JEM-EUSO: la misión espacial para la detección Del Universo a … · 2011-07-07 · • The AMS...
Transcript of JEM-EUSO: la misión espacial para la detección Del Universo a … · 2011-07-07 · • The AMS...
JEM-EUSO: la misión espacial para la detecciónDel Universo a las energías más extremas.
. M.D.Rodríguez Frías for JEM-EUSO Spanish Consortium. http://spas.uah.es/SPace & AStroparticles (SPAS) Group. UAH.
I. Why the origin of Cosmic Rays is stillunknown ?
II. Why a space-based experiment for CosmicRays detection ?
III.Spanish contribution to JEM-EUSO:Mid-IR camera & 137 HVPS.
Overview
MD. Rodríguez Frías. ASTROMADRID, June 29, 2011.
Due to magnetic deflections in EGMF & GMF, veryhigh statistics at EHECR are crucial to identifysources and established:
“Particle-Astronomy” @ E> 1020 eV
Why the origin of CR’s is still unknown ?
I. CR-Astronomy is only possible @ E>100 EeV.
II. Huge statistics at EHECR’s is needed
Why the origin of CR’s is still unknown?
MD: Rodríguez-Frías. JEM-EUSO meeting @ Spain, February 9th, 2009.
Anisotropy of UHECR has been established @ > 99% CL27 events with P = 2x10-10@ E=57 EeV, z=0.017 & =3.2º. GZK sphere: D~100 Mpc.
Pierre Auger Collaboration. Science,
Particle Astronomy
- 1,000 events : E>7x1019eV- Several dozen clusters are expected. All sky coverage
If we get >1,000 events,
by Boris Khrenov 2006
Progress of EECRs Observation in the near future:
4×105JEM-EUSO(nadir)
JEM-EUSO (tilt)
Why a Space-based experiment for CR´s detection ?
Why a space-based experiment for CR’s detection ?
Experiment Acceptance(km2 sr) Operational Period
Operational Life
(years)
Observational Efficiency
( % )
Exposure(km2 sr year)
Relative Exposure
Auger SouthSD
FD=Hybrid 7,0007,000
2006-20152006-2015
10+10+
10010
7.0 ×1047.0 ×104
10.1
Telescope ArraySDFD
1,4006,700 2008-2015 10
10
10010
1.4×1046.7×103
0.20.1
TUS 30,000 2009-2014 5 20 3.0×104 0.5
JEM-EUSOnadirtiltedTotal
520,0002,580,,000
2016-20172018-
23+(5)5+(5)
202020
2.1×1051.5 ×1061.7 ×106
4 in two years25+(42)30+(42)
EUSO ~ 1000 x AGASA ~ 30 x AugerEUSO (Instantaneous) ~ 5000 x AGASA
~ 150 x Auger
AGASA
JEM-EUSO tilt-mode
JEM-EUSO FoV
Japan : T. Ebisuzaki, Y. Uehara, H. Ohmori, Y. Kawasaki, M. Sato, Y. Takizawa, K. Katahira, S. Wada, K. Kawai,H. Mase (RIKEN), F. Kajino, M. Sakata, H. Sato, Y. Yamamoto, T. Yamamoto, N. Ebizuka, (Konan Univ.), M.Nagano, Y. Miyazaki (Fukui Inst. Tech.), N. Sakaki, T. Shibata (Aoyama Gakuin Univ.), N. Inoue (Saitama Univ.), Y.Uchihori (NIRS), K. Nomoto (Univ. of Tokyo), Y. Takahashi (Tohoku Univ.), M. Takeda (ICRR, Univ. Tokyo), Y. Arai,Y. Kurihara, H.M. Shimizu, J. Fujimoto (KEK), S. Yoshida, K. Mase (Chiba Univ.), K. Asano, S. Inoue, Y. Mizumoto,J. Watanabe, T. Kajino (NAOJ), H. Ikeda, M. Suzuki, T. Yano (ISAS, JAXA), T.Murakami, D. Yonetoku (KanazawaUniv.), T. Sugiyama (Nagoya), Y. Ito (STEL, Nagoya Univ.), S. Nagataki (YITP, Kyoto Univ.), A. Saito(Kyoto Univ.),S. Abe, M. Nagata (Kobe Univ.), T. Tajima (KPSI, JAEA)、M. Chikawa (Kinki Univ.), and M. Tajima (HiroshimaUniv.)USA : J. H. Adams Jr., S. Mitchell, M.J. Christl, J. Watts Jr., A. English, R. Young (NASA/ MSFC) , Y. Takahashi, D.Gregory, M. Bonamente, K. Pitalo, J. Hadaway, J. Geary, R. Lindquist, P. ReardonT. Blackwell (Univ. Alabama