RIKEN – GRC
Ultra-High Energy Cosmic Ray Observation
from Space: The JEM-EUSO program
M. Casolino, T. Ebisuzaki,
Y. Kawasaki, Y. Takizawa
on behalf of the JEM-EUSO collaboration
UHEAP 2016
Chicago, 29/2/2016
Advantages
Statistics:
Several orders of magnitude of active area
Uniform sky coverage
Uniform distance from shower
Expensive, space constraints
Small signal Large optics
Disadvantages
Non-hybrid
Naturally complementary to ground
Observations from Space
Historical notes (2)
Approved by ESA on Columbus.
Canceled after Columbia accident.
Moved to JEM (Japanese) module
Previous space missions
Past Present Future
JEM-EUSO
Limadou – CSES
PAMELA
AGILE
Fermi
Space Stations
MIR, ISS
CAPRICE, MASS, TS93
Balloons
NINA-1 and NINA-2
Satellite
NINA-2 Satellite
Sil-Eye 1
Sil-Eye 2
Alteino
LAZIO
ALTEA
Gamma-400
K-EUSO
ApJ 457, L 103 1996
ApJ 532, 653, 2000
arXiv:0810.4994, PRL,
NJP11,105023
Nature,
Astrop. Phys
Science 2011
arXiv:1103.4055
ApjL 799 4 2015
2008AdSpR..41..168C
2008AdSpR..41.2037D
2008AdSpR..41.2043C
Prl 111 1102 203
PrL 106 1101 2011
PrL105 121101 2010 --
Physics Reports
544, 4, 323-370 Apj 795 91 2013
Apj 770 2 2013
Apj 791 2 2014
Acceleration
mechanisms
are still
unkown even
at GeV-TeV
range
Pamela galactic particles
2006-2008
g30- 1000GV, p = 2.820 +- 0.003 (stat) +- 0.005 (syst)
g30- 1000GV, he = 2.732 +- 0.005 (stat)
+ 0.008 -0.003 (syst)
• Different spectral index
for proton and helium.
• Helium percentage is
growing with rigidity
• Challenges Supernova
only origin of cosmic
ray and/or
acceleration/propagation
models.
• +positron source Science 2011, 332 no. 6025 pp. 69-72
JEM-EUSO
International collaboration
• 16 countries, 200+ researchers
• Science Evaluated positively by ESA, NASA, Roscosmoc and national agencies
• Funding for detectors and precursors ongoing in all countries
12
- pioneer the study of
Extreme Energy
Cosmic Rays (EECR)
from Space
- increase exposure to
EECR by at least one
order of magnitude
- discover the sources of
UHECRs
JEM-EUSO goals
Road to space
Development of novel technologies
- Optics
- Detectors
- Electronics
Construction of precursors and pathfinders
- ground
- balloon
-space
AMS Launch
May 16, 2011
JEM-EUSO: Extreme Universe Space Observatory onboard Japanese Experiment Module
~ 4 ~
JEUSO-110025-01-E-TR-ZZZ
since the mean distance to EAS and atmospheric absorption both increase. First few years of the
then later to
Figure 1-2. Artistic illustration of the JEM-EUSO telescope attached to the Japanese Experiment Module of the International Space Station, under nadir (left) and tilt (right) mode of observation.
The JEM-EUSO telescope can reconstruct the incoming direction of the EECRs with accuracy
better than few degrees. Its observational aperture of the ground area is a circle with 250 km
radius, and its atmospheric volume above it, with a 60° FoV, is ~1 Tera-ton or more. The target
volume for upward neutrino events exceeds 10 Tera-tons. The instantaneous aperture of JEM-
EUSO is larger than the Pierre Auger Southern Observatory by a factor ranging from 65 to 280,
depending on its observation mode (nadir or tilted, Fig.1-3).
JEM-EUSO, planned to be attached to JEM/EF of ISS, will be launched in the JFY 2016 by
H2B rocket and conveyed to ISS by HTV (H-II transfer Vehicle).
