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IceCube Multi-Messenger studies & follow up programs

IceCube Multi-Messenger studies & follow up programs . Marek Kowalski and Elisa Bernadini HAP meeting 19.9.2012. The multi- messenger approach to neutrinos : Correlating neutrinos with electromag . signal to improve sensitivity for astrophysical neutrinos.

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IceCube Multi-Messenger studies & follow up programs

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  1. IceCubeMulti-Messenger studies & follow up programs Marek Kowalskiand Elisa Bernadini HAP meeting 19.9.2012

  2. The multi-messengerapproachtoneutrinos: • Correlatingneutrinoswithelectromag. signaltoimprovesensitivityforastrophysicalneutrinos

  3. Example I: AGNs andthesearchforflares • Search for flares with a high-energy neutrino telescope is • motivatedby high variability of the electromagnetic emission Gamma-ray light curve of 3C273 Fermi-Large Area Telescope Observations of the Exceptional Gamma-ray Outbursts of 3C 273 in 2009 September, Abdoet al. 2010 ApJ 714 L7 hadronic adaptedfrom C. Spiering Relevant time scaleforneutrinoemissionisunknown! leptonic adapted from

  4. Multiflareanalysisof IceCube-59 (2009-2010) data • Time-clustering algorithm combined with unbinnedmaximum likelihood method.D. Goraet. al., Astropart. Phys. (2011) • Application to selected sources and periods of interest ICRC 2011; astroph 1111.2741 No significant deviation from background

  5. Example 2: high energyneutrinosfrom Supernovae Gravitative collaps of a very massive, rotating star (>25 M): • Core-collapse Supernovae with mildly-relativistic jets inside that don’t reach the surface neutrino factory! Time scale~10 s • Emission of core-collapse SNe of type IIN only explained by shock interaction with progenitor wind significant neutrino emission. Time scale ~ weeks B~108 GeV Tdyn~1 s • Currentsearchmethods: • Individual interestingSNe, • e.g. SN2008D Abbasi et al. A&A, 2011 • StackingofnearbySNe Simulation: MacFadyen (2000) Relevant time scalesforneutrinoemissionknown

  6. Neutrino follow-up: OnlineOffline The problem: monitoringofelectromagneticskyisvery incomplete, particular in theoptical, X-rayandhardgammarays. The solution: Trigger othertelescopes on interestingneutrino signaturestoobtaindatafrom AGNs, SNe, GRBs thatwould otherwiseneverbeentaken(EB 2005, MK & Mohr 2007) Enhencementofsensitivitydepends on signal, e.g. forSNe improvementofupto a factor 3 possible.

  7. Optical (Bonn) • X-ray (Bonn) • Gamma-Ray (DESY) IceCube follow-up programs: AGN/SN/GRB IceCube

  8. Optical (Bonn) • X-ray (Bonn) • Gamma-Ray (DESY) IceCube follow-up programs: AGN/SN/GRB Bonn/DESY/Madison Iridium IceCube

  9. Optical (Bonn) • X-ray (Bonn) • Gamma-Ray (DESY) IceCube follow-up programs: Swift (X-ray) Magic & Veritas AGN/SN/GRB Bonn/DESY/Madison Optical Telescopes ROTSE & PTF Iridium IceCube

  10. Optical (Bonn) • X-ray (Bonn) • Gamma-Ray (DESY) IceCube follow-up programs: Swift (X-ray) Magic & Veritas AGN/SN/GRB Bonn/DESY/Madison Optical Telescopes ROTSE & PTF Iridium IceCube

  11. IceCube online data processing pipeline Trigger 2000 Hz Level 1 30 Hz Neutrino- Level 0.002 Hz Neutrino- Multiplets Farm for online reconstruction Latency 2009: 4-8 hours since 2010: ~5 minutes

  12. Triggeringthefollow-up Neutrino- Level 0.002 Hz Time-scaleforclustersearch: secondsto~3 weeks -1 -3 -2 Now Likelihoodbaseddoublettrigger Cluster trigger Optical follow-up: ROTSE/PTF ~ 25 few per year X-ray follow-up ~ 7 per year Gamma-ray follow-up ~ 3 per year

  13. Optical Neutrino Follow-up ROTSE telescopes ROTSE 3c Astronomy Picture ofthe Day, July 27, 2012

  14. Optical Neutrino Follow-up The Telescope Network • ROTSE (since 2008) • - 0.45 m diameter • - 3.5 deg2FoV PTF (since 2011) - 1.2 m diameter - 8 deg2FoV 27

  15. Optical Neutrino follow-up Hunting Supernovae No such Supernova observedin 2008/2009 Abbasi et al., A&A 2012

  16. Optical neutrino follow-up Supernova constraints Abbasi et al., A&A 2012 Are there GRB-like jets inside of core-collapse supernovae? GRBs Less than 4.2% of all core-collapse SNe contain a jet with Γ = 10 und Ejet = 3×1051erg SNe ?

  17. X-rayfollow-upwith SWIFT/XRT 1 day 1 hour 1 week Hunting GRB afterglows 0.4° • First observations with < 4 hours delay • Tiling needed due to small FoV of Swift • Currently: One field per orbit • Swift team implementing 7 fields per orbit

  18. Gamma-rayfollow-upwith MAGIC & Veritas • Trigger on neutrinocluster in directionofpredefinedcandidatelist • Trigger thresholdsetaccordingACT time allocation (~3 per year) MAGIC: 3.2 σ; Veritas: 3.5 σ • SensitivitytostrongestMkr 421 flare, assumingν:γ=1

  19. Correlatingtheneutrinoalertswithflaringprobability Long-term monitoring and use of historical data!! M. Tluczykont, E.B. et al., Astronomy and Astrophysics 524 A48 (2010)

  20. IceCubeisfullysubscribedto Multi-Messenger- online or offline!

  21. IceCubeisfullysubscribedto Multi-Messenger- online or offline! • Somefuturedirections & wishes: • IceCube – high energysingleeventtrigger • Gamma-rayfollow-up–moreAGN phenomenology: • light curvefeatureneutrinosignal • Optical follow-up– widefieldopticalimagerstomonitorthefullsky

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