Andrea Santangelo, IAAT-KCTVulcano 31.05.2008
Andrea Santangelo
Flavors of the Extreme Universe Space Observatory (EUSO)
The JEM-EUSO and S-EUSO missions
Institut für Astronomie und AstrophysikKepler Center for Astro and Particle Physics
Karls Eberhard Universität Tübingen
Andrea Santangelo, IAAT-KCT
Outline
• Why space? • The Basic concept: the EUSO mission• The near term future: JEM-EUSO
– Technology– Status
• The long term future: Super-EUSO– Science Requirements– Technological developments
Andrea Santangelo, IAAT-KCT
Why From Space ?
“Although it is impossible to predict what Auger will find in the next few years, it seems certain that it will be necessary to monitor massive volumes of atmosphere to study charged cosmic rays and neutrinos with energies above 1020 eV. Observations from a space platform are likely to be essential, particularly for the study of very high energy neutrinos.”
(from the “Statement by the Pierre Auger Collaboration on UHECR within the Cosmic Vision Process”, 2004).
Andrea Santangelo, IAAT-KCT
Has something changed from the time this statement was done?
Andrea Santangelo, IAAT-KCTBad Honnef, February 12, 2008
Clear Evidence of Suppression of Flux > 4 x 1019 eV• Rough agreement with HiRes at highest energies
Andrea Santangelo, IAAT-KCT
Open Questions remain
– Is this the GZK suppression? Or are the source running out of fuel?
– Do we have a high statistics description of the spectrum?
– Do we see a recovery of the spectrum?– Has the spectrum an end?
• A high precision measurement of the UHECR spectrum around and beyond the „GZK“ feature
Some – but few (~1 with Auger) - events above 1020 eV Only a few per millenium per km2 above 1020 eV
Andrea Santangelo, IAAT-KCT
First scan gave ψ < 3.1°, z < 0.018 (75 Mpc) and E > 56 EeV
Where, Which, What are the sources?
Science: 9 November 2007
Andrea Santangelo, IAAT-KCTBad Honnef, February 12, 2008
Sources of UHECR (4)
• It‘s a question of Exposure…(Allard, 2007; Olinto et al., ICRC07)
thousendsfewN
eVE
yrsrkm.A.
exp
919
25
10
1057
(Blasi & De Marco)
(S-EUSO proposal, 2007)
Armengaud, ICRC07
Andrea Santangelo, IAAT-KCT
A key requirement for UHECR Astronomy
yrsrkm10A 26exp
L10A 6exp
• Identification of individual sources of UHECR and measurement of their energy spectrum
yrsrkm1Linsley1 2
Andrea Santangelo, IAAT-KCT
Neutrinos at UHE?
Andrea Santangelo, IAAT-KCT
Cosmogenic Neutrinos
Speculative models
Astrophysical models
Region of‘safe’ neutrino astronomy ?
EUSO Red Book, 2004; Bottai, 2004 Mannheim, 1995
Kalashev et al., 2002
Protheroe & Johnson, 1995
Andrea Santangelo, IAAT-KCT
ConstrainsSemikoz & Sigl, 2004
Strong constrains:Gamma-ray flux at GeVAuger results on photon
Semikoz & Auger Collab., ICRC07
SHDM models are strongly constrained by the absence of identified photon candidates in the Auger data
Andrea Santangelo, IAAT-KCT
Cosmogenic Neutrinos
)(p CMB
)()(e ee - oscillation:
e : : : : (at generic
source)
: : (at earth)
max.mixing, 13=0Berezinsky & Zatsepin, (1969, 1970)
Berezinsky (2005)
Andrea Santangelo, IAAT-KCT
A question of thresholdLipari, 2007
eV10x1E 19th
Integral and differential neutrino interaction rates. Solid line: downward, dashed upward emerging tau leptons.
Engel et al., 2001 (thick curves)
Semikoz & Sigl, 2004 (thin curves)
Andrea Santangelo, IAAT-KCT
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 during the night, 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
Andrea Santangelo, IAAT-KCT
The Extreme Universe Space Observatory
Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW hadronsN )NC(
hadronslN )CC(
ll
l
Andrea Santangelo, IAAT-KCT
A compact, monocular, instrument …
The 300-400 nm fluorescence light is imaged by a large Fresnel lens optics onto a finely segmented focal plane detector.
