The Most Energetic Particles in Nature

Transcription

1 ASIAA/CCMS/IAMS/LeCosPA/NTU-Phys Joint Colloquium, April 7, 2015 The Most Energetic Particles in Nature Karl-Heinz Kampert University of Wuppertal Area Grant Karl-Heinz Kampert Taipei Colloq,

2 Karl-Heinz Kampert University Wuppertal Taipei Colloq, Energy Spectrum of Cosmic Rays log(flux) 32 orders of magn. 1 event per m 2 and sec Knee (1 per m 2 -year) 32 orders of magnitude: hair Universe γ ankle (1 per km 2 -year) log(energy/ev)

3 Karl-Heinz Kampert University Wuppertal Taipei Colloq, Satellite 1 event per m 2 and sec <1 m 2 log(flux) 32 orders of magn. Knee (1 per m 2 -year) Balloons <5 m 2 Air Shower Exps 0.1 km 2 γ ankle (1 per km 2 -year) 3000 km 2 log(energy/ev)

4 Key Questions about Ultra High-Energy Cosmic Rays Where do they come from? What are they made of? How do their accelerators work? Is there a maximum limit to their energy? What can they tell us about fundamental and particle physics? Karl-Heinz Kampert 4 Taipei Colloq,

5 Features of CR spectrum sr -1 ev 1.5 ) J(E) (m -2 sec courtesy R. Engel ATIC PROTON RUNJOB Equivalent c.m. energy 3 4 s pp KASCADE (QGSJET 01) KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Tibet ASg (SIBYLL 2.1) (GeV) 5 HiRes-MIA Image of non-thermal Universe ~E -2.7 Knee ~E -3.1 HiRes I HiRes II Auger SD Scaled flux E HERA (e-p) RHIC (p-p) Tevatron (p-p) LHC (p-p) Ankle GZK? Particle Energy (ev) Karl-Heinz Kampert University Wuppertal 5 Taipei Colloq,

6 Features of CR spectrum sr -1 ev 1.5 ) courtesy R. Engel ATIC PROTON Equivalent c.m. energy 3 Galactic CRs? RUNJOB 4 s pp (GeV) 5 KASCADE (QGSJET Diffusion 01) losses HiRes-MIA from Galaxis? HiRes I KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Tibet ASg (SIBYLL 2.1) HiRes II Auger SD J(E) (m -2 sec Scaled flux E SNR? SNR? p,he-knee HERA (e-p) magn. confinement RHIC (p-p) Emax ~ Z p Tevatron (p-p) Fe-knee p... LHC (p-p) Extragal. CRs? classical ankle model Fe extragal. component AGN? Particle Energy (ev) Karl-Heinz Kampert University Wuppertal 6 Taipei Colloq,

7 Features of CR spectrum J(E) (m -2 sec -1 sr -1 ev 1.5 ) 2.5 Scaled flux E courtesy R. Engel 13 ATIC PROTON RUNJOB SNR? SNR? Equivalent c.m. energy 14 3 Galactic CRs? p,he-knee HERA (e-p) magn. confinement RHIC (p-p) Emax ~ Z Tevatron (p-p) LHC (p-p) 17 s pp KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Tibet ASg (SIBYLL 2.1) Particle Energy (ev) (GeV) 18 5 KASCADE (QGSJET Diffusion 01) losses HiRes-MIA from Galaxis? HiRes I p Fe Fe-knee extragal. component HiRes II Auger SD Extragal. CRs?? AGN? Karl-Heinz Kampert University Wuppertal 7 Taipei Colloq,

8 20 ev CRs in our Galaxy? Lamor radii at 20 ev compared to Milky-Way E 18 Z B µg R kpc Size B-Field needs to be very large Interesting feature: Can do astronomy with cosmic rays! Conjecture: Extragalactic origin Karl-Heinz Kampert University Wuppertal 8 Taipei Colloq,

9 UHECR Astronomy Cosmic Magnetic Fields R L = kpc Z -1 (E / EeV) (B / μg) -1 R L = Mpc Z -1 (E / EeV) (B / ng) -1 γ, ν weak deflection E > 19 ev Halo B? strong deflection E < 18 ev Milky way B ~ μg (E,Z) 0.8 Extra-galactic B < ng? 20 ev L L coh E Mpc 1 Mpc B Z 1 ng Karl-Heinz Kampert University Wuppertal Taipei Colloq,

