Neutrino Astroparticle Physics XXV Physics in Collision Lutz Köpke University of Mainz, Germany July 8, 2005

Physics in collisions? actually not ... fixed target physics: 1012 1015 1018 1021 eV 50 GeV 1.4 TeV 40 TeV 1400 TeV center of mass energy neutrino energy atmospheric neutrinos GZK: p+CMB n+X+  probe physics beyond LHC ...limits exist all the way up to 1025 eV

Physics motivation ... astrophysics and particle physics  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:

Particle propagation in the Universe Protons/nuclei: deviated by magnetic fields, reactions with radiation (CMB) protons E>1019 eV (30 MLy) protons E<1019 eV neutrinos gammas (0.01 - 3 MLy) Cosmic accelerator Katz Photons: absorbed on dust and radiation

Neutrino source candidates Microquasar (SS433 etc.) Active Galaxy (optically dense, e.g. FRII) Black hole with 108 x mass of sun  106 Ly extra-galactic Supernova remnant  1 Ly Crab nebula Black hole with  mass of sun galactic

Required sensitivity ... for discovering extraterrestrial neutrinos -5 many specific models for non-resolved sources ... -5 atmospheric -6 WB bound MPR bound  Mannheim, Protheroe and Rachen (2000)  Waxman, Bahcall (1999) derive generic limits from  limits on extragalactic p‘s -ray flux log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7 GZK AGN core (SS) -8 AGN Jet (MPR) GRB (WB) -9 log (E /GeV) 2 3 4 5 6 7 8 9 10 TeV PeV EeV

Can it be done ? Reaction probability [H2O, d=1km]: Haim-Harrari: neutrino physics is the art to learn a lot from nothing .... Reaction probability [H2O, d=1km]: W=NAd  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 Extended source with e:: =1:2:0 production (e.g.  decay) : for 23  45°, 130°: e:: =1:1:1 on earth

Principle detection methods high energies (E> 1011 eV) radio, acoustics, particles ... moon, ice, salt mountain ... detectors (earth based, balloon/satellite) extremely high energies (E>1018 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(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 ! O(km) long muon tracks direction determination by Cherenkov light timing  15 m Electromagnetic and hadronic cascades ~ 5 m

The neutrino telescope world map Baikal Antares Nemo Nestor KM3Net? Amanda/IceCube

Importance of complete sky coverage Need earth as shielding agains cosmic rays for  (if E < 100 TeV) South Pole (ice) AMANDA, ICECUBE Mediterranean (ocean) Antares, Nestor, 1 km3 ... galactic center in middle 4  coverage for e ,  !

Importance of large energy coverage Neutrino flavor Log(ENERGY/eV) 12 18 15 6 21 9 ne nm nt supernovae Full flavor ID Showers vs tracks IceCube flavor ID, direction, energy IceCube triggered, partial reconstruction TeV PeV

Importance of low background Nestor cosmic ray muons  : 105-106 x dominated by cosmic ray muons  need low misreconstruction  e: background much lower (but smaller detection volume)  scattering helps ... IceCube  Detector noise: low in inert ice (1 kHz/PMT)

Importance of good angular resolution Expected  resolution for 1 km3 detectors ...can‘t compete with -telescopes ..but for many analyses not crucial Ice size of moon water atmospheric 

Price and ease of construction moon ... use existing moon …and radio antennas Ice water KM3Net: < 200 MEUR IceCube: M$273 (US accounting) 50 M$ detector cost

Northern hemisphere detectors NESTOR Astrop. Phys. 23, 377 (2005) Baikal NT200 Antares Nestor 1100 m deep data taking since 1998 new: 3 distant strings under construction 2400 m deep completion: early 2007 1 of 12 floors deployed 4000 m deep completion: 2007?

