2000-06-18

AMANDA

AMANDA Supernova detection

• 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 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

2000-06-18

AMANDA

Multi-messenger Astronomy

• Take advantage of complete suite of information carriers Particle Probes ( HE 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 106 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

• Particle Physics and Cosmology Dark Matter (WIMPs from sun and earth) Relativistic Monopoles Charm production Neutrino mass EHE ’s from topological defects

• Interdisciplinary Science Optical, mechanical, and thermal properties

of Antarctic ice

2000-06-18

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

• Cherenkov photons are detected by array of PMTs

• Tracks are reconstructed by maximum likelihood method using photon arrival times.

2000-06-18

AMANDAAMANDA-II

Feb. 00

2000-06-18

AMANDA

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

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

Source_______Rate(/km2yr)E > 1 TeV

SNa R eatAGN (3C273 )Mk421, Mk501GR B (γ fluct. ode l)

31-1001-10 fro γ flux~ a few(fro a rare burst)

SourceRate(/km2yr sr)E > 1 TeV_ ____

AGNAGN jetsGR BAt

400 -8004510100 0

Point Sources Diffuse Sources

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.

SourceRejectionmethod____ Background

Diffuse flux 1. up-down (109/yr)(atm.)

Poit Source(e.γ. AGN)

1. up-dow2. directio3. ee rγy?

(10 9/yr)(at.)x(dΩ/2p)

Bursts(e.γ. GR B)

1. up-dow2. directio3. tie stap4. ee rγy?

(10 9 /yr)(at.)x(dΩ/2p)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

Observednumber of

events

Predictednumber ofneutrinos

Triggered 1.2*109 4500

Reconst.Upgoing

5.1*104 570

Passing final cuts 193 235

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

2000-06-18

AMANDA

AMANDA Effective Area

• AMANDA-II 30,000-50,000 m2

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

2000-06-18

AMANDA

Diffuse Flux

• Generally 103 larger than point fluxes

• Atm. backgrounds 103 worse

• E2 < 1.6*10-6 GeVcm-2s-1sr-1

AMANDA

2000-06-18

AMANDA

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

2000-06-18

AMANDA

Sky Plot of Events

• 1097 events

• No obvious clustering

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

Equatorial Coordinates

2000-06-18

AMANDA

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

2000-06-18

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/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

2000-06-18

AMANDA

SPASE-AMANDA

• Calibration of absolute pointing

• Calibration of pointing resolution

• Calibration of signal efficiency

SPASE: South Pole Air Shower Experiment

2000-06-18

AMANDA

Angular DistributionsTwo distinct analysis techniques, but not independent

(a)MC (normalized)

(b)

2000-06-18

AMANDA

Signal-background SeparationArb. 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

• New energy estimators will lead to improved limits

2000-06-18

AMANDA

WIMPs from Sun/Earth

2000-06-18

AMANDA

Angular Spread of WIMP signal

• Angular spread decreases as WIMP mass increases, reducing atm. 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 108.

2000-06-18

AMANDA

WIMPs from the Earth

• AMANDA limits comparable to MACRO and Baksan

• AMANDA sensitivity will increase at low mass due to special string trigger

Optimized search for vertical neutrinos

2000-06-18

AMANDA

WIMPs from the Earth with Ice3

• Ice3 will improve the sensitivity several orders of magnitude

Optimized search for vertical neutrinos

2000-06-18

AMANDA

WIMPs from the Earth with Ice3

• Ice3 will completely cover the DAMA area

Optimized search for vertical neutrinos

2000-06-18

AMANDA

WIMPs from the Sun with Ice3

• Ice3 will improve the sensitivity several orders of magnitude.

2000-06-18

AMANDA

WIMPs from the SUN with Ice3

• Ice3 will improve the sensitivity several orders of magnitude

2000-06-18

AMANDA

WIMP search with Ice3

The WIMP search has been tested for two different geometries

2000-06-18

AMANDA

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

2000-06-18

AMANDA

GRB Science

• Verify fireball model• GRBs may be sources of highest energy cosmic

rays• Test of special relativity• Search for t appearance at m2> 10-17 eV2

• Search for emission in coincidence with BATSE or MILAGRO

2000-06-18

AMANDA

HE emission from GRB’s ?

10-1

10-6

1 100Burst Duration (s)

Waxman and Bahcall

Combined Limit (90% CL)

Flue

nce

(TeV

cm-2)

- Not so far

2000-06-18

AMANDA

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 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.

2000-06-18

AMANDA

Ice3 Muon Event (simulated)

• OMs that detect Cherenkov photons are colored circles

• Earliest photons are red, latest photons are blue.

2000-06-18

AMANDA

Ice3 Electron neutrino Event

• Color circles indicate OMs that detect Cherenkov photons.

• Earliest photons are red, latest photons are blue.

2000-06-18

AMANDA

Ice3 Tau Event (double-bang)

• Color circles indicate OMs that detect Cherenkov photons.

• Earliest photons are red, latest photons are blue.

2000-06-18

AMANDA

AMANDA Results

• Supermassive Black Holes (AGN) E-2 point source: f (>10 GeV) <10-7 (cm-2s-1) E-2 diffuse flux : E2f< 1.10- GeV cm-2s-1sr-1

• GRB in coincidence with BATSE < 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

2000-06-18

AMANDA

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

2000-06-18

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 , 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.

2000-06-18

AMANDA

Optical Absorption Length

• ~200m for blue light

• Varies with depth, correlated with ice ages

2000-06-18

AMANDA

Optical Scattering Length

• Variation with depth only recently included in detector simulation

2000-06-18

AMANDA

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