Mariola Lesiak-Bzdak. Results of the extraterrestrial and atmospheric neutrino-induced cascade searches with IceCube

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1 Results of the extraterrestrial and atmospheric neutrino-induced cascade searches with IceCube Mariola Lesiak-Bzdak Stony Brook University for IceCube Collaboration Geographic South Pole" Outline: } Motivation } The IceCube detector Atmospheric cascade neutrino searches } Extraterrestrial cascade neutrino searches Summary } } 1 IceCube detector Amundsen-Scott " South Pole Station"

2 Cosmogenic Neutrinos Cosmic ray spectrum RHIC pp LHC } Cosmic rays lose their energy due to interactions with cosmic radiation background (CMB) } Above ev Greisen-Zatsepin- Kuzmin cut-off : p + γ CMB à Δ + à π + + n à ν µ + µ + + n E p > ev à π 0 + p à γ γ + p GZK cutoff" Greisen, Zatsepin, and Kuzmin (1966) } Neutrinos: } straight line propagation } unabsorbed } not GZK supresed } point back to their source 2

3 Searches for a Diffuse Neutrino Flux Diffuse Flux = effective sum from all (unresolved) extraterrestrial sources (e.g., AGNs) } Signal: } Extraterrestrial neutrinos from ~E -2 sources } Background: Southern sky Northern sky } Atmospheric neutrinos } Energy information used to separate signal from background GRBs 3 AGNs Atmospheric ν, µ Harder Spectrum ν (E -2 ) Energy } Sensitive to all three neutrino flavors

4 Atmospheric neutrinos Southern sky Northern sky } Conventional atm. ν flux: } Originates from decays of pions and kaons } γ~3.7 } Prompt atm. ν flux } Decay of charmed mesons } γ~2.8 } No measurement of prompt neutrinos yet } Astrophysical ν: } γ~2.0 (model) de/dn ~ E -γ 4

5 Neutrino detection principle } Neutrino interacts with nuclei in ice producing secondary particle } Secondary particle emits Cherenkov light as it travels through ice (cone ~41 ) μ N } Cherenkov light is detected by a 3D array of optical sensors (Digital Optical Modules) ν μ 5

6 IceCube detector For more see Kurt Woschnagg s talk 6 9 strings 22 strings 40 strings 59 strings 79 strings 86 strings (2006) (2007) (2008) (2009) (2010) (2011)

7 Neutrino event signatures ν e Nè cascade 7 ν μ N è μx IC79 data ν τ N è τ cascade 1 è cascade 2 cascade 1 Color coding: red earliest blue - latest Tracks with length ~1km ν µ + N µ + X angular resolution <1 o energy resolution <0.2 log(e) used for point source searches and diffuse flux searches Cascades e-m and hadronic cascades ν e(τ) + N e(τ) + X ν l + N ν l + X l = e, µ,τ energy resolution 0.1 log(e) used for diffuse flux searches Composites starting tracks τ double bangs good directional and energy resolution N - target nucleon X - hadronic shower ν e(τ) (CC) ν l (NC)

8 } Signal: 8 IC79 Atmospheric Cascades with DeepCore } Atmospheric (ν e +ν μ ) NC and ν e CC } Background: } Atmospheric μ andν μ CC } 281 days of IC79-string data } Analysis strategy: } IceCube strings used as a Veto } Demand spherical light distribution pattern and reconstruct its vertex } Reconstructed vertex to be contained inside the fiducial volume } Combination of cut variables in Boosted Decision Tree More on physics with DeepCore - see slides by T. DeYoung

9 Atmospheric Cascades with DeepCore } Found 1029 events in 281 days of IC79 data } Observed number of cascade signal events: 496 ± 66(stat) ± 88(syst) where observed number of ν e induced cascades is: 240 ± 66(stat) ± 109(syst) IceCube Coll will add arxiv link when available } Energy range between 80 GeV and 6 TeV First observation of atmospheric neutrino-induced cascades in Deep Core 9

10 IC79 Atmospheric cascades IC79 Deep Core ν e } The atmospheric ν e flux in energy range between 80 GeV and 6 TeV consistent with current models of atmospehric neutrino flux Prompt ν from decay of charm not yet measured 10

11 IceCube Diffuse Neutrino-Induced searches } Look for neutrino events at high energy, above the rapidly falling atmospheric neutrino spectrum } Cascade events (CC ν e and ν τ, NC ν µ,τ,e ) contained showers } IC22 (25% of IceCube final size): } No excess of events observed } Energy range 24 TeV < E < 6.6 PeV } Published: PRD84 (2011) } IC40 (46% of IceCube final size): Brightest hit from 134 TeV ~10,000 p.e. s } 332 days of IC40-string data } Results shown here 11

12 } Method: IC40 Diffuse ν-induced Cascades Search } combination of cut variables in Boosted Decision Tree } Two branches: } Low energy (>1.8 TeV) sample aimed at detection of atm. neutrinos, high background contamination } High energy (>100 TeV) sample aimed at detection of astrophysical neutrinos } Energy used to separate atmospheric and extraterrestrial ν Atmospheric ν, µ Harder Spectrum ν (E -2 ) Energy BDT vs reconstructed energy for combined samples before final cut on BDT 90% Low energy sample High energy sample 12

