Ultra-High Energy Cosmic Rays: an Experimental Overview and extension plans

Transcription

1 Solvay-Francqui Workshop on Neutrinos: from reactors to the cosmos Ultra-High Energy Cosmic Rays: an Experimental Overview and extension plans Karl-Heinz Kampert University of Wuppertal Brussels, May 27-29, 2015 Karl-Heinz Kampert - Univ. Wuppertal 1 Solvay-Francqui Workshop, Brussels, May 2015

2 Karl-Heinz Kampert University Wuppertal Solvay-Francqui Workshop, Brussels, May 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 Outline The End of the UHECR Energy Spectrum: GZK-effect or Exhaustion of Sources? Chemical Composition: getting heavier?! Arrival Directions: surprisingly isotropic EeV neutrinos and photons: smoking gun Further Searches: neutrons, monopoles, Future: Upgrades of Auger and TA Karl-Heinz Kampert - Univ. Wuppertal 3 Solvay-Francqui Workshop, Brussels, May 2015

4 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 - Univ. Wuppertal 5 Solvay-Francqui Workshop, Brussels, May 2015

5 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 - Univ. Wuppertal 6 Solvay-Francqui Workshop, Brussels, May 2015

6 Hybrid Observation of EAS Concept pioneered by the Pierre Auger Collaboration (Fully operational since 06/2008 (Now also used by Telescope Array (TA)) light trace at night-sky (calorimetric) Fluorescence light Also: Detection of Radio- & Microwave-Signals Karl-Heinz Kampert - Univ. Wuppertal Particle-density and -composition at ground 7 Solvay-Francqui Workshop, Brussels, May 2015

7 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 130 radio antennas Karl-Heinz Kampert - Univ. Wuppertal 8 Solvay-Francqui Workshop, Brussels, May 2015

8 Auger Hybrid Observatory 3000 km 2 area, Argentina 27 fluorescence telescopes plus Water Cherenkov tanks Karl-Heinz Kampert - Univ. Wuppertal 9 Solvay-Francqui Workshop, Brussels, May 2015

9 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 - Univ. Wuppertal Solvay-Francqui Workshop, Brussels, May 2015

10 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 - Univ. Wuppertal 11 Solvay-Francqui Workshop, Brussels, May 2015

11 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 - Univ. Wuppertal 12 Solvay-Francqui Workshop, Brussels, May

12 Telescope Array 700 km 2, Utah (USA) 3 m 2 Scintillator Detectors on a 1.2 km square grid 14 (12) station 256 PMTs/camera Karl-Heinz Kampert - Univ. Wuppertal 13 Solvay-Francqui Workshop, Brussels, May 2015

13 Auger and TA Telescope Array (TA) Delta, UT, USA 507 detector stations, 680 km 2 36 fluorescence telescopes Auger and TA can see the same sky Auger: 01/ /2012 TA: 05/ /2012 same scale i km 2 yr Auger vertical + inclined Auger vertical (01/ /2012) Auger inclined (01/ /2012) TA (05/ /2012) Auger e(d) h 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 - Univ. Wuppertal 14 Solvay-Francqui Workshop, Brussels, May 2015

14 Event Example in Auger Observatory Energy calibration based on experimental data (including invisible energy correction) Cross Correlation OBSERVATORY de/dx (PeV/g cm 2 ) calorimetric meas. Longitudinal Profile E = 68 EeV X max =770 g/cm Slant Depth (g cm 2 ) ~ 20 km Karl-Heinz Kampert - Univ. Wuppertal 16 Solvay-Francqui Workshop, Brussels, May km Signal (VEM) Infill Standard inclined S(00) Lateral Profile µ+e measurement S(00)=222 VEM θ = 54 S38=343 VEM E = 71 EeV Distance to Shower Core (m)

15 Energy Spectrum Karl-Heinz Kampert - Univ. Wuppertal 17 Solvay-Francqui Workshop, Brussels, May 2015

16 All Particle Energy Spectrum Kampert & Tiniakov, CR Physique, 15 (2014) 318 E [ev ] E 3 J( E ) ev 2 km 2 sr 1 yr TA 2013 preliminary Auger 2013 preliminary E / E = 14 % log ( E /ev ) Good agreement between experiments - some differences at the highest energies - Karl-Heinz Kampert - Univ. Wuppertal 18 Solvay-Francqui Workshop, Brussels, May 2015

