for almost vertical upward moving muons.

• The simulated WIMP signal is reduced to 30% after reducing background by 10 8 .

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AMANDA

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 2000-06-18

AMANDA

WIMPs from the Earth with Ice

3 Optimized search for vertical neutrinos • Ice 3 will improve the sensitivity several orders of magnitude 2000-06-18

AMANDA

WIMPs from the Earth with Ice

3 Optimized search for vertical neutrinos • Ice 3 will completely cover the DAMA area 2000-06-18

AMANDA

WIMPs from the Sun with Ice

3 • Ice 3 will improve the sensitivity several orders of magnitude.

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AMANDA

WIMPs from the SUN with Ice

3 • Ice 3 will improve the sensitivity several orders of magnitude 2000-06-18

AMANDA

WIMP search with Ice

3 The WIMP search has been tested for two different geometries 2000-06-18

AMANDA

Search for HE

from GRB

2000-06-18

GRB search bin Off source GRB Position GRB burst 16 s 1 hour 1 hour BKG - off time on time BKG - off time

AMANDA

GRB Science

• Verify fireball model • GRBs may be sources of highest energy cosmic rays • Test of special relativity • Search for n t appearance at D m 2 > 10 -17 eV 2 • Search for n emission in coincidence with BATSE or MILAGRO 2000-06-18

AMANDA

HE

emission from GRB’s ?

- Not so far 10 -1 Combined Limit (90% CL) 10 -6 Waxman and Bahcall 1 Burst Duration (s) 100 2000-06-18

AMANDA

Future : Ice

!!

• Neutrino astronomy needs a detector size of about 1 km 3 effective volume!

in • 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 Hartell which 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.

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AMANDA

Ice

Muon Event (simulated)

• OMs that detect Cherenkov photons are colored circles • Earliest photons are red, latest photons are blue.

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AMANDA

Ice

Electron neutrino Event

• Color circles indicate OMs that detect Cherenkov photons. • Earliest photons are red, latest photons are blue.

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AMANDA

Ice

Tau Event (double-bang)

• Color circles indicate OMs that detect Cherenkov photons. • Earliest photons are red, latest photons are blue.

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AMANDA

AMANDA Results

• Supermassive Black Holes (AGN)   E -2 E -2 point source: f n (>10 GeV) <10 diffuse flux : E 2 f n < 1.6*10 -6 -7 (cm GeV cm -2 -2 s s -1 -1 ) sr -1 • GRB in coincidence with BATSE  F n < 5x10 10 km -2 yr -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 2000-06-18

AMANDA

Publications

• Many conference reports • In Sweden 2 Ph.D. Thesis and 4 Lic.

• First neutrino results in Astroparticle Physics

(2000) 1, (AMANDA-B4) 2000-06-18 • 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

AMANDA

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 2000-06-18

AMANDA

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 2000-06-18

AMANDA 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.

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AMANDA

Optical Absorption Length

• ~200m for blue light • Varies with depth, correlated with ice ages 2000-06-18

AMANDA • Variation with depth only recently included in detector simulation

Optical Scattering Length

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AMANDA

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 2000-06-18