Neutrino astronomy with AMANDA and IceCube Per Olof Hulth Stockholm University [email protected].

Neutrino Neutrino astronomyastronomy

withwithAMANDA and AMANDA and

IceCubeIceCubePer Olof HulthPer Olof Hulth

Stockholm UniversityStockholm University

[email protected]@physto.se

02-10-31 Per Olof Hulth Stockholm university

Short summary of Short summary of neutrinos for pedestriansneutrinos for pedestrians

There are three different “families” of There are three different “families” of leptonsleptons Electron neutrino (Electron neutrino (ee) and the electron (e) and the electron (e--)) Muon neutrino (Muon neutrino () and the muon ) and the muon Tau neutrino (Tau neutrino () and the tau ) and the tau

The neutrinos penetrates huge amount The neutrinos penetrates huge amount of matter without being absorbedof matter without being absorbed E.g. a 1 MeV neutrino from the sun has an E.g. a 1 MeV neutrino from the sun has an

absorption length of 20 light years in lead!!absorption length of 20 light years in lead!!


Some neutrino numbersSome neutrino numbers The Sun sends every second out The Sun sends every second out

200.000.000.000.000.000.000.000.000.000.000.000.000 200.000.000.000.000.000.000.000.000.000.000.000.000 (2*10(2*103838) neutrinos) neutrinos

At Earth At Earth wewe receive about 40.000.000.000 receive about 40.000.000.000 neutrinos/cmneutrinos/cm22/second/second

From Big Bang we have 330 000 000 neutrinos/mFrom Big Bang we have 330 000 000 neutrinos/m33 (Energi (Energi 0.0004 eV) but only half a proton0.0004 eV) but only half a proton

340 000 000 neutrinos are creataed in our body every day 340 000 000 neutrinos are creataed in our body every day ((4040K)K)


Neutrinos from Neutrinos from SupernovaSupernova

When a star When a star explodes 99% of explodes 99% of the energy is the energy is emitted in emitted in neutrinosneutrinos

A star exploded A star exploded 1054. Today the 1054. Today the Crab nebulaCrab nebula


R. Svensson Zdziarski AA.Ap.J.349:415-28(1990)

Kneiski TM, Mannerheim K, Hartmann D.Ap.J. Submitted 2000)

Gamma astronomy

€

γ+γBackgnd⇒ e++e−

Space is not transparent for High Energy Photons!


Three open questions Three open questions in Astrophysicsin Astrophysics

What is the missing dark matter in the What is the missing dark matter in the Universe?Universe?

What is the origin of the Highest Energy What is the origin of the Highest Energy Cosmic rays?Cosmic rays?

What is powering the Gamma Ray Bursts What is powering the Gamma Ray Bursts (GRB)?(GRB)?


You need 20 times more matter to keep the system together

than what is observed

DARK MATTER

!!!!


Most popular modelMost popular model

New type of matter (WIMPs)New type of matter (WIMPs) Supersymmetric particles from Big Supersymmetric particles from Big

BangBang Neutralinos.Neutralinos.


WIMPs from Sun/Earth

Look for excess of neutrinos from centre of the Earth and the Sun!!

Dark Matter search


Cosmic rays

About 100 muons/m2sek

proton

muons

mesoner


Cosmic rays

Energies up to 50 Joules!

What is the process creating these particles???


A possible candidate for a source for cosmic rays


Gamma Ray Bursts

The sources of GRBs on cosmologic distances!

The most “violent” objects in the Universe

Source 9 Billion light years away!


Gamma Ray BurstsGamma Ray Bursts

Could be danger Could be danger to be too close…to be too close…


Messengers of Astronomy

Only neutrinos cover the whole energy range


Neutrino production

€

p+γ ⇒ Δ+⇒

€

p+π0 → p+2γ

n+π +→ n+μ++νμ

If protons are accelerated we expect about equal amount of gammas and neutrino!!

€

μ+→ e++ν μ +ν e


log(E2 Flux)

log(E/GeV)TeV PeV EeV

3 6 9

pp core AGN p blazar jetTop-Bottom model

GRB (W&B)

Various recentmodels for transient sources

Classes of Models


Neutrino astronomy so Neutrino astronomy so farfar

Only two neutrino sources in space Only two neutrino sources in space has been observed.has been observed.

