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Detecting Neutrino Transients with optical Follow-up Observations

Detecting Neutrino Transients with optical Follow-up Observations. Marek Kowalski Humboldt-University, Berlin TeV-III Venice , 2007. Gravitative collaps of a very massive, rotating star (>25 M  ):. Simulation: MacFadyen (2000). Testing the Supernovae-GRB connection. Observation:

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Detecting Neutrino Transients with optical Follow-up Observations

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  1. Detecting Neutrino Transients with optical Follow-up Observations Marek KowalskiHumboldt-University, BerlinTeV-III Venice, 2007

  2. Gravitative collaps of a very massive, rotating star (>25 M): Simulation: MacFadyen (2000) Testing the Supernovae-GRB connection Observation: Rate of GRBs is just ~1% of SNe Ib/c. Question: Could there be mildly relativistic jets ( of a few) inside many SNe? GRBs Neutrinos could provide the answer: SN @ 10 Mpc: 30 neutrino events in a cube-kilometer detector! Ando & Beacom, PRL (2005); Razzaque, Meszaros & Waxman, PRL (2005). SNe ?

  3. SNe Dt=10 s Constraints on Quantum Gravity  Energy (TeV) Jacob, Piran 2006

  4. Optical Neutrino Follow-up IceCube

  5. Optical Neutrino Follow-up optical detection network of optical telescopes IceCube Neutrino-Trigger IceCube

  6. GRB / Supernova identification Supernova lightcurves Search for transient sources: • Supernova (rising lightcurve) Strizinger et al. (2003)

  7. GRB / Supernova identification GRB afterglows Search for transient sources: • Supernova (rising lightcurve) • Gamma-Ray Burst (afterglow) • Gamma-Dark Bursts (orphan afterglows) F ~ t-1.2 10 minutes 100 seconds Time of explosion: Kahn et al., 2006

  8. GRB / Supernova identification Time of explosion: MK, A. Mohr, 2007

  9. single neutrinos 2o x 2o 250 nm a day For IceCube 100 seconds Neutrino burst trigger IceCube pointing Doublet background rate: doublets Kappes et al., 2007 Background rate of 5 per year, but Field-of-View of 2o x 2o needed.

  10. others • Robonet-1.0 3 x 2.0 m FoV: 0.1 x 0.1 follow-up of ROTSE Global network of robotic telescopes • ROTSE III 4 x 0.45 m FoV: 1.9 x 1.9 rapid follow-up

  11. Correlating every neutrino (~105/a)? Mirror Area X Field of View

  12. Next generation of Wide-Field-Imagers: full sky coverage of the optical sky with 3-7 day cadence. Correlating every neutrino (~105/a)? Offline correlation of every neutrino will be possible! Mirror Area X Field of View

  13. Supernova sensitivity Ando & Beacom PRL2005 Sensitivity can be doubled by optical follow-up! MK, A. Mohr, 2007

  14. Conclusion • An observation proposed using neutrinos to trigger follow-up observations (see also talk by M. Tluzykont) • Significant sensitivity improvement for SNe, and perhaps GRBs • For some cases it is the only way to identify the source • Robotic telescopes for follow-up observations exist and are ready

  15. Can we observe all SNe within a certain distance and do the correlation with neutrinos offline? Galaxy data from HyperLeda, [Paturel et al. 2003 A&A,412, 45]

  16. Can we observe all SNe within a certain distance and do the correlation with neutrinos offline? Galaxy data from HyperLeda, [Paturel et al. 2003 A&A,412, 45] Galaxy B-band magnitude converted to SNe rate using type dependent conversion [Cappelaro 99]

  17. ~20th magnitude detection limit (1 m) ~0.003 background Distribution of Supernovae (simulation) Triple coincidence Ando & Beacom flux Rate [arbitrary unit] Double Coincidence Distance [Mpc]

  18. Optical Neutrino Follow-up

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