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Multiwavelength Approach to Transient Neutrino Point Sources

This article discusses the use of multiwavelength observations to identify and study potential neutrino point sources. It explores the photon-neutrino link, light curve interpretation, and the potential for future multi-messenger approaches.

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Multiwavelength Approach to Transient Neutrino Point Sources

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  1. http://icecube.wisc.edu IceCube: Multiwavelength Approach to Transient Neutrino Point Source Candidates Elisa Resconi, for the IceCube coll. (Max-Planck-Institute for Nuclear Physics, Heidelberg) TeV Particle Astrophysics II 28-31 August 2006. Madison, WI

  2. l n 106 : 1 Fn (E, W) IceCube event IceCube event 1. Construction of the Neutrino Sample Elisa Resconi

  3. 2. Extraction of Astronomical Information Fn (E, W) = Fatm + Fgalactic + Fextra- galactic Cosmic ray showers in the Earth’s atmosphere: • p, K decay  E-3.7  20% uncertainty “diffuse” flux: CR interaction with interstellar gas. “point-like”: galactic sources  E-2  ? “diffuse” flux: p decay from pg interaction with 2.7oK cosmic radiation “point-like”: extra-galactic sources  E-2  ? TeV-Blazar discussed here See also at this conference: “Implications of neutrino flux limits” J. Becker for IceCube, talk “Search for a Diffuse Flux of TeV to PeV Muon Neutrinos with AMANDA-II” J. Hodges for IceCube, poster

  4. On-Source Off-Source Fgalactic(E,W), Fextra-galactic(E,W)point-like sources Ref. M. Ackermann, “The multimessenger approach ..”, Barcelona, 07.06 = 00-04 AMANDA-II preliminary: 2000-2004 (1001 live days), 4282 n from northern hemisphere No significant excess found Blind analysis strategy Variable sources ? Elisa Resconi

  5. Nr of n 1 2001 2002 2000 2003 Time Multi-wavelength approach: photon light curves used for the improvement in identify possible neutrinos emitted by astronomical sources Synthetic light curve Photon Rate (counts/sec) dFatm(t)/dt = 1 / year 3o sky-bin 1 n / day sky-bin ~ 310 -3 How can we discriminate these events ? What can we learn from photon observations?

  6. 3. Transient Point Sources • The photon-neutrino link • Access to photon data • Analysis of photon data Selection of neutrino “proxy” waveband Availability / calibration / dead-time correction ….. WHAT IS A FLARE ? Elisa Resconi

  7.  ,  γ γ synchr e,  γ synchr pγγsynchr. γ synchr. casc. (e±) γsynchr casc. (e±) γsynchr 3.1 The photon – neutrino link: HBL (LBL)  e,  Synchrotron proton blazar model (ref. A. Mücke et al, Astroparticle Phy, 18 (2003) 593-613) proton (highly magnetized environment) electron γ X LBL HBL P.Giommi et al.,A&A 445, 843-855 (2006) Elisa Resconi

  8. HBL X- AND γ-ray  emission X- ray band γ- ray band C O R R E L A T I O N Interpretation primary electron AND secondary electron (casc.) only p, if only synchrotron (no ) sporadic, no monitor, difficult to combine Data huge amount of data, monitor + high sensitivity Strategy Light curve interpretation define “flares” define periods of high activity collect all the data available, improve definition of “flare” Elisa Resconi

  9. 3.3 Photon data: WHAT IS A FLARE ? Light Curve Interpretation: • characteristic flux level(s) • impulsive events (flares) • statistical studies on the timescales of variability • correlated activities across wavebands • periods of HE neutrino emission: • Construction of an hypothesis test Maximum Likelihood Blocks applied to X- and -ray light curves [E. Resconi, L. Costamante, D. Franco, E. Flaccomio, A. Gross, icecube/200608002]

  10. All-Sky-Monitor, RXTE, 10 years X-ray monitor zoom Mkn 421 X-ray: an example All-Sky-Monitor (RXTE), Mkn 421 Elisa Resconi

  11. All-Sky-Monitor, Maximum-Likelihood-Blocks zoom Mkn 421 Elisa Resconi

  12. All-Sky-Monitor, Maximum-Likelihood-Blocks, Characteristic level zoom Mkn 421 Rchar Elisa Resconi

  13. Hypothesis test: need to be blind! •  sample determined a priori • Time periods selected a priori •  in the time periods /  atmospheric expected All-Sky-Monitor, Maximum-Likelihood-Blocks, Characteristic level zoom Mkn 421 Elevated levels or flares : ~ 15 % + 3 Rchar Characteristic level (band) Depends on: source + detector Elisa Resconi

  14. TeV -ray: preliminary • The light curves are very sporadic • Compilation of historical light curves: under construction Mkn 421, Whipple public data, Maximum Likelihood Blocks Elisa Resconi

  15. Multi-wavelength: X- vs -ray “Orphan” region Correlated corridor -rayflux “Anti-orphan” region X-rayflux, PCA (MLB blocks) Elisa Resconi

  16. Future: … transition to a ‘multi-messengers’ approach -IceCube as a ( half ) – All-Sky-Monitor in neutrino: - Filed of view: northern sky - High duty cycle • Idea: use neutrinos in order to trigger gamma-ray telescopes (see E. Bernardini, “The multimessenger approach..” Barcelona, 07.06) -Critical points under discussion: - selection of the sources: the phenomenology is limited - statistical interpretation of possible coincidences: -ray flare rate, catalogue … - blindness of the data: minimal impact with off-line analysis • Status: TEST run between AMANDA and Magic of 3 months approved. Elisa Resconi

  17. Summary • Looking in the right direction and in the right moment is a good idea! • From existing models: selection of proxy wavebands (HBL discussed) • Photon light curves under compilation • Photon light curve analysis with a global method (MLB) • Selection of periods of possible neutrino emission: • global & • non arbitrary • Next: test on the data Elisa Resconi

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