17 All Particle Energy Spectrum Kampert & Tiniakov, CR Physique, 15 (2014) 318 E [ev ] E 3 J( E ) ev 2 km 2 sr 1 yr TA 2013 preliminary Auger 2013 preliminary p-fit GZK-fit to TA data m=4.4, α=2.39 E / E = 14 % log ( E /ev ) Good agreement between experiments - some differences at the highest energies - Karl-Heinz Kampert - Univ. Wuppertal 19 Solvay-Francqui Workshop, Brussels, May 2015

18 All Particle Energy Spectrum Kampert & Tiniakov, CR Physique, 15 (2014) 318 E [ev ] E 3 J( E ) ev 2 km 2 sr 1 yr TA 2013 preliminary Auger 2013 preliminary Iron Proton GZK-fits to Auger data E / E = 14 % log ( E /ev ) Good agreement between experiments - some differences at the highest energies - Karl-Heinz Kampert - Univ. Wuppertal 20 Solvay-Francqui Workshop, Brussels, May 2015

19 All Particle Energy Spectrum Kampert & Tiniakov, CR Physique, 15 (2014) 318 E [ev ] E 3 J( E ) ev 2 km 2 sr 1 yr TA 2013 preliminary Auger 2013 preliminary p He Exhaustion of sources (+GZK) CNO MgAlSi Fe E / E = 14 % Fit by Blasi et al. JCAP 2014 arxiv: v log ( E /ev ) Energy spectrum itself is ambiguous concerning interpretations Karl-Heinz Kampert - Univ. Wuppertal 21 Solvay-Francqui Workshop, Brussels, May 2015

20 Limiting Energy of Sources (Emax~Z) + GZK Model inspired by Allard, Astropart. Phys , 2012 Simulations done with CRPropa 2.0 yr -1 ] 38 m=0; α=1.55 In this case GZK-effect is not responsible for cut-off! Auger ICRC2013 sr -1-2 km 2 [ev 3 diff flux X E 37 all p primary p He Z obs =12-26 Z obs = lg (E [ev]) Protons Emax,p = 18.9 ev Iron Emax, Fe = 26 Emax,p = 20.3 ev Karl-Heinz Kampert - Univ. Wuppertal 22 Solvay-Francqui Workshop, Brussels, May 2015

21 Mass Composition Karl-Heinz Kampert - Univ. Wuppertal 23 Solvay-Francqui Workshop, Brussels, May 2015

22 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 slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

23 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 slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

24 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 proton slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

25 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 iron slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

26 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 <X max > iron slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

27 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 RMS(X max ) <X max > iron slant depth [g/cm ] Karl-Heinz Kampert - Univ. Wuppertal 24 Solvay-Francqui Workshop, Brussels, May 2015

28 Xmax and RMS(Xmax) as a fct of E <Xmax> (g/cm 2 ) data ± σ stat ± σ sys Energy (ev) Auger; Phys. Rev. D 90, (2014) 80 proton EPOS-LHC Sibyll2.1 iron QGSJetII-04 OBSERVATORY σ( X max ) [g/cm 2 ] using post-lhc models 0 Auger Phys. Rev. D 90, (2014) Energy (ev) proton iron OBSERVATORY Auger data show a smooth change to a heavier composition above 5 EeV Karl-Heinz Kampert - Univ. Wuppertal 25 Solvay-Francqui Workshop, Brussels, May 2015

29 Auger - TA Comparison Xmax [g/cm 2 ] Auger; Phys. Rev. D 90, (2014) bias-free due to anti-bias cuts data ± σ stat ± σ sys OBSERVATORY proton iron <X max > [gm/cm 2 ] Telescope Array Collaboration, APP 64 (2015) 49 models are folded with exp. acceptance pre LHC models Proton Iron Data QGSJETII 03 QGSJET 01c SYBILL EPOS-LHC Sibyll2.1 QGSJetII E [ev] Energy log (E/eV) Karl-Heinz Kampert - Univ. Wuppertal 26 Solvay-Francqui Workshop, Brussels, May 2015

