A. Karle UW Madison 1

2 Why neutrino astronomy? Astrophysical Accelerators Neutrinos allow for observation of ‘hidden regions’ of cosmic accelerators (BH, pulsars, initial epochs of SN explosions). The penetrating power of νs is important also for moderately opaque sources from which we may be seeing ϒ spectra that are significantly distorted DM annihilation CasA Supernova Remnant in X-rays  Accretion disk with jets

A. Karle UW Madison 3 Drilling experience AMANDA drilling (1950m) 90 hrs IceCube drilling (2450m) 35 hrs Thermal power: 5MW

NSF, Aug 7, 2007Tom Gaisser, IceCube Status4 Detector reliability Very good survival rate during installation. 98.5% of all deployed sensors are commissioned and being used in the first science run. In 1000 DOM years of accumulated live time only 2 sensors failed after commissioning. –Estimated survival rate after 15 years: % –Estimate based on the assumption of a constant failure rate.

A. Karle UW Madison 5 IceCube Laboratory and Data Center n Commissioned for operation in January n 3 Winter-over scientists operate and maintain instrument during winter n Only two winter-overs planned for 2008 n 17 racks of electronics n Power: 60 kW total for full IceCube

NSF, Aug 7, 2007Tom Gaisser, IceCube Status6 IceCube 22: 2007 operation since “physics” start May 23, run until July 30, run –95.9% uptime –Trigger In-ice: > 7 hits in 5  s IceTop > 5 hits in 2  s –Typical rates: in i3+AMANDA(twr) mode: 610 Hz In i3-only: 525 Hz Since start of I3 physics filtering (July 7 - now): –99.4% uptime (special ops –like CV flashing- while running at least partial I3 detector) Data –200 GBytes/day raw data written to disk –25 GBytes/day filtered and sent north via satellite –Monitoring files posted daily at

NSF, Aug 7, 2007Tom Gaisser, IceCube Status7 List of deployed filters (31/07/07) Name in FilterMaskPrescale (1/N)Summary of event selection IceCubeMuonFilter1 (Linefit.theta >= 70.0 and NChannelInIce >=10) OR (Linefit.theta >= 60.0 and NChannelInIce >=40) CascadeFilter1 TensorOfInertia.evalratio>.109 and Linefit.velocity<.25 (all based on LCSpan 1) EHEFilter1NChannelInIce >= 80 MoonFilter1No events currently selected (moon down) LowEnergyContainedFilter1 Linefit.velocity (0.1,0.5) & NChannelInIce < 16 & Many Others (see proposal) IceTopSMT5Any event with an IceTop SMT trigger present IceTopSMT_Large1Any event with NChannelIceTop >= 16 IceTopSMT_InIceCoincidence1 Any event with BOTH InIce SMT and IceTop SMT triggers present InIceSMT_IceTopCoincidence5 Any event with an InIce SMT and any IceTop station hit FilterMinBias200Any event seen in the JEB.

NSF, Aug 7, 2007Tom Gaisser, IceCube Status8 Offline Data Flow From Pole to North by satellite Physics analysis Decompressed Calibrated Refiltered

9 IceTop InIce Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV Goal of 80 strings of 60 optical modules each 17 m between modules 125 m string separation : 1 string : 8 strings AMANDA-II 19 strings 677 modules : 13 strings deployed IceCube Current configuration - 22 strings - 52 surface tanks Completion by /08: add 14 to 18 strings and tank stations 1450m 2450m AMANDA now operating as part of IceCube

NSF, Aug 7, 2007Tom Gaisser, IceCube Status10 IC22 Events Downward cosmic-ray event (“muon bundle”) Upward candidate event ( Red hits = early; yellow/green/blue = later ) IceCube DOM locations blue, AMANDA OM locations red

11 Azimuth distributions: IC9 and IC22 Downgoing muons. Azimuth distribution illustrates detector response. At lower energies one can see azimuthal structure due to detector geometry. Rate for 22 strings ~4 times higher

12 IC22 - Online zenith distribution Zenith distribution is compared to simulations. (Crosses: data, line: MC, normalized) Events with zenith angle > 80° pass online filter and are sent to North. (There are numerous other filter streams, eg. Nu_e and nu-tau, GRB, WIMPs, …) Cos(zenith)

NSF, Aug 7, 2007Tom Gaisser, IceCube Status13 IceTop – 2 tanks per station Preliminary energy spectrum with 2006 data