BAIKAL NT200+ Excellent example that smart ideas can compensate small size and budget … concentrate on  induced showers data taking since 1998 3 external strings in operation since April 05 sensitivity quadrupled

Antares string based detector, 0.01 km3 instrumented volume  prototype strings 2003, March 2005  1st „final“ string mid 2005  detector completion early 2007 submarine cable 40 km ~ 40 km - 2400 m

Antares test string 2005 string based detector, 0.01 km3 instrumented volume ... detectors moving with currents….  acoustic positioning < 10 cm (2mm for fixed distance)  1st „final“ string mid 2005  detector completion early 2007

AMANDA and IceCube 0.02 km3 AMANDA 1 km3 IceCube Optical module (677) ..collaborations merged March 2005 ... 0.02 km3 AMANDA 1 km3 IceCube Optical module (677) IceTop 0 m 1996-2000 1400 m 2400 m > 70 strings > 4200 modules  1500 atmospheric ‘s /year  80000 atmospheric ‘s /year

the South-Pole laboratory South Pole Station First IceCube string 1400m 2400m IceCube Counting House 1500 m AMANDA 2000 m [not to scale]

The new station operating at least until 2035

First IceCube string ... January 2005: 60 optical modules Deepest module at 2450 m

IceCube coincident events .. IceTop – IceCube Amanda – IceCube

The testbeams atmospheric neutrinos cosmic ray muons Eμ  E-3.8 Energy spectrum with unfolding technique atmospheric neutrinos 1 GeV 1 TeV Amanda Frejus Eν  E-3.8 cosmic ray muons Eμ  E-3.8 Eprimär  E-2.7 EHadrfon  E-2.7 0.02 1 TeV 1000 TeV ... Primary energy corrected Preliminary

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: 2 orders of magnitude improvement in sensitivity

Neutrinos from unresolved sources Expect deviation at high energy (hard flux) cascades (2000 data)  (2000 data) Preliminary

Very high energies Special 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

Experimental bounds and future ..closing in on Waxman-Bahcall bound  gain factor 30 in sensitivity with 1 km3 detectors present AMANDA sensitivity --- Preliminary DUMAND test string FREJUS MACRO atmospheric -5 AMANDA limits -6 BAIKAL log [E2 · flux(E) / GeV cm-2 s-1 sr-1] -7 GZK -8 IceCube (3y) -9 2 3 4 5 6 7 8 9 10 log (E /GeV)

Search for localized sources (AMANDA) Maximum significance 3.4  compatible w. atmospheric  Preliminary quite expected ... 92% of experiments would yield even higher maximum 2000-2003 (807 days) 3329  from northern hemisphere 3438  expected from atmospheric   also search for neutrinos from unresolved sources

... measured limits and future 10-12 Macro Super-K 10-13 IMB Baksan Amanda 10-14 neutrino induced muon flux /(cm2 s) 10-15 2007 Antares+Nestor AII+IceCube 10-16 2012 KM3Net IceCube 10-17 10-18 declination (degrees)

... steady progress in sensitivity average flux upper limit [cm-2s-1] sin(d) AMANDA-B10 AMANDA-II IceCube 1/2 year * optimized for E-2, (*) E-2, 3 signal * >10 GeV 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 time Preliminary

... closing in on predictions  predictions very model dependent  ... some can be tested now .. e.g. SS-433 micro quasar: 10-5 SS-433 10-6 integrated neutrino flux /(cm2 s) [E>1 GeV] 10-7 Distefano 2002 10-8 preliminary

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! May '02 July '02 June '02 sliding search window Error bars: off-source background per 40 days

GRB n search in AMANDA Cascade channel: worse pointing but 4! Search for  candiates correlated with GRBs - background established from data : <20° PRELIMINARY Cascade channel: worse pointing but 4!  effective area  50000 m2 ()  limit assumíng WB spectrum: Eν2Φν < 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!

