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Cosmic Ray Physics with the IceCube Observatory

Cosmic Ray Physics with the IceCube Observatory. Hermann Kolanoski Humboldt- Universit ä t zu Berlin and DESY for the IceCube Collaboration. IceCube Detector. Detector Completion Dec 2010. CR Analyses air showers in IceTop muon (bundle)s in IceCube atm. neutrinos in IceCube

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Cosmic Ray Physics with the IceCube Observatory

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  1. Cosmic Ray Physics with the IceCube Observatory Hermann Kolanoski Humboldt-Universitätzu Berlin and DESY for the IceCube Collaboration H.Kolanoski - Cosmic Ray Physics with IceCube

  2. IceCube Detector Detector Completion Dec 2010 • CR Analyses • air showers in IceTop • muon (bundle)s in IceCube • atm. neutrinos in IceCube • IceCube - IceTopcoinc. IceCubewithIceTopisa 3-dim Air ShowerDetector unprecedented volume H.Kolanoski - Cosmic Ray Physics with IceCube

  3. Threshold energy ≈ 100 TeV (with infill) Maximum energy (Limited by km2size) Coincident events A= 0.3 km2sr Emax≈ EeV IceTop only ( < 60o) A= 3 km2sr Emax = 3 EeV Muons in IceCube 10 TeV < Eprim < 10 EeV Energy range of IceCube/IceTop (IceTop EAS) < PeV > EeV (in-ice µ,ν) Anchor to direct measurement of composition ~300 TeV Look for transition to extra-galactic < EeV H.Kolanoski - Cosmic Ray Physics with IceCube

  4. Outline • IceCube and IceTop • Cosmic ray spectrum • Primary composition from different measurements • PeV-Gamma Rays • Scalerrates: heliospheric physics, GRB, … • Atmospheric muons (and neutrinos) in-ice • muonspectrum and composition • high-pTmuons • CR Anisotropy at PeV energies (IceTop) H.Kolanoski - Cosmic Ray Physics with IceCube

  5. Final IceTop Detector Array 2011 In-fill ~125 m final detector: 81 stations (162 tanks) mostly ~ 125 m; In-fill array: 3 inserts +5 closest stations H.Kolanoski - Cosmic Ray Physics with IceCube

  6. IceTop Signal Recording leading edge voltage charge [PE] 3.3 ns; 128 bins  420 ns baseline DOMs time [ns] Calibration: Vertical Equivalent Muons 1 VEM ≈ 125 PE signal distribution in untriggeredcalibration runs muon signal e.m. background  snow height on tanks H.Kolanoski - Cosmic Ray Physics with IceCube

  7. Trigger and Data Selection Single DOM above threshold (~0.2 VEM):  digitization of waveform (3.3 ns bins) Local Coincidence (‘HLC hits’): both tanks above threshold  readout of full waveform to IceCube Lab Soft Local Coincidence (‘SLC hits’): all DOMs above threshold send a timestamp and integrated charge  catch single muons Single tank trigger for calibration with single muons Reconstruction: standard ( 3 stations)   0.3 PeV infill extension:   100 TeV Select extended air showers: H.Kolanoski - Cosmic Ray Physics with IceCube

  8. Shower Size Spectrum with IT73 • IT73 (90% of final) • cos𝛉 > 0.8 • A = 52×104 m2 • >3 stations IT73 data (preliminary) 1000 events per bin per year 100 10 (log10S125 = 0.05) IT73 simulation Work in progress roughly PeV VEM H.Kolanoski - Cosmic Ray Physics with IceCube

  9. Effective Area IT73/IC79 configuration, >3 stations , cos𝛉>=0.8, A=0.52 km2 IceTop only IC-IT coinc. H.Kolanoski - Cosmic Ray Physics with IceCube

  10. Cosmic Ray Spectrum work on systematics in progress IceTop IT73 only: >5 stations cos𝛉>=0.8, A=52.1×104 m2 ‘flattening’, also observed in IT26, Kascade-G. H.Kolanoski - Cosmic Ray Physics with IceCube