Figure 1-3. Area observed by the JEM-EUSO telescope in one shot under mode.
ISS-CREAM
Sp-X Launch 2014
JEM-EUSO
Launch Tentatively
planned for 2019
CALET on JEM
HTV Launch 2014
View from NASA: “Cosmic Ray Observatory on the ISS”
image from Drs. Julie A. Robinson, Program Scientist, ISS, NASA & W. Vernon Jones, Senior Scientist, SMD, NASA
EUSO in Russia: Klypve
• In the Federal Space Program
• Adding Fresnel lenses increases f.o.v. several times
• Highest ranking in joint 2014 evaluation by NASA and TsNIIMASH (Russia)
1. EUSO-TA: Ground
detector installed in 2013 at
Telescope Array site:
currently operational
2. EUSO-BALLOONS: 1st
balloon flight from Timmins,
CA (French Space Agency)
Aug 2014; NASA Ultra long
duration flight: 2017
3. MINI-EUSO (2017): Precursor from International
Space Station (ISS: 30kg
2017). Approved by Italian
and Russian Space agencies
4. K-EUSO (2019 JFY): ISS Approved by Russian
Space Agency
5. JEM-EUSO (2023): ISS
US-led EUSO-NEXT 2035
The EUSO program Ultra-High Energy
cosmic rays from space
MINI-EUSO
400 km
EUSO-TA (2013-)
EUSO-BALLOONS 40 km
EUSO-TA
JEM-EUSO
(2023+)
EUSO-TA
First data taking campaign in
March 2015, 6 shifts.
Also used for Auger/Fast tests
• Laser: Mobile (up to 100km)
CLF of TA
• Cosmic ray
• Meteors
3rd groove surface roughness measurement
Electrical noise
RMS surface roughness requirement : < 0.0200um (=20nm)
Lens precision: 20 nm
Validation of EUSO technology
Optics and electronics can
see cosmic rays
Self-trigger with euso
electronics on laser
Laser: distances of
20,40,60,100 km.
Equivalent to space+atm.
Absorption
(50 mJ laser)
First Cosmic ray event
EUSO, 1 frame, 2.5micros EUSO, 2*2 TA signal
BRM, May 2015
1018 eV, triggered from TA
Meteor candidates
The objects cross ~6 deg in 0.7-2 s, so 8.5 deg/s. This gives full rotation around Earth in ~42 s, so it can't be a satellite.
Meteor candidates
The objects cross ~6 deg in 0.7-2 s, so 8.5 deg/s. This gives full rotation around Earth in ~42 s, so it can't be a satellite.
2. EUSO-Balloon flights
1st flight, Aug 2014 Timmins (CA)
Payload built by JEM-EUSO collaboration CNES (French Space Agency) mission
EUSO-Balloon 2nd flight, March 2017 Wanaka, New Zealand
NASA Mission. 1st Super Pressure Science Flight Payload built by JEM-EUSO collaboration New lenses, Focal Surface, Electronics More than 30 days First UV UHECR shower observation from above
Special Issue on the EUSO Mission • 20+ papers addressing science and technology of EUSO
• The EUSO-Balloon pathfinderThe JEM-EUSO instrument
• Ground-based tests of JEM-EUSO components at the Telescope Array site, “EUSO-TA”
• Space experiment TUS on board the Lomonosov satellite as pathfinder of JEM-EUSO
• The JEM-EUSO observation in cloudy conditions
• Calibration aspects of the JEM-EUSO mission
• JEM-EUSO: Meteor and nuclearite observations
• JEM-EUSO observational technique and exposure
• Ultra high energy photons and neutrinos with JEM-EUSO
• Science of atmospheric phenomena with JEM-EUSO
• Performances of JEM–EUSO: energy and X max reconstruction
• The atmospheric monitoring system of the JEM-EUSO instrument
• The infrared camera onboard JEM-EUSO
• Proposal of a Computing Model Using GRID Resources for the JEM-EUSO Space Mission
3. MINI-EUSO
