Intergalactic Magnetic Field and Arrival Direction of Ultra-High-Energy Protons

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1 Intergalactic Magnetic Field and Arrival Direction of Ultra-High-Energy Protons Dongsu Ryu (Chungnam National U, Korea) Hyesung Kang (Pusan National U, Korea) Santabrata Das (Indian Institute of Technology Guwahati)

2 What are cosmic rays (CRs)? cosmic rays -> in physics, high energy particles from the space cosmic rays -> in astrophysics, nonthermal particles or particles above the Maxwellian distribution in the p space observational example: particle spectra in the Solar wind (Mewaldt et al 2001) - thermal + CR populations - suprathermal particles leak out of the thermal pool into the CR population gas CR

3 Why do we care about CRs? - CRs are ubiquitous in astrophysical plasma. - heliosphere (solar system) solar wind, interplanetary shocks - ISM of our Galaxy E CR ~ E B ~ E gas ~ E CMBR ~ erg/cm 3 sources: SNRs, stellar wind (OB stars), pulsars - ICM inside clusters of galaxies and the large scale structure of the Universe E CR,p ~ E gas thermal, E CR,e ~ 0.01 E CR,p, E B ~ (0.1-1) E gas kinetic sources: AGNs, galactic winds, turbulence, structure shocks CRs are dynamically important, and more importantly produce observable radiations

4 CRs observed at Earth particle energy spectrum power-law spectrum -knee energy: ev ankle energy: ev - N(E) ~ E -2.7 below the knee and steeper above - E: up to ~10 21 ev - universal acceleration mechanism working on a wide range of scales shock acceleration UHECRs: above the ankle 32 orders of magnitude E -2.7 direct measurements E -3.1 extragalactic origin air shower measuremen ts 12 orders of magnitude

5 CRs observed at Earth - power-law spectrum below the knee: N(E) ~ E composition: interstellar proton/electron ~ E 2.7 F 0.1 JACEE[11] Akeno[12] Tien Shan[13] MSU[14] Tibet[15] CasaMia[16] DICE[17] HEGRA[18] CASA-BLANCA[19] KASCADE[20] fixed target HERA RHIC TEVATRON LHC

6 Ultra high energy cosmic rays (UHECRs) galactic? extragalactic? p He knee 1 C,O, Fe knee 2 GZK cutoff E -2.7 ankle ultra high energy cosmic rays (Nagano & Watson 2000)

7 Experiments to study UHECRs The High Resolution Fly s Eye (HiRes) fluorescence detectors, collected the record exposure, close to the AGASA exposure (3000 km 2 sr year), for the highest energy events (E>10 20 ev). HiRes 1 HiRes 2

8 Akeno Giant Air Shower Array (AGASA) array of surface detectors of EAS in Japan collected the record exposure of about 3000 km 2 sr year 111 scintillators + 27 muon detors

9 P. Auger Observatory (Auger) the Southern Observatory in Argentina km2 - surface detector array: 1,600 water Cherenkov thanks, 1.5 km grid - 4 fluorescence detectors: total of 24 telescopes each with 300x300 FoV 65 km the Northern Observatory planed in Colorado, USA Korean Numerical Astrophysics Group Meeting October 23, 2009

10 Telescope Array (TA) in Utah, USA - surface detector array: 500 scintillators - 3 fluorescence detectors

11 TA led by Japan and USA, Korea and Russia participate in it fluorescence detector station scintillation detectors

12 JEM-EUSO (Extreme Universe Space Observatory) - wide field of view (FOV) fluorescence detector from the space - future project, led by Japan, several countries including Korea participate in it

13 Comparison of the experiments

14 Issues of UHECRs to be addressed - energy spectrum? - composition? - sources? <- correlation with astronomical objects - etc

15 GZK cutoff Yakutsk yes, Agasa no, HiRes yes, Auger - yes (Hires 2008) Berezinsky 2009) (Auger 2009) However, fluxes are different by up to factor of a few in different experiments!

16 Issues of UHECRs to be addressed - energy spectrum? - composition? - sources? <- correlation with astronomical objects - etc

17 Composition of UHECRs now a key for the problem of UHECRs Auger tries to argue that UHECRs are mostly heavy! (Auger 2009) Hires still insists that UHECRs are mostly protons.