  11. CR Spectrum with IT26 arXiv 1202.3039, submitted to ApP preliminary H.Kolanoski - Cosmic Ray Physics with IceCube

  12. CR Spectrum: Comparison with other Experiments H.Kolanoski - Cosmic Ray Physics with IceCube

  13. Cosmic Rays: spectrumandcomposition IceCube/IceTop's Strength electro-mag. particles: MeV’s shower axis LE Muons GeV’s IceTop HE Muons TeV’s m IceCube EM H.Kolanoski - Cosmic Ray Physics with IceCube

  14. In-ice Composition Sensitive Variables I IC/IT40 Composition Analysis S125: shower size at the surface K70: size of muon bundle in-ice Pure Iron In-ice Pure proton IceTop Neural Network output H.Kolanoski - Cosmic Ray Physics with IceCube

  15. First Attempt for Composition (IC40) IC/IT40 Composition Analysis: Results Submitted to Astrop. Phys. Preliminary Preliminary Preliminary ~ 1month of IC40 subarray (with little snow) energy from 1 to 30 PeV (only) systematics dominated major progress expected for the next analyses with larger detector separation power (expected to improve) H.Kolanoski - Cosmic Ray Physics with IceCube

  16. In-ice Composition Sensitive Variables II IT73/IC79 Composition Analysis Exploit additional mass sensitive observables Muon stochastic loss Avg. muon energy loss In-ice • for same deposited energy: • more stochastic loss • more HE muons • lighter elements IceTop H.Kolanoski - Cosmic Ray Physics with IceCube

  17. Supporting Composition Measurements Zenith angle dependence of shower size Muon counting in air shower data Iron assumption preliminary 1 VEM charge enhanced if signalem  signalmuon preliminary Proton assumption Surface muon content simulation IT26 spectrum analysis 1-100 PeV- arXiv:1202.3039 H.Kolanoski - Cosmic Ray Physics with IceCube

  18. PeV Gamma with InIce Veto against muons IceTop shower with no activity in IceCube HI column densities preliminary upper limit E = 1.2 – 6.0 PeV (90% c.l.) • sensitivity for E = 1 PeV (90% c.l.) --- sensitivity E = 1 – 10 PeV (90% c.l.) H.Kolanoski - Cosmic Ray Physics with IceCube

  19. PeV Gamma: Point source sensitivity IceCube 5 year sensitivity to point sources lowest declination reached by the Galactic plane TeV-sources extrapolated to 1PeV without cut-off preliminary H.Kolanoski - Cosmic Ray Physics with IceCube

  20. Low energy transient rate variations from Sun, SN, GRB, ... Sun flare observation Dec 13, 2006: [ApJ Lett 689 (2008) L65] Galactic CR Spectrum • GOES • spacecraft Since than: IceTop increased spectral sensitivity taking differential rates at multiple thresholds rate increase at 2 different thresholds GRB sensitivity: Large events but unmonitored part of the sky H.Kolanoski - Cosmic Ray Physics with IceCube

  21. May 17, 2012 – GLE 71 SPE1 Observations SPE2 SPE3 MPE IceTop Rates plotted here are averages of the four groups shown above. preliminary • ~1% enhancement in SPE1 & SPE2 • Tiny enhancements in SPE3/MPE • Unusual slow decay or second phase H.Kolanoski - Cosmic Ray Physics with IceCube

  22. Cosmic rays in IceCube (deep ice) H.Kolanoski - Cosmic Ray Physics with IceCube

  23. High Energy Muons in the Deep Ice enlarged energy range witout coincidence single HE muon muon bundle Muon Multiplicity 10 TeV  10 EeV Nµ~A0.23 E0.77 Q3.5 dN/dQ Q ~ Nµ Test composition models H.Kolanoski - Cosmic Ray Physics with IceCube

  24. Spectra from Muon Bundles preliminary preliminary preliminary room for prompt muons from charm? H.Kolanoski - Cosmic Ray Physics with IceCube

