Speaker
Mr
Tri L. Astraatmadja
(Nikhef)
Description
This is a preliminary study to examine the prospect of detecting TeV photons from
$\gamma$-ray bursts (GRB) using km-size neutrino telescope, specifically for the
ANTARES neutrino telescope. Although optimized to detect upgoing neutrino-induced
muons, km$^3$ neutrino telescopes nevertheless has a potential to detect high-energy
photons by detecting downgoing muons from electromagnetic cascade induced by the
interaction of TeV photons with The Earth's atmosphere. The photon energy spectrum of
a GRB is modeled by a simple power law and is normalized by simple energetic
considerations. Taking into account the absorption of TeV photons by cosmic infrared
backgrounds, the arriving number of photons on top of The Earth atmosphere is
determined. Muon production in the atmosphere is determined by considering two main
channels of muon productions: Pion photoproduction and direct muon pair production.
The muon energy loss during their traverse from the surface to the bottom of the sea
is determined using the standard muon energy loss formula. Assuming different
detector sizes, the total of number of signals from single GRB events located at
different redshifts and zenith distances is determined. Assuming background noises
consisting of cosmic ray-induced downgoing muons, the detection significance is
calculated. It is concluded that to obtain at least $3\sigma$ detection significance,
a GRB has to be located at redshift $z \lesssim 0.07$ if the detector's muon
effective area is $A^{\mu}_{\rm eff} \sim 10^{-2}\;{\rm km}^{2}$, or redshift $z
\lesssim 0.15$, if the muon effective area is $A^{\mu}_{\rm eff} \sim 1\;{\rm km}^{2}$.
Primary author
Mr
Tri L. Astraatmadja
(Nikhef)