13 IC40 Diffuse ν-induced Cascades Results, Low Energy Sample } Observed 67 events with 2.8σexcess over atm. μ considering statistical background uncertainty Background contributions Total Number of Events in 332 days Atm. μ 41.1 Atm. Conventional ν Atm. Conventional + Prompt ν GeV s -1 cm -2 sr -1 E Observed (90%) 67

14 IC40 Diffuse ν-induced Cascades Results, High Energy Sample Background contributions Atm. μ 0/0.36 Atm. Conventional ν 0.03 Total Number of Events in 332 days } Found 3 events in a final sample (after all cuts) in a total livetime of 332 days } 1.3σ excess over atm. μ considering statistical background uncertainty } 2.75σ excess over atm. μ based on a background estimate from extrapolation } Systematic studies ongoing Atm. Conventional + Prompt ν GeV s -1 cm -2 sr -1 E Observed (90%) 3 14

15 IC79+IC86 EHE extraterrestrial neutrinos } Search for Extremely High Energy events (energy >10 9 GeV) } Sensitive to all ν flavors } Combine data from IC79-string and IC86-string (very similar detector configurations) } Effective lifetime of days: } IC-79: 5/2010 5/2011 (319.07days) } IC-86: 5/2011 5/2012 (353.67days) Strings not present in IC79 configuration 15

16 IC79+IC86 Event Selection } Selection of events based on deposited energy and direction } Deposited energy (Cherenkov photons) } Number of recorded photoelectrons } Number of triggered DOMs (>300) } Straight line fit to the hit pattern (à Zenith angle) downgoing upgoing cos(zenith) Background MC log 10 (NPE) 16

17 IC79+IC86 Passing Events } Two events in days pass all selection criteria } Expected number of events and significance not including systematic uncertainties: } events from atm. μand conventional νbackground (2.9 σ) } events from atm. μand conventional and prompt νbackground (2.2 σ) } Cascade-like events: } Expected from CC and NC events First observation of high energy (~PeV) neutrino-induced cascades in IceCube 17

18 IC79+IC86 Expected Number of Events } Two events in days pass all selection criteria Background contributions Atm. μ Atm. Conventional μ Background events Total Number of Background Events in days Coincidence μ Total Total with prompt Cosmogenic ν Signal Models Event All Rates E ν 100 PeV Yoshida et al Kotera et al. (FRII) Ahlers et al. (maximal) Signal events Ahlers et al. (best fit) IceCube data 2 0 First observation of high energy (~PeV) neutrino-induced cascades in IceCube 18

19 IC79+IC86 Events NPE and Energy } Preliminary reconstructed energy estimated at 1.1 PeV and 1.3 PeV with 35% including stat. uncertainty and syst. uncertainties associated with the ice properties and the absolute DOM sensitivity 19

20 Cascade Position and Energy Reconstruction 20

21 Preliminary IceCube sensitivity WB bound } Preliminary IceCube sensitivity to all flavor neutrino flux by the ultra-high energy neutrino analysis with an effective lifetime of days (red). The systematic errors are not included 21

22 Summary } For the first time atmospheric neutrino-induced cascades observed with Deep Core in energy range 80 GeV - 6 TeV } Diffuse cascade searches: } IC40 low energy sample: observed 67 events (2.8σ) (E>1.8 TeV) } IC40 high energy: observed 3 events (2.75σ) (E>100 TeV) } EHE search with IC79+IC86: } 2 events observed over an expected background of (with prompt 0.190) events (2.9 σ and 2.2 σ, respectively) } Cascade-like events (any flavour, CC/NC interaction inside the detector) with energy estimates of 1.1 and 1.3 PeV } More physics topics with IceCube see talks by T. DeYoung and K. Woschnagg 22

23 Canada University of Alberta US Bartol Research Institute, Delaware Pennsylvania State University University of California - Berkeley University of California - Irvine Clark-Atlanta University University of Maryland University of Wisconsin - Madison University of Wisconsin - River Falls Lawrence Berkeley National Lab. University of Kansas Southern University, Baton Rouge University of Alaska, Anchorage University of Alabama, Tuscaloosa Georgia Tech Ohio State University Stony Brook University IceCube Collaboration Sweden Uppsala Universitet Stockholms Universitet UK Oxford University Germany Universität Mainz DESY-Zeuthen Universität Dortmund Universität Wuppertal Humboldt-Universität zu Berlin MPI Heidelberg RWTH Aachen Universität Bonn Ruhr-Universität Bochum Belgium Université Libre de Bruxelles Vrije Universiteit Brussel Universiteit Gent Université de Mons-Hainaut Switzerland EPFL, Lausanne 36 institutions, ~250 members Japan Chiba University 23 ANTARCTICA! Amundsen-Scott Station! New Zealand University of Canterbury

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