Ultra-High Energy AstroParticles!

Ultra-High Energy AstroParticles! Angela V. Olinto The University of Chicago ICFA 2008

International Committee for! Future Accelerators!

Ancient Accelerators!!

Ancient Accelerators!! from 10 3 to 10 9 years old!

Ancient Accelerators!! from 10 3 to 10 9 years old! Ancient but Powerful!! ~ 10 TeV!! ~ 10 3 TeV! Hadrons ~ 10 8 TeV!!!!

How do they accelerate! to such high energies?! We ll call you as soon as we know! May take a couple of years

A New Era of AstroParticle Physics! Beginning to unveil the nature of! the Most Energetic Accelerators in Nature! Multimessengers that require Multiple Techniques: Cosmic Rays: ground arrays, atmospheric fluorescence, balloons, satellites, space station HE Gamma-rays: ground arrays, satellites HE Neutrinos: underground ice and water, balloons, radio telescopes

A New Era of AstroParticle Physics! Beginning to unveil the nature of! the Most Energetic Accelerators in Nature! UHE Cosmic Rays: Pierre Auger South, Telescope Array HE Gamma-rays: FGST, Milagro, MAGIC, HESS, VERITAS HE Neutrinos: IceCube, Antares, ANITA

Cosmic Ray! Spectrum! E cm = PeV (E uhecr /ZeV) 1/2 (2A) 1/2 Non-thermal Phenomena Extreme Accelerators E max > 10 20 ev Features: knee, ankle, GZK cutoff accelerators propagation interactions 32 orders of magnitude E -2.7 RHIC Tevatron LHC E -3.1 Ankle (1 particle /km 2 yr) 12 orders of magnitude

knee ankle Engel 08

Each Energy! range tells its story! 10 8 ev < E < 10 11 ev Solar Modulation 10 11 ev < E < 10 17.5-18.5? ev Galactic Propagation 10 17-18 ev < E < 10 20-2? ev Extragalactic Sources

Each Energy! range tells its story! 10 8 ev < E < 10 11 ev Solar Modulation Barger et al 08

Galactic Accelerators! E < 10 17.5-18.5? ev Galactic Propagation Galactic Sources?

Galactic Accelerators! E < 10 17.5-18.5? ev Galactic Propagation Galactic Sources? CREAM Kascade Grande IceTop FGST ACTs

Galactic Accelerators! E < 10 17.5-18.5? ev Galactic Propagation Galactic Sources?

Tycho SN SNR1006 CHANDRA NASA/CXC/SAO

HESS - TeV! s! smoking guns of CR acceleration! RX J1713-20 " Gamma-rays X-rays CHANDRA Hinton, WatsonFest, Leeds

see Anders Borgland

R. Dubois

Galactic Accelerators! E cm = PeV (E uhecr /ZeV) 1/2 (2A) 1/2 E < 10 17.5-18.5? ev Galactic Propagation SNR shock acceleration in the Galaxy? Ankle (1 particle /km 2 yr)? HESS SNe

Extragalactic Accelerators! 10 17-18 ev < E < 10 20-2? ev Extragalactic Sources

Extragalactic Accelerators! E cm = PeV (E uhecr /ZeV) 1/2 (2A) 1/2 E -2.7 Extreme Accelerators E max > 10 20 ev = 10 8 TeV! Extragalactic Accelerators? E -3.1 Ankle (1 particle /km 2 yr)

to reach 10 20 ev! Challenging Accelerators! LHC magnetic field," radius ~ 10 7 km (Sun Mercury)!

E = Ze B L! 10% efficiency 10 20 ev Protons 10 20 ev Iron B(G) L(cm)

E = Ze B L! 10% efficiency GRBs 10 20 ev Protons 10 20 ev Iron B(G) others L(cm)

Ultra High Energy Cosmic Ray Accelerators?! Galaxy Jets from Black Holes? Gamma Ray Bursts? Neutron Stars? Magnetars?