System electronics, single photon counting, fast 10 ns, track time sampling (Gate time unit) 833 nsec
Entrance pupil diameter > 2.0 m, F/# < 1.25
Focal surface, single photon counting, high pixelization, 2*105 pixels
Double sided Fresnel lenses, 2.5 m diameter
Filter, deposited on the lens
Andrea Santangelo, IAAT-KCT
EUSO
tons 10few 12
•Large distance > 400 km
•Large FOV
•
30
srkm 106A 25geo
% 2510cycle
sr10)96(A effEuso 24 km
€
AEusoexp ≈ (1.8 ÷ 2.7) ×105 km2 ⋅sr
Andrea Santangelo, IAAT-KCT
JEM-EUSO
Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW
ISS Flight direction
51.6°
Japanese Experiment Module (KIBO) on International Space Station
Andrea Santangelo, IAAT-KCT
Robotic Arm
JEM Exposure Facility:
Number of ports: 10
Power : 120Vdc 、 Max10kW
Communication : low speed ( MIL-STD-1553B )
medium speed ( Ethernet )、
High speed :FDDI )
Coolant : controlled temperature 20±4℃
Outline of JEM Exposure Facility
Andrea Santangelo, IAAT-KCT
JEM-EUSO Telescope will be attached to Exposure Facility of Japanese Experiment Module (JEM/EF) of ISS in about 2013
Vertical Mode Tilted ModeLarger effective area (x3) with ~35°tilt
JEM-EUSO Telescope on ISS
Andrea Santangelo, IAAT-KCT
JEM-EUSO
•Large distance > 400 km
•Large FOV
•
30
srkm 106A 25geo
% 2510cycle
tons 10few 12
yrsrkm10)5.42(A 25exp
yr5Life yrsrkm10A 26
tilted Higashide, Wada et al., 2007
Are
a of
FO
V [
km2 ]
Tilt Angle [degree]
Andrea Santangelo, IAAT-KCT#26
Optics Requirements–FoV 30° –Pupil entrance pupil 2 m–F/# 1.0–Spot dimension ~ 0.1°–Spectral range 300-400 nm
Progress 1: Refractive-Diffractive Optics better designed
NEW MATERIAL CYTOP
> +70%
> 50%
Towards a Super Optics?A pixel size of 2.5 mm would greatly increase the S/N
3 double-sided curved Fresnel Lenses with a central flat (color correcting) fine precision lens.
Andrea Santangelo, IAAT-KCTBad Honnef, February 12, 2008
Progress 2: Industrial technical advancements
Helping advancing the JEM-EUSO capacity
MAPMT36PMTx36ch
Andrea Santangelo, IAAT-KCT
New optical material (CYTOP) and Advanced Design
Higher QE devices
Advanced Trigger algorithm
Tilt mode : 5 times exposure at E 3x1020 eV
Progress: From EUSO to JEM-EUSO
Fenu & Santangelo, 2008
Andrea Santangelo, IAAT-KCT
Sources…
Simulation (1000 Events) De Marco/Blasi 2003
Andrea Santangelo, IAAT-KCT
Important calendar (forthcoming)
• June 2008– Third International JEM-EUSO Meeting
• July 2008– Selection for the Later Phases
• April 2009– Down-selection for B/C/D
• Year 2009-2012– Production, Assembly & Verification
• Expected launch by HIIB-HTV in 2013
Andrea Santangelo, IAAT-KCT
S-EUSO and “Cosmic Vision”
Opening Particle Astronomy“A Space Observatory for next generation studies of the Universe at Ultra High energies”
Submitted to ESA in response of the AO for the first cycle of missions of the Programme “Cosmic Vision 2015-2020”
Maximize the Statistics in the 1019-1021 eV energy range
Andrea Santangelo, IAAT-KCT
Andrea Santangelo, IAAT-KCT
Andrea Santangelo, IAAT-KCT
•Variable orbit 1000 km
• FOV
• 26geo km108.0A
•Free Flyer
3025
yr5Life % 2010cycle
yrsrkm104.22.1A 26exp
sr km104.2A 26instaper
Tilted mode (?)