  25. Comparison to Poly-Gonato Model Poly-Gonato (+G-H3a extra-galactic) E1.7-weighted room for prompt muons? total (polygonato + extragal.) no efficiency correction included heavier than iron (extrapolated from low energies) extragalactic H.Kolanoski - Cosmic Ray Physics with IceCube

  26. Atmospheric nm at high energies remaining background for comic neutrinos H.Kolanoski - Cosmic Ray Physics with IceCube

  27. Cosmic Rays: High-pTmuons High-pT muons modeled by QCD simulation (π, K, c, …) O(10 m) preliminary bundle > 135 m LS muon exponential preliminary power law pQCD H.Kolanoski - Cosmic Ray Physics with IceCube

  28. High-pTMuons: Zenith Angle Distribution d > 135 m strong disagreement for QGSJET & Sybill MC=data • Zenith angle dependences: • π, K interaction vs. decay competition • prompt: no dependence •  larger K/π ratio and/or more prompt? QGSJET π DPMJET K c H.Kolanoski - Cosmic Ray Physics with IceCube

  29. Cosmic Ray Anisotropy Large Scale ─ Compared to Northern Sky the orientation of the dipole moment does not correspond to the relative motion in the Galaxy (Compton-Getting effect) diffusive transport from nearby sources? observed small scale (10°) structures  few pc distance in-ice only H.Kolanoski - Cosmic Ray Physics with IceCube

  30. Cosmic Ray Anisotropy Measurements with IceCube and IceTop IceTop Air showers in IceTop : in principle much better energy resolution, binning limited by statistics potential of including composition sensitivity • CR Rate ~ 10 Hz in IT81 (E > 100 TeV) • ~3 x 108events / year • Sensitive to  > 10-4anisotropy IceCube Muons in IceCube: lower energy; larger zenith range; higher sensitivities small scale structures • CR Rate ~ 2 kHz in IC86 (E > 10 TeV) • ~6 x 1010 CR events / year • Sensitive to  > 10-5 anisotropy H.Kolanoski - Cosmic Ray Physics with IceCube

  31. IC59 - 20 TeV IC59 - 400 TeV IT73 - High energy (~2 PeV), preliminary Energy Dependence of CR Anisotropy preliminary (IT73) • Anisotropy changes in position, size • Above 400 TeV there’s indication of an increase in strength. H.Kolanoski - Cosmic Ray Physics with IceCube

  32. Summary IceCube/IceTop is a unique 3-dim Air Shower Detector Results: • Cosmic Ray energy spectrum (‚flattening‘ at ~ 23 PeV) • CR composition (first coinc. results, different methods  model test), PeV γ rays • connecting direct measurements with dominantly extra-galactic CR • physics of airshowers: high-pT muons, composition, K/π, charm, … • transient events: heliospheric physics, GRB, … • CR anisotropy in PeV range, likely increase with energy H.Kolanoski - Cosmic Ray Physics with IceCube

  33. H.Kolanoski - Cosmic Ray Physics with IceCube

  34. Backup Slides H.Kolanoski - Cosmic Ray Physics with IceCube

  35. Energy Resolution

  36. Snow Corrections Feb. 2012 Events selected by core location Snow corrected (in shower reco) H.Kolanoski - Cosmic Ray Physics with IceCube

  37. CR Spectrum: Comparison with IT26 and IT40 H.Kolanoski - Cosmic Ray Physics with IceCube

  38. e/m N observation first interaction μ X / g cm-2 earlier more N e/m earlier μ X / g cm-2 StrategiesofCompositionAnalyses • IceTop & InIce • IceTop EM vsInIceMUON • IceTop • - zenith angle ofe.m. • - curv. ofshower front • - GeV-muonsin IceTop: • IceTop & Radio (future?) • - shower max. Xmax proton heavier nucleus Complementarymethods  reducemodeldependency ~ 680 gcm-2 H.Kolanoski - Cosmic Ray Physics with IceCube

  39. Big Coincident Event H.Kolanoski - Cosmic Ray Physics with IceCube

  40. CR Spectrum: Comparison with other Experiments H.Kolanoski - Cosmic Ray Physics with IceCube

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