Highest Energies! E cm = PeV (E uhecr /ZeV) 1/2 (2A) 1/2 Pointing Feature E -2.7 E -3.1 Ankle (1 particle /km 2 yr) RHIC Tevatron LHC

Cosmologically Meaningful Termination! p+! cmb " # + " p + $ 0 " n + $ + Proton Horizon ~10 20 ev GZK Cutoff Greisen, Zatsepin, Kuzmin 1966

Chargeless vs Charged! @ Highest Energies! Photons: 1600s: G. Galilei Cosmic Rays 1912: V. Hess Attenuation Length! Lee 95

GZK Feature! E -2.7 E -3.1 Ankle (1 particle /km 2 yr) Cosmologically Meaningful Feature

AGASA (1984-2003)! 100 km 2 area,! 111 scintillators, 1km spacing! High Resolution Fly s Eye (1997-2006) 2 fluorescence telescopes! 1998 No GZK cutoff Consistent w/ GZK cutoff

GZK Effect! # Spectral Feature + LSS # Anisotropies in Sky Distribution #!Particle* Astronomy!!! *(electrically charged)

Horizon - observed Protons! AO, Armengaud, Allard, Kravtsov 07

Horizons:! 10 19 ev ~ 1 Gpc! 100 Mpc Gpc 10 20 ev < 100 Mpc!

THE SLOAN GREAT WALL

AO, Armengaud, Allard, Kravtsov 07 Protons with > 10 20.5 ev!

AO, Armengaud, Allard, Kravtsov 07 Protons with > 10 19.5 ev!

Charged Particle Astronomy! Window of opportunity 10 19 to 10 21 ev Maximize the Statistics in this window

The Pierre Auger Observatory! HIGH QUALITY LARGE QUANTITY

Auger South! 1660 tanks in a 3,000 km 2 Surface Array 4 Fluorescence Detector Sites

tanks aligned seen from Los Leones!

4 times 6 telescopes overlooking the site!

Cosmic Ray! Spectrum! E -2.7 E -3.1 Ankle (1 particle /km 2 yr) Cosmologically Meaningful Feature

Energy spectrum from SD showers with $ " 60! calib. uncert. 10% FD syst. unc. 22% 5165 km 2 sr yr ~ 0.8 full Auger year

Energy spectrum from SD showers with $ " 60! Slope = -2.62 ± 0.03 Exp. Obs. >10 19.6 ev 132 ± 9 51 > 10 20 ev 30 ± 2.5 2 significance = 6" calib. uncert. 10% FD syst. unc. 22% 5165 km 2 sr yr ~ 0.8 full Auger year

ankle

AGASA! High Resolution! Fly s Eye! No GZK cutoff Consistent w/ GZK cutoff

AGASA! High Resolution! Fly s Eye! HiRes 2008 No GZK cutoff Consistent w/ GZK cutoff

AGASA! AUGER 08 High Resolution! Fly s Eye! HiRes 2008 No GZK cutoff Consistent w/ GZK cutoff

Spectrum facts! There is an ankle There is a cut-off Galactic/Extragalactic transition? or Pair-production of pure-proton source? GZK suppression? or Limit of the acceleration process? E max analyse composition! analyse arrival directions!

Composition & Spectrum!

Auger South Low Energy Extension! HEAT High Elevation Angle Telescopes AMIGA Auger Muon and Infill Ground Array

Telescope Array! Aperture 1.4 10 3 km 2 sr Millard County Utah/USA 20 km 24 x 24 Scintillators (1.2 km spacing) 900 km 2 ~0.3 Auger South 3 x Fluorescence Stations AGASA x 1020 by stereo km Low Energy Hybrid Extension

knee ankle Engel 08

High Energy Cosmic Rays! OBSERVABLES: Spectrum Composition Sky Distribution

Composition-sensitive observables! Depth of shower maximum development: X max atmospheric depth (g/cm 2 )! low E! high E! high E! low A! high A! Stochastic process large fluctuations! small fluctuations!