inHuntsville), H. Crawford, E. Judd, C. Pennypacker (LBL, UC Berkeley), K. Arisaka, D. Cline, J. Kolonko, V.Andreev (UCLA), A. Berlind, T. Weiler, S. Csorna (Vanderbilt Univ.), R. Chipman, S. MaClain (Arizona)France : D. Allard, J-N. Capdevielle, J. Dolbeau, P. Gorodetzky, J. J. Jaeger, E. Parizot, T. Patzak, D. Semikoz, J.Waisbard (APC-Paris 7)Germany: M. Teshima, T. Schweizer (Max Planck Munich), A. Santangelo, E.Kendziorra, F.Fenu (Univ. Tuebingen),P. Biermann (MPI Bonn), K. Mannheim (Wuerzburg), J. Wilms (Univ. Erlangen)Italy : M. Focardi, E. Pacce, P. Spillantini (Univ.Firenze), V. Bratina, L. Gambicorti, A. Zuccaro (CNR-INOA,Firenze), A. Anzalone, O. Catalano, M.C. Maccarone, P. Scarsi, B. Sacco, G. LaRosa (IAS-PA/INAF), G. D’AliSaiti, D. Tegolo (U. Palermo), R. Battiston (Perugia), M. Casolino, M.P. De Pascale, A. Morselli, P. Picozza, R.Sparvoli (INFN and Univ. Rome “Tor Vergata”), P. Vallania (INAF-IFSI Torino), P. Galleotti, C. Vigorito, M. Bertaina(Univ. Torino)
Mexico: G. Medina-Tanco, J.C. D’Olivo, J.F.Valdes (Mexico UNAM), H. Salazar, O. Martines (BUAP), L. Villasenor(UMSNH)Republic of Korea : S. Nam, I. H. Park, J. Yang (Ehwa W. Univ.)
Russia: Garipov G.K., Khrenov, B.A., Klimov P.A. Panasyuk M.I., Yashin I.V. (SINP MSU), D. Naumov, Tkachev. L(Dubna JINR)Switzerland : A. Maurissen, V. Mitev (Neuchatel, Switzerland) :
Spain: M.D.Rodriguez-Frias, L.del Peral, JA. Morales de los Ríos, G. Sáez, H. Prieto, N. Pacheco, J. HernandezCarretero(UAH), M.D. Sabau, T. Belenguer, C. González-Alvarado (NTA), F. López, A. De Castro,. S. Briz F.Cortés UC3M), J. Licandro, E. Jóven, M. Serra, V. Ali, O. Vaduvescu (IAC).
JEM-EUSO Collaboration
Parameters of Mission
Time of launch: year 2016 Operation Period: 3 years (+ 2 years) Launching Rocket : H2B Transportation to ISS: non pressurized Carrier of
H2 Transfer Vehicle (HTV) Site to Attach: Japanese Experiment Module/
Exposure Facility #2 Height of the Orbit: ~430km Inclination of the Orbit: 51.6°
Mass: 1983 kg Power: 926 W (operative),
352 W (non-operative) Data Transfer Rate: 285 kpbs
Approved Phase A 2007-mid 2009 by JAXA.
Phase B1+ SRR: mid 2009-2011.
Phase B2+BBM+PDR: 2012.
Construction, Assembly & Verification: 2013-2015.
Launch by HIIB-HTV & Commissioning 2016.
Operation period:2016-2018 (Nadir mode).2019- (Title mode).
Resources:90.000 k€-26.000 k€ Europe ( 33% Europe, 66% Others).
JEM-EUSO Status
ESA committees Reviews • 2010: ESA: “Fundamental Physics Roadmap Advisory Team
(FPR-AT)”• 2010: ESA “Astronomical Working Group (AWG)”.• 2010: Program ELIPS (European programme for Life and P
hysical sciences and applications) accepted by the ESA committee for “Human Spaceflight, Microgravity and Exploration”.
• 2010: The Science Unit of The European Space FoundaKon (ESF) has informed positively the JEM-EUSO space mission.
• April 2011 ESA Topical Team for Coordination of the European Involvement in JEM-EUSO.
Spanish contribution since 2007 (MOU: UAH-RIKEN).
JEM-EUSO funded in Spain (2009-2011) fromMICINN+CAM+UAH.
Dec 2009: Feasibility Study. Aug 2010: Phase A. Dec 2011: Phase B1 & SRR (ongoing).
Just submitted to MICINN for the first time a coordinatedproject for Phase B2 (BBM & PDR) to be delivered to Japanby Dec 2012.
