Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The quest for UHECR and ν

from spaceAndrea Santangelo

IAAT, Eberhard Karls Universität&

IASF-CNR Sez. Palermo

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Outline

• UHECR and ν 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 (?)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

E > 5×1019 eV(~1016 keV)

Their origin, nature and even their route to the Earth presents an extraordinary puzzle

UHECR

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

One Piece of the Puzzle, the GZK featurethe GZK effect

p + h → n+

p + h → p+(p + h → p+ e++e- )

Greisen (1966) and, independently, Zatsepin and Kuz’min (1966)

A + h → (A-1) + NA + h → (A-2) + 2NA + h → A+ e++e-

Photopion production!

Photodisintegration (Puget et al., 1976) Pair production (Blumenthal, 1970)

E 2*1020 eV (nuclei)

eV1044

mmm2E 19

2N

th

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Energy (eV)

Rad

io

CM

B

Vis

ible

GeV

-r

ays

1 TeV = Fermilab

Flu

x

IRB

///////////

Ressell & Turner

X-r

ays e+e-

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

cosmic rays

Halzen, Ressell & Turner

Energy (eV)

e+e-

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Physics with Astroparticles

Battiston, 2002

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The Observational Scenario is still uncertain and still under debate

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Several Observations…

Tens of events at energies > 5×1019 eV have been detected so far…

Six ground based experiments have reported ~ 20 events at E>1020 eV

Flux of 1 particle per km2 per century!!

3.2X1020eV Fly’s eye (Bird et al. 1995)

3.4X1020eV AGASA (M. Teshima, 2000)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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..

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

AGASA HiRes

GZK-HypothesisExtended spectrumSuper-GZK

~2.4 σ(~2.0 σ)

~3.0 σ(~1.5σ)

~ 0 σ~ 0σ

~2.3 σ

( ) --- AGASA -10%Statistics

M. Teshima, 2002

De Marco et al., 2003

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The Pierre Auger Observatory (South…)

1600 (600 op.) water Cherenkov detectors

4 stations with 24 fluorescence telescope (6+6 op.)

Jan 2005 68% AGASA

srkm 107A 23Auger

eff

century km particle 1

2

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

srkm 10)96(A 24effEuso

•Large distance > 400 km

•Large FOV

•

30

srkm 106A 25geo

% 2510cycle

A. Bunner, 1967Kakimoto et al. , 1996

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

•Large Target Mass of the atmosphere

tons 10few 12

•Large Distance R but small proximity effect

% in R/R

•Full sky coverage looking at both North and South sky

coverage 4

Large encircled area: A Space Device (…EUSO) Small encircled area: AUGER

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Full sky coverage

By A.Kravtsov

Matter and Galaxies within 93 Mp

South and North Sky are very different

Great Attractor, Local Void, Galactic Center South

Local Super Cluster North

The base of the Scientific Rationale of Auger North Decision June 2005

A. Olinto, 2003

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Comparison of UHECRs Experiments

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Ongoing Studies/Concepts

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The Extreme Universe Space Observatory

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

A Main UV Telescope + LIDAR

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

channels 10)42( 5

m2EPD

64M36M

MAPMT

10ns

ResolutionPulse Double

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Number of events expected in five years of operation

EUSO Red Book, 2004

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

FLUORESCENCE CHERENKOV ?

Bottai, 2004

Neutrino Observations in atmosphere

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

EUSO

AUGER

GZK gives only granted flux of cosmic neutrinos

(Kalashek, Kuzmin, Semokov, Sigl)

Phys. Rev. D66 2002

Region of‘safe’ neutrino astronomy

EUSO Red Book, 2004; Bottai, 2004

Speculative models

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

skimming

downward

Paolo Lipari, 2004

~GZK(A)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The trigger efficiency

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The Tracking Ultraviolet Set-up Mission

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

TUS main figures

Mission is planned for 2007-2009R&D to be completed within 2005

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Between Present and future: OWL

srkm 103A 26geo

srkm 10)63(A 25effOWL

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

The future

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

“Opening Particle Astronomy to probe and understand the evolving Universe”

A scientific Theme proposed in response to the ESA D-Sci “Call for themes for

Cosmic Vision 2015-2025”

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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

A powerful enough detector will allow to study (within the GZK neighbourhood) :• Source densities,• Source intensities,• Individual source spectra.• …

Blasi & De Marco, 2003

Blasi & De Marco, 2003

Effective Aperture

50-100 times Auger 10 times EUSO

Energy threshold close to 1018 eV

2 Main “Requirements”

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Plagnol, 2005 Code provided by E. Parizot, 2005

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Conclusion : A precise study of individual source spectrum (, Emax) would benefit strongly from an increase of efficiency : UHECR Astronomy

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

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

EUSO

AUGER

q.e=50%Eth=3EeVD=7.5mFOV= EUSO X 3

GZK(A)~ 40 events/year

GZK(A)~0.3 events/year in EUSO

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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…)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Design of a mirror optics, based on the Schmidt camera principle, with FOV up to 25°

• 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

A proposed 5 m EPD mirror system

correcting plate and/or filter

mirrorlight shield

focal plane

FEATURES

Piero Mazzinghi, Vojko Bratina (INOA)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

OWL/AIRWATCH Maksutov Type Telescope Scale: 0.03 DJL 17-Mar-99

833.33 MM

Fresnel-Maksutov Optics

D. Lamb et al., NASA/MSFCUniversity of Alabama, Huntsville

0.1o Pixel Angular Resolution in UV ~ 104 away from Diffraction Limit

Maksutov-Mangin (Pitalo-Lamb)makes =0.02 FOV=50, Ro/R = 0.7

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Assembling in space …

By robots on the launchers

On the ISS stay there or move as a free flyer

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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 MPIR&D goals: increase SiPM size from 1 mm up to (3-5)mm increase in QE up to 70%

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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)

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

Task 4: Mission Concept (?)

• Formation flights

• Stereo operation

• Variable Orbits

Le Thuile, March 13th 2005 XXXXth Rencontres de MORIONDVery High Energy Phenomena in the Universe

Andrea Santagelo,IAAT

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 R&D 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…