10 Potential Sources of 20 ev particles GRB 12 GRB? Neutron Stars E max ~ β s z B L Active Galactic Nuclei (AGN) LHC SNR Magnetic Fieldstrength (Gauß) Karl-Heinz Kampert University Wuppertal LHC white dwarfts Interplanetary Space Hillas Diagramm 1AU Galact. Active Galactic Nuclei? SNR Size 20 ev proton disk halo jets from radio galaxies 1km 6 km 1pc 1kpc 1Mpc Realistic constraints more severe small acceleration efficiency synchrotron & adiabatic losses interactions in source region { Fe Galactic Clusters IGM AGN-Jets Colliding Galaxies Taipei Colloq,

11 Radio Images of Cosmic Accelerators Cas A (3.4 kpc) Supernova Remnants E < 16 ev Cygnus A (250 Mpc) Accreting Supermassive Black Holes E ~ 20 ev? NRAO/AUI 1.4, 5, & 8.4 GHz Fornax A (20 Mpc) Karl-Heinz Kampert University Wuppertal Taipei Colloq,

12 The Cosmic Zevatron sr -1 ev 1.5 ) J(E) (m -2 sec Scaled flux E courtesy R. Engel ATIC PROTON RUNJOB ev protons in LHC would require size of Earth orbit around Sun LHC p-energy SNR? HERA (e-p) RHIC (p-p) Equivalent c.m. energy How s pp much (GeV) would LHC need to grow to accelerate 20 ev? Tevatron (p-p) KASCADE (QGSJET 01) KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Tibet ASg (SIBYLL 2.1) LHC (p-p) HiRes-MIA HiRes I HiRes II Auger SD Particle Energy (ev) Karl-Heinz Kampert University Wuppertal 12 Taipei Colloq,

13 1962: The First 20 ev Event VOLUME, NUMBER 4 PHYSICAL RK VIEW LKTTKRS 15 I'EBRUARY 196) EVIDENCE FOR A PRIMARY COSMIC-HAY PARTICLE WITH ENERGY John Linsley Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts (Received January 1963) ev~ Extensive Air Shower Volcano Ranch Air Shower Array, New Mexico Karl-Heinz Kampert University Wuppertal detector array 13 Taipei Colloq,

14 1962: The First 20 ev Event VOLUME, NUMBER 4 PHYSICAL RK VIEW LKTTKRS 15 I'EBRUARY 196) EVIDENCE FOR A PRIMARY COSMIC-HAY PARTICLE WITH ENERGY John Linsley Laboratory for Nuclear Science, Massachusetts Institute of Technology, Cambridge, Massachusetts (Received January 1963) ev~ particle densities 0.6 Volcano Ranch Air Shower Array, New Mexico Karl-Heinz Kampert University Wuppertal 15 KlLOMETERS Taipei Colloq,

15 1965: Discovery of CMB 1978 G. Gamow Penzias & Wilson 4.08 GHz (7.35 cm) Karl-Heinz Kampert University Wuppertal 16 Taipei Colloq,

16 1966: End to the CR Spectrum? Greisen, Zatsepin & Kuz min Linsley s event Karl-Heinz Kampert University Wuppertal 17 Taipei Colloq,

17 GZK-effect: Rapid Energy Loss of p & nuclei in CMB p CMB p π photo-pion production p + CMB!! p + 0 CMB 4 A Photopair, p Expansion photo disintegration A + CMB! (A Greisen-Zatsepin-Kuz min (1966) threshold: E p E γ > (m Δ 2 - m p 2) E GZK 6 19 ev GZK-Horizon ~ 60 Mpc 1) + n... Karl-Heinz Kampert University Wuppertal 18 Taipei Colloq, Energy Loss Pathlength (Mpc) CMBR z = 0 Total, p Photopion, p Energy (ev) Photopion, Fe Photopair, Fe Photodisintegration, Fe

