Status and prospects of the IceCube Neutrino Telescope E. Resconi, MPIfK Heidelberg for the IceCube Collaboration VLVT08, Toulon, Var, France, 22-24 April 2008

IceTop InIce AMANDA 18 strings 13 Strings 19 Strings 2007-2008: 2006-2007: 13 Strings 2005-2006: 8 Strings 2004-2005 : 1 String IceTop Air shower detetor threshold ~ 300 TeV Total: 40 strings IC22 + AMANDA Physics Run: Ended March 2008 IC40 + AMANDA Physics Run: Started April 2008 InIce 70-80 Strings , 60 Optical Modules 17 m between Modules 125 m between Strings AMANDA 19 Strings 677 Modules See B. Fox talk

The IceCube Collaboration Bartol Research Inst, Univ of Delaware, USA Pennsylvania State University, USA University of Wisconsin-Madison, USA University of Wisconsin-River Falls, USA LBNL, Berkeley, USA UC Berkeley, USA UC Irvine, USA Clark-Atlanta University, USA Univ. of Maryland, USA University of Kansas, USA Southern Univ. and A&M College, Baton Rouge, LA, USA University of Alaska – Anchorage, USA Institute for Advanced Study, Princeton, NJ, USA Chiba University, Japan EPFL Lausanne Switzerland University of Canterbury, Christchurch, New Zealand Université Libre de Bruxelles, Belgium Vrije Universiteit Brussel, Belgium Université de Mons-Hainaut, Belgium Universiteit Gent, Belgium Universität Mainz, Germany RWTH Aachen Universität, Germany Uppsala Universitet, Sweden Stockholms Universitet, Sweden University of Oxford, UK Universiteit Utrecht, Netherland DESY Zeuthen, Germany Universität Wuppertal, Germany Universität Dortmund, Germany Humboldt Universität, Germany MPIfK Heidelberg, Germany Amundsen-Scott Station, Antarctica

IceCube Structure Detector Components Detection Channels IceTop In-Ice Array AMANDA Detection Channels Muon Cascades Composite/Tau Physics Channels GRBs Diffuse Sources Point Sources Atmospheric Neutrinos WIMPs Supernova Cosmic Rays Exotic Particles Elisa Resconi

IceCube Structure Detector Components Detection Channels IceTop In-Ice Array AMANDA Detection Channels Muon Cascades Composite/Tau Physics Channels GRBs Diffuse Sources Point Sources Atmospheric Neutrinos WIMPs Supernova Cosmic Rays Exotic Particles Elisa Resconi

IceCube Structure Detector Components Detection Channels IceTop In-Ice Array AMANDA Detection Channels Muon Cascades Composite/Tau Physics Channels GRBs Diffuse Sources Point Sources Atmospheric Neutrinos WIMPs Supernova Cosmic Rays Exotic Particles Elisa Resconi

IceCube Structure Detector Components Detection Channels IceTop In-Ice Array AMANDA Detection Channels Muon Cascades Composite/Tau Physics Channels GRBs Diffuse Sources Point Sources Atmospheric Neutrinos WIMPs Supernova Cosmic Rays Exotic Particles Elisa Resconi

Muon Channel Observables Up-wards  AMANDA IceCube Arrival time ~ 5-7 nsec ~ 3 nsec Incoming direction 2° - 3° < 1° fov 2 fov 2 Estimated energy ± 0.5 order of magnitude Elisa Resconi

Muon Channel Atmospheric Neutrinos Ultimate Background: Systematics: reduce discrepancy among models - Extend the spectrum at low energies Signal: - Search for the prompt component - Testing alternative oscillation scenarious - Measurement of the energy IceCube Collaboration, astro-ph/0711.0353 Elisa Resconi

Muon Channel Diffuse Flux Multi-messenger argument Proton luminosity Upper bound HE  flux K. Mannheim, R.J. Protheroe, J. P. Rachen, Phys.Rev. D63 (2001) 023003 Cosmic Rays Neutrinos AMANDA-II 4 years IceCube 1 year MPR W&B Elisa Resconi