The solar neutrinos (Nobel price 2002)The solar neutrinos (Nobel price 2002) Neutrinos from SN1987 in the Large Neutrinos from SN1987 in the Large

Magellanic Cloud (180 000 light Magellanic Cloud (180 000 light years)years)

Energy of neutrinos only 1-30 MeVEnergy of neutrinos only 1-30 MeV


Neutrino physics (again)

We have three types of neutrinos:

Electron neutrino e

Muon neutrino

Tau neutrinon

E.g. Neutron decay :

neutron -> proton + e- + e


Neutrino interaction

The muon can travel several km in e.g. ice

< 1 degree


Cherenkov radiation

cosn

v/c, n= refraction index

A charged particle moving with the speed of light in the medium will generate a shock wave of light


The AMANDA telescope at the

South Pole

Why the South Pole?

A 3000 meter thick glaciar

A scientific base with all infra structure

No fishes and no 40K


AMANDA


South Pole

02-10-31 Per Olof Hulth Stockholm universityJoakim Edsjö SU

02-10-31 Per Olof Hulth Stockholm university Joakim Edsjö SU


neutrin

o

myon


neutrin

o

myon

106 muons from cosmic rays/muon

from neutrinos

!!!!

Select only muons from below!!!!

Select only muons from below!!!!


Hot water heaters

-55 C

-25 C-2400 m

-50 m


-840 m


AMANDA

Year DetectorTotal

number ofOM

1995/1996 AMANDA-B4 86

1996/1997 AMANDA-B10 302

1998/1999 AMANDA-B13 428

1999/2000 AMANDA-II 680


AMANDA AMANDA Event Event

SignaturesSignatures::

MuonsMuons

AMANDA AMANDA Event Event

SignaturesSignatures::

MuonsMuons

CC muon neutrino

interactions Muon tracks

+ N + X

DATA


Equatorial coordinates: declination vs. right ascension.

Point Sources Amanda II Point Sources Amanda II (2000)(2000)

Skyplot is scrambled in event time for blind analysis,Plot has been released, and

results will be available soon. Examples for a few candidates will

be given.


Super-Kamiokande

MACRO

-90 0-45 9045

10-15

10-13

10-14

cm-2 s

-1

Declination (deg)

AMANDA B10 and A-II: some limits and projected sensitivity

SS433*

Mrk501 (HEGRA 97,)

A-II, sensitivity on SS433

A-II, limit on SS433

A-II, limit on Mrk 501

AMANDA B10 average Sensitivity for sel. soruces

A-II projected sensitivityCombined 97-02

To appear in ApJ: astro-ph/0208006


Amanda Analysis activities

•AMANDA-B10 1997 analysis at the end

•AMANDA-B10 1999 analysis started

•AMANDA-II 2000 filtering done, first analyses started

•AMANDA-II 2001 online filtering continuously done

In order to do a “blind analysis” only 20% of the data is used for tuning cuts


IceCube has been designed as a IceCube has been designed as a discovery instrument with improveddiscovery instrument with improved::

telescope areatelescope areadetection volumedetection volumeenergy measurement of secondary muons and energy measurement of secondary muons and electromagnetic showerselectromagnetic showersidentification of neutrino flavoridentification of neutrino flavorangular resolutionangular resolution

IceCube!!


The IceCube The IceCube CollaborationCollaboration

11 European, 1 Japanese, 1 South American and 11 US Institutions(many of them are also AMANDA member institutions)

1. Bartol Research Institute, University of Delaware, Newark, USA2. BUGH Wuppertal, Germany3. Universite Libre de Bruxelles, Brussels, Belgium4. Dept. of Physics, Chiba University, Japan 5. CTSPS, Clark-Atlanta University, Atlanta USA6. DESY-Zeuthen, Zeuthen, Germany7. Imperial College, London, UK8. Institute for Advanced Study, Princeton, USA9. Dept. of Technology, Kalmar University, Kalmar, Sweden10. Lawrence Berkeley National Laboratory, Berkeley, USA11. Dept. of Physics, Southern University and A\&M College, Baton Rouge, LA, USA12. Dept. of Physics, UC Berkeley, USA 13. Institute of Physics, University of Mainz, Mainz, Germany14. Dept. of Physics, University of Maryland, USA15. University of Mons-Hainaut, Mons, Belgium16. Dept. of Physics, Pennsylvania State University, University Park, PA, USA17. Dept. of Physics, Simon Bolivar University, Caracas, Venezuela18. Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA19. Physics Dept., University of Wisconsin, River Falls, USA20. Division of High Energy Physics, Uppsala University, Uppsala, Sweden21. Fysikum, Stockholm University, Stockholm, Sweden22. Dept. of Physics, University of Alabama, Tuscaloosa, USA23. Vrije Universiteit Brussel, Brussel, Belgium24. Utrecht, Holland (since 29th of October 2002)