18 The GZK - Horizon Expect anisotropies for protons at E> 19 ev Karl-Heinz Kampert University Wuppertal Taipei Colloq,

19 Situation ~8 years ago Experiments: AGASA, HiRes, Haverah Park, Yakutsk, SUGAR does the GZK-suppression exist? - Flux data contradictory AGASA no suppression HiRes possibly a suppression Composition mostly protons Apparent isotropy Apparent continuation of spectrum in AGASA gave birth to exotic source and propagation scenarios Top Down Models - Topological Defects, Super-Heavy Dark Matter Particles, WIMPzillas, Cryptons,... Z-Burst Model massive neutrinos Energy (ev/particle) expect EHE γ s and ν s Karl-Heinz Kampert University Wuppertal 20 Taipei Colloq, ) 1.5 sec -1 sr -1 ev -2 J(E) (m 2.5 Scaled flux E ATIC HERA (γ-p) RHIC (p-p) PROTON RUNJOB 14 Equivalent c.m. energy 3 Tevatron (p-p) s pp KASCADE (QGSJET 01) KASCADE (SIBYLL 2.1) KASCADE-Grande (prel.) Akeno LHC (p-p) 18 (GeV) 5 19 HiRes-MIA HiRes I HiRes II AGASA HIRES 20 6 AGASA

20 A New Generation: Hybrid Observation of EAS Concept pioneered by the Pierre Auger Collaboration (Fully operational since 06/2008) (Concept employed also by Telescope Array (TA)) Pioneer of FD and first detection: Tanahashi, INS-Tokyo 1958, 1969 light trace at night-sky (calorimetric) Kampert & Watson, EPJ H37 (2012) 359 Fluorescence light Also: Detection of Radio- & Microwave-Signals Karl-Heinz Kampert University Wuppertal Particle-density and -composition at ground 21 Taipei Colloq,

21 Pierre Auger Observatory ~65 km Loma Amarilla HEAT Coihueco 3000 km 2 BLS XLF CLF ~65 km 1660 detector stations on 1.5 km grid Los Morados 27 fluores. telescopes at periphery Los Leones Province Mendoza, Argentina 160 radio antennas Karl-Heinz Kampert University Wuppertal 22 Taipei Colloq,

22 A R G E N T I N A SANTIAGO Pampa Amarilla Province of Mendoza 1400 m a.s.l. 35 South, 69 West 3000 km 2 Karl-Heinz Kampert Taipei Colloq,

23 Water Cherenkov Station stations in total Karl-Heinz Kampert 24 Taipei Colloq,

24 Water Cherenkov Station GPS electronics local trigger 40 MHz digit. W communication ISM band (0.9 GHz) stations in total battery solar panel Three 9 PMT XP ltr water Karl-Heinz Kampert 25 Taipei Colloq,

25 Karl-Heinz Kampert 26 Taipei Colloq,

26 Auger Hybrid Observatory Google maps Karl-Heinz Kampert 27 Taipei Colloq,

27 24 telescopes (6 per site) 12 m 2 mirrors, Schmidt optics 30 x30 deg field of view 440 PMTs/camera MHz FADC readout 2.2 m opt. Filter (MUG-6) UV optical filter Camera with 440 PMTs Karl-Heinz Kampert 28 Taipei Colloq,

28 nchargedrz01.mov K.-H. Kampert, Univ. Wuppertal 29

29 Central Campus Visitors are welcome (almost visitors already) Karl-Heinz Kampert 30 Taipei Colloq,

30 14 telescopes TA detector in Utah 39.3 N, W ~1400 m a.s.l. Refurbished HiRes Middle Drum (MD) 3 com. towers Surface Detector (SD) 507 plastic scintillator SDs 1.2 km spacing ~700 km 2 CLF Long Ridge (LR) ELS Fluorescence Detector(FD) 3 stations 38 telescopes 12 telescopes 12 telescopes Black Rock Mesa (BR) 2014/3/20 H. VHEPA2014 FD and SD: fully operational since 2008/May Karl-Heinz Kampert 31 Taipei Colloq,

31 Auger and TA Telescope Array (TA) Delta, UT, USA 507 detector stations, 680 km 2 36 fluorescence telescopes same scale i h km 2 yr Auger and TA can see the same sky Auger: 01/ /2012 TA: 05/ / Auger vertical + inclined Auger vertical (01/ /2012) Auger inclined (01/ /2012) TA (05/ /2012) Auger e(d) TA d [ ] Pierre Auger Observatory Province Mendoza, Argentina 1660 detector stations, 3000 km 2 27 fluorescence telescopes Auger exposure ~ times that of TA Karl-Heinz Kampert University Wuppertal 32 Taipei Colloq,

32 Event Example in Auger Observatory OBSERVATORY 12 km ~ 20 km Karl-Heinz Kampert University Wuppertal 33 Taipei Colloq,

