Scientific Case for All Sky Coverage with the Northern Auger

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Scientific Case for All Sky Coveragewith the
Northern Auger
Katsushi Arisaka
University of California, Los Angeles Department
of Physics and Astronomy arisaka_at_physics.ucla.edu
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Northern Auger FAQ
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Talk Outline

• Ultimate Goals
• Current Experimental Status
• Theoretical Developments
• Why Northern Auger?
• Why Now?

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Ultimate Goals

• Energy Frontier of Particle Physics, Cosmology
  and Astronomy
• Earliest Universe GUT, Planck Scale
• Extreme Universe AGN, GRB
• Charged-Particle Astronomy
• Need for Multi-Messenger Approach
• Gamma ray Veritas, GLAST
• Charged Particle Auger, EUSO
• Neutrino Icecube, Auger
• Gravitational Wave LIGO, LISA

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The Extreme Universe
Big Bang
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The Extreme Universe
AGN
Pulsar
SNR
Radio Galaxy
GRB
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High Energy Neutrino
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Gravitational Wave
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UHECR (AGASA, gt40EeV)
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COBE (90MHz)
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WMAP (W-Band)
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Energy Spectrum of Cosmic Rays
Extra Galactic
Galactic
?
E-2.7
E-3.1
?
Knee
Ankle
E-2.7
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Remarks (1)

• Origins of UHCR beyond the GZK cutoff may be
  different from the origins between the Ankle and
  GZK cutoff.
• The origins between the Ankle and GZK cutoff is
  not understood yet, and it will remain unsolved
  regardless of the existence of the GZK cutoff.

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Remarks (2)

• Between the Ankle and GZK cutoff is the window of
  opportunities of Charged Particle Astronomy.
• Magnetic field is weak enough for UHECR to point
  backwards to cosmological distance.
• Universe is still transparent.

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Current Experimental Status

• AGASA
• Energy Spectrum
• Large Scale Anisotropy
• Clustering
• Compostion
• HiRes
• Energy Spectrum
• Large Scale Anisotropy
• Clustering

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AGASA Energy Spectrum
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AGASA Anisotropy (1017.9-1018.3eV)

• Use 216,000events over 15 years operation
• 20o x 20o window
• gt4s near G.C. and -3s near A.G.C.

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Arrival Direction of UHECR (gt4x1019eV) by AGASA
5 ? effect

• 6 doublets and 1 triplet within 2o cone

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Remarks (3)

• No ZGK cutoff (i.e. local origin) and isotropic
  arrival direction (i.e. cosmological origin) are
  inconsistent.
• We must be careful about selection bias on any
  kind of anisotropy or clustering analysis.
• Energy cut
• Angular cut

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V1-V2 plot in Galactic coordinate
Outer Galaxy regionbIIlt60, 90ltlIIlt180
1. From 1019eV 2. Extended linearly
20ox20o
?bII
?lII
Log(E)gt19.00
19.15
19.70
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Correlation as function of energy ratio between
two events
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Possible Scenario
Rigidity dependent? Photo-disintegration
cutoff? First bump --- 1ry and 2ndry p/n Second
bump --- 1ry He Third bump --- 1ry BCNO
Naturally, Fe is expected at 2-3x1020eV.
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HiRes vs. AGASA
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HiRes-I (gt1019eV)
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Theoretical Developments

• Bottom Up
• Top Down
• Propagation

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Possible Zevatrons

• Neutron Stars
• From the Galaxy inconsistent with isotropic
  distribution ? ?
• AGN- Central Regions
• Cosmological Distance GZK cutoff ? ?
• No correlation with Super-GZK events ? ?
• AGN- Radio Lobes
• Cosmological Distance GZK cutoff ? ?
• M87 Strong B-Field ?
• Gamma Ray Bursts
• Isotropic distribution ? ?
• Energy emission compatible with UHECR ? ?
• Cosmological Distance GZK cutoff ? ?

HiRes
AGASA
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Top-down Models (inspired by AGASA spectrum)

• Topological Defects
• Cosmic Strings, Domain Walls, Magnetic Monopoles
  
• Produce UHE Gamma, Neutrinos
• Super-heavy Relics
• Trapped in Galactic Halo (like Cold Dark Matter)
• Composition and Arrival Direction are the key
  to distinguish

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Propagation models (inspired by AGASA spectrum)

• Messengers is Neutrinos
• Zo Burst
• Violation of Lorentz Invariance (VLI)
• Strong B (?G) in Local Super cluster.

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One Possible Scenario (by Gunter Sigl)

• Origins are in Local Supercluster
• Pancake profile
• Scale height of 5 Mpc
• Scale length of 20 Mpc.
• The observer is
• 20Mpc away from the center
• 2Mpc from the middle plane
• Random magnetic field of 0.5?G
• Largest eddy is 10Mpc
• Smallest eddy is 2Mpc

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Energy Spectrum of Local Supercluster model
AGASA
HiRes
G. Sigl, astro-ph/0210049
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Averaged Angular Distributions of Local
Supercluster model

• AGASA-like feature can be reproduced by
• 0.5?G magnetic field in Local Supercluster
• 20Mpc source distribution

G. Sigl, astro-ph/0210049
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Large Scale Anisotropy of Local Supercluster model
0.05?G
0.5?G
G. Sigl, astro-ph/0210049
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Why Northern Auger?

• Why all sky coverage?
• Why North?
• Why Hybrid North?
• Why more statistics?
• Why now?

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Northern Auger FAQ
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Why All Sky Coverage?

• Multi-pole Moment Analysis
• Isotropic Cosmological Origin
• Dipole Galactic Halo
• Quadra-pole Local Super-cluster
• Origin of Point Sources
• Galactic vs. Extra Galactic
• Within GZK-sphere vs. Cosmological

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Why North?

• Need to verify AGASA point-sources on North.
• Need to verify discrepancy of AGASA vs. HiRes
  spectrum on North.
• Important to see outside of the Galactic plane,
  where B-field is weak and uniform.

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Why Hybrid?

• Charge particle Astronomy between Ankle and
  GZK-cutoff
• Statistics is high enough.
• Need lt1o angular resolution for momentum
  analysis.
• Need superior composition measurements.

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Why More Statistics ?

• A factor of two makes difference in Low
  statistics
• Super-GZK events
• Neutrino events

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Neutrino Flux and Sensitivities
RICE limit
GLUE limit
AGASA
Atmospheric
Auger (?e, ??) 0.3 ev/yr
AMANDA limit
ANITA 30 days
Proton blazars
Strong DIS
TD
WB
IceCube (?µ) 3 yrs
No DIS
GZK
GRB
Auger (??) 1 ev/yr/decade
Auger ?? 90 limit (5 yrs)
IGM
Compiled by Stephane Coutu
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Why Now ?
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Why Timely ?

• Timely for multi-messenger survey of the extreme
  Universe.
• Gamma Rays
• Veritas, Hess, Magic
• GLAST, Swift
• Neutrinos
• AMANDA, ICECUBE
• ANTARES, NESTOR
• Gravitational Waves
• LIGO, VIRGO
• LISA

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Budget Comparison
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Comparison of Experiments
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Sensitivity of Future Experiments