Composition observable:! shower maximum! Expectations from different hadronic models + fluctuations in X max smaller for heavier nuclei

Shower maximum over 2 decades in E! + fluctuations in X max to be exploited

Allard et al 08 Horizons for E tot =60 EeV!

Observed Composition Allard et al 07

Shower maximum over 2 decades in E! + fluctuations in X max to be exploited

Shower maximum over 2 decades in E! + fluctuations in X max to be exploited

Shower maximum over 2 decades in E!????? Need input from LHCf & TOTEM to test Hadronic interaction models + fluctuations in X max to be exploited

Photon limit! Top-down models predict large UHE photon flux SHDM models: decay of superheavy dark matter accumulated in Galactic halo Showers at E = 10 19 ev, " = 0º : TD models: supermassive particle decay from topological defect interaction or annihilation Photon-induced showers look very different

Auger results (photon limit)! Super heavy dark matter (SHDM) models are excluded as UHECR sources!

Auger results (photon limit)! Topological defects (TD) are still possible UHECR sources

Cosmologically Meaningful Termination! Implies Cosmogenic Neutrinos!! p+! cmb " # + " p + $ 0 " n + $ + Proton Horizon ~10 20 ev GZK Cutoff Greisen, Zatsepin, Kuzmin 1966

Auger results! TD models closer to be constrained by Auger neutrino limits

Neutrinos at EeV Soon!

Neutrinos Soon!! IceCube 22-! Point Source search! 2.2. sigma spot!

Cosmogenic Neutrino are just around the corner? Bigas Cazon 06

High Energy Cosmic Rays! OBSERVABLES: Spectrum Composition Sky Distribution

Main Auger result! Highest energy cosmic rays have an anisotropic distribution! First evidence that CR astronomy is possible! Correlation with z < 0.018 AGNs in the 12 th Véron-Cetty/Véron catalogue Opening of a new era: Study of particle acceleration in HE astrophysical sources Multi-messenger study of sources HEP interactions at 300 TeV cm!

Auger main anisotropy result! * - VCV AGN catalogue - 27 highest energy events UHECRs

Auger main anisotropy result! correlation is most significant above E = 56 EeV whre the CR flux drops (supports GZK interpretation)

Significance of the anisotropy result! Not an AGN correlation result!! 1st step: search for correlations between arrival directions of UHECR and various source catalogues (data from 2004/01/01 to 2006/05/26) Very large raw significance found w/ 12 th VCV catalogue of AGNs Even after generous penalty factors for a posteriori searches and scanning of parameter space Did not seem to be fluctuation! Auger collaboration set up a prescription for future data! Most significant a posteriori correlation signal : 3.2 expected from isotropic distribution 12 out of 15 events E > 56 EeV closer than 3.1 from an AGN in 12 th VCV with z! 0.018 (D! 75 Mpc)

Significance of the anisotropy result! 2nd step: predefine a region in the sky of excess CR flux & test if next UHECRs come from this region 21% chance from isotropic distribution Independent data set, prescribed parameters unambiguous significance Result: 99% CL that excess in the original data set is not a random fluctuation from an isotropic CR distribution 8 correlating events out of 13 (2.7 expected) CR distribution is anisotropic at the highest energies!! Corroborated by other analyses, independent of source catalogue!

Astrophysical Implications?! UHECR sources are extragalactic!!! They exist within the GZK sphere!!!! What are the sources? Not clear yet! Very low statistics to check against any specific model Can UHECRs come from AGNs? YES! Do UHECRs have to come from AGNs? NO!! NOT Galactic Accelerators: Neutron Stars, Magnetars, Microquasars shocks in the Galaxy NOT very Distant Accelerators: Clusters of Galaxies(cluster shocks) Quasars, BL Lacs

E = Ze B L! 10% efficiency GRBs 10 20 ev Protons 10 20 ev Iron B(G) others L(cm)

E = Ze B L! X GRBs 10% efficiency 10 20 ev Protons 10 20 ev Iron B(G) X others X X L(cm)

Centaurus A, Virgo, etc.!