30 Auger - TA Comparison 850 Auger; Phys. Rev. D 90, (2014) bias-free due to anti-bias cuts data ± σ stat ± σ sys proton 850 Telescope Array Collaboration, APP 64 (2015) 49 models are folded with exp. acceptance Data SYBILL 2.1 X max [g/cm 2 ] OBSERVATORY iron <X max > (g/cm 2 ) Proton Iron 650 Sibyll E [ev ] Energy log(e/ev) ] 2 X max [g/cm Auger-Data TA MD 2014 folded with TA-acceptance Auger 2014 TA MD preliminary TA-Data (2014) Joint Working Group (UHECR2014; arxiv: ) Two data sets are in excellent agreement, even without accounting for the respective systematic uncertainties on the Xmax scale Karl-Heinz Kampert - Univ. Wuppertal lg(e/ev) 27 Solvay-Francqui Workshop, Brussels, May 2015

31 Xmax Distributions max 17.8 Auger collaboration, Phys. Rev. D 90, (2014) entries (normalized) <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< <lg(E/eV)< X max [g/cm 2 ] [9 of 15] Karl-Heinz Kampert - Univ. Wuppertal 28 Solvay-Francqui Workshop, Brussels, May 2015

32 Fits to Xmax Distributions Auger collaboration, Phys. Rev. D 90, (2014).9 N EPOS-LHC log(e/ev) = p = X max [g/cm 2 ] Here shown for EPOS-LHC loge= >19.5 Sibyll 2.1 log(e/ev) = N p EPOS-LHC log(e/ev) = p = 0.37 N p = X max [g/cm 2 ] 5 Sibyll EPOS-LHC log(e/ev) > 19.5 log(e/ev) > 19.5 N Fe N He p Auger p = 0.53 p = X max [g/cm 2 ] above 19 ev p,he components 50 diminish for N, Fe to take over QGSJET II-04 QGSJET II Karl-Heinz Kampert - Univ. Wuppertal 29 Solvay-Francqui Workshop, Brussels, May 2015

33 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 Post-LHC Models data suggest seeing the exhaustion of sources! p N He ankle E [ev] Fe suppression region???? Karl-Heinz Kampert - Univ. Wuppertal 30 Solvay-Francqui Workshop, Brussels, May 2015

34 Interpretation Karl-Heinz Kampert - Univ. Wuppertal 31 Solvay-Francqui Workshop, Brussels, May 2015

35 Implications of a heavy composition Astroparticle Physics (2012) Contents lists available at SciVerse ScienceDirect Astroparticle Physics (2012) Astroparticle Physics journal homepage: Astroparticle Physics 54 (2014) Astroparticle Physics 54, 48 (2014) Contents lists available at ScienceDirect Astroparticle Physics journal homepage: Extragalactic propagation of ultrahigh energy cosmic-rays q Denis Allard Laboratoire Astroparticule et Cosmologie (APC), Université Paris 7/CNRS, rue A. Domon et L. Duquet, Paris Cedex 13, France act On the heavy chemical composition of the ultra-high energy cosmic rays Dan Hooper a,b, Andrew M. Taylor c,d, * Astroparticle Physics 33 (20) Astroparticle Physics 33 (20) Contents lists available at ScienceDirect Astroparticle Physics journal homepage: a Fermi National Accelerator Laboratory, Theoretical Astrophysics, Batavia, IL 605, USA ent of Astronomy and Astrophysics, Chicago, IL 60637, USA Heidelberg, Germany UHECR composition models Andrew M. Taylor Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland abstract PHYSICAL REVIEW D 84, 5007 (2011) HECR composition at the highest energies, as ob he actual source composi sou Need for a local source of ultrahigh-energy cosmic-ray nuclei Andrew M. Taylor, 1 Markus Ahlers, 2 and Felix A. Aharonian 3,4 1 ISDC, Chemin d Ecogia 16, Versoix, CH-1290, SWITZERLAND te for Theoretical Physics, SUNY at Stony Brook, Stony Brook, New York e for Advanced Studies, 5 Merrion Square, Dublin 2, IRELAND hysik, Postfach 3980, D Heidelberg, GERMANY published 7 November 2011) tors indicate an increasingl end continues on Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition Subm. to JCAP 2013 R. Aloisio 1,2,V.Berezinsky 2,3 and P. Blasi 1,2 Karl-Heinz Kampert - Univ. Wuppertal 32 Solvay-Francqui Workshop, Brussels, May 2015