Muon Channel Diffuse Flux The IceCube Collaboration, arXiv:0705:1315. Elisa Resconi

Muon Channel Point Source & Sky-map: bin and un-binned method Source list Autocorrelation Time clusters Photons light curves Elisa Resconi

Detector Energy Window (TeV) Exposure Time (days) 24h 0h 15o 30o 45o 60o 75o -3 -2 -1 1 2 3 1997 1997-99 2000 2000-04 1997 2000 2004 AMANDA B10 AMANDA II Detector Energy Window (TeV) Exposure Time (days) Limit (TeV-1 cm-2 s-1) AMANDA-B10 (1997-99) ~1 – 1000 623 4.0·10-10 AMANDA-II (2000-04) 1.6 - 2600 Phys.Rev.D75:102001,2007 1001 5.5·10-11 (2005-06) 7.0·10-11

? Detector Energy Window (TeV) Exposure Time (days) 2007 2006 IceCube 9 strings IceCube 22 strings (+ AMANDA) Detector Energy Window (TeV) Exposure Time (days) Limit (L) Sensitivity (S) (TeV-1 cm-2 s-1) IC9 (2006) ~ 5 - 1000 137 1.2·10-10 (L) IC22 (2007) IC22 + AMANDA ~ 5 – 5000 ~ 0.5 - 10 240 ~10-11 (S) Only for specific scenarios IC80 ~ 5 - 5000 3 years 2·10-12 (S)

Muon Channel Point Source Multi-messenger argument Non-thermal activity Single source candidate Nr. Observed / Nr. expected Flux Upper Limit 10-7 GeV cm-2 s-1 32 sources pre-selected Active Galactic Nuclei Mkn 421 6 / 7.37 0.42 Mkn 501 8 / 6.39 0.85 1ES1959+650 5 / 4.77 0.78 3C273 8 / 4.72 1.00 M87 6 / 6.08 0.49 The IceCube coll., astro-ph/0611063 Elisa Resconi

X-ray Binary Systems SS433 4 / 6.14 0.27 LSI +61 303 5 / 4.81 0.74 Nr. Observed / Nr. expected Flux Upper Limit 10-7 GeV cm-2 s-1 32 sources pre-selected X-ray Binary Systems SS433 4 / 6.14 0.27 LSI +61 303 5 / 4.81 0.74 Cyg X-1 8 / 7.01 0.77 Cyg X-3 7 / 6.48 0.68 The IceCube coll., astro-ph/0611063 Elisa Resconi

Muon Channel Point Source Time Optimized Multi-messenger arguments Non-thermal activity Single source candidate Transient behavior Search for transient  Variability in astrophysics: an old problem a plethora of methods Elisa Resconi

Periodicity (multiwavelength) Active Galactic Nuclei Mkn 421 Mkn 501 1ES1959+650 X- and -rays 3C273 Radio and X-rays X-ray Binary Systems SS433 LSI +61 303 Cyg X-1 Cyg X-3 ….. Radio Periodicity (multiwavelength) Elisa Resconi

The hint: 1ES1959+650    Good X-g correlation X-ray: ASM, PCA    Good X-g correlation “orphan” flare: difficult to accommodate in leptonic models -ray: Whipple

Muon Channel WIMPs hep-ex/9804007

Muon Channel WIMPs Sun and Earth target Sun: signature for neutralino: low energy nearly horizontal tracks May – September period used for the Sun Analysis principles: - blindness: azimuth of the Sun blinded sequential reduction of atmospheric muons: muon group L2 Sample optimized for lower energies hypothesis test: Null Hp = no signal in the bin direction Sun

Muon Channel WIMPs T. Burgess, PhD thesis, Joakim et al. http://www.physto.se/~edsjo/darksusy)

