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A Combined Astrophysical and Dark Matter Interpretation of the IceCube HESE and Throughgoing Muon Events Yicong Sui Washington University in St. Louis Y. S, B. Dev, arXiv:1804.04919 [hep-ph] Pheno2018 University of Pittsburgh May 8, 2018

  1. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range

  2. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111)

  3. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477)

  4. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477)

  5. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Flux

  6. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Flux

  7. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Reconstruction Flux

  8. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Reconstruction Flux

  9. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Reconstruction Best Fit Flux

  10. 2 Astro Comp Flux: Setup and Fitting ● Instead of one single component, we assume 2 astrophysical components 1 st component 2 nd component Cut off factor At Low Energy At all range (111) (111) or (477) Reconstruction Best Fit Flux

  11. Fitting Results

  12. Fitting Results

  13. Fitting Results 3σ

  14. Fitting Results 3σ 1 st comp almost 0

  15. Fitting Results 3σ 1 st comp almost 0 3σ 2σ

  16. Fitting Results 3σ 1 st comp is not 0 1 st comp almost 0 3σ 2σ

  17. Best Fit Event Spectrum

  18. Best Fit Event Spectrum

  19. Best Fit Event Spectrum

  20. Best Fit Event Spectrum

  21. Best Fit Event Spectrum Using 2 comp flux to fit both HESE and TG is doable but having ● discrepancy at bins ~ 100 TeV

  22. Best Fit Event Spectrum Using 2 comp flux to fit both HESE and TG is doable but having ● discrepancy at bins ~ 100 TeV 1 st comp is not contributing in (111+111) case but contributes in ● (111+477 ）

  23. Best Fit Event Spectrum Using 2 comp flux to fit both HESE and TG is doable but having ● discrepancy at bins ~ 100 TeV 1 st comp is not contributing in (111+111) case but contributes in ● (111+477 ） Glashow Resonance

  24. Best Fit Event Spectrum Using 2 comp flux to fit both HESE and TG is doable but having ● discrepancy at bins ~ 100 TeV 1 st comp is not contributing in (111+111) case but contributes in ● (111+477 ） Glashow Resonance Statistically, (111+477) fit is slightly favored than (111+111) ●

  25. DM+1Comp Flux: Model and Fitting Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  26. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  27. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  28. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  29. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  30. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  31. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  32. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic neutrinos Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  33. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  34. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos DM decaying process Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  35. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos DM decaying process Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  36. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM decaying process Sum up contribution from all DM, galactically or extra-galactically Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  37. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM decaying process Sum up contribution from all DM, galactically or extra-galactically Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  38. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  39. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  40. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Reconstruction Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  41. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Reconstruction Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  42. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Fitting Reconstruction Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  43. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Fitting Reconstruction Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  44. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Fitting Reconstruction Flavor composition for DM event: (111) Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  45. DM+1Comp Flux: Model and Fitting Now, let’s assume the flux has 1 DM component and 1 astrophysical ● component Expand after SSB Almost monochromatic A.~Atre, T.~Han, S.~Pascoli and B.~Zhang, “The Search for Heavy Majorana Neutrinos” neutrinos Monte Carlo simulation DM neutrino DM decaying process Sum up contribution flux+ astro flux from all DM, galactically or extra-galactically Fitting Reconstruction Flavor composition for DM event: (111) Flavor composition for astro event: (111) and (477) Feldstein et al (PRD '13); Esmaili, Serpico (JCAP '13); Murase et al (PRL '15); Boucenna et al (JCAP '15); Dev et al (JCAP '16); di Bari et al (JCAP '16); Cohen et al (PRL '17);

  46. Fitting Results

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