Neutrino Astroparticle Physics

Lutz KöpkeUniversity of Mainz, Germany

July 8, 2005

XXV Physics in Collision

Physics in collisions?

1012 1015 1018 1021 eV

50 GeV 1.4 TeV 40 TeV 1400 TeV

actually not ... fixed target physics:

center of mass energy

neutrino energy

atmosphericneutrinos

GZK: p+CMB n+X+

...limits exist all the way up to 1025 eV

probe physics beyond LHC

Physics motivation

origin and acceleration of cosmic rays understand cosmic cataclysms find new kind of objects?

neutrino properties ( , cross sections ..)

dark matter (neutralino annihilation)

• tests of relativitiy ....• search for big bang relics ...• effects of extra dimension etc. ...

pp ± + X e,.... p + + X e , ....

Beam dump:

... astrophysics and particle physics

Particle propagation in the Universe

gammas (0.01 - 3 MLy)

Protons/nuclei: deviated by magnetic fields, reactions with radiation (CMB)

protons E>1019 eV (30 MLy)

protons E<1019 eV

neutrinos

Cosmicaccelerator

Katz

Photons: absorbed on dust and radiation

Neutrino source candidatesActive Galaxy(optically dense, e.g. FRII)

Black hole with108 x mass of sun

106 Ly

extra-galactic

Supernova remnant Microquasar(SS433 etc.)

Crab nebula

Black hole with mass of sun

1 Ly

galactic

WB bound

MPR bound

Mannheim, Protheroe and Rachen (2000) Waxman, Bahcall (1999)

derive generic limits from limits on extragalactic p‘s -ray flux

log

[E2

· flu

x(E

) / G

eV c

m-2 s

-1 s

r-1]

-9

-7

-8

-6

-5

atmospheric

2 43 5 8 109 log (E /GeV)6 7

AGN

core

(SS)

AGN Jet (

MPR)

GRB (WB)

GZK

Required sensitivity

many specific models fornon-resolved sources ...

... for discovering extraterrestrial neutrinos

TeV PeV EeV

Can it be done ?

Reaction probability [H2O, d=1km]: W=NAd 4 •10-7 • E[TeV]

... sources millions to billions light years away ...

Needs huge detectors making use of natural media Require high energies Need to detect all flavors

Haim-Harrari: neutrino physics is the art to learn a lot from nothing ....

Extended source with e:: =1:2:0 production (e.g. decay) :for 23 45°, 130°:

e:: =1:1:1 on earth

Principle detection methods

radio, acoustics, particles ...

moon, ice, saltmountain ...

detectors (earth based, balloon/satellite)

extremely high energies (E>1018 eV)high energies (E> 1011 eV)

grid of light sensors for Cherenkov radiation

Single photon detection

... information: timing and amplitude of photons - position of PMTs

IceCube

…typically 300 MHz digitization

Detection of , e ,

O(km) long muon tracks

direction determination by Cherenkov light timing

15 m

O(10) x less background for e – but you don’t profit from long -range Regeneration of - no absorption in earth even at very high energies !

Electromagnetic and hadronic cascades

~ 5 m

The neutrino telescope world map

Antares

Nemo

Nestor

Amanda/IceCube

Baikal

KM3Net?

Importance of complete sky coverage

South Pole (ice)AMANDA, ICECUBE

galactic center in middle

Mediterranean (ocean) Antares, Nestor, 1 km3 ...

4 coverage for e , !

Need earth as shielding agains cosmic rays for (if E < 100 TeV)

Importance of large energy coverage

Neutrino flavor

Log(ENERGY/eV)

12 18156 219

e

e

supernovaeFull flavor ID

Showers vs tracks

IceCube flavor ID,direction, energy

IceCube triggered,partial reconstruction

TeV PeV

Importance of low background

Nest

or

cosmic ray muons

IceC

ube

Detector noise: low in inert ice (1 kHz/PMT)

: 105-106 x dominated by cosmic ray muons need low misreconstruction

e: background much lower (but smaller detection volume) scattering helps ...

Importance of good angular resolution

Expected resolution for 1 km3 detectors

Icewater

...can‘t compete with -telescopes

..but for many analyses not crucial

atmospheric

size of moon

Price and ease of construction

Ice

IceCube: M$273 (US accounting)50 M$ detector cost

moon

... use existing moon…and radio antennas

water

KM3Net: < 200 MEUR

Northern hemisphere detectors

1100 m deepdata taking since 1998new: 3 distant strings

Antares Nestor

under construction2400 m deepcompletion: early 2007

1 of 12 floors deployed4000 m deepcompletion: 2007?

Baikal NT200 NESTORAstrop. Phys. 23, 377 (2005)

BAIKAL NT200+Excellent example that smart ideas can compensate small size and budget

data taking since 19983 external strings in operation since April 05 sensitivity quadrupled

… concentrate on induced showers

-2400m

40 km

submarine cable

Antares

~ 40 km

string based detector, 0.01 km3 instrumented volume

prototype strings 2003, March 2005 1st „final“ string mid 2005 detector completion early 2007

Antares test string 2005

... detectors moving with currents….

acoustic positioning < 10 cm (2mm for fixed distance)

string based detector, 0.01 km3 instrumented volume

1st „final“ string mid 2005 detector completion early 2007

AMANDA and IceCube

Optical module (677)

1500 atmospheric ‘s /year

1996-2000

..collaborations merged March 2005 ...