Green’s Function Fluence Limit (allows for comparison with SK) Further investigations ...  Search without temporal/spacial constr.: Eν2Φν < 6.7x 10-6 GeV cm-2 s-1 sr-1  detailed investigations of GRB 030329 - large model dependencies !! SuperKamiokande (1454) AMANDA sensitivity AMANDA limit Green’s Function Fluence Limit (allows for comparison with SK) Future goal: determination of limits independent of specific model PRELIMINARY

Indirect search for dark matter  neutralino is best particle physics candidate for dark matter  stable if R-parity conserved (for most parameters)  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-  Nuclear Recoil and indirect searches are complementary and not equivalent !!

WIMP search in AMANDA Limits on muon flux from Earth center AMANDA results submitted for publication Limits on muon flux from Earth center Limits on muon flux from Sun AMANDA 1y Antares 3 years 1km3 (IceCube) SK Disfavored by direct search (CDMS II) New solar system WIMP diffusion model -> more realistic neutralino velocity distribution (Lundberg&Edsjoe) Detection threshold (mu): ~50GeV (extrapolate to get limits for E>1 GeV) Cuts optimized for each mass independently

New particles 10-14 Soudan high sensitivity to rare new particles if signature unambigous .... ... (slowly) moving bright particles ... KGF MACRO Amanda 10-15 Orito upper limit (cm-2 s-1 sr-1) 10-16 Baikal e.g magnetic monopoles: Cherenkov-light  (n·g/e)2 (1.33*137/2)2  electrons 10-17 1 km3 10-18 8300 times stronger than for ! 0.50 0.75 1.00  = v/c

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.: preparation Dec.: construction Jan.: construction Feb.: commissioning 35% of money spent ...

Signatures in IceCube … 1013 eV (10 TeV) 6x1015 eV (6 PeV) Multi-PeV  +N+... ± (300 m track!)  +hadrons signature of  signature of 

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 design report 2008 construction 2009-2013? multianode PMTs with Winston cones) .... but time scale tight

Anita - quest for GZK neutrinos  surveys > 1 million km2  under construction  launch Dec 2006 refracted radio Antarctic ice neutrino

... very rare - very high energy events many proposals for radio and acoustic detectors in ice, water, salt, from moon .. Preliminary! e.g. IceCube extension: >>km attenuation length sparse instrumentation 100-fold volume increase >100 > 10 GZK neutrinos/year IceCube

RICE AGASA Amanda, Baikal 2002 2004 Glue AUGER nt Anita 2008 0.1 km3 2008 km3 satellites radio later

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

... Limits on selected sources 0.21 4.50 2 SS433 1.25 5.36 10 Crab Nebula 0.40 5.21 4 Cygnus X-1 0.77 5.04 6 Cygnus X-3 0.38 3.71 5 1ES1959+650 0.68 5.58 Markarian 421 Flux Upper Limit F90%(En>10 GeV) [10-8cm-2s-1] Expected backgr. (4 years) Nr. of n events Source Sensitivity /~2 for 200 days of “high-state” (HEGRA) Crab Nebula: MC probability for excess 64% … out of 33 Sources Systematic uncertainties under investigation selected objects → no statistically significant effect observed

Effective Area and Angular Resolution for Muons IceCube Effective Area and Angular Resolution for Muons Galactic center for a E-2 nm spectrum with quality selection and BG suppression (atm m reduction by ~106) Median angular reconstruction uncertainty ~ 0.8 further improvement expected using waveform info Energy resolution: s[log10(Em)]  20%-30%

neutrino induced muon flux /(cm2 s) 10-12 10-14 10-15 10-16 10-17 10-18 10-13 neutrino induced muon flux /(cm2 s) declination (degrees) Macro Amanda Super-K Baksan IMB 2007 2012 KM3NeT IceCube Antares+Nestor AII+IceCube GX339-4 SS-433 MK501 /~1

Sun Crab Nebula Cassiopeia. A LMC Cygnus-X1 SMC 90 000 light years Approximate AMANDA horizon 90 000 light years