NSF, Aug 7, 2007Tom Gaisser, IceCube Status14 Reconstruction of big, coincident event: E ~ 0.5 EeV by IceTop 0.5 EeV  ~2000  at 2.5 km

NSF, Aug 7, 2007Tom Gaisser, IceCube Status15 Cosmic-ray physics with IceCube Measure spectrum/composition – from 1 EeV –IceTop alone –In-Ice alone (muon bundles) –Hybrid, coincident events Calibration with IceTop tagged events Measure physics background –Muons and muon bundles

NSF, Aug 7, 2007Tom Gaisser, IceCube Status16 Atmospheric with IceCube-9 Note severe cuts needed to reject background with only 9 strings. Situation will improve as detector grows Phys. Rev. D (to be published) arXiv:

NSF, Aug 7, 2007Tom Gaisser, IceCube Status17 Growth of detector AMANDA ANTARES +IC9 +IC IC22 Full IceCube 2011  Km3Net

NSF, Aug 7, 2007Tom Gaisser, IceCube Status18 IC 9 in 2006 Point source catalog Many involve jets  IC-9 point source search reported at ICRC2007

NSF, Aug 7, 2007Tom Gaisser, IceCube Status19 Point source search, example: MILAGRO MGRO in Cygnus Note: small signal with signal/background ~1 Photon flux: data & model fits to MGRO J

NSF, Aug 7, 2007Tom Gaisser, IceCube Status20 IceCube Sensitivity IC9 sensitivity ~10 -7 GeV -1 cm -2 s -1 ( E GeV ) -2 –~2 orders of magnitude above predicted signal from MGRO J –Cuts remove large fraction of signal (90% for atmospheric spectrum, less for harder spectrum) Sensitivity grows faster than detector size –For example, IC22 sensitivity is 4-5 times IC9 while size ratio is 2.5 –Angular resolution improves with longer tracks

NSF, Aug 7, 2007Tom Gaisser, IceCube Status21 Expectations for point source search with IceCube Expected signals small – < few events per year –Background of atmospheric in search bin comparable to expected signal –Optimize search techniques Unbinned searches Sensitivity to expected hard spectrum Source stacking Multi-messenger approach: –Use correlation with physically related variability in multi-wavelength  data –Examples: flaring AGNs; GRB

NSF, Aug 7, 2007Tom Gaisser, IceCube Status22 Multi-messenger/multi-wavelength Coordination with MAGIC, VERITAS, HESS… Two IceCube talks this week at Optical follow-up scheme proposed –Like ROTSE to look for GRB afterglow or SN light curve or choked GRB –Trigger on 2 or more in time/direction window Two guest investigator proposals to GLAST

NSF, Aug 7, 2007Tom Gaisser, IceCube Status23 Search for neutrinos from GRB Cascade (Trig & Roll) Cascade (Rolling)  search All flavor limits by AMANDA GRB models Waxman-Bahcall PRL 78 (1997) 2292 Murase-Nagataki A PRD 73 (2006) Supranova, Razzaque et al. PRL 90 (2003) Choked bursts Meszaros-Waxman PRL 87 (2001) Limits on neutrinos from GRB from AMANDA: -from cascades ( e,  ), Ap.J. 664 (2007) 397 -from neutrino-induced muons, Ap.J (to be published)

NSF, Aug 7, 2007Tom Gaisser, IceCube Status24 Prospects for detecting GRB ’s with IceCube AMANDA limits –Already disfavor some models –Sensitivity close to classic Waxman-Bahcall fireball prediction (expected ~ 1 in 400 GRBs) IceCube sensitivity ~20 times AMANDA –200 GRB / yr expected from GLAST –Expect 3  detection of Waxman-Bahcall level in 70 GRB with full IceCube –Non-observation would indicate GRB jets are pure Poynting flux (Blandford) rather than baryon loaded plasma (Piran, Meszaros, …)

NSF, Aug 7, 2007Tom Gaisser, IceCube Status25 Cascades—a way to avoid background of atmospheric  M.Kowalski [astro-ph/ Atmospheric -induced cascade events: - 9-strings: 10 events / year - 22-strings: 30 events / year Prompt -induced cascades from charm - 15 events/year with 22 string-array Diffuse extraterrestrial neutrino flux (expected from AGNs or GRBs) - With 22 strings Waxman-Bahcall rate (with source evolution) E 2  <5x10 -8 GeV -1 sr -1 s -1 may be detectable