36 Implications of a heavy composition Astroparticle Physics (2012) Contents lists available at SciVerse ScienceDirect Astroparticle Physics (2012) Astroparticle Physics journal homepage: Astroparticle Physics 54 (2014) Astroparticle Physics 54, 48 (2014) Contents lists available at ScienceDirect Astroparticle Physics journal homepage: Extragalactic propagation of ultrahigh energy cosmic-rays q Denis Allard Laboratoire Astroparticule et Cosmologie (APC), Université Paris 7/CNRS, rue A. Domon et L. Duquet, Paris Cedex 13, France act On the heavy chemical composition of the ultra-high energy cosmic rays Dan Hooper a,b, Andrew M. Taylor c,d, * Astroparticle Physics 33 (20) UHECR composition models Andrew M. Taylor Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland abstract...and many more papers of this type Astroparticle Physics 33 (20) Contents lists available at ScienceDirect Astroparticle Physics journal homepage: a Fermi National Accelerator Laboratory, Theoretical Astrophysics, Batavia, IL 605, USA ent of Astronomy and Astrophysics, Chicago, IL 60637, USA Heidelberg, Germany PHYSICAL REVIEW D 84, 5007 (2011) HECR composition at the highest energies, as ob he actual source composi sou Need for a local source of ultrahigh-energy cosmic-ray nuclei Andrew M. Taylor, 1 Markus Ahlers, 2 and Felix A. Aharonian 3,4 all require very hard injection spectra unless 1 ISDC, Chemin d Ecogia 16, Versoix, CH-1290, SWITZERLAND te for Theoretical Physics, SUNY at Stony Brook, Stony Brook, New York e for Advanced Studies, 5 Merrion Square, Dublin 2, IRELAND hysik, Postfach 3980, D Heidelberg, GERMANY published 7 November 2011) tors indicate an increasingl end continues on a nearby source (population) is assumed Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition Subm. to JCAP 2013 R. Aloisio 1,2,V.Berezinsky 2,3 and P. Blasi 1,2 Karl-Heinz Kampert - Univ. Wuppertal 32 Solvay-Francqui Workshop, Brussels, May 2015

37 Comparison to Astrophys. Scenarios E 2 dn/de [ev cm -2 s -1 sr -1 ] A= A=3-6 A=7-19 A=20-39 A= log Energy [ev] E Fe, max = 20.2 ev α=1.1 Taylor, Ahlers, Hooper; arxiv: Emax p = 18.8 ev index α=1.1 cosm. evolution: m=0 maximum energy scenario requires very hard (non-fermi like) injection spectra <X max > [g cm -2 ] 850 Auger 2014 protons Iron log Energy [ev] Auger protons Iron Karl-Heinz Kampert - Univ. Wuppertal 33 Solvay-Francqui Workshop, Brussels, May 2015 RMS(X max ) [g cm -2 ] log Energy [ev]

38 Comparison to Astrophys. Scenarios E 2 dn/de [ev cm -2 s -1 sr -1 ] A= A=3-6 A=7-19 A=20-39 A= log Energy [ev] E Fe, max = 20.5 ev α=1.6 Taylor, Ahlers, Hooper; arxiv: Emax p = 19.1 ev index α=1.6 cosm. evolution: m=-3 maximum energy scenario requires very hard (non-fermi like) injection spectra or local sources <X max > [g cm -2 ] 850 Auger 2014 protons Iron log Energy [ev] Auger protons Iron Karl-Heinz Kampert - Univ. Wuppertal 34 Solvay-Francqui Workshop, Brussels, May 2015 RMS(X max ) [g cm -2 ] log Energy [ev]

39 Comparison to Astrophys. Scenarios E 2 dn/de [ev cm -2 s -1 sr -1 ] A= A=3-6 A=7-19 A=20-39 A= log Energy [ev] E Fe, max = 20.5 ev α=1.8 Taylor, Ahlers, Hooper; arxiv: Emax p = 19.1 ev index α=1.8 cosm. evolution: m=-6 maximum energy scenario requires very hard (non-fermi like) injection spectra or local sources <X max > [g cm -2 ] 850 Auger 2014 protons Iron log Energy [ev] Auger protons Iron Karl-Heinz Kampert - Univ. Wuppertal 35 Solvay-Francqui Workshop, Brussels, May 2015 RMS(X max ) [g cm -2 ] log Energy [ev]

