Difficulties of Star-forming Galaxies as the Source of IceCube Neutrinos. Takahiro Sudoh (UTokyo)
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1 Difficulties of Star-forming Galaxies as the Source of IceCube Neutrinos Takahiro Sudoh (UTokyo)
2 IceCube Neutrino Astrophysical TeV - PeV neutrinos Isotropic arrival direction extragalactic origin? No identified individual source Various source models Cosmic-ray sources (GRB, AGN) Cosmic-ray reservoirs (star-forming galaxy, cluster) Star-forming galaxies among possible sources high density & strong magnetic field --> efficient production of high-energy neutrinos?
3 Neutrino from Galaxies Previous studies Simple estimate by using IR luminosity (e.g. Tamborra+14, Chang+15) or EGB observation (e.g. Bechtol+17) Bechtol+17 : SBGs should not produce more than 30 % of IceCube data at 100 TeV (for ) Sensitive to gamma-ray spectral index (parameter) It may still be possible that SBGs make larger contribution (e.g. Xiao+16, Chakraborty & Izaguirre 16) Xiao+16 : SBGs may contribute ~50 % of the > 100 TeV flux
4 This Work New calculation of contribution of galaxies to diffuse gamma-ray/neutrino backgrounds with a cosmological galaxy formation model Realistic estimation based on physical quantities of individual galaxies at various redshifts Robust calibration using gamma-ray luminosities of nearby galaxies
5 Semi-Analytical Model of Galaxy Formation Analytical calculation of dark halo merger trees (based on Press- Schechter) + phenomological treatment of baryonic processes in DM haloes Calculate properties of galaxies a various out put redshifts SFR, size, mass, morphology, SF mode (quiescent/burst), etc. Reproduce many observations We use the Mitaka model (Nagashima & Yoshii 2004) Cole+00
6 Semi-Analytical Model of Galaxy Formation Analytical calculation of dark halo merger trees (based on Press- Schechter) + phenomological treatment of baryonic processes in DM haloes Calculate properties of galaxies a various out put redshifts SFR, size, mass, morphology, SF mode (quiescent/burst), etc. Reproduce many observations (Nagashima and Yoshii 2004) We use the Mitaka model (Nagashima & Yoshii 2004)
7 Modelling Neutrinos from Galaxies Neutrinos from a galaxy Pion production efficiency CR spectrum at injection Neutrino spectrum from a pp interaction (Kelner+06) : determined from Lγ of nearby galaxies : calculated from properties of each galaxy (see next slide)
8 Calculation of Pion Production Efficiency = : Advection timescale = ( : dark halo circular velocity) Diffusion timescale = ( : diffusion coefficient) and lower limit is set to H (gas scale height) : for elliptical and for disk Diffusion coefficient D(E) depends on B (magnetic field) : assuming in each galaxy (outer scale of turbulence) : equal to scale height ( ) (turbulence spectrum) : Kolmogorov-type ( ) from and morphology of each galaxy
9 Calculation of Pion Production Efficiency = : Advection timescale = ( : dark halo circular velocity) Diffusion timescale = ( : diffusion coefficient) and lower limit is set to H (gas scale height) : for elliptical and for disk Diffusion coefficient D(E) depends on B (magnetic field) : assuming in each galaxy (outer scale of turbulence) : equal to scale height ( ) (turbulence spectrum) : Kolmogorov-type ( ) from and morphology of each galaxy Directly derived from galaxy formation model
10 Model Calibration M31, Arp220, NGC4945, NGC1068 not used in this work Calculate from SFR, for nearby galaxies Minimize to fix C
11 Model Calibration Lγ = GeV (for NGC2146) GeV (for others) is set to 2 in all galaxies Model agrees very well with observation!
12 Result (Gamma-ray & Neutrino) Star-forming galaxies make ~10 % contribution to IGRB and less than 10 % contribution to IceCube data even when in all galaxies (optimistic)
13 Result (Dependence on Modelling) We check dependence on modelling of H and E.g.) If we set in all galaxies, the result changes by a factor of ~2 but still cannot explain data.
14 Summary Calculated γ-ray and neutrino fluxes with a cosmological galaxy formation model Calibrated models from Lγ of nearby six galaxies SFG can explain less than 10 % of IceCube data other source(s) should be dominant
15 Appendix derived values for nearby galaxies in our model Input: SFR,
16 Appendix Cosmic ray energy density : Estimated for E = GeV The result is not changed when we use E = 100 MeV or 10 GeV instead.
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