III. JEM-EUSO Consortium @ Spain
4 research centers: UAH, INTA, UC3M & IAC. 4 Space companies: SENER, LIDAX, SENSIA &
ARQUIMEA
IR Camera Overall Description
• The AMS IR Camera is based on a microbolometer sensor, minimizing the risk associated to the low TRL of PbSe sensors and providing access to a more typical spectral band (8-14 microns) for this kind of measurement.
• The AMS IR Camera current design is a multiband system, taking advantage of the flat spectral response of its detector over a wide spectral range (but at the expense of an increased data rate).
Parameter Pre-design value
Measurement Range 220K – 300 K (200K – 320K TARGET)
Spectral Range
B1: 10.2-11.2 microns
B2: 11.5-12.5 microns
B3: 14.4-15.4 microns (CALIBRATION over CO2 absorption line)iFoV 60ºx45º
Angular Resolution 0.1 º @ FOV center (= 4.4 mrad) [0.25º THRESHOLD]
Absolute temperature accuracy TBD. Depends on final NETD for the selected bands and calibration accuracy [+/-3K TARGET]
Mass 14 kg (20% margin included) [7kg TARGET]
Power 22 W (20% margin included) [11W TARGET]
Dimensions 400x300x225mm [300x300x500mm MAX.]
IR Camera Detector (Microbolometer)
1. Candidates already identified in December 2009 report.2. Baseline is ULIS-IR microbolometer, with the following parameters:
3. A 6-month qualification plan using a set of 20 detectors has been prepared. It should be executed before PDR. Alternative detectors may be subjected to ITAR (but this should not be a problem for the JEM-EUSO mission).
IR Camera Optical Design
2 3 5 6
7 8
10 11 12
13
EUSO Scale: 2.00 ORA 18-Jun-10
12.50 MM
EFL=10 mm #F=1 REFRACTIVE INDICES (8-12 microns)GLASS Name (nm) 12000.00 10400.00 8000.00GERMANIUM 4.002215 4.003118 4.005632
Cold Stop
IR Camera Thermal & Mechanical Design
• Filters and calibration blackbody (BB) inserted between the optics and the detector (roughly at exit pupil).
• IMAGING mode. Filters B1 and B2 are exchanged each ~10 seconds in order to obtain overlapped images of the camera FoV (60ºx45º). Stereo reconstruction is possible with this configuration for each spectral band.
• CALIBRATION mode. A complete sequence (B1-B2-B3-BB) is performed in less than ~40 seconds to avoid any loss of data. Calibration frequency needs to be analyzed.
SATELLITE IF
Mechanism
Baffle & optics
Filter 3
Black Body
Shielding & MLI
Optical bench
Detector & TEC
Radiator
ICU-CCU-PSU
Filter 2
Filter 1
Sensia (UC3M SPIN OFF) contribution to JEM-EUSO Mission
Simulation of the radiometric transfer problem in cloudscenarios of interest in JEM-EUSO
Algorithms development for cloud temperature retrievalbased on a microbolometer IR camera
Development of a laboratory a camera breadboard basedon a VOx focal plane array for testing multispectralresponse.
VOx engine
LWIR optics50 mm
Blackbody
Output Image
Control and acquisition system
LIDAX contribution to JEM-EUSO IRCAM Phase AMain Goals
• Consolidate thermo-mechanical architecture and definition of Thermal Control S/S
• Support to System Engineering in the elaboration of Requirement List and SRR documentation
LIDAX contribution to JEM-EUSO IRCAM Phase A
• Thermal Control S/S requirements capture based on:– Current opto-mechanical design– Current Tolerancing analysis– Components temperature range specification– Thermal Environment
• Thermal Control S/S Architecture trade-off– ¿Active or Passive?– Heating or cooling– Sensors ¿?
• Thermal analysis at Instrument and S/S level will support this architecture
• Contribution to documentation• Structural analysis
Use the experience and know-how of Arquimea in the design of ASICs for space application (“rad-hard” techniques and high reliability)
European foundry service specialized in microbolometer (α-Si) deposition techniques would be used for microbolometer deposition over custom
ROIC.
Custom microbolometer designed to fit specific requirements of the project.
ARQUIMEA Custom Microbolometer Development
ARQUIMEA Multispectral monolithic device
IR camera proposal follows a bi-spectral philosophy.As baseline a filter-wheel is proposed. But this approximation implies a hard impact in mass,volume and power budgets.A new innovative approximation is proposed: integrate in the same device the filters andthe microbolometer. This would permit remove the filter wheel obtaining a monolithicmultispectral device (in this case just a bi-spectral device is needed, but the approximation isvalid for more wavelengths)