Centaurus A! 3.4 Mpc

AGN Acceleration Models

Astro/Phys Implications! Intergalactic Fields B rms < 10-9 G (Mpc/L c ) 1/2 If Proton Primaries - need to understand >100 TeV interactions - X max, %X max, N µ + Cosmogenic Neutrinos around the corner If Heavy Primaries need to understand The Astrophysical Accelerators + Cosmogenic Neutrinos low flux

Magnetic Deflection Plausible B galactic E> 56EeV Engel et al 08

What Next?! Auger SOUTH 2007 Auger NORTH, JEM-EUSO,.

Source Spectra! Armengaud 10-3 /Mpc 3 AN+S 7 10 5 L Blasi & DeMarco

The Pierre Auger Observatory! of Ultra-High Energy Cosmic Rays! Argentina! Australia! Brasil! Bolivia*! Northern site Czech Republic! France # #! Germany! Italy! Mexico! Netherlands! Poland! 20 000 km 2! Portugal#! Slovenia! Spain! UK#! USA! Vietnam*! 3 000 km 2! Southern site > 300 PhD scientists from! > 70 Institutions! and 17 countries! *Associate Countries!

Auger South Area!

Auger North Area!

Auger North in SE Colorado

Auger SOUTH 3,000 km 2 = 1,157 mile 2 Hexagonal grid - 1.5 km separation FD sites - 4 (180 o ) Auger SOUTH & NORTH! Auger NORTH 20,000 km 2 ~ 8,000 mile 2 SQUARE GRID - 1.414 mile separation (2.26 km) 1 large PMT / tank 40 FD telescopes 7x Area for 2x the price

Auger NORTH! Auger SOUTH 3,000 km 2 = 1,157 mile 2 Hexagonal grid - 1.5 km separation FD sites - 4 (180 o ) Auger NORTH 20,000 km 2 ~ 8,000 mile 2 1 mile! SQUARE GRID - 1.414 mile separation 1 large PMT / tank 40 FD telescopes 1609 m!

Apertures & Energy Threshold! Anisotropies

Nadir (2 yrs) 35 o tilt (3 yrs) - 3 x area, but E th > 10 20 ev Fluorescence only ~ 20% duty cycle no muons info

Lindsleys

A New Era of AstroParticle Physics! Beginning to unveil the nature of! the Most Energetic Accelerators in Nature! UHE Cosmic Rays: Pierre Auger North, JEM-EUSO HE Gamma-rays: FGST, HAWC, AGIS, CTA HE Neutrinos: IceCube, Km3Net

A New Era of AstroParticle Physics! Beginning to unveil the nature of! the Most Energetic Accelerators in Nature! UHE Cosmic Rays: Pierre Auger North, JEM-EUSO HE Gamma-rays: FGST, HAWC, AGIS, CTA HE Neutrinos: IceCube, Km3Net

Particle Astrophysics @ UHEs! The Energy Frontier FGST TeV PeV EeV ZeV 12 15 18 21 IceCube IceRay ANITA II KM3net Auger S ARIANNA Auger N JEM EUSO 12 15 18 21 Auger South JEM EUSO TA/TALE Auger North 12 15 18 21! HAWC! desert Auger S JEM EUSO AGIS Auger N CTA Leading & FUTURE Projects & CR

AstroParticle Physics @ UHEs! The Energy Frontier TeV PeV EeV ZeV 12 15 18 21 IceCube IceRay ANITA II KM3net Auger S ARIANNA Auger N JEM EUSO 12 15 18 21 Auger South JEM EUSO TA/TALE Auger North 12 15 18 21! HAWC! desert Auger S JEM EUSO GLAST AGIS Auger N CTA Leading & FUTURE Projects & CR