80000 atmospheric ‘s /year

IceTop

1400 m

2400 m

1 km3 IceCube

0 m

> 70 strings> 4200 modules

0.02 km3 AMANDA

South Pole Station

IceCube Counting HouseFirst IceCube string

1400m

2400m

1500 m

2000 m

AMANDA

[not to scale]

the South-Pole laboratory

The new station operating at least until 2035

January 2005:60 optical modulesDeepest module at 2450 m

First IceCube string ...

IceTop – IceCube

IceCube coincident events ..

Amanda – IceCube

The testbeams

1 TeV 1000 TeV

Eμ E-3.8

Eprimär E-2.7

... Primary energy corrected

Energy spectrum with unfolding technique

atmospheric neutrinos

1 GeV 1 TeV

Amanda

Frejus

Eν E-3.8

EHadrfon E-2.7 0.02

Preliminary

cosmic ray muons

Atmospheric neutrinos... IceCube will be abundant source of atmospheric neutrinos:

AMANDA (5y) 10000, 70 between 10-100 TeV IceCube (5y) 300000, 2000 between 10-100 TeV

e.g. study of equivalence principle, velocity induced oscillations:

cc

2 orders of magnitude improvement in sensitivity

Neutrinos from unresolved sources

Preliminary

(2000 data) cascades (2000 data)

Expect deviation at high energy (hard flux)

Very high energiesSpecial analysis for very high energies above 1000 TeV ....

large energy deposits (bremsstrahlung) Earth starts absorbing

70 TeV: interaction length = earth diameter

AMANDA reach (5y): 10-7 cm-2 s-1 sr-1

90% energy range: 1.8 105 - 1.8 109 GeV

GZK

log

[E2

· flu

x(E

) / G

eV c

m-2 s

-1 s

r-1]

-9

-7

-8

-6

-5

FREJUSMACRO

atmospheric

2 43 5 8 109log (E /GeV)

6 7

BAIKAL

AMANDA limits

DUMAND test string

IceCube (3y)

Experimental bounds and future

..closing in on Waxman-Bahcall bound

gain factor 30 in sensitivity with 1 km3 detectors

present AMANDA sensitivity

--- Preliminary

2000-2003 (807 days)3329 from northern hemisphere3438 expected from atmospheric

Maximum significance 3.4 compatible w. atmospheric

Search for localized sources (AMANDA)

quite expected ...92% of experiments would yield even higher maximum

Prelim

inar

y

1E-18

1E-17

1E-16

1E-15

1E-14

1E-13

1E-12

-90 -60 -30 0 30 60 90

Reihe1

Reihe2

Reihe3

Reihe4

Reihe5

10-12

10-14

10-15

10-16

10-17

10-18

10-13

neut

rino

indu

ced

muo

n flu

x /(c

m2 s

)

declination (degrees)

Macro

BaksanIMB

2012KM3Net IceCube

2007 Antares+NestorAII+IceCube

... measured limits and future

Super-K

Amanda

optimized for E-2, (*) E-2, 3 signal

1997 : ApJ 583, 1040  (2003) 2000 : PRL 92, 071102 (2004)

2000-02 : PRD 71 077102 (2005)

IceCube: Astrop Phys 20, 507 (2004)

*

lim 0.68·10-8 cm-2s-1

ave

rag

e fl

ux

up

per

lim

it [

cm-2s-1

]

sin

AMANDA-B10

AMANDA-II

IceCube 1/2 year

*

Preliminary

... steady progress in sensitivity

time

>10

GeV

... closing in on predictions

BaksanMakro

AII (1Y) AII (3y)

AII (4y)

1,00E-08

1,00E-07

1,00E-06

1,00E-05

Distefano 2002

10-5

10-7

10-8

10-6

inte

grat

ed n

eutri

no fl

ux /(

cm2 s

) [E>

1 G

eV]

predictions very model dependent ... some can be tested now .. e.g. SS-433 micro quasar:

preliminary

SS-433

Additional studies Search for excess in galactic plane Search for neutrino clusters (sliding time window) coincidence with enhanced EM emision x-ray, radio and -ray) curosity: 1 neutrino candidate close to orphan peak (no radio signal)

...no statistically significant effects need multiwavelength campaigns!

Error bars: off-source background per 40 days

May '02 July '02June '02

sliding search window

GRBsearch in AMANDASearch for candiates correlated with GRBs - background established from data

effective area 50000 m2 () limit assumíng WB spectrum: Eν

2Φν < 3 x 10-8 GeV cm-2 s-1 sr-1 () < 9.5x10-8 GeV cm-2 s-1 sr-1 (cascades) No coincident events observed observed!

: <20°

PRELIMINARY

Cascade channel:worse pointing but 4!

