Muon Detection of TeV Gamma Rays from Gamma‐Ray Bursts

Álvarez-Muñiz, J.; Halzen, F.

doi:10.1086/307591

Cited by 20 publications

(17 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Previous works had addressed these problems. In a similar vein with this paper, Alvarez‐Muñiz & Halzen (1999) have calculated the muon flux from GRBs at various redshifts and physical properties, but for the muon production only the photopion channel – which falls quickly with increasing energies – is considered. Recently, Halzen, Kappes & Ó Murchadha (2009) rectified this problem and discussed the various channels from which muons can be produced, including muon pair production.…”

Section: Introductionmentioning

confidence: 90%

On the detection of TeV γ-rays from GRB with km3 neutrino telescopes - I. Muon event rate from single GRBs

Astraatmadja

2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

This is a preliminary study to examine the prospect of detecting Tetraelectronvolt 10 12 eV (TeV) photons from γ -ray bursts (GRB) using km-sized neutrino telescopes, specifically for the ANTARES neutrino telescope. Although optimized to detect upgoing neutrino-induced muons, neutrino telescopes nevertheless have a potential to detect high-energy photons by detecting downgoing muons from the electromagnetic cascade induced by the interaction of TeV photons with the Earth's atmosphere. The photon energy spectrum of a GRB is modelled by a simple power law and is normalized by simple energy considerations. Taking into account the absorption of TeV photons by cosmic infrared backgrounds, an optical depth table calculated from a model by Finke, Razzaque & Dermer is used and 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 production: 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 number of detectable muons from single GRB events located at different redshifts and zenith distances is determined. The background is calculated assuming it consists primarily of cosmic ray induced downgoing muons. The detection significance is calculated and it can be concluded that to obtain at least 3σ detection significance, a typical GRB has to be located at redshift z 0.07 if the detector's muon effective area is A μ eff ∼ 10 −2 km 2 , or redshift z 0.15, if the muon effective area is A μ eff ∼ 1 km 2 .

show abstract

Section: Introductionmentioning

confidence: 90%

On the detection of TeV γ-rays from GRB with km3 neutrino telescopes - I. Muon event rate from single GRBs

Astraatmadja

2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…In the decay of the charged pions, neutrinos of energy O(10 14 eV) are produced with the approximate ratios (ν e :ν μ :ν τ ) = (1:2:0), 40 changing to about (1:1:1) at the Earth due to oscillations (Learned & Pakvasa 1995;Athar et al 2006). First calculations of this prompt neutrino flux (Waxman & Bahcall 1997;Alvarez-Muniz & Halzen 1999) used average GRB parameters and the GRB rate measured by BATSE to determine an all-sky neutrino flux from the GRB population. The AMANDA-II neutrino telescope (Achterberg et al 2007(Achterberg et al , 2008 performed searches for this so-called Waxman-Bahcall GRB flux or similar GRB fluxes (Achterberg et al 2007(Achterberg et al , 2008 with negative results.…”

Section: Introductionmentioning

confidence: 99%

SEARCH FOR MUON NEUTRINOS FROM GAMMA-RAY BURSTS WITH THE IceCube NEUTRINO TELESCOPE

Abbasi¹,

Abdou²,

Abu‐Zayyad³

et al. 2010

ApJ

Self Cite

103

166

View full text Add to dashboard Cite

We present the results of searches for high-energy muon neutrinos from 41 gamma-ray bursts (GRBs) in the northern sky with the IceCube detector in its 22 string configuration active in 2007/2008. The searches cover both the prompt and a possible precursor emission as well as a model-independent, wide time window of −1 hr to +3 hr around each GRB. In contrast to previous searches with a large GRB population, we do not utilize a standard Waxman-Bahcall GRB flux for the prompt emission but calculate individual neutrino spectra for all 41 GRBs from the burst parameters measured by satellites. For all of the three time windows, the best estimate for the number of signal events is zero. Therefore, we place 90% CL upper limits on the fluence from the prompt phase of 3.7 × 10 −3 erg cm −2 (72 TeV-6.5 PeV) and on the fluence from the precursor phase of 2.3 × 10 −3 erg cm −2 (2.2-55 TeV), where the quoted energy ranges contain 90% of the expected signal events in the detector. The 90% CL upper limit for the wide time window is 2.7 × 10 −3 erg cm −2 (3 TeV-2.8 PeV) assuming an E −2 flux.

show abstract

“…at Earth due to oscillations [7]. First calculations of this prompt neutrino flux [6,8] used average GRB parameters and the GRB rate measured by BATSE to determine an all-sky neutrino flux from the GRB population.…”

Section: Introductionmentioning

confidence: 99%

“…In the decay of the charged pions, neutrinos of energy O(10 14 eV) are produced with the approximate ratios (ν e :ν µ :ν τ ) = (1:2:0) 2 , changing to about (1:1:1) at Earth due to oscillations [7]. First calculations of this prompt neutrino flux [6,8] used average GRB parameters and the GRB rate measured by BATSE to determine an all-sky neutrino flux from the GRB population.…”

Section: Introductionmentioning

confidence: 99%

IceCube: Neutrino Messages from GRBs

Kappes¹

2010

AIP Conference Proceedings

View full text Add to dashboard Cite

Abstract. The mystery of where and how Nature accelerates the cosmic rays is still unresolved a century after their discovery. Gamma ray bursts (GRBs) have been proposed as one of the more plausible sources of extragalactic cosmic rays. A positive observation of neutrinos in coincidence with a GRB would identify these objects as sources of the highest-energy cosmic rays and provide invaluable information about the processes occurring inside these phenomena. Calculations show that a kilometer-scale neutrino telescope is necessary for this task. The idea of such a detector is now becoming reality as IceCube at the South Pole nears completion. The contribution reviews the status of the construction and operation of IceCube and summarize the results from searches for neutrinos from GRBs and similar phenomena with IceCube and its predecessor, AMANDA. At the end, an outline of future plans and perspectives for IceCube is given.

show abstract

Muon Detection of TeV Gamma Rays from Gamma‐Ray Bursts

Cited by 20 publications

References 14 publications

On the detection of TeV γ-rays from GRB with km3 neutrino telescopes - I. Muon event rate from single GRBs

On the detection of TeV γ-rays from GRB with km3 neutrino telescopes - I. Muon event rate from single GRBs

SEARCH FOR MUON NEUTRINOS FROM GAMMA-RAY BURSTS WITH THE IceCube NEUTRINO TELESCOPE

IceCube: Neutrino Messages from GRBs

Contact Info

Product

Resources

About