40 Negative Cosmological Evolution? A strong negative cosmological evolution has been found in low-luminosity, highsynchrotron peaked (HSP) BL Lac objects based on Fermi data M. Ajello et al., ApJ, 780: ] -3,z) [Mpc 48 / γ Φ(L -4 logl = γ L< 46 erg/s logl = γ logl = γ z We may see mostly nearby low-power sources! Karl-Heinz Kampert - Univ. Wuppertal 36 Solvay-Francqui Workshop, Brussels, May 2015

41 Anisotropies Karl-Heinz Kampert - Univ. Wuppertal 37 Solvay-Francqui Workshop, Brussels, May 2015

42 UHECR Sky surprisingly isotropic E [ev ] J(E;E > E a ) µ E g 2 isotropic distribution E=4-8 EeV equatorial coordinates E 3 J( E ) ev 2 km 2 sr 1 yr Auger 2013 preliminary apple log E log E 1 1/2 1 + exp log W c g g log ( E /ev ) Auger Collaboration ApJ 802:111 (2015) Karl-Heinz Kampert - Univ. Wuppertal 38 Solvay-Francqui Workshop, Brussels, May 2015

43 UHECR Sky surprisingly isotropic E [ev ] J(E;E > E a ) µ E g 2 dipole like anisotropy E>8 EeV equatorial coordinates E 3 J( E ) ev 2 km 2 sr 1 yr Auger 2013 preliminary apple log E log E 1 1/2 1 + exp log W c g g log ( E /ev ) Auger Collaboration ApJ 802:111 (2015) Amplitude: (4.4±1.0)%; p=6.4-5 Karl-Heinz Kampert - Univ. Wuppertal 39 Solvay-Francqui Workshop, Brussels, May 2015

44 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 E>57 EeV dipole like anisotropy E>8 EeV TA: ApJ 790:L21 (2014) equatorial coordinates 29 TA (5σ pre-trial) (3.4σ post-trial) Auger (3σ pre-trial) Auger Collaboration ApJ 802:111 (2015) Amplitude: (4.4±1.0)%; p=6.4-5 Karl-Heinz Kampert - Univ. Wuppertal Auger: APP 34(20) Solvay-Francqui Workshop, Brussels, May 2015

45 Weak excess of events around Cen A giant lobes ~ 280 kpc physical age ~ 560 Myr distance ~ 3.8 Mpc E > 55 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 3.2 p=1.4% 15 68% isotropic 95% isotropic 99.7% isotropic data moon Angular distance from Cen A [deg] Auger Collaboration: ApJ 802:111 (2015) Feain et al., ApJ 740 (2011) 17 Karl-Heinz Kampert - Univ. Wuppertal 40 Solvay-Francqui Workshop, Brussels, May 2015

46 ed quite remarkable, certainly challenging original expectationsthatassumedonly smic ray sources with a light composition at the highest energies. distribution were anisotropic, these results could be understood for instance as due large deflections caused by the intervening magnetic fields if a large fraction of the Point Source Iftheactual Searches n this energy Cross-correlation range were with Swift heavy, AGN as is indeed Cross-correlation suggested Swift log(l[erg/s])>44, by mass-composition D=130 Mpc studies ham et al. 20a; Aab et al. 2014). Alternatively, it could also be explained in a io in which the number of individual sources 70 contributing to the CR0.1 fluxes is large , the lack of autocorrelation has been used 65 in Abreu et al. (2013a) 0.01 to set lower 60 s on the 43 density of sources if the0.001 deflections involved are + not large log( L min [erg/s] ) + f E th [EeV] e have 42.5also studied the cross-correlation between events and nearby extragalactic 1e e R sources. The parameters corresponding to the minima obtained when scanning D [Mpc] Ψ [deg] s in different flux-limited catalogs with the aim of identifying possible scenarios of rgy, distance and angular scale are listed in Table 1 (first three rows). The penalized bilities that these minima are dueto fluctuations of an isotropic background are of the of a few percent. In all three cases the object distance corresponding to the minima is 0 to 90 Mpc, although it happens for different angular scales and energy thresholds. a further scan is performed on the minimum intrinsic AGN luminosity, additional a appear (see rows 4 and 5 in Table 1). We note that the penalized probability is for Swift AGNs within 130 Mpc and brighter than 44 erg/s, corresponding to ess of pairs for events above 58 EeV on angular scales of 18,whilefortheradio es the penalized probability is 11%. Summary of searches Objects E th Ψ D L min f min P [EeV] [ ] [Mpc] [erg/s] 2MRS Galaxies % Swift AGNs % Radio galaxies % Swift AGNs % Radio galaxies % Centaurus A % 1: Karl-Heinz Summary Kampert of- Univ. the parameters Wuppertal of the minima found in the cross-correlation analyses. f Example: Correlation to bright SWIFT AGN best for: D < 130 Mpc L > 44 erg/s Ψ < pairs correlate with the AGN, for 32.8 expected p = 1.3% Auger Collaboration ApJ 804:15 (2015) No significant excesses were found around the Galactic Center, the Galactic Plane, or the Super- Galactic Plane. 41 Solvay-Francqui Workshop, Brussels, May 2015