18 Issues of UHECRs to be addressed - energy spectrum? - composition? - sources? <- correlation with astronomical objects - etc

19 Anisotropy and Correlation with the LSS of the Universe (Auger 2007) in galactic coordinate (l,b) Cen A M87 supergalactic plane Fornax A 27 events with E > 57 EeV AGNs with z < Strong positional correlation between 27 UHECRs > 57 EeV and AGNs as tracers of matter in the Local universe within 75 Mpc for a search window S (angular separation) < 3.1 o.

20 Now with 58 UHECRs with > 55 EeV (energy has been re-constructed) studied the correlation with AGNs within 75 Mpc. for a search window S (angular separation) < 3.1 o. (Auger 2009) The signature of the correlation has weakened, but there a is statistically significant correlation.

21 Studied the correlation between 58 UHECRs with > 55 EeV and astronomical objects in different catalogs. Blue isotropic Red - model Black - data (Auger 2009) Also found statistically significant correlations.

22 (Hires 2008) M87 Cen A in galactic coordinate (l,b) 457 AGN, 14 QSO 2 correlated events 11 uncorrelated events E > 56.0 EeV, z < 0.018, θ < 3. 1 o Expect 3.2 correlated events for random distribution No evidence for correlation

23 Agasa small scale clustering with > 40 EeV HiRes null clustering Auger weak excess of pairs for > 57 EeV or 55 EeV Yakutsk correlation with AGNs unknown but maybe no HiRes no correlation with AGNs Aguer significant correlation with AGNs HiRes correlation with BL Lac objects Auger correlation with astronomical objects in various catalogs

24 Do arrival directions of UHECRs point sources? Probably not! Milky Way Galactic B - disk: 5-10 µg - halo: < 1 µg? Larmor radius: 1 kpc E B 1 ( )( ) 18 r L Z 10 ev 1 µ G for Super-GZK protons, weak deflection (~10 o ) & R GZK ~ 100Mpc anisotropic arrival direction observer source Source intergalactic space intergalactic B - clusters: 1-10 µg - filaments: ~ 10-8 G - voids: <~ G below ~ ev, strong deflection & R >100 Mpc and larger isotropic arrival direction

25 What is the signatures of the local LSS that are imprinted in arrival directions of UHECRs? (Das, Kang, Ryu, Cho 2008; Ryu, Das, Kang 2009 submitted) To address the question, we calculate in a model universe 1. <S> = angular distance btw a CR event & its nearest source <θ> = angular distance btw a CR event & its true source (deflection angle) <- a model for the IGMF in the LSS & simulations for the propagation of UHECRs 2. <Q> = angular distance between sources <- hypothetical distributions of sources and observers 1) large scale structure formation simulation for sources and observers 2) turbulence dynamo model for B 3) propagation of UHECR protons

26 Statistics of angular separations S = angular separation to the nearest object = angular distance between the nearest source direction and the CR arrival direction θ = deflection angle = angle distance between the source direction and the CR arrival direction D θ true source S and D s are calculable from observed events, but θ and D θ are not! observer θ S nearest object D S wrong identification! arrival direction of a UHECR

27 What is the signatures of the local LSS that are imprinted in arrival directions of UHECRs? (Das, Kang, Ryu, Cho 2008; Ryu, Das, Kang 2009 submitted) To address the question, we calculate in a model universe 1. <S> = angular distance btw a CR event & its nearest source <θ> = angular distance btw a CR event & its true source (deflection angle) <- a model for the IGMF in the LSS & simulations for the propagation of UHECRs 2. <Q> = angular distance between sources <- hypothetical distributions of sources and observers 1) large scale structure formation simulation for sources and observers 2) turbulence dynamo model for B 3) propagation of UHECR protons

28 isotropic distribution of sources Q= angular distance to nearest neighbor Q N obj for Q N iso obj πq 11 2 iso = 442, o = 4π non-isotropic distribution (LSS) Q Q Q AGN AGN 442 = Q i= 1 = 3.55 i o / N AGN for 442 AGNs in the VC catalog - Q decreases with N AGN & the degree of anisotropy of the source distribution. - It is an intrinsic property of the source distribution (nothing to do with CRs)

