XXXXth Rencontres de MORIOND

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The quest for UHECR and ?from space

• Andrea Santangelo
• IAAT, Eberhard Karls Universität
• IASF-CNR Sez. Palermo

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Outline

• UHECR and ? in a nutshell (see Monday Afternoon
  for details)
• Why from space ?
• How from space ?
• The actual idea and proposals ? EUSO
• The Future toward a Cosmic Vision 2015-2025
  Mission for Particle Astronomy (?)

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UHECR
E gt 51019 eV (1016 keV)
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One Piece of the Puzzle, the GZK feature

• the GZK effect

Greisen (1966) and, independently, Zatsepin and
Kuzmin (1966)
p hn ? np p hn ? pp (p hn ? p ee- )
Photopion production!
Photodisintegration (Puget et al., 1976) Pair
production (Blumenthal, 1970)
A hn ? (A-1) N A hn ? (A-2) 2N A hn ?
A ee-
E 21020 eV (nuclei)
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Energy (eV)
1 TeV Fermilab
CMB
Radio
IRB
Flux
/ / / / / / / / / / /
Visible
???ee-
X-rays
GeV g-rays
Ressell Turner
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Energy (eV)
cosmic rays
???ee-
n
Halzen, Ressell Turner
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Physics with Astroparticles
Battiston, 2002
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• The Observational Scenario is still uncertain and
  still under debate

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Several Observations
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HiRes collaboration, astro-ph/0208301
This discrepancies call for a study with a new
approach may need an experiment combining ground
array with fluorescence such as the Auger project
to resolve this issue..
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M. Teshima, 2002
De Marco et al., 2003
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The Pierre Auger Observatory (South)
1600 (600 op.) water Cherenkov detectors 4
stations with 24 fluorescence telescope (66 op.)
Jan 2005? 68 AGASA
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John Linsley in 1979 in the Field Committee
Report of NASA Call for Projects and Ideas in
High Energy Astrophysics for the 1980s
The concept to observe, by means of Space Based
devices looking at Nadir Nighttime, the
fluorescence light produced by an EAS proceeding
in the atmosphere
In 1995 Yoshi Takahashi of UHA rediscovered the
original idea and proposed the MASS program wich
later became a reality with the OWL and EUSO
studies
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A. Bunner, 1967
Kakimoto et al. , 1996

• Large distance gt 400 km
• Large FOV

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• Large Target Mass of the atmosphere

• Large Distance R but small proximity effect

• Full sky coverage looking at both North and South
  sky

Large encircled area A Space Device (EUSO)
Small encircled area AUGER
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Full sky coverage
South and North Sky are very different
Great Attractor, Local Void, Galactic Center ?
South
Local Super Cluster ? North
A. Olinto, 2003
By A.Kravtsov
The base of the Scientific Rationale of Auger
North? Decision June 2005
Matter and Galaxies within 93 Mp
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Comparison of UHECRs Experiments
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• Ongoing Studies/Concepts

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The Extreme Universe Space Observatory
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A Main UV Telescope LIDAR
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Number of events expected in five years of
operation
EUSO Red Book, 2004
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Neutrino Observations in atmosphere
FLUORESCENCE
CHERENKOV ?
Bottai, 2004
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EUSO Red Book, 2004 Bottai, 2004
Speculative models
AUGER
Region of safe neutrino astronomy
EUSO
(Kalashek, Kuzmin, Semokov, Sigl) Phys. Rev. D66
2002
GZK gives only granted flux of cosmic neutrinos
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Paolo Lipari, 2004
skimming
GZK(A)
downward
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The trigger efficiency
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The Tracking Ultraviolet Set-up Mission
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TUS main figures
Mission is planned for 2007-2009
RD to be completed within 2005
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Between Present and future OWL
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• The future

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Opening Particle Astronomy to probe and
understand the evolving UniverseA scientific
Theme proposed in response to the ESA D-Sci Call
for themes for Cosmic Vision 2015-2025
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Opening Particle Astronomy

• This will open up the field of "Particle
  Astronomy" and its correlations with radio,
  photo, X and g astronomy.
• To Search for UHE neutrinos

Blasi De Marco, 2003
A powerful enough detector will allow to study
(within the GZK neighbourhood) Source
densities, Source intensities, Individual
source spectra.
2 Main Requirements
Effective Aperture 50-100 times Auger
10 times EUSO
Energy threshold close to 1018 eV
Blasi De Marco, 2003
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Code provided by E. Parizot, 2005
Plagnol, 2005
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Based on the analysis of Blasi De Marco, 2003
source density of 10 -5 sources/Mpsec (in fact,
10-4 to 10-6).
Plagnol, 2005
Conclusion A precise study of individual source
spectrum (g, Emax) would benefit strongly from an
increase of efficiency UHECR Astronomy
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q.e50 Eth3EeV D7.5m FOV EUSO X 3 GZK(A) 40
events/year
GZK(A)0.3 events/year in EUSO
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Task 1 Optics

• Large Area (pupil ? 2m ? 5-7m) and Large field
  of view ( 90 full angle) Optical systems
• Deployability/Assembling in space
• Materials (High Throughput, Light weight,
  contaminants)
• Filter (coatings multilayers)

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A proposed 5 m EPD mirror system
Piero Mazzinghi, Vojko Bratina (INOA)
Design of a mirror optics, based on the Schmidt
camera principle, with FOV up to 25
light shield
mirror
correcting plate and/or filter
FEATURES

• Entrance pupil MUST be in the mirror centre of
  curvature
• Mirror is then larger than EPD (depending on
  FOV)
• Light shield is anyway necessary for stray light
  reduction
• The correcting plate greatly improves
  performances
• F/ investigated as low as 0.6
• Detector diameter smaller than any other
  proposed solution
• Weight saving solution (both for optics and
  detector)
• Obscuration acceptable for FOV up to 25
• Vignetting almost constant for all FOV
• Low sensitivity to misalignment (except
  decenter)
• Optical system design scalable to any dimension

focal plane
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Fresnel-Maksutov Optics
0.1o Pixel Angular Resolution in UV 104
away from Diffraction Limit
D. Lamb et al., NASA/MSFC University of Alabama,
Huntsville
Maksutov-Mangin (Pitalo-Lamb) makes ??0.02?
FOV50?, Ro/R 0.7
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Assembling in space
On the ISS? stay there or move as a free flyer
By robots on the launchers
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Task 2 Sensors? Detectors

• High Efficiency Sensors
• Compact and light-weight (solid state ?)
• High Efficiency detectors (how high ? The
  highest)
• Large area, large number of pixels (channels)
  106?
• Maximizing filling factor, cooling system
• Light collector/filter

SiPM at MPI
RD goals increase SiPM size from 1 mm up to
(3-5)mm increase in QE up to 70
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Task 3 Electronics

• Front End (fast, low power, miniaturized, mixed
  analogue/digital)
• Smart Triggering systems (efficient, highly
  selective, configurable, adaptive)
• OBDH electronics (fast analysis of large amount
  of data, compliant with usually limited telemetry
  resources interaction with the Atmosphere
  Monitoring System)

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Task 4 Mission Concept (?)

• Formation flights
• Stereo operation
• Variable Orbits

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Conclusions

• Space-Based observation of UHECR can provide a
  breakthrough in the field
• EUSO can be consider a pathfinder in the field,
  and the studies associated have provided
  unvaluable info for new developments
• To succeed, the support of the entire HEAP
  community is mandatory
• A solid and realistic RD program must be
  developed, already started
• Convince the High Energy Astrophysics Community
  that UHECR studies could provide a step forward
  in our understanding of the Universe