IceCube Structure Detector Components Detection Channels IceTop In-Ice Array AMANDA Detection Channels Muon Cascades Composite/Tau Physics Channels GRBs Diffuse Sources Point Sources Atmospheric Neutrinos WIMPs Supernova Cosmic Rays Exotic Particles Elisa Resconi

Cascades Channel Observables AMANDA IceCube Arrival time ~ 5-7 nsec ~ 3 nsec Incoming direction ~ 30° fov 4 fov 4 Estimated energy 20 % 20 % Elisa Resconi

Cascade Channel Diffuse Flux IceCube Collaboration (O. Tarasova et al.) ICRC 2007 arXiv:0711.0353 [astro-ph] , pages 83-86. AMANDA 2000-2004 All the -track like are removed Energy Resolution: O(log(E))=0.18 Flux of atmospheric e <  preliminary All flavors upper limit: 90% = 3.9610-7(E/GeV) -2 (GeV sr s cm2)

Cascade Channel GRB Information from satellite: Multi-messenger arguments Example: Search for coincidences AMANDA-II / BATSE GRBs AMANDA 2000-2004 BATSE – AMANDA (Feb 13/2000- May 26/2000) Information from satellite: Start time of the burst Duration of the burst (T90) See A. Achterberg et al., ApJ 666:397, 2007 (astro-ph/0702265)

Cascade Channel GRB Strategy: AMANDA 2000-2004 Determine the detector stability using pre-burst and post-burst experimental data Selection criteria: - cascade hypothesis likelihood parameter - cascade hypothesis reconstructed cascade energy Search for statistical excess in the on-time experimental data (after unblinding) Likelihood parameter for cascade reconstruction Stability plot

Cascade Channel GRB Not mentioned in this talk: Sliding window (rolling) Single burst analysis All flavor GRBs limit from AMANDA-II

GRB, future effective area Preliminary

Future On-line Strategies IceCube Deep Core: low energy extension High Energy optimization Elisa Resconi

On-line Strategies Neutrino Trigger of Multi-wavelength Campaign Significant Neutrino Observation Elisa Resconi

Prototype-test already done! NToT 5. AMANDA – MAGIC Alerts sent Reaction within one day 27th September to 27th November 2006 ( E. Bernardini et al., astro-ph/0509396 ) Prototype-test already done! NToT (see E. Bernardini et al …) 5. Elisa Resconi

IceCube – ROTSE, optical follow-up for GRB and SN M. Kowalski, A. Mohr, astro-ph/0701618 IceCube Time Elisa Resconi

Towards Lower Energy (E < 1 TeV) G. Wikstrom 5 years 1- Indirect Dark Matter Search 2- Galactic Gamma-ray Sources 3- Atmospheric Neutrinos E. Akhmedov, M. Maltoni, A. Smirnov, hep-ph/0612285

Towards Lower Energy (E < 1 TeV) Olaf Schulz

Towards Lower Energy (E < 1 TeV) Preliminary design Towards Lower Energy (E < 1 TeV) Olaf Schulz

Towards Lower Energy (E < 1 TeV) Access the Southern Hemisphere    ACTIVE VETO Olaf Schulz

Towards Lower Energy (E < 1 TeV) Access the Southern Hemisphere G. Wikstrom 5 years Design study under going: Nr of strings 6 (or more) - 60 DOMs per string, position under study First strings for deep core next season Veto configuration able to reject 10^6 atmospheric muons Sensitivity for galactic sources, neutrino oscillation etc under way Olaf Schulz

Get better at the Highest Energies (E > 1 PeV) Preliminary design Olaf Schulz

Conclusions Past: AMANDA paved the way for IceCube Analysis structure, methods Best limits published since 1997 Present: Half of IceCube is in the ice Analysis running No significant hardware issues Future: get on-line, stretch the energy range Alert other instruments Access the lowest energies (IceCube Deep Core) Get better at higher energies