Green’s Function Fluence Limit(allows for comparison with SK)

SuperKamiokande (1454)

AMANDA sensitivity

AMANDA limit

Further investigations ... Search without temporal/spacial constr.: Eν

2Φν < 6.7x 10-6 GeV cm-2 s-1 sr-1 detailed investigations of GRB 030329 - large model dependencies !!

PRELIMINARY

Future goal: determination of limits independent of specific model

Indirect search for dark matter

0214

0113

31211

01

~~~~~ HNHNWNBN

neutralino is best particle physics candidate for dark matter stable if R-parity conserved (for most parameters)

Nuclear Recoil and indirect searches are complementary and not equivalent !!

can self-annihilate (Majorana particle) and produce neutrinos gravitationally trapped in center of earth, sun or center of galaxy

e.g.: + b + b

c + - +

; W+W-

Disfavored by direct search (CDMS II)

Limits on muon flux from Earth center

WIMP search in AMANDAAMANDA results submitted for publication

Limits on muon flux from Sun

1km3 (IceCube)

AMANDA 1y

Antares 3 yearsSK

e.g magnetic monopoles:

Cherenkov-light (n·g/e)2

(1.33*137/2)2

10-16

10-15

10-14

10-18

10-17

= v/c1.000.750.50

up

per

lim

it (

cm-2 s

-1 s

r-1)

KGF

Soudan

Baikal

Amanda

1 km3

electrons

MACRO

Orito

New particles

8300 times stronger than for !

high sensitivity to rare new particlesif signature unambigous ....

... (slowly) moving bright particles ...

The (near) future

complete construction of 1 km3 IceCube detector 2010 can already work with incomplete detector …

complete construction of smaller mediterranean detectors 2007? decide on location/design of 1km3 mediterranean detector 2006? Complete construction of KM3Net? 2012?

new ideas for detection of extremely high energy neutrinos .... extend the search to higher energies with even bigger detectors

IceCube: 11/2004 - 9/2010

Up to 18 holes per season:

Nov.: preparationDec.: constructionJan.: constructionFeb.: commissioning

Deploymentof string N

Drilling of hole N

0h 12h 24h 36h 48h 60h 72h 84h

Time

35% of money spent ...

Signatures in IceCube …

signature of signature of

1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV

+N+...

± (300 m track!)

+hadrons

1 km3 array in Mediterranean

Extensive exploration and R&D (NEMO)

efforts of all groups (Antares, Nestor, Nemo) being joined to form single collaboration

• EU-funded design study (10 M€ requested)• on list of proposed large EU-projects (ESFRI)• problems mainly „political“ (site e.g.) • new technological develoments

multianode PMTs with Winston cones) .... but time scale tight

design report 2

008

constructio

n 2009-2013?

Anita - quest for GZK neutrinos

refracted radio

Antarctic iceneutrino

surveys > 1 million km2

under construction launch Dec 2006

Preliminary!

... very rare - very high energy events many proposals for radio and acoustic detectors in ice, water, salt, from moon ..

e.g. IceCube extension:>>km attenuation lengthsparse instrumentation100-fold volume increase

>100

> 10 GZK neutrinos/y

ear

IceCube

RICEAGASA

Amanda, Baikal

2002

2004

2008

AUGER Anita

0.1 km3

later km3

satellitesradio

Glue

Summary

plenty of results (limits)closing in on predictions …

1 km3 IceCube construction started 30 times efffective area

mediterranean detectors under construction taskforce for 1 km3 detector

innovative concepts for even larger detectors

..no extraterrestrial neutrinos found yet ...but:

0.214.502SS433

1.255.3610Crab Nebula

0.405.214Cygnus X-1

0.775.046Cygnus X-3

0.383.7151ES1959+650

0.685.586Markarian 421

Flux Upper Limit 90%(E>10 GeV)

[10-8cm-2s-1]

Expectedbackgr.(4 years)

Nr. of n events

(4 years)

Source

selected objects → no statistically significant effect observed

… out of 33 Sources

Systematic uncertainties under investigation

Crab Nebula: MC probability for excess 64%

Sensitivity /~2for 200 days of “high-state” (HEGRA)

... Limits on selected sources

Galactic center

for a E-2 spectrum

with quality selection and BG suppression (atm reduction by ~106)

• Median angular reconstruction uncertainty ~ 0.8• further improvement expected using waveform info

IceCubeEffective Area and Angular Resolution for Muons

Energy resolution: [log10(E)] 20%-30%

1E-18

1E-17

1E-16

1E-15

1E-14

1E-13

1E-12

-90 -60 -30 0 30 60 90

Reihe1

Reihe2

Reihe3

Reihe4

Reihe5

10-12

10-14

10-15

10-16

10-17

10-18

10-13

neut

rino

indu

ced

muo

n fl

ux /(

cm2 s

)

declination (degrees)

Macro

Amanda

Super-K

BaksanIMB

2007

2012KM3NeT IceCube

Antares+NestorAII+IceCubeGX339-

4SS-433

MK501 /~1

Cygnus-X1

Sun

Cassiopeia. A

Approximate AMANDA horizon

90 000 light years

SMC

LMC

Crab Nebula