Detecting Neutrino Transients with optical Follow-up Observations Marek Kowalski Humboldt-University, Berlin TeV-III Venice, 2007.

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Presentation transcript:

Detecting Neutrino Transients with optical Follow-up Observations Marek Kowalski Humboldt-University, Berlin TeV-III Venice, 2007

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 SNe ? Neutrinos could provide the answer: 10 Mpc: 30 neutrino events in a cube-kilometer detector! Ando & Beacom, PRL (2005); Razzaque, Meszaros & Waxman, PRL (2005). Simulation: MacFadyen (2000) Gravitative collaps of a very massive, rotating star (>25 M  ):

Constraints on Quantum Gravity  Energy (TeV) SNe  t=10 s Jacob, Piran 2006

IceCube Optical Neutrino Follow-up

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

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

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

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

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

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

Correlating every neutrino (~10 5 /a)? Mirror Area X Field of View

Correlating every neutrino (~10 5 /a)? Next generation of Wide- Field-Imagers: full sky coverage of the optical sky with 3-7 day cadence. Offline correlation of every neutrino will be possible! Mirror Area X Field of View

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

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

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

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

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

Optical Neutrino Follow-up