High-Energy Neutrinos from Gamma-Ray Burst Fireballs

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High-Energy Neutrinos from Gamma-Ray Burst Fireballs Irene Tamborra GRAPPA Center of Excellence, University of Amsterdam TAUP 2015 Turin, September 9, 2015

Outline IceCube detection of high-energy neutrinos Neutrinos from gamma-ray burst fireballs Diffuse emission from gamma-ray bursts Conclusions This talk is based on work in collaboration with Shin ichiro Ando, arxiv: 1504.00107, JCAP (2015, in press).

High-energy neutrino astronomy is happening! 34 year year ~7 2015 > 5σ% sigma talk by Karle IceCube observed 54 events over four years in the 25 TeV-2.8 PeV range. Zenith Distribution compatible with isotropic flux. Flavor distribution consistent with e : µ : =1:1:1. 7 evidence for astrophysical flux * IceCube Collaboration, Science 342 (2013) 6161, PRL 113 (2014) 101101, PRD 91 (2015) 2, 022001. F. Halzen @ INvISIBLES 2015. See also: IceCube Collaboration, ApJ 809 (2015) 1, 98, PRL 115 (2015) 8, 081102.

Where are these neutrinos coming from? New physics? Galactic origin [sub-dominant contribution or new unknown sources?] Extragalactic origin [flux compatible with Waxman&Bahcall bound] Star-forming galaxies Active galactic nuclei Gamma-ray bursts Warning: More statistics needed! No strong preference so far. * Anchordoqui et al., JHEAp 1-2 (2014) 1.

Neutrinos from gamma-ray bursts Sizable emission of high-energy neutrinos from gamma-ray bursts expected. * Waxman & Bahcall, PRL 78 (1997) 2292, PRD 64 (2001) 023002. Guetta et al., Astropart. Phys. 20 (2004) 429.

Neutrinos from gamma-ray bursts sec -1 sr -1 ] -2 Φ [GeV cm 2 E -2 10 10 10-3 -5 10-7 GRB dedicated searches Quasi-diffuse Flux from 57 GRBs with NeuCosmA ARA Testbed Limit ARA37 3yrs expected ANTARES NeuCosmA x3 IceCube IC40+59 x3-9 10-11 10 4 6 8 10 Neutrino energy [log (E/GeV)] 10 Dedicated stacking searches on GRBs unsuccessful up to now. Existing detectors are achieving relevant sensitivity. Does the diffuse emission from ALL GRB families contribute to the IceCube flux? * Allison et al., arxiv: 1507.00100. IceCube Collaboration, ApJ 805 (2015) 1, L5. ANTARES Collaboration, A&A 559 (2013) A9.

Neutrino emission from gamma-ray bursts High energy neutrinos are produced through the following reactions: p + γ n + π +,p+ π 0 p + γ K + + Λ/Σ. * Image credit: Gomboc, Contemp. Phys. 53 (2012) 339. * Kelner, Aharonian, PRD 78 (2008) 034013. π + µ + ν µ, µ + ν µ + ν e + e + π µ ν µ, µ ν µ + ν e + e K + µ + + ν µ, n p + e + ν e.

Neutrinos emission from gamma-ray bursts Short-duration bursts (t < 2s) L iso = 1051 erg/s, = 650, tv = 0.01s. Long-duration bursts (t > 2s) High-luminosity GRBs L iso = 1052 erg/s, = 500, tv = 0.1s. * Meszaros, Rept. Prog. Phys. 69 (2006) 2259. Low-luminosity GRBs = 5, tv = 100s. L iso = 1048 erg/s, Image credit: NASA web-site.

Neutrino emission ( ) ( from ) ( gamma-ray ) ( ) bursts We revisited the analytical modeling of prompt emission from fireballs, including pion and kaon decays as well as adiabatic, radiative and hadronic cooling processes. Neutrino spectrum normalized in terms of the photon fluence: 0 ( ) dnν h p,i de ν E ν = N i [1 (1 χ p ) τpγ ] de ν inj,i h γp 0 ( ) dnγ de γ E γ de γ inj Example of predicted HL-GRB flux w/o flavor oscillations at z=1.!"!" $ resonance cooling processes )! * +,! -)!.+/012+34 * 5!" %!" $ (!! (, # -2 3, 4-./+0-56 # 1!" %! +!" #!" #!" $!" %, -./+01!" (!" )!" *!"!"!" (!" #!" $!" %, -./+01!" (!" )!" *!"!" * Tamborra, Ando, JCAP (2015). See also Guetta et al., Astropart. Phys. (2004). Huemmer, Baerwald, Winter, PRL (2012). Li, PRD (2012).