47 Conclusions from CR Anisotropy Studies 1) Absence of significant correlations to Galactic Center and Galactic Plane EeV sources are unlikely of Galactic origin 2) Only a small deviation from overall isotropic sky either large deflections by B-fields, e.g. due to heavy primaries (supported by Auger composition studies) or number of sources is very large (bounds by Auger from lack of autocorrelations: ρ -4 Mpc -3 ) Karl-Heinz Kampert - Univ. Wuppertal 42 Solvay-Francqui Workshop, Brussels, May 2015

48 Neutrinos Karl-Heinz Kampert - Univ. Wuppertal 43 Solvay-Francqui Workshop, Brussels, May 2015

49 A look to the PeV Neutrino Sky +: Shower like events x: Track like events IceCube Collaboration: Phys. Rev. Lett. 113 (2014) 11 Galactic coordinates No significant clustering seen (p=84%) cross correlations to catalogs no signal yet cross correlations to UHECR (Auger+TA) ongoing Karl-Heinz Kampert - Univ. Wuppertal 44 Solvay-Francqui Workshop, Brussels, May 2015

50 Constraints from Neutrino-Isotropy High level of Isotropy source density must be fairly high Int. Flux F=ρ L is known Mean Luminosity per source must be low Kowalski; Assumption: steady point sources allowed region Density & Luminosity compare well to UHECRs! Remark: Neutrinos can come from far away sky may remain isotropic UHECRs come from within GZK sphere limited number of sources sky needs to become anisotropic Karl-Heinz Kampert - Univ. Wuppertal 45 Solvay-Francqui Workshop, Brussels, May 2015

51 Back to the GZK-Question: Smoking Gun of GZK-effect smoking gun signals by EeV ν s and γ s 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 - 17 c?on+in+eev+range+may+provide+complementary+informa?on+to+direct+u Karl-Heinz Kampert - Univ. Wuppertal 18 E ν [ev] Note, these calculations assume that the flux suppression is caused solely by the GZK-effect 46 Solvay-Francqui Workshop, Brussels, May 2015

52 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 - Univ. Wuppertal 47 Solvay-Francqui Workshop, Brussels, May 2015

53 Sensi?vity+to+all+flavours+&+channels+ Sensitivity to all ν flavors and channels + Karl-Heinz Kampert - Univ. Wuppertal 48 Solvay-Francqui Workshop, Brussels, May 2015

54 (1) Selection 3+observables+ of inclined showers (1)+Elongated+footprint+ (2)+Apparent+velocity+V+of+propaga?on+of++ shower+front+at+ground+along+major+axis+l+ Ver?cal+shower V+>>+c+ Horizontal+shower V+ +c+ (3)+Reconstructed+θ$ 12+ Karl-Heinz Kampert - Univ. Wuppertal 49 Solvay-Francqui Workshop, Brussels, May 2015

55 (2) Identifying νs in surface detector data With+the+SD,+we+can+dis?nguish+muonic+from+electromagne?c+shower+fronts+ (using+the+?me+structure+of+the+signals+in+the+water+cherenkov+sta?ons).+ signal [VEM] signal [VEM] signal [VEM] time [ns] Karl-Heinz Kampert - Univ. Wuppertal PMT 1 PMT time [ns] PMT time [ns] signal [VEM] signal [VEM] signal [VEM] PMT time [ns] PMT time [ns] PMT time [ns] 50 Solvay-Francqui Workshop, Brussels, May

