Neutrino astronomy with AMANDA and IceCube

Per Olof Hulth Stockholm University [email protected]

Short summary of neutrinos for pedestrians



There are three different “families” of leptons

  

Electron neutrino (



e ) and the electron (e ) Muon neutrino (

 

) and the muon

( )

Tau neutrino (

 

) and the tau

( ) 

The neutrinos penetrates huge amount of matter without being absorbed

02-10-31 

E.g. a 1 MeV neutrino from the sun has an absorption length of 20 light years in lead!!

Per Olof Hulth Stockholm university

Some neutrino numbers

 The Sun sends every second out 200.000.000.000.000.000.000.000.000.000.000.000.000 (2*10 38 ) neutrinos  At Earth we receive about 40.000.000.000 neutrinos/cm 2 /second  From Big Bang we have 330 000 000 neutrinos/m 3 but only half a proton (Energi 0.0004 eV)  340 000 000 neutrinos are creataed in our body every day ( 40 K) 02-10-31 Per Olof Hulth Stockholm university

Neutrinos from Supernova

 When a star explodes 99% of the energy is emitted in neutrinos  A star exploded 1054. Today the Crab nebula 02-10-31 Per Olof Hulth Stockholm university



Gamma astronomy

  

Backgnd



e

 

e

-

Space is not transparent for High Energy Photons!

R. Svensson Zdziarski AA.Ap.J.349:415-28(1990) Kneiski TM, Mannerheim K, Hartmann D.Ap.J. Per Olof Hulth Stockholm university 02-10-31

Three open questions in Astrophysics

  

What is the missing dark matter in the Universe?

What is the origin of the Highest Energy Cosmic rays?

What is powering the Gamma Ray Bursts (GRB)?

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You need 20 times more matter to keep the system together than what is observed DARK MATTER !!!!

Most popular model

 New type of matter (WIMPs)  Supersymmetric particles from Big Bang  Neutralinos.

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WIMPs from Sun/Earth

Dark Matter search

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

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Cosmic rays

muons mesoner About 100 muons/m 2 sek

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Cosmic rays

Energies up to 50 Joules!

What is the process creating these particles???

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A possible candidate for a source for cosmic rays

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Gamma Ray Bursts

Source 9 Billion light years away!

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The sources of GRBs on cosmologic distances!

The most “violent” objects in the Universe

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Gamma Ray Bursts



Could be danger to be too close…

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Messengers of Astronomy

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Only neutrinos cover the whole energy range

Per Olof Hulth Stockholm university

  

Neutrino production

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p

     

p n

   0   

p

 2  

n

        

e

     

e

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

Per Olof Hulth Stockholm university

Classes of Models

log(E 2  Flux)

pp core AGN p



blazar jet Top-Bottom model

Various recent models for transient sources 02-10-31 GRB (W&B) 3 6 9 TeV PeV EeV Per Olof Hulth Stockholm university log(E/GeV)

Neutrino astronomy so far

 Only two neutrino sources in space has been observed.

 The solar neutrinos (Nobel price 2002)  Neutrinos from SN1987 in the Large Magellanic Cloud (180 000 light years)  Energy of neutrinos only 1-30 MeV 02-10-31 Per Olof Hulth Stockholm university

Neutrino physics (again)

We have three types of neutrinos: Electron neutrino  e Muon neutrino Tau neutrinon     02-10-31 E.g. Neutron decay : neutron -> proton + e +  e Per Olof Hulth Stockholm university

Neutrino interaction

02-10-31    -

< 1 degree

Per Olof Hulth Stockholm university

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

Cherenkov radiation

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

q 02-10-31 cos q=1/( n b) b= v/c, n= refraction index Per Olof Hulth Stockholm university

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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 40 K

Per Olof Hulth Stockholm university

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AMANDA

South Pole 02-10-31 Per Olof Hulth Stockholm university

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

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10 6 muons from cosmic rays/muon from neutrinos !!!!

Select only muons from below!!!!

-50 m

Hot water heaters

-55 C

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-25 C -2400 m

Per Olof Hulth Stockholm university

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-840 m

AMANDA

Year Detector 1995/1996 AMANDA-B4 Total number of OM 86 1996/1997

AMANDA-B10

302 1998/1999 1999/2000 AMANDA-B13

AMANDA-II

428 680 02-10-31 Per Olof Hulth Stockholm university

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DATA

AMANDA Event Signatures: Muons

CC muon neutrino interactions



Muon tracks

02-10-31  

+ N

 

+ X

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Point Sources Amanda II (2000)

02-10-31 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.

Per Olof Hulth Stockholm university Equatorial coordinates: declination vs. right ascension.

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AMANDA B10 and A-II

: some limits and projected sensitivity 10 -13 10 -14 AMANDA B10 average Sensitivity for sel. soruces

To appear in ApJ: astro-ph/0208006

A-II, limit on SS433 A-II, sensitivity on SS433 10 -15 -90 MACRO SS433* A-II projected sensitivity Combined 97-02 A-II, limit on Mrk 501 -45 0 45 Declination (deg) Per Olof Hulth Stockholm university 90

Mrk501 (HEGRA 97,

/=1

)

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

02-10-31 In order to do a “

blind analysis

” only 20% of the data is used for tuning cuts Per Olof Hulth Stockholm university

IceCube!!