33 Event Example in Auger Observatory OBSERVATORY energy determination based solely on experimental observables! Use events that were independently rec High quality selection incl. fiducial field o Resolutions compared to Monte-Carlo s Physical shower-to-shower fluctuations Cross Correlation Sampling fluctuations: 15% (< 12%), E 1475 events highest energy event: 8 19 ev de/dx (PeV/g cm 2 ) Longitudinal Profile E = 68 EeV X max =770 g/cm Slant Depth (g cm 2 ) ~ 20 km 12 km S38 /VEM Signal (VEM) S(00) E FD /ev (Maximum-likelihood fit, 1475 events) Lateral Profile Fit ±1 s S(00)=222 VEM θ = 54 S38=343 VEM E = 71 EeV Distance to Shower Core (m) Karl-Heinz Kampert University Wuppertal 34 Taipei Colloq,

34 Auger Combined E-Spectrum (0-80 ) Update from: PRL 1, 0611 (2008), Physics Letters B 685 (20) events E [ev ] Auger 2013 preliminary E 3 J( E ) ev 2 km 2 sr 1 yr γ1=3.23±0.07 * * Eankle=5 18 ev γ2=2.63±0.04 E50% = 4 19 ev apple Is J(E;E this > E a the ) µ E g GZK-effect... log E log 2 E 1/2 1 + exp? log W c g g log ( E /ev ) OBSERVATORY Karl-Heinz Kampert University Wuppertal 35 Taipei Colloq,

35 GZK-Effect or Exhausted Sources? E [ev ] GZK- effect E 3 J(E)[eV 2 km -2 sr -1 yr -1 ] E 3 J( E ) ev 2 km 2 sr 1 yr 1 Proton, E cut = 20 ev Proton, E cut = 20.5 ev Iron, E cut = 20 ev Iron, E cut = 20.5 ev Karl-Heinz Kampert University Wuppertal g g E [ev] p-sources J(E;E > E a ) µ E g 2 Fe-sources log (E/eV) E/E = 14 % log ( E /ev ) Auger 2013 preliminary 45 7 apple log E log E 1 1/2 1 + exp log W c sr -1 yr -1 ] -2 km 2 J [ev 3 E EZ max p 3 1 exhausted sources / Z E max p Allard et al He log (E/eV) 36 Taipei Colloq, N Fe

36 Longitudinal Shower Development Primary Mass KHK, Unger, APP 35 (2012) EPOS 1.99 Simulations Example of a 3 19 ev EAS event in FD )] 2 energy deposit [PeV/(g/cm 50 Auger event OBSERVATORY photon proton iron slant depth [g/cm 2 ] Karl-Heinz Kampert University Wuppertal 37 Taipei Colloq,

37 Decomposition of Xmax-Distributions Auger collaboration, Phys. Rev. D 90, (2014) p fraction He fraction N fraction Fe fraction Sibyll 2.1 QGSJET II-4 EPOS-LHC we seem to see the exhaustion of sources! p N He suppression region E [ev] Fe???? Karl-Heinz Kampert University Wuppertal 38 Taipei Colloq,

38 Cosmogenic Neutrinos and Photons Smoking Gun of GZK-effect a guaranteed signal in presence of GZK p + CMB!!! n + +! EeV! p + 0! EeV -4 p, best fit with Fermi-LAT bound (Ahlers) KHK, Unger, APP 35 (2012) s -1 sr -1 ] -2 dn/de [ GeV cm 2 E p, FRII & SFR, E = max 20 Fe, FRII & SFR, E max =26 x ev (B. Sarkar) ev (B. Sarkar) p & mixed, SFR & GRB, E =Z x - max GZK-Fe GZK-p ev (Kotera) TopDown models GZK-p GZK-Fe c?on+in+eev+range+may+provide+complementary+informa?on+to+direct+u Karl-Heinz Kampert University Wuppertal E ν [ev] Taipei Colloq,

39 Absence of Photons TopDown ruled out Update from: Astropart. Phys. 31 (2009) 399; ICRC2015 sr -1 y -1 ] -2 [km 0 Integral Flux E>E Y top down models Hyb 2009 upper limits 95% C.L. Y A Hyb 2011 TA A SHDM SHDM' TD Z-burst GZK OBSERVATORY -3 GZK SD SD photon upper limits 2 orders of magnitude improvement during last years! Energy[eV] Photon upper limits rule out Top-Down Models and start to constrain GZK-expectatinons Karl-Heinz Kampert University Wuppertal 40 Taipei Colloq,