Diffuse background ingredients time z =0 z =1 neutrinos, photons neutrinos, photons Gamma and neutrino energy fluxes Distribution of sources with redshift Comoving volume (cosmology) z =5

Diffuse emission from gamma-ray bursts I X (E ν )= zmax z min Lmax ( ) c 1 dnνµ dz d L iso R X (z)φ X ( L iso ) L min 4 H H 0 Γ 0 ΩM (1 + z) 3 + Ω Λ de ν osc GRB redshift distribution luminosity function neutrino flux Recent work based on BATSE, Fermi and Swift data. Analytical modeling of the prompt emission from fireballs. * Tamborra & Ando, JCAP (2015).

Diffuse emission from gamma-ray bursts!" ( 1234563 7 # 81 <7 =89,3:82> # 8+! 8+?! ;!" )!" *!"!"!"!!!"!#!"!$ 14,-. +,-. /0,-. 00,-.!"!%!"!&!" #!" $!" % 7 89,3:;!" (!" )!" *!"!" GRBs can make up to few % of the high-energy IceCube flux in the sub-pev region. LL-GRBs can be main sources of the IceCube flux in the PeV range. * Tamborra & Ando, JCAP (2015). See also: Liu & Wang (2013), Murase & Ioka (2013), Razzaque & Yang (2015), Baerwald, Bustamante, Winter (2015).

Diffuse emission from gamma-ray bursts!" ) ;! % <5! =;! ><?07@<6* % </! </A! B!" (!"!"!"!!!"!% 56789:7 *-. *+, 34 012 44 012 Γ min Γ Γ max t v,min t v t v,max HL-GRB 100 500 1000 10 3 0.1 1 LL-GRB 2 5 20 10 100 200 sgrb 100 650 1000 10 3 10 2 0.05!"!$!"!# /012 Conclusions robust with respect to variation of model parameters. +,-./01!" ( :;<=>?< +, @ #.: D@ E.A5<B.;/ #.4!.4F! C!" )!" * 99 567!"!"!"!!!"!# +,-./23 89 567 GRBs cannot explain the IceCube flux for sub-pev energies, but could contribute around PeV energies for certain choices of the model parameters.!"!$ 4567!"!%!" #!" $!" % @.A5<BC!" (!" )!" *!"!" * Tamborra & Ando, JCAP (2015).

Conclusions Gamma-ray bursts account up to few % of the observed IceCube flux for E< 1 PeV. Low-luminosity gamma-ray bursts dominate the diffuse emission in the PeV range. High-luminosity and low-luminosity GRBs have comparable intensities, while the contribution from the short-duration component is small. Our findings confirm the most-recent IceCube results on GRB searches. Larger exposure is mandatory to detect neutrinos from high-luminosity GRBs.

Thank you for your attention!

Back-up slides

Neutrino emission from gamma-ray bursts +,-./ 2!,-31!"!"!" *!" )!" (!" #!" $!" %!"!!" "!"!!" %!" $!" #!"!"!" *!" )!" (!" %!" $!" #!"!!" "!"!!" #!" $!" % +!032 2!!587 2! 97 4",#5! + 62 :",#;! 2! 4587 4",#5! :",#; 4 +!012 +!032 78 9:;!" #!" $!" % +,-./01!" (!" )!" *!"!" 2! 4567 Cooling times in the jet comoving frame for HL-GRBs. * Tamborra, Ando,JCAP (2015).

Neutrino emission from gamma-ray bursts )! * +,! -)!.+/012+34 * 5!" %!" $ (!! (!" #!" $ Predicted GRB flux for HL-GRB at z=1 and without flavor oscillations.!" %!, # -2 3, 4-./+0-56 # 1 +!" (!" #!" $!" %, -./+01!" (!" )!" *!"!" * Tamborra, Ando,JCAP (2015).

Neutrino emission from gamma-ray bursts!" $ +, -./ Predicted GRB flux with flavor oscillations at z=1.!" % 1 # 27 81 923-452:; # 6!" (,, -./!" ) 0-./!" *!" #!" $!" % 1 23-456!" (!" )!" *!"!" * Tamborra, Ando, JCAP (2015). See also Guetta et al., Astropart. Phys. (2004). Huemmer, Baerwald, Winter, PRL (2012). Li, PRD (2012).

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