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CPPM : M. Ageron, I. Al Samarai, V. Bertin, J. Brunner, J. Busto, D. Dornic, S. Escoffier

CPPM : M. Ageron, I. Al Samarai, V. Bertin, J. Brunner, J. Busto, D. Dornic, S. Escoffier IRFU : B. Vallage LAM : S. Basa, B. Gendre, A. Mazure TAROT : M. Boer, A. Le Van Suu (OHP), A. Klotz (CESR). Scientific motivations. Detection of transient sources such as: Gamma Ray Bursts

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CPPM : M. Ageron, I. Al Samarai, V. Bertin, J. Brunner, J. Busto, D. Dornic, S. Escoffier

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  1. CPPM: M. Ageron, I. Al Samarai, V. Bertin, J. Brunner, J. Busto, D. Dornic, S. Escoffier IRFU: B. Vallage LAM: S. Basa, B. Gendre, A. Mazure TAROT: M. Boer, A. Le Van Suu (OHP), A. Klotz (CESR)

  2. Scientific motivations Detection of transient sources such as: • Gamma Ray Bursts • Core Collapse Sne • AGNs • Microquasars • … • Observed in many wavelengths (X, visible…) • Potential neutrino emitters • So far, only 1 detection of extrasolar neutrinos : SN1987A Microquasar luminosity vs time

  3. Scientific motivations Some of the most interesting: GRBs: • Highly energetic gamma bursts (~1051 ergs) • Observed at a rate <1 per day with gamma satellites • Other detections are triggered by a satellite alert (Optical telescopes, neutrino telescopes…) • Failed GRBs: • Not visible in gamma but potentially neutrino emitters • How to trigger a detection for such objects?

  4. The GRBs/SNe Connection • Rate of local GRBs << SN rate

  5. The GRBs/SNe Connection • Rate of local GRBs << SN rate • Core Collapse SNe : jets with different velocities: • Highly relativistic GRBs () • Mildly relativistic  « Failed GRBs » (few%) (hidden in gamma)

  6. Expected neutrino flux from a FGRB in ANTARES In « failed GRBs »: • No gamma counterpart • Still, protons are accelerated • p-p interaction Mesons • Mesons decay into neutrinos Ando & Beacom (PRL 95,061103(2005)) Razzaques, Meszaros,waxman (PRL 93,181101(2004)) (PRL 94, 109903(2005))

  7. Expected neutrino flux from a FGRB in ANTARES In « failed GRBs »: • No gamma counterpart • Still, protons are accelerated • p-p interaction Mesons • Mesons decay into neutrinos Antares threshold Ando & Beacom (PRL 95,061103(2005)) Razzaques, Meszaros,Waxman (PRL 93,181101(2004)) (PRL 94, 109903(2005))

  8. For 1 SNe • The Multiplet trigger can push the horizon of detection further than the HE event trigger does • For the Multiplet • (>= 2 neutrinos) trigger: • Horizon at 10 Mpc When applying HE event conditions, • For 1 HE neutrino: Horizon at 1 Mpc LE events HE events

  9. Idea: Optical detection of transient sources triggered by ”special” neutrino events. • Main advantage: covers the full hemisphere • TAROT Sud (Chili) • FOV :2° x 2° • Fast repositioning (10s) • Good sensitivity (V<19) ANTARES: 900 PMTs

  10. Triggers: Multiplet of neutrinos Single HE neutrino Alert Keys of success: 1. High performance of the online reconstruction 2. Good event selection Upward-going event GCN alert On-line reconstruction • TAROT Sud (Chili) • FOV :2° x 2° • Fast repositioning (10s) • Good sensitivity (V<19) ANTARES: 900 PMTs

  11. Median Angular resolution vs energy  Angular resolution as good as 0.5° for highest energetic events • A very fast algorithm is needed Reconstruction taking 10ms / event is implemented • The better is the reconstruction angular resolution the easier it is to find the source in the image analysis phase Reconstruction on at least 3 detector lines required to avoid mirror solutions

  12. Keys of success (2/2) Event selection The TaToO project Background estimation: • Trigger: Doublet of neutrinos • A detection would be have 3 significance • High energy events Background: • Dominated by atmospheric neutrinos Seen on at least three detector lines After cuts on energy estimators: ΔΩ = 3° x 3° Δt = 15 min MC Emoy ~4 TeV Median Ang. Res.~ 0.75°

  13. Keys of success (2/2) Event selection The TaToO project • High energy events Background: • Dominated by atmospheric neutrinos Number of hits used in track fit 2008 data After cuts on energy estimators: MC Total amplitude 2008 data Emoy ~4 TeV Median Ang. Res.~ 0.75° • Tuned actual cuts to send 1 to 2 alerts/ month to TAROT; mostly would be from HE trigger

  14. Example of HE neutrino Representation 3D Representation 2D (height/time) z t

  15. F ~ t-1.2 Core-collapse SNe GRB afterglow 10 Minutes TAROT observation strategy after alert reception: Real time (T0) : 6 images of 3 minutes T0+1 day, +3 days, +9 days and +27 days This detection strategy is appropriate to follow the main objects time profile and to allow a reasonable time for image analysis The Observation strategy Two promising source classes for this detection:

  16. Still to be done: Test the subtraction algorithm: some problems due to the very variable PSF (variable atmospheric conditions, image quality on the CCD edges) Include the tool in an automatic system Tuning a tool originally used for SNe identification Increasing luminosity Decreasing luminosity Badly substracted Example A standard image Subtraction result

  17. TAToO is a promising detection tool of transient sources using neutrino telescopes as a trigger • This is the only method to detect satellites hidden sources as FGRBs • Several alerts sent already to Tarot • Image analysis tools are studied • In the future, this system is intended to be coupled with other detectors (Rotse, Swift, ATA…)

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