40 Inclined+showers+ Search for EeV Neutrinos &+UHE+neutrinos+ in inclined showers Protons+&+nuclei+ini?ate+showers+ high+in+the+atmosphere.++ Shower+front+at+ground:++ mainly+composed+of+muons+ electromagne?c+component+ absorbed+in+atmosphere.+ Neutrinos+can+ini?ate+ deep + showers+close+to+ground.+ Shower+front+at+ground:+ electromagne?c+++muonic+ components+ Searching+for+neutrinos+ + searching+for+inclined+showers+ +with+electromagne?c+component+ ν τ$ 6+ Karl-Heinz Kampert 41 Taipei Colloq,

41 Upper Limits on Neutrinos Single flavour, 90% C.L. -5 IceCube 2013 (x 1/3) [30] ] sr -1-6 Auger (this work) ANITA-II 20 (x 1/3) [29] Auger Collaboration, subm. to PRD 2015 Cosmogenic ν models p, Fermi-LAT best-fit (Ahlers ') [33] p, Fermi-LAT 99% CL band (Ahlers ') [33] p, FRII & SFR (Kampert '12) [31] -2 s -1 dn/de [ GeV cm 2 E Waxman-Bahcall '01 [13] E ν [ev] Neutrino upper limits start to constrain cosmogenic IceCube 2013 neutrino (x 1/3) [30] Cosmogenic fluxes ν modelsof p-sources Karl-Heinz Kampert University Wuppertal Auger (this work) Fe, FRII & SFR (Kampert '12) [31] 42 Taipei Colloq,

42 Upper Limits on Neutrinos Single flavour, 90% C.L. -5 IceCube 2013 (x 1/3) [30] Cosmogenic ν models Auger Collaboration, subm. to PRD 2015 Auger (this work) Fe, FRII & SFR (Kampert '12) [31] ] sr -1-6 ANITA-II 20 (x 1/3) [29] p or mixed, SFR & GRB (Kotera ') [9] -2 s -1 Waxman-Bahcall '01 [13] dn/de [ GeV cm -7-8 E 2-9 Karl-Heinz Kampert University Wuppertal E ν [ev] FigureNeutrino 4. Top panel: upper Upper limits limit start (at 90% still C.L.) above to the normalization of the di use flux of UHE neutrinos as given in Eqs. cosmogenic (2) and (3), neutrino from the Pierre fluxes Auger for Fe-sources Observatory. We 43 Taipei Colloq,

43 UHECR Sky surprisingly isotropic E [ev ] E 3 J( E ) ev 2 km 2 sr 1 yr 1 Auger 2013 preliminary J(E; E > Ea ) µ E g g 18.0 g2 log E log E1/2 1 + exp log Wc log ( E /ev ) hot/warm spot 20.5 Feain et al., ApJ 740 (2011) 17 E>57 Cen A TA: ApJ 790:L21 (2014) dipole like anisotropy E>8 EeV EeV TA (5σ pre-trial) (3.4σ post-trial)? 29 Auger Collaboration ApJ (2015) in press Amplitude: (4.4±1.0)%; p=6.4-5 Karl-Heinz Kampert University Wuppertal 19.5 Auger: APP 34(20) Auger (3σ pre-trial) Taipei Colloq,

44 Weak excess of events around Cen A giant lobes ~ 280 kpc physical age ~ 560 Myr distance ~ 3.8 Mpc E > 58 EeV fmin=2e-4, out to 15 there are 14 events, 4.5 expected, P=1.4% Number of events events E>58 observed EeV expect 4.5 p=1.5% 15 68% isotropic 95% isotropic 99.7% isotropic data moon Angular distance from Cen A [deg] Auger ; ApJ (2015) in press Feain et al., ApJ 740 (2011) 17 Karl-Heinz Kampert University Wuppertal 45 Taipei Colloq,

45 Résumé Data from the Auger Observatory indicate that the flux suppression is mostly due to seeing the exhaustion of the sources: 1) change towards a heavier composition 2) constraints on GZK photons and neutrinos 3) highly isotropic sky Magnetic Fieldstrength (Gauß) Neutron Stars LHC GRB? white dwarfts Interplanetary Space 1AU Galact. Active Galactic Nuclei? SNR Size 20 ev proton disk halo jets from radio galaxies 1km 6 km 1pc 1kpc 1Mpc { E max ~ β s z B L Galactic Clusters Logical next step: Measure composition event-by-event into the flux suppression region composition becoming increasingly heavier? enable composition enhanced anisotropy studies do particle physics at s 0 TeV Fe IGM Karl-Heinz Kampert University Wuppertal 46 Taipei Colloq,

