the quest for uhecr and ν from space
DESCRIPTION
The quest for UHECR and ν from space. Andrea Santangelo IAAT, Eberhard Karls Universit ä t & IASF-CNR Sez. Palermo. Outline. UHECR and ν in a nutshell (see Monday Afternoon for details) Why from space ? How from space ? The actual idea and proposals EUSO - PowerPoint PPT PresentationTRANSCRIPT
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
Flux
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
64M36MMAPMT
10nsResolutionPulse 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 launchersOn 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…