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

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

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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

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SLIDE 1

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

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SLIDE 2

IceCube results(arXiv:1405.5303)

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20 40 60 80 102 103 Declination (degrees) Deposited EM-Equivalent Energy in Detector (TeV) Showers Tracks

(a)

100 101 102 103 104 109 108 107 Energy TeV Flux GeV cm 2s1sr1

(b) E 2φ(E) ∝ E −0.3

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 2 / 9

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SLIDE 3

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved diffused high energy ν flux

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

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SLIDE 4

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved 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

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SLIDE 5

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved 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

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SLIDE 6

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved 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

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SLIDE 7

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved 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

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SLIDE 8

Bottom-up approach

The pp collisions of CRs in the ISM collisions produce the

  • bserved 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

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SLIDE 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

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SLIDE 10

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

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SLIDE 11

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

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SLIDE 12

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 np(n = 10cm3) → low efficiency for ν production

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

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SLIDE 13

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 np(n = 10cm3) → low efficiency for ν production

2 Star burst galaxies (SBGs) Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 4 / 9

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SLIDE 14

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 np(n = 10cm3) → 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 np(n = 102cm3) → high efficiency for ν production

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

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SLIDE 15

SNR and HNR in NSFG’s+SBG’s neutrino flux

HNR IC 100 101 102 103 104 109 108 107 Energy TeV Flux GeV cm 2s1sr1

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 5 / 9

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SLIDE 16

SNR and HNR in NSFG’s+SBG’s neutrino flux

SNR HNR IC 100 101 102 103 104 109 108 107 Energy TeV Flux GeV cm 2s1sr1

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 6 / 9

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SLIDE 17

SNR and HNR in NSFG’s+SBG’s neutrino flux

SNR+HNR IC 100 101 102 103 104 109 108 107 Energy TeV Flux GeV cm 2s1sr1

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

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SLIDE 18

Conclusions

Diffuse neutrino flux might have a (dominant) stellar remnant

  • rigin

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

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SLIDE 19

Thank you for your attention

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

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SLIDE 20

Back up slides

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

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SLIDE 21

ηπ:SBGs vs NSFGs

SBG NSFG 100 1000 104 105 0.0 0.2 0.4 0.6 0.8 Ep (TeV) ηπ

Figure: ν’s production efficiency (ηπ) as a function of the proton energy

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 2 / 9

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SLIDE 22

RSF as a function of z

1 2 3 4 5 6 7 0.02 0.04 0.06 0.08 0.10 z RSF Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 3 / 9

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SLIDE 23

SBGs

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

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SLIDE 24

SBGs

z≈1 z≈4 z=0

SPIRAL SF-AGN(Spiral) STARBURST SF-AGN(SB) AGN1 / AGN2 ELLIPTICAL

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 5 / 9

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SLIDE 25

HNRs in SBG neutrino flux (arXiv: 1310.1362)

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 6 / 9

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SLIDE 26

SBGs

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

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SLIDE 27

Fermi γ ray flux

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 8 / 9

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SLIDE 28

Fermi γ ray flux

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

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SLIDE 29

SN ν at IceCube

Invisibles 15 Workshop: ”Invisibles Meets Visibles” 25 June 2015 10 / 9