NSF, Aug 7, 2007Tom Gaisser, IceCube Status26 Take advantage of -oscillations: use the  channel No atmospheric background But rare, ~1 event / yr in full IceCube

27 AMANDA+IC22: Improves low-energy capability for point source search including from WIMP annihilation in Sun AMANDA+IC22 AMANDA Angular Resolution Effective Area AMANDA gives to IceCube more area at lower energy from ~ 100 GeV IceCube gives to AMANDA a better angular resolution up to ~ 50 TeV Optimization scheme in order to fight atmospheric neutrinos (dominant at this energy): - Search for from dark matter - X-ray Binary: energy spectrum and time characteristic - Pulsar Wind Nebulae: energy spectrum - SNr near Molecular Clouds: stacking AMANDA+IC22 IC22 preliminary

NSF, Aug 7, 2007Tom Gaisser, IceCube Status28 AMANDA/IceCube as MeV detector …first proposed by Halzen, Jacobsen & Zas, astro-ph/  PMT noise low (~ 300 Hz)  ice uniformly illuminated  detect correlated rate increase on top of PMT noise

NSF, Aug 7, 2007Tom Gaisser, IceCube Status29 Supernova watch with IceCube IceCube SN DAQ –Now running with 1300 DOMs –Total noise rate shown  Connection to SNEWS –Planned for 07/08 season –Depends on good monitoring Sensitivity –Example shows SN at gal. cntr.  –Good probability of detection out to LMC

IceCube deployment AMANDA IceCube string and IceTop station deployed 12/05 – 01/06 IceTop station only DOMs deployed to date ONLY 3 ? FAILED SO FAR 3 more seasons planned Crucial planning period during the next 4 – 6 months IceCube string and IceTop station deployed 01/05 IceCube string and IceTop station deployed 12/06 – 01/ IceTop station only in 06 / Deployed in 07 / / / / / 08

NSF, Aug 7, 2007Tom Gaisser, IceCube Status31 Extras

NSF, Aug 7, 2007Tom Gaisser, IceCube Status32 Detector operation (Snapshot as of 31-07/07) PnF Physics Filter Rates FilterHzFilterHz CascadeFilter EHEFilter FilterMinBias IceCubeMuonFilter IceTopSMT IceTopSMT_InIceCoincidence IceTopSMT_Large InIceSMT_IceTopCoincidence JAMSMuonFilter0LowEnergyContainedFilter MoonFilter (*)0MuonFilter Latest Status from Experiment Control *Moon data is taken only when it is > 15 degrees above horizon

NSF, Aug 7, 2007Tom Gaisser, IceCube Status33 Properties of coincident events

NSF, Aug 7, 2007Tom Gaisser, IceCube Status34 Compare AMANDA-IC9

NSF, Aug 7, 2007Tom Gaisser, IceCube Status35 Point source search with IC9 IC9 Neutrino effective area (Dumm, Finley & Montaruli, ICRC2007)

NSF, Aug 7, 2007Tom Gaisser, IceCube Status36 Growth of detector volume

37 Photon data: light curves combination Elisa Resconi M. Tluczykont, M. Shayduk, O. Kalekin, E. Bernardini

38 What do we gain?  Analysis cuts re-optimized using the blocks distribution  For the moment NO energy spectrum optimization (to be come soon)  How does it look like the Detection Probability ?? Preliminary

NSF, Aug 7, 2007Tom Gaisser, IceCube Status39 Optical follow-up Teresa Montaruli for Multi-wavelength conference, Adler Planetarium, Aug 9

NSF, Aug 7, 2007Tom Gaisser, IceCube Status40 Take advantage of -oscillations: use the  channel No atmospheric background Assume diffuse flux at AMANDA limit – 3 x Waxman-Bahcall limit –A total of ~0.48 events per year is expected for all tau signature in IC-22 Lollipops: ~0.16 events per year Inverted Lollipops: ~0.19 per year Double Bangs: ~0.13 per year

July 22, 2007Tom Gaisser41 All strings with 60 DOMs on

July 22, 2007Tom Gaisser42 Local coincidence count rates versus depth (std. occupancy plot) Note that rates are lower in this standard occupancy plot -- Note: SMT >= 8 per string is required

Future high- energy extensions ?

Low energy core ? AMANDA has no veto coverage from top, (which is where the muons come from) Ice below 2100m is exceptionally clear, significantly better even than current ice model. A. Karle