56 (2) Identifying νs in surface detector data From+the+observa?onal+point+of+ view,+signals+extended+in+?me:+ Trace+example:+ToT+trigger+&+large+AoP+ Induce+Time&over&Threshold+ (ToT)+triggers+in+the+SD+ sta?ons and/or+ Defini?on+of+Area&over&Peak+(AoP)+ Have+large+Area&over&Peak+ value+(aop+ +1+muonic+front)+ Searching+for+neutrinos+ + Searching+for+inclined+showers+with+sta?ons++ with+tot+triggers+and/or+large+aop+ 9+ Karl-Heinz Kampert - Univ. Wuppertal 51 Solvay-Francqui Workshop, Brussels, May 2015

57 Combined Fisher Discriminant Events 4 Training data Search data Monte Carlo ν 3 2 Fisher > 3.28 ν candidate region Fisher value Karl-Heinz Kampert - Univ. Wuppertal F 52 Solvay-Francqui Workshop, Brussels, May 2015

58 EeV Neutrino Limits Auger Collaboration, PRD 2015; editors suggestion Single flavour, 90% C.L. s -1 sr -1 ] 5 6 IceCube 2013 (x 1/3) [30] Auger (this work) ANITA-II 20 (x 1/3) [29] Cosmogenic ν models p, Fermi-LAT best-fit (Ahlers ') [33] p, Fermi-LAT 99% CL band [33] p, FRII & SFR (Kampert '12) [31] Fe, FRII & SFR (Kampert '12) [31] p or mixed, SFR & GRB (Kotera ') [9] Waxman-Bahcall '01 [13] -2 dn/de [ GeV cm 2 E E ν [ev] Karl-Heinz Kampert - Univ. Wuppertal 53 Solvay-Francqui Workshop, Brussels, May 2015

59 EeV Neutrino Limits Single flavour, 90% C.L. -5 IceCube 2013 (x 1/3) [30] ] sr -1-6 Auger (this (2015) work) ANITA-II 20 (x 1/3) [29] Auger Collaboration, PRD 2015; editors suggestion 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 - Univ. Wuppertal Auger (this work) Fe, FRII & SFR (Kampert '12) [31] 54 Solvay-Francqui Workshop, Brussels, May 2015

60 EeV Neutrino Limits Single flavour, 90% C.L. -5 IceCube 2013 (x 1/3) [30] Auger Collaboration, PRD 2015; editors suggestion Cosmogenic ν models Auger (this (2015) 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 - Univ. 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 55 Solvay-Francqui Workshop, Brussels, May 2015

61 Cosmogenic Neutrinos Expectations Taylor, Ahlers, Hooper; arxiv: present upper limits by Auger 1 n = 0 / proton only n = 3/mixed n = 0/mixed ARA-37 (3yr) ARA (3yrs) E 2 J [ev cm 2 s 1 sr 1 ] n = n = 3/mixed 6/mixed } maximum energy scenarios that describe UHECR spectra and composition E [ev] Cosmogenic neutrino fluxes may be ~2 orders of magnitudes lower than generally expected!! Karl-Heinz Kampert - Univ. Wuppertal 56 Solvay-Francqui Workshop, Brussels, May 2015

62 Quest about origin of UHECR flux suppression of fundamental importance for understanding UHECR sources and prospects of future EeV neutrino experiments Karl-Heinz Kampert - Univ. Wuppertal 57 Solvay-Francqui Workshop, Brussels, May 2015

63 Answering these questions requires Upgrades of TA and Auger Observatory Karl-Heinz Kampert - Univ. Wuppertal 58 Solvay-Francqui Workshop, Brussels, May 2015

64 TAx4 SD Upgrade 500 more SDs 2 more FD stations SD: 700 -> 3000 km 2 Hybrid: x3 acceptance Optimized for UHECR above cutoff (fully efficient above ~60 EeV) collect statistics more rapidly funding approved by JSPS Karl-Heinz Kampert - Univ. Wuppertal 59 Solvay-Francqui Workshop, Brussels, May 2015

