HERMES: propagating UHECRs in a magnetized Universe
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1 HERMES: propagating UHECRs in a magnetized Universe M. De Domenico 12, H. Lyberis 3, M. Settimo 4 1 School of Computer Sciences, University of Birmingham, UK 2 Laboratorio sui Sistemi Complessi, Scuola Superiore di Catania, Italy 3 Istituto de Fisica, Universidade Federal do Rio de Janeiro, Brazil 4 University of Siegen, Germany Prague, 21 st Jun 2012
2 Who was HERMES? New (full MC) simulator of: UHECR propagation Magnetic fields (Gal, XGal) Cosmology Source distrib., injection 1D of nuclei and ν, 3D propagation (in regular or turbulent magnetic fields) of nuclei without energy loss: developed and completed by Manlio as part of his PhD thesis (Feb 2012) M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 2
3 Who is HERMES? Upgrades! Merging of existing modules for 3D propagation with energy losses Upgrades! Merging with new code ELECA for the propagation of γ and e + /e (M.Settimo, M. De Domenico, H. Lyberis, Scineghe 2012) M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 3
4 Outline of this talk Part 0. HERMES backbone General philosophy, scheme of modules Part I. Simulating the propagation of nuclei Cross sections Energy losses in the extragalactic background radiation (EBR) Propagation in a magnetized Universe Part II. Propagation of secondary particles Propagation of ν Status of the propagation of γ and e + /e M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 4
5 Part 0: HERMES backbone M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 5
6 HERMES: sketch of modules M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 6
7 Part I: Simulating the propagation of nuclei M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 7
8 Modeling EBR and interaction length Model D Finke et al. (ApJ, 2010, arxiv: ) Star Formation Rate Hopkins & Beacom (ApJ, 2006, arxiv: ) Initial Mass Function Salpeter (ApJ, 1955) Figures: energy density of EBR vs energy of background photons HERMES Interaction length: M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 8
9 HERMES: energy losses and particle production Cosmology Fully customizable: Hubble parameter, energy and matter densities... Source evolution: Star Formation Rate (SFR), AGN, QSO, GRB and (1+z) m Energy loss Include only those ones having a significant impact on the propagation of UHECR: Adiabatic loss: expansion of the Universe [A 1, γ, ν] (CEL) Pair production: creation of e + /e pairs [A 1, γ] (CEL) (Multi)Photo-pion production: creation of π [A 1] (MC) Photodisintegration: fragmentation of the original nucleus, creation of lighter nuclides due to Giant Dipole Resonance and Quasi-Deuteron effect [A 2] (MC) M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 9
10 HERMES: Simulating Aγ EBR interactions Fe 1 1 H Cross sections Rachen parameteriz. Giant dipole reson. Quasi-deuteron effect Baryonic resonances Multipion production Nuclear rest frame Energy loss Adiabatic Pair production Photopion production Photodisintegration CMB + Infrared/Opt Lab frame Squares indicate values from Stanev (p) & Allard (Fe) M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 10
11 HERMES: Puget-Stecker-Bredekamp β stable chain The modular structure allows high customization Default: TALYS v1.2 cross sections and β stable chain Any change to TALYS cross-sections can be easily updated We are in touch with E. Khan (IPNO) for measured cross-sections and chains M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 11
12 HERMES: (many!!) exclusive channels considered M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 12
13 HERMES: sources and composition Available options: - Continuous/Discrete sources distr. - Different evolutions - Power-law injection - Equal/Different abundances - Equal/Different luminosity allowed for each source Panels: - Auger data rescaled by +15% - Hires data - Flux of UHECR from HERMES (lines) - Uniform source distrib z Equal intrinsic luminosity - Norm. at E = ev M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 13
14 HERMES: composition at Earth Preliminary Elongation rate: Estimation at Earth is due to fast parameterizations based on extreme value theory for 3 different hadronic models (M. De Domenico, S. Riggi, GAP ) [journal paper in preparation] Panels: - UHECR from HERMES (lines) - Uniform source distrib z Equal intrinsic luminosity - Check, check & check in progress! Preliminary M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 14
