andrea santangelo

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


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).


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


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


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


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


A key requirement for UHECR Astronomy

yrsrkm10A 26exp

L10A 6exp

• Identification of individual sources of UHECR and measurement of their energy spectrum

yrsrkm1Linsley1 2


Neutrinos at UHE?


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


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


Cosmogenic Neutrinos

)(p CMB

)()(e ee - oscillation:

e : : : : (at generic

source)

: : (at earth)

max.mixing, 13=0Berezinsky & Zatsepin, (1969, 1970)

Berezinsky (2005)


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)


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


The Extreme Universe Space Observatory

Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW hadronsN )NC(

hadronslN )CC(

ll

l


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


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


JEM-EUSO

Andrea Santangelo, IAAT-KCTMadrid, September 17, 2007, 5th FW

ISS Flight direction

51.6°

Japanese Experiment Module (KIBO) on International Space Station


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


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


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.


Progress 2: Industrial technical advancements

Helping advancing the JEM-EUSO capacity

MAPMT36PMTx36ch


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


Sources…

Simulation (1000 Events) De Marco/Blasi 2003


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


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


•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


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)


Is such a challenging mission technologically and technically feasible ?


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


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


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


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.


Parameters (1)


Parameters (2)


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


“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


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)


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)


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)

andrea santangelo

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