65 Auger Upgrade E [ev] Auger 2013 preliminary E 3 J(E) ev 2 km 2 sr 1 yr measure composition event-by-event into flux suppression region log (E/eV) p fraction He fraction N fraction Fe fraction Sibyll 2.1 QGSJET II-4 EPOS-LHC p He CNO Pierre Auger Collaboration? E [ev] Fe? Karl-Heinz Kampert - Univ. Wuppertal 60 Solvay-Francqui Workshop, Brussels, May 2015

66 Auger Upgrade 4 m 2 to reduce poisson statistics at d>800 m Scintillators on top of each Water Cherenkov Tank (non invasive, fast to install, robust technology, relatively inexpensive) Karl-Heinz Kampert - Univ. Wuppertal 61 Solvay-Francqui Workshop, Brussels, May 2015

67 Scintillator Signals dominated by e+γ +Em had ) 2 2 WCD Top Scin 20 ev, vertical 20 ev, 45 +Em had ) WCD Top Scin µ Em pure / (Muon+Em µ 1 scintillator on top WCD Em pure / (Muon+Em 1 WCD scintillator on top θ= 0 [deg] log(e)=20.00 [ev] θ= 45 [deg] log(e)=20.00 [ev] -1 r [m] r [m] signal contribution from electrons and muons in EAS significantly different in scintillator and water Cherenkov tank e/γ µ F Linear system of equations solved by matrix inversion SSSD SSSD l ASSD A = SSD Fem S WCD b A WCD A WCD F µ SWCD S WCD, µ = δ S WCD γ S SSD Karl-Heinz Kampert - Univ. Wuppertal alternative approach: shower Universality 62 Solvay-Francqui Workshop, Brussels, May 2015

68 Primary Identification on Shower-by-Shower Basis CORSIKA Shower libraries were generated with different energies (fixed and continuous) primaries zenith angles interaction models performance then studied per station and per event Fe Merit Factor (discrimination power): f p,fe = hs Fei hs p i q 2 Fe + 2 p Note: enhanced SD helps also improving photons and neutrino detection p ƒp,fe=1.68 example plot Karl-Heinz Kampert - Univ. Wuppertal 63 Solvay-Francqui Workshop, Brussels, May 2015

69 Reconstructed Xmax and σ(xmax) ] 2 <X max > [g/cm p, EPOS-LHC Fe, EPOS-LHC photo-dis. Maximum rigidity ] 2 RMS(X max ) [g/cm p, EPOS-LHC Fe, EPOS-LHC photo-dis. Maximum rigidity Scenario 1 Scenario lg(e/ev) 20 Scenario 1 Scenario lg(e/ev) Shower fluctuations and detector resolutions included models can be distinguished with high significance Karl-Heinz Kampert - Univ. Wuppertal 64 Solvay-Francqui Workshop, Brussels, May 2015

70 p-astronomy use arrival directions of 141 measured events with θ < 60 and E> ev and randomly assign Xmax according to maximum rigidity model with % p-like at high E and let 50% of p-like events correlate with Swift-BAT sources this reproduces well the present situation ~ 3σ effect p-like events are removed only p-like events included ~ 5σ effect Karl-Heinz Kampert - Univ. Wuppertal 65 Solvay-Francqui Workshop, Brussels, May 2015

71 Auger Upgrade: Status The Pierre Auger Observatory Upgrade Preliminary Design Report April 17, 26, 2015 positively evaluated by International Advisory Committee endorsed by International Finance Board R&D well advanced, prototypes running engineering array 03/2016 construction 11/ data taking into 2024 costs: 12.5 M funding: positive signs, but not yet approved Organization: Pierre Auger Collaboration Observatorio Pierre Auger, Av. San Martín Norte 304, 5613 Malargüe, Argentina OBSERVATORY Karl-Heinz Kampert - Univ. Wuppertal 66 Solvay-Francqui Workshop, Brussels, May 2015

72 Major Achievements in the last ~7 years Clear observation of flux suppression, origin unknown Relevant bounds on cosmogenic ν and γ First evidence for large scale anisotropies First hints on directional correlations to nearby matter Increasingly heavier composition above ankle pp cross section at ~*ELHC, LIV-bounds,... muon deficit in models at highest energies geophysics (elves, solar physics, aerosols...) Karl-Heinz Kampert - Univ. Wuppertal 67 Solvay-Francqui Workshop, Brussels, May 2015