Diffuse neutrinos from extragalactic supernova remnants: dominating - PowerPoint PPT Presentation

Diffuse neutrinos from extragalactic supernova remnants: dominating the 100 TeV IceCube flux Ignacio Izaguirre 25 June 2015 Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 1 / 9

IceCube results(arXiv:1405.5303) 80 Showers Tracks 10 � 7 60 Flux � GeV cm � 2 s � 1 sr � 1 � Declination (degrees) 40 20 0 10 � 8 -20 -40 -60 -80 10 � 9 10 2 10 3 10 0 10 1 10 2 10 3 10 4 Deposited EM-Equivalent Energy in Detector (TeV) Energy � TeV � (b) E 2 φ ( E ) ∝ E − 0 . 3 (a) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 2 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux We assume that the CRs are accelerated by stellar remnants Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux We assume that the CRs are accelerated by stellar remnants We consider two types of stellar remnants: Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux We assume that the CRs are accelerated by stellar remnants We consider two types of stellar remnants: Supernova remnants (SNRs) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux We assume that the CRs are accelerated by stellar remnants We consider two types of stellar remnants: Supernova remnants (SNRs) CR sources Capable of generating ν flux up to 100 − 150 TeV Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

Bottom-up approach The pp collisions of CRs in the ISM collisions produce the observed diffused high energy ν flux We assume that the CRs are accelerated by stellar remnants We consider two types of stellar remnants: Supernova remnants (SNRs) CR sources Capable of generating ν flux up to 100 − 150 TeV Hypernova remmants (HNRs) Small fraction of SNRs (1 ⋍ %) with extreme energetic ejecta Capable of generating ν flux up to 1 − 10 P eV Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. In our calculation we have considered two type of galaxies: Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. In our calculation we have considered two type of galaxies: 1 Normal star formation Galaxies (NSFGs) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. In our calculation we have considered two type of galaxies: 1 Normal star formation Galaxies (NSFGs) Galaxies with a star formation rate (SFR) similar to the Milky Way Low n p ( n = 10cm 3 ) → low efficiency for ν production Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. In our calculation we have considered two type of galaxies: 1 Normal star formation Galaxies (NSFGs) Galaxies with a star formation rate (SFR) similar to the Milky Way Low n p ( n = 10cm 3 ) → low efficiency for ν production 2 Star burst galaxies (SBGs) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

NSFGs vs SFGs The galactic environment surrounding the stellar remnant plays a crucial role for the ν production. In our calculation we have considered two type of galaxies: 1 Normal star formation Galaxies (NSFGs) Galaxies with a star formation rate (SFR) similar to the Milky Way Low n p ( n = 10cm 3 ) → low efficiency for ν production 2 Star burst galaxies (SBGs) Old, Metal poor galaxies (z ⋍ 1-2) Relative rate of SBGs → (10-20)% of the NSFGs Galaxies with a high SFR High n p ( n = 10 2 cm 3 ) → high efficiency for ν production Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

SNR and HNR in NSFG’s+SBG’s neutrino flux 10 � 7 HNR Flux � GeV cm � 2 s � 1 sr � 1 � 10 � 8 IC 10 � 9 10 0 10 1 10 2 10 3 10 4 Energy � TeV � Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 5 / 9

SNR and HNR in NSFG’s+SBG’s neutrino flux 10 � 7 Flux � GeV cm � 2 s � 1 sr � 1 � SNR 10 � 8 IC HNR 10 � 9 10 0 10 1 10 2 10 3 10 4 Energy � TeV � Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 6 / 9

SNR and HNR in NSFG’s+SBG’s neutrino flux 10 � 7 SNR+HNR Flux � GeV cm � 2 s � 1 sr � 1 � 10 � 8 IC 10 � 9 10 0 10 1 10 2 10 3 10 4 Energy � TeV � Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 7 / 9

Conclusions Diffuse neutrino flux might have a (dominant) stellar remnant origin SNRs-HNRs in NSFGs-SBGs are plausible candidates ◮ The SNR ν flux will be dominant at ≃ 100 TeV energies ◮ The SNR-HNR in NSFGs-SBGs ν dominated flux scenario will result in a break on the spectrum Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 8 / 9

Thank you for your attention Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 9 / 9

Back up slides Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 1 / 9

η π :SBGs vs NSFGs 0.8 0.6 SBG 0.4 η π NSFG 0.2 0.0 10 4 10 5 100 1000 E p ( TeV ) Figure: ν ’s production efficiency ( η π ) as a function of the proton energy Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 2 / 9

R SF as a function of z 0.10 0.08 0.06 R SF 0.04 0.02 0 1 2 3 4 5 6 7 z Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

SBGs Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

SBGs ELLIPTICAL AGN1 / AGN2 SF-AGN(SB) SPIRAL SF-AGN(Spiral) STARBURST z=0 z ≈ 1 z ≈ 4 Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 5 / 9

HNRs in SBG neutrino flux (arXiv: 1310.1362) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 6 / 9

SBGs Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 7 / 9

Fermi γ ray flux Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 8 / 9

Fermi γ ray flux Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 9 / 9

SN ν at IceCube Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 10 / 9