29 What is the signatures of the local LSS that are imprinted in arrival directions of UHECRs? (Das, Kang, Ryu, Cho 2008; Ryu, Das, Kang 2009 submitted) To address the question, we calculate in a model universe 1. <S> = angular distance btw a CR event & its nearest source <θ> = angular distance btw a CR event & its true source (deflection angle) <- a model for the IGMF in the LSS & simulations for the propagation of UHECRs 2. <Q> = angular distance between sources <- hypothetical distributions of sources and observers 1) large scale structure formation simulation for sources and observers 2) turbulence dynamo model for B 3) propagation of UHECR protons

30 Numerical simulation of structure formation of the universe - Λ cold dark matter cosmology (Ryu, Kang et al 2003, 2005, ApJ) Ω Λ = 0.73, Ω DM = 0.27, Ω gas = 0.043, h = 0.7, n = 1, σ 8 = computational box: (143 Mpc) 3 : grid-based Eulerian TVD code cells for gas and gravity, DM particles - with passively evolving B field: B=0 initially, generated at shocks via Biermann Battery and amplified by flow motions, growth is limited by x X-ray emissivity magnetized cosmic web gas temperature ε = erg cm -3 s -1 and higher T = K and higher

31 sources: - AGNs-like sources that trace the large scale structure of the universe - on average about 500 sources in (75 Mpc) 3 volume observers: - inside groups of galaxies like our Local Group - about 1350 observers in simulation box sources Q=angular distance to nearest neighbor each observer sees about 500 sources Q Q sim sim N 1 o N observer source = 3.68 observer ~ j Q N AGN i N Q 3.55 j, i source that is, the source distribution in our simulation is similar to the distribution of AGNs in the V-C catalog o observers (100 h -1 Mpc) 3

32 Intergalactic magnetic field (IGMF) (Ryu, Kang, Das et al 2008, Science) In our model = (B x, B y, B z ) - vorticity (ω) & E turb of local flows magnitude of B based on a turbulence dynamo model - passively evolved B field directional information magnetized cosmic web E B 2 B = = φ( ω t) 8π Ε turb conversion factor from MHD turbulence simulations no fine tuning to normalize B! G G 10-5 G

33 resulting averaged magnetic field strength in the largescale structure of the universe at z = 0 - inside clusters <B> ~ a few µg - around clusters (T > 10 7 K) <B> ~ 0.1 µg - in filaments (10 5 K < T < 10 7 K, or WHIM) <B> ~ 10 ng distribution of the intergalactic magnetic field in a (~18x27 Mpc) 2 2D slice

34 Faraday rotational measure (RM) due to our model IGMF (Akahiro, Ryu 2009, in prep.) our model IGMF predicts 50 h -1 Mpc - RM >~ 100 rad m -2 through clusters - RM ~ a few rad m -2 intersecting filaments -consistent with observations: Clarke et al Xu et al h -1 Mpc

35 Simulation of the propagation of UHE protons - protons were injected at sources ( ) γ E E N inj 19 for 6 10 ev E 10 with γ = 2.0, 2.4, 2.7 ev - propagation was followed by solving the equation of motion + energy losses (photo-pion, photo-pair on CMB) - events with E >= 60 EeV were registered at observers 21 observer source G G 10-5 G

36 trajectories of UHE protons through the IGMF if source and observer are in different filaments, rectilinear flight across voids small deflection angle If source and observer are in the same filaments, deflected flight along the filament large deflection angle even for close sources

37 S = angular separation to the nearest object θ = deflection angle (angular separation to the true source) for events with E >= 60 EeV for events with E >= 60 EeV mean median quartile <S> sim ~3.6 o <θ> sim ~ 14 o ~ 3 x <S> sim S median ~ 2.8 o θ median ~ 7 o ~ 2.5 x S median The large diffraction (<θ> sim ~ 14 o ) due to the IGMF does not spoil the correlation between the UHECR events and the LSS of the universe (<S> sim ~3.6 o ), because the IGMF itself is correlated with the LSS of the Universe! <θ> due to the Galactic field ~ 3.5 o (BBS-S model) << <θ> due to the IGMF