15 HERMES: comparison with other simulators Probability to reach the Earth above a given energy E thr Surviving probability Protons: - Uniform sources - E 2.7 inj. - ΛCDM Cosmology - CMB only GZK horizon Nuclei: - Uniform sources - E 2.7 inj. - ΛCDM Cosmology - CMB+Infrared/Opt Distance within which 90% of UHECRs reach the Earth above E thr M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 15
16 HERMES: magnetic fields Turb. EMF: Kolmogorov 3D Reg. GMF: HMR BSS-S Turbulent magnetic field: Fisher distribution of deflections as expected! Trajectories in turb. GMF (Giacalone-Jokipii isotropic method) Available models: Reg. GMF: ASS/BSS Harari et al, Stanev, Tyniakov-Tkachev Turb. GMF/EMF: Kolmogorov-like k γ New models can be easily included M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 16
17 Part II: Propagation of secondary particles M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 17
18 HERMES: neutrinos (1D propagation) Preliminary! M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 18
19 ELECA: ELEctromagnetic CAscading (λ PP /Mpc) 10 Interaction length log Adiabatic CMB CIB CIOB URB Total Lee 98 Protheroe log (Energy/GeV) 10 / Mpc) (λ 10 eγ Interaction length log CMB Total ICS Lee 96 TPP Lee 96 Synchrotron (10 ng) Adiabatic 1 ng 0.1 ng log (Energy/GeV) 10 MC code to propagate extragalactic UHE γ and e + /e Main interaction processes with the EBR: 1 Pair Production (for photons) 2 Inverse Compton Scattering and Triple Pair Production (for e + /e ) are treated with a full MC; 3 Synchrotron and adiabatic energy losses are treated as continuous processes. (M.Settimo, M. De Domenico, H. Lyberis, Scineghe 2012) M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 19
20 Conclusions Summary A new full MC simulator of UHECRs has been developed: Outlook 3D Propagation in a magnetized Universe Energy losses in the EBR Cosmology, Source distribution, UHECR injection Propagation of ν, γ and e + /e ASCII configuration file as input: very customizable, about 50 different parameters/options Good agreement with existing results 1 Nuclei/magnetic fields: final stages of consistency checks 2 ELECA: cross-checks in progress, but promising 3 Public release soon M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 20
21 Acknowledgments Today HERMES is the result of our joint efforts to build a 3D MC propagator of nuclei including energy loss and the propagation of all secondaries particles, including γ and e + /e. We would like to thank O. Deligny, D. Allard, E. Khan, S. Mollerach, M. Risse, P. Schiffer and T. Winchen for many useful discussions We would also like to thank D. Allard, S. Riggi, the Simprop and PARSEC teams for having kindly provided us with simulated particles or tables used for comparisons M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 21
22 Extra slides M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 22
23 HERMES: 1D output example z 0 A 0 Z 0 E 0 z f A f Z f E f Type Process In the 3D version you have also 3-coords for: Position, Momentum and Propagation Time Output is structured to allow cascade reconstruction... M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 23
24 HERMES: energy losses and particle production Friedmann-Robertson-Walker Universe: Cosmology 1 de E dz dt dz = dt dz = β proc(z,e), process 1 H 0(1+z) H 0 Hubble param. Homogeneous Isotropic Energy loss rate [ Ω M (1+z) 3 +Ω Λ +(1 Ω M Ω Λ )(1+z) 2] 1 2 Sum extended to all interactions acting during the propagation. Include only those ones having a significant impact on the propagation of UHECR: Adiabatic loss: expansion of the universe [A 1, γ, ν] (CEL) Pair production: creation of e + /e pairs [A 1, γ] (CEL) (Multi)Photo-pion production: creation of π [A 1] (MC) Friedmann equations Ω M Density of cold+baryonic mass Ω Λ Density of dark energy Photodisintegration: fragmentation of the original nucleus, creation of lighter nuclides [A 2] (MC) Available source evolutions: Uniform, Star Formation Rate, AGN, QSO and GRB M. De Domenico, H. Lyberis, M. Settimo HERMES: propagating UHECRs in a magnetized Universe 24
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