L10A 7exp
Andrea Santangelo, IAAT-KCT
the scientific requirements
Effective Aperture E>5x106 km2 sr yr (Nadir Mode)
Low energy threshold ~100% @ E≤4 (goal 1) x1019 eV
Average angular resolution Δα < 2° (goal 1°) @ E≤1020 eV
Energy resolution ΔE/E ≤ 0.1 @ E≤1019 eV
EAS maximum determination ΔXMAX ≤ 50 (20) g cm-2
Orbit height variable 800 (goal 500) -1200 km
Operational life 5 yr on-orbit operational life (goal is 10 years)
Andrea Santangelo, IAAT-KCT
Is such a challenging mission technologically and technically feasible ?
Andrea Santangelo, IAAT-KCT
Entrance Pupil with correcting
plate and/or filter
Light shield
Focal surface
4.48 m Ø
7.5 m
Effort 1: Optics • Schimdt Telescope, a
single spherical mirror (Zerodur 1 mm thick)+ a front correcting plate
7.0/#f
m12Dpm
m48.4DFS
m5.7Dep
7.0os
2015f optimpr
Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW
Optics DeployabilityA 4 m deployable mirror for LIDAR application is under development on a ESA contract (ITT AO/1-4629/NL/CP Ref. 2053, Advanced Lidar Concept, ALC)
Courtesy of Carlo Gavazzi Space SpA
OWL Concept study
Stecker et al. 2004
Andrea Santangelo, IAAT-KCT
Effort 2: Focal Surface • GAPD, Geiger Mode Avalanche
Photodiodes is the baseline sensor• High filling factor • High detection efficiency (>60%)• Single Photon Counting
3f pdeimpr 6.0pde
6045f totimpr
5x5 mm2 GAPD (SiPM) developed by MPI and MEPhl
4x4 mm2 GAPD developed by FBK and IRST (Italy)
Otte, ICRC07
eV10x1E 19th
Andrea Santangelo, IAAT-KCT
Conclusions• JEM-EUSO is in Phase A Study, in the framework of the second call for
the utilization of the japanese module of the ISS. If selected it will be launched in the 2013 time window.
• JEM-EUSO is expected to significantly contribute to UHECR astronomy and possibly It will detect UHE Neutrino. But it will be also a pathfinder…
• A Free Flyer Mission with an exposure of A> a few 106 km2 sr yr +energy threshold of E<1019 eV hosting deployable Optics and High Quantum Efficiency Photo Sensors is feasible S-EUSO is being considered for “enabling technology” studies.
• S-EUSO is expected to identify and study the spectral properties of celestial sources of Cosmic Rays. UHE Neutrino will be detected and studied, and new physics could emerge.
Andrea Santangelo, IAAT-KCT
Parameters (1)
Andrea Santangelo, IAAT-KCT
Parameters (2)
Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW
Japan : T. Ebisuzaki, Y. Uehara, H. Omori, Y. Kawasaki, M. Sato, Y. Takizawa, T. Wada, K. Kawai (Riken), F. Kajino, M. Sakata, H. Sato, Y. Yamamoto, N. Ebizuka, (Konan Univ.), Y. Miyazaki (Fukui Inst. Tech.), N. Sakaki, T. Shibata (Aoyama Gakuin Univ.), N. Inoue (Saitama Univ.), Y. Uchihori (NIRS), K. Nomoto (Tokyo), Y. Takahashi (Tohoku Univ.), M. Takeda (ICRR, Univ. Tokyo), Y. Arai, Y. Kurihara, H. Shimizu, J. Fujimoto (KEK), S. Yoshida (Chiba Univ.), K. Asano, S. Inoue, Y. Mizumoto, J. Watanabe (NAOJ), H. Ikeda, M. Suzuki, T. Yano (ISAS, JAXA), T.Murakami, D. Yonetoku (Kanazawa Univ.), N. Sugiyama (Nagoya), Y. Ito, Y. Muraki (STEL, Nagoya Univ.), S. Nagataki (YITP, Kyoto Univ.), A. Saito(Kyoto Univ.), S. Abe, M. Nagata (Kobe Univ.), T. Tajima (KPSI, JAEA)USA : J. H. Adams, S. Mitchell, M.J. Christl, J. Watts Jr., A.English (NASA MSFC) , Y. Takahashi, D. Gregory, M. Bonamente, P. Readon, V. Connaughton, K. Pitalo, J.Hadaway, J. Geary,R. Lindquist, P. Readon (Univ. Alabama in Huntsville), H. Crawford, C. Pennypacker (LBL, Univ. California, Berkeley), K. Arisaka, D. Cline (UCLA), T. Weiler, S. Czorna (Vanderbilt Univ.)France : J-N. Capdevielle, P. Gorodetzky, P. Salin, D. Semikoz, G. Sigl (CNRS), J. Dolbeau (Coll. de France), E. Parizot, T. Patzak, F. Vanucci (Univ. Paris 7), J. Weisbard (IN2P3)Germany: M. Teshima (Max Planck Munich), A. Santangelo (Tuebingen), P. Biermann (MPI Bonn), K. Mannheim (Wuerzburg)Italy : S. Bottai. P. Spillantini, A. Zuccaro (Firenze), Anzalone, O. Catalano, G. D'Ali Saiti, M.C. Maccarone, P. Scarsi, B. Sacco (Palermo), B. M. Casolino, M.P. De Pascale, A. Morselli, P. Picozza, R. Sparvoli (Roma 2), M. Bertania, A. Cappa, M. Dattoli, P. Galeotti, P. Vallania, C. Vigorito, (Torino), A. Gregorio (Trieste) Mexico: G. Medina-Tanco (Mexico UNAM), H. Salazar (Puebla)Republic of Korea : S. Nam, I. H. Park (Ehwa W. Univ.)Russia: Garipov G.K., Khrenov B.A., Klimov P.A. Panasyuk M.I., Yashin I.V. (SINP MSU), Naumov, D., Tkachev. L (Dubna JINR)Switzerland : A. Maurissen, V. Mitev (Neuchatel, Switzerland)
9 countries, 46 institutions, 120 membersJEM-EUSO Collaboration
Andrea Santangelo, IAAT-KCT
“SSAC strongly recommends enabling technology studies…”
“…in the field of UHE Cosmic Rays”
(that is S-EUSO)
• Clarify with ESA the critical technologies…
• Feedback from ESA
Andrea Santangelo, IAAT-KCT
Future key goal: be competitive for the next run of proposals in 2010
• Identify the critical enabling technologies
• Address the Agencies (ESA+National)
• Try to have access to R&D resources from ESA + Agencies
• Decisions will be taken in June-July (at the next SPC)
Andrea Santangelo, IAAT-KCT
the scientific requirements
Effective Aperture E>5x106 km2 sr yr (Nadir Mode)
E~107 km2 sr yr
Low energy threshold 100% at E≤1019 eV
Average angular resolution Δα 1° -3° @ E≤1020 eV
Energy resolution ΔE/E ≤ 0.1 @ E≤1019 eV
EAS maximum determination ΔXMAX ≤ 20 g cm-2
Orbit height variable 800 (goal 500) -1200 km
Operational life 5 yr on-orbit operational life (goal is 10 years)
Andrea Santangelo, IAAT-KCT
Comparison of the Observational Effective Aperture
Experiment Acceptance(km2 sr) Operational Period
Operational Life
(years)
Observational Efficiency
( % )
Exposure(km2 sr year )
Relative Exposure
Auger SouthSD
FD=HybridAuger North SD
7,0007,000
21,000
2006-20152006-2015(conceptual)
10+10+(10+)
10010
100
7.0 ×104
7.0 ×104
21.0 ×104
10.1(3)
Telescope ArraySDFD
6,7001,400
2008-2015 1010
10010
1.4×104
6.7×103
0.20.1
TUS 30,000 2009-2014 5 20 3.0×104 0.5
JEM-EUSO nadirtiltedTotal
1200,0006,000,000
2013-20152015 -
23+(5)5+(5)
202020
4.8×105
3.6 ×106
4.1 ×106
6.9 in two years52+(87)59+(87)