1 / 40

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

hoai
Download Presentation

Cosmic Ray Physics with the IceCube Observatory

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related