46 UHECR: Near Future Auger upgrade: mass composition with ground array TA upgrade: area * 4 s als uild origin of the flux suppression 29 hadronic interactions beyond LHC more rapid increase of statistics Karl-Heinz Kampert University Wuppertal 47 Taipei Colloq,

47 UHECR: Long Term Plan Global Cosmic Ray Observatory (GCOS) few sites in N+S, km 2 感谢您的关注! Karl-Heinz Kampert University Wuppertal 48 Taipei Colloq,

48 Bounds on LIV and Smoothness of Class. Space-Time Klinkhamer/Risse; PRD77 (2008) ; ; Klinkhamer, AIP Conf.Proc.977: ,2008 Observation of 20 ev events proofs absence of Vacuum Cherenkov-Radiation Provides limits on smoothness of space & LIV-effects Conservative limit on any small-scale structure of space: LEP/LHC: -19 m c/(1 TeV). Use published 27 Auger events + 1 AGASA + 1 Fly s-eye single scale classical space-time foam at UHECRs: b -26 m c/(2 GeV) by far best (3 to 8 orders of magn.!) existing bounds of Standard Model Extension parameters of nonbirefringent modified Maxwell theory Results complemented by TeV γ-rays Conjecture: fundamental length scale of quantum space time may be different from Planck length and may be linked to cosmological constant Karl-Heinz Kampert University Wuppertal 49 Taipei Colloq,

49 p-air Cross-Section from Xmax distribution top of atmosphere ΔX1 X1: point of 1st interaction Data: 18 ev < E < 18.5 ev Λ f = g/cm ΔXmax ΔX1 dp dx 1 = 1 int e X 1/ int /g] 2 dn/dx max [cm 1 Λ int X max [g/cm 2 ] Difficulties: mass composition can alter Λ fluctuations in Xmax experimental resolution ~ 20 g/cm 2 p Air = hm Airi int In practice: σp-air by tuning models to describe Λ seen in data Karl-Heinz Kampert University Wuppertal 50 Taipei Colloq,

50 p-air and pp Cross s=57 TeV Equivalent c.m. energy -1 1 s pp [TeV] 2 Cross section (proton-air) [mb] log Energy (Energy/eV) [ev] 0 inel Nam et al Siohan et al Baltrusaitis et al Mielke et al Honda et al Knurenko et al ICRC07 HiRes Aglietta et al Aielli et al This work Karl-Heinz Kampert University Wuppertal 0.9TeV 2.36TeV 7TeV 14TeV LHC σp-air= (505 ± 22stat ( +26 )sys ) mb 34 QGSJet01c QGSJetII.3 Sibyll 2.1 Epos 1.99 σpp = [92 ± 7stat ( +9 )sys ± 7.0Glauber] mb tot prod 11 σpp = [133 ± 13stat ( +17 )sys ± 16Glauber] mb 20 (Proton-Proton) [mb] σ inel OBSERVATORY Conversion from p-air to p-p cross section by Glauber-approach Auger Collaboration, PRL 9, (2012) ATLAS 2011 CMS 2011 ALICE 2011 TOTEM 2011 UA5 CDF/E7 Auger ICRC LHC s [GeV] 4 Auger QGSJet01 QGSJetII.3 Sibyll2.1 Epos1.99 Pythia Phojet [ ] 51 Taipei Colloq, OBSERVATORY

51 Interaction Models lack Muons in EAS Auger Collaboration, Phys. Rev. D 91, (2015); editors suggestion log Nµ EPOS LCH QGSJet II-04 QGSJet II-03 QGSJet01 E = 19 ev, θ = 67 Auger data Fe 7.2 N He p X max /g cm 2 EPOS LHC QGSJet II-04 QGSJet II-03 QGSJet01 Auger data lnr µ ( 19 ev ) ± (sys. ) Fe ± ln A ± (sys. ) p Fe ± ln A ± (sys. ) p Fe ± ln A ± (sys. ) p Fe ± ln A ± (sys. ) p µ-deficit points to deficiencies of hadronic interaction models LHC forward physics program highly relevant joint efforts by people from both communities Karl-Heinz Kampert University Wuppertal 52 Taipei Colloq,