IceCube has been designed as a discovery instrument with improved

: telescope area detection volume energy measurement of secondary muons and electromagnetic showers identification of neutrino flavor angular resolution

02-10-31 Per Olof Hulth Stockholm university

The IceCube Collaboration

11 European, 1 Japanese, 1 South American and 11 US Institutions (many of them are also AMANDA member institutions) 14.

15.

16.

17.

18.

19.

20.

21.

22.

23.

1.

2.

3.

4.

5.

6.

7.

8.

9.

10.

11.

12.

13.

Bartol Research Institute, University of Delaware, Newark, USA BUGH Wuppertal, Germany Universite Libre de Bruxelles, Brussels, Belgium Dept. of Physics, Chiba University, Japan CTSPS, Clark-Atlanta University, Atlanta USA DESY-Zeuthen, Zeuthen, Germany Imperial College, London, UK Institute for Advanced Study, Princeton, USA Dept. of Technology, Kalmar University, Kalmar, Sweden Lawrence Berkeley National Laboratory, Berkeley, USA Dept. of Physics, Southern University and A\&M College, Baton Rouge, LA, USA Dept. of Physics, UC Berkeley, USA Institute of Physics, University of Mainz, Mainz, Germany Dept. of Physics, University of Maryland, USA University of Mons-Hainaut, Mons, Belgium Dept. of Physics, Pennsylvania State University, University Park, PA, USA Dept. of Physics, Simon Bolivar University, Caracas, Venezuela Dept. of Astronomy, Dept. of Physics, SSEC, University of Wisconsin, Madison, USA Physics Dept., University of Wisconsin, River Falls, USA Division of High Energy Physics, Uppsala University, Uppsala, Sweden Fysikum, Stockholm University, Stockholm, Sweden Dept. of Physics, University of Alabama, Tuscaloosa, USA Vrije Universiteit Brussel, Brussel, Belgium

80 strings 60 modules/string Volume 1 km 3 Depth 1400-2400 m 02-10-31 IceCube:Top View AMANDA 100 m Grid North Counting House SPASE-2 Per Olof Hulth Stockholm university Skiway South Pole Dome

IceTop

IceCube

80 Strings 4800 PMT 1400 m 02-10-31 2400 m Per Olof Hulth Stockholm university AMANDA South Pole Skiway



- flavors and energy ranges

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

02-10-31 Neutrino flavor   e  e  6 9 12 15 18 Log(ENERGY/eV) 21 Per Olof Hulth Stockholm university

AMANDA-II

µ-events in IceCube

E µ =10 TeV E µ =6 PeV

02-10-31 1 km

Measure energy by counting the number of fired PMT.

(This is a very simple but robust method)

Diffuse Fluxes: Predictions and Limits

Mannheim & Learned, 2000 Macro Baikal Amanda IceCube 1 pp core AGN (Nellen) 2 p  core AGN Stecker & Salomon) 3 p  „maximum model“ 4 p  5 p  (Mannheim et al.) blazar jets (Mannh) AGN (Rachen & Biermann) 6 pp AGN (Mannheim) 7 GRB (Waxman & Bahcall) 8 TD (Sigl) 02-10-31 Per Olof Hulth Stockholm university

Compare to Mrk 501 gamma rays

Field of view: Continuous 2



sr

(northern sky) AMANDA B10 prelim. limit

Sensitivity of 3 years of IceCube

02-10-31 Per Olof Hulth Stockholm university

Neutrinos from Gamma Ray Bursts

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

0.2



dN/dE (Waxman/Bahcall 99)

Only 200 GRB needed to detect/rule out WB99 flux 02-10-31 Per Olof Hulth Stockholm university

Cascade event



e + N --> e + X

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 Sensitivity for diffused flux about the same as for muons 02-10-31 Per Olof Hulth Stockholm university

E = 375 TeV

“Double Bang”

 

+ N -->



- + X

 

+ X

• E << 1 PeV: Single cascade (2 cascades coincide) • E ≈ 1 PeV: Double bang • E >> 1 PeV: Second cascade + tau track 02-10-31 Per Olof Hulth Stockholm university

Tau neutrinos and oscillations Enhanced role of tau neutrinos because of neutrino oscillation!?

Cosmic beam:  e =  µ =   because of oscillations   not absorbed by the Earth (regeneration) Pile-Up near 1 PeV where ideal sensitivity IceCube sensitive to  m 2 >10 -17 eV 2 02-10-31 Per Olof Hulth Stockholm university

Dark matter detection with IceCube

WIMPS from Earth WIMPS from Sun

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Ice 3 will significantly improve the sensitivity!

Per Olof Hulth Stockholm university

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

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Summary

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

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

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Hotwater Drilling Experience with AMANDA: 19 holes Upgrade:from 2 to 5 MW Projected time to 2450 m depth: 40 h Diameter: 50 cm Drill 2 holes per week; 16 holes per season QuickTime™ and a Photo - JPEG decompressor are needed to see this picture.

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Optical sensor Installation of one sensor: ≈10 min QuickTime™ and a Photo - JPEG decompressor are needed to see this picture.

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Mats Pettersson Gymnasielärare från Angereds gymnasium Göteborg vid sydpolen 14 november 2001 02-10-31 Per Olof Hulth Stockholm university

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

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

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

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