IceCube:Top View

AMANDA

SPASE-2South Pole

Dome

Skiway

100 m

Grid North

Counting House

80 strings

60 modules/string

Volume 1 km3

Depth 1400-2400 m


IceCube

80 Strings4800 PMT

1400 m

2400 m

AMANDA

South Pole

IceTop

Skiway


- flavors and energy ranges

Filled area: particle id, angle, energyShaded area: energy and angle.

Neutrino flavoreLog(ENERGY/eV)1218156219νe


µ-events in IceCube

1 km

Eµ=10 TeV Eµ=6 PeV

AMANDA-II

Measure energy by counting the number of fired PMT.(This is a very simple but robust method)


1 pp core AGN (Nellen)2 p core AGN Stecker & Salomon)3 p „maximum model“ (Mannheim et al.)4 p blazar jets (Mannh)5 p AGN (Rachen & Biermann)6 pp AGN (Mannheim)7 GRB (Waxman & Bahcall)8 TD (Sigl)

Mannheim & Learned,2000

MacroBaikal

IceCube

Amanda

Diffuse Fluxes: Predictions and Limits


Compare to Mrk 501 gamma rays

Sensitivity of 3 years of IceCube

Field of view:Continuous

2 sr (northern sky) AMANDA B10

prelim. limit


Only 200 GRB needed to detect/rule out WB99 flux

Test signal: 1000 GRB a la Waxman/Bahcall 1999 Expected no. of events: 11 upgoing muon eventsExpected background: 0.05 events

Sensitivity (1000 bursts): 0.2 dN/dE (Waxman/Bahcall 99)

Neutrinos from Gamma Ray Bursts


Cascade event

E = 375 TeV

The length of the actual cascade, ≈ 10 m, is small compared to the spacing of sensors

1 PeV ≈ 500 m diameter

Fully active calorimeter with linear energy resolution

e + N --> e- + X

Sensitivity for diffused flux about the same as for muons


+ N -->- + X

+ X

• E << 1 PeV: Single cascade (2 cascades coincide)

• E ≈ 1 PeV: Double bang

• E >> 1 PeV: Second cascade + tau track

“Double Bang”


Cosmic beam: e = µ = because of oscillations

not absorbed by the Earth (regeneration)

Pile-Up near 1 PeV where ideal sensitivity

IceCube sensitive to m2>10-17 eV2

Enhanced role of tau neutrinos because of neutrino oscillation!?

Tau neutrinos and oscillations


Dark matter detection with IceCube

Ice3 will significantly improve the sensitivity!

WIMPS from Earth WIMPS from Sun


Supernova detection

• e + p n + e+ (10-40 MeV)

•PMT noise increase due to the positrons

• AMANDA/IceCube records the noise of the PMTs over 0.5 sec and summing up total rate over 10 sec intervals.

•Detectors to be connected to Supernova Early Warning System

In addition to the MeV e neutrinos, 10-100 muon neutrinos are expected after a few hours in the TeV energy range.

AMANDA IceCube


SummarySummary

IceCube will open a significant new IceCube will open a significant new window on the Universe.window on the Universe.

Hopefully we will observe Hopefully we will observe something which has not been something which has not been discussed in this presentation.discussed in this presentation.


Hotwater Drilling

QuickTime™ and aPhoto - JPEG decompressor

are needed to see this picture.

Experience with AMANDA: 19 holesUpgrade:from 2 to5 MWProjected time to 2450 m depth: 40 hDiameter: 50 cm Drill 2 holes per week; 16 holes per season


Optical sensor

Installation of one sensor: ≈10 min QuickTime™ and a

Photo - JPEG decompressorare needed to see this picture.


Mats Pettersson Gymnasielärare från Angereds gymnasium Göteborg vid sydpolen 14 november 2001

02-10-31 Per Olof Hulth Stockholm universityJoakim Edsjö SU


Joakim Edsjö SU

Neutrino astronomy with AMANDA and IceCube Per Olof Hulth Stockholm University [email protected].

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Transcript of Neutrino astronomy with AMANDA and IceCube Per Olof Hulth Stockholm University [email protected].