38 S = angular separation to the nearest object S vs D s for events with E >= 60 EeV 27 Auger events mean median quartile -<S> sim ~ 3.6 o, while <S> Auger ~ 3.23 o (one outliner excluded) - S median ~ 2.8 o from simulation, while ~2.4 o (?) for Auger - 15 out of 27 Auger events are within quartile marks

39 S = angular separation to the nearest object θ = deflection angle (angular separation to the true source) AGNs = source candidates CR event true source θ S nearest object S Auger ~ Q AGN = 3.55 o and S sim ~ Q sim = 3.68 o that is, S sim ~ S Auger ~ Q sim ~ Q AGN both AGNs and UHECRs follow the matter distribution of the local LSS

40 large deflection angle, <θ> ~ 14 o, do we still expect anisotropy & correlation with the LSS of the univese? S z observer sources of UHECRs in the Local supercluster scattering centers = irregularities of B field that scatter particles S x S y Local supercluster suppose - all sources of UHECRs reside inside the Local supercluster - there are strong turbulent magnetic fields in the Local supercluster - there are no source of CRs and no IGMFs in the void region then - the arrival directions of UHECRs would not be isotropic - instead, they should exhibit some correlation with the Local supercluster - but their arrival directions do not point their individual sources

41 the number of events for which the nearest object is the true source f = the total number of events f = probability of successful identification of sources, when the nearest AGNs are regarded as the true sources. If AGNs are the sources of UHE protons, the fraction of the closest AGNs to be the true sources in the Auger data could be small, ~1/3! CR event nearest = true nearest true angular separation to the nearest object

42 Main results - The deflection angles of UHECRs, that is, the angular distances between the directions of UHECRs and their true sources, are quite large with <θ> ~ 14 o and θ median ~ 7 o. -Nevertheless, the separation angles between the directions of UHECRs and the nearest AGNs are substantially smaller with <S> ~ 3.6 o, which is consistent with that from the recent Auger data, <S> sim ~ <S> Auger. Note that our simulation predicts <S> ~ (1/4) <θ>. - Even with large θ, the arrival directions of UHECRs with E>~ 60 EeV are anisotropic and correlated with the LSS of the Universe. - In addition, <S> sim ~ <S> Auger ~ <Q> sim ~ <Q> ANG. It means that S does not carry the information of θ, but the information of Q, that is, the distribution of AGNs. - The above implies that the AGNs found closest to the direction of UHECRs are not necessary the true sources of UHECRs. In our simulations, the fraction that the closest AGNs are to be the true sources of UHECRs is only <f> ~ 0.3.

43 Kolmogorov-Smirnov test between Auger data and our simulation all 500 AGN-like objects within 75 Mpc are assumed to be the sources of UHECRs 28 out of 500 AGN-like objects within 75 Mpc are assumed to be the sources of UHECRs D -> maximum difference P -> significance level - Null hypothesis: the two distribution is statistically identical. For left, with p ~0.37, the null hypothesis cannot be rejected. - The model with a larger number of sources is preferred.

44 trajectories of UHE protons through the IGMF if source and observer are in different filaments, rectilinear flight across voids small deflection angle If source and observer are in the same filaments, deflected flight along the filament large deflection angle even for close sources

45 number of sources within 75 Mpc U-shape with a minimum <- clear signature of the LSS of the universe. 500

46 Supplemental results - The model with a larger number of sources is preferred. - The U-shape distribution with a minimum of S (also q) is expected. <- clear signature of the LSS of the universe.

47 r g ( E/60 EeV) Mpc Z ( B /10 G) 6 8 1/ 2 Z B D l θ 4 8 c ( E/60 EeV) 10 G 10Mpc 100kpc 1/ 2 - heavies nuclei have larger θ - how about S? photodisintegration is not included. D<100 Mpc

48 A model with - a few nearby sources - heavy nuclei injected at sources - our IGMF -> will it work?

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