• Approved & financed by Italian Space Agency
• Approved & financed by Russian Space Agency
• Inside the ISS
• 2 Fresnel lenses and one PDM
• 30W @ 27V
• 30kg not incl SSD
Cad model by F. Capel
Alteino & Lazio detectors inside PIRS module of ISS
To Soyuz
To ISS
LAZIO and Alteino detectors on ISS (2005)
Grounding
28V power
supply
PCMCIA
card
• UV emissions from night-Earth 6.5 km resolution, from 2.5mus and above +-51°
Noise from different lightning conditions, moon phase
Noise from different inclinations
• Map of the Earth in UV
• Study of atmospheric phenomena
TLE in the ms range
lightning – cr correlation
• Bioluminescence of Animal and vegetal organisms
white sea
plankton
MINI-EUSO
Scientific objectives
• First use of Fresnel lenses
in space
• Optimization of
characteristics and
performances of EUSO
• Raise the technological
readiness level of the
Hardware
• Ttest new HW in space
MINI-EUSO Technologial objectives
Japan-led
JEM module
Refractor
2.5 t
2kW
10*Auger
Russian-led
MRM module
Reflector (mirror)
600kg
600W
2*Auger
From JEM-EUSO to K-EUSO
K-EUSO
• In the Russian Federal Space Program
• Passed the stage of preliminary design with Roscosmoc
• Technical requirements, accomodation, operations study performed by Energia space corporation
• Evolution of KLYPVE Russian
detector (reflector)
• Mission of opportunity Launch in FY 2019
Uniform response over both hemispheres
Some (5%)
disuniformity due
to clouds,
continents and
moon phase
Science of K-EUSO
KLYPVE detector goes
from technological
demonstrator to instrument
capable of:
1. Study of UHECR fux
from space with uniform
response
2. flux E>3 1019 eV
north & south
4. Anysotropy
3. Earth observations
Additional Science objectives
105
Search for Strange Quark Matter
Measurement of Meteorites
Study of Transient Luminous effects
In ms range Map of night Earth in UV
Bioluminescence
Possible N-S spectral difference
N_events E>5.7e19 eV 120
Used Auger and TA spectra 2015 in each hemisphere
N_events E>5.7e19 eV 700
1yr sky map assuming TA hotspot
N_ho
t
N_B
G
Significan
ce
Total # of
events
1yr 16.2 3.8 3.1 117.3
2yr 32.5 7.6 4.4 234.7
6yr 97.4 22.9 7.5 704.0
6 years
1 year
Programmatic status of K-EUSO 1. 2013 MSU proposal of KLYPVE included in
Russian space program
2. 12-2013 MSU invited JEM-EUSO collaboration to join KLIPVE
4. 2014 JAXA call mission of opportunity
5. 2-2014 Proposal Submitted
6. 8-2014 passed MDR 7. Roscosmos-NASA joint 9-2014 Signing of
science protocol and role sharing between MSU and Riken, 12/2014 with int. Partners
8. 12-2014 SRR docs submitted to JAXA (>500 pages)
9. passed SRR in April 2015
2015 Funding from JAXA for assessment of
EUSO technology in space 13,200,000円
H27.6.1-H28.2.28
USA-led
JEM module
Refractor
2.5 t
2kW
20*Auger
Russian-led
MRM module
Reflector (mirror)
600kg
600W
2*Auger
Full cylindrical geom Dragon launcher
From JEM-EUSO to K-EUSO … to JEM-EUSO
Space X Falcon-9 rocket
& Dragon spacecraft • Reusable
• Return cargo capability – 3 ton
• Pressurized and unpressurized cargo
• Two flights to ISS
• 6ton upload mass
• 14 m payload volume
• Optional trunk extension for a total of up to 4.3 m length, payload volume 34 m3
Conclusions
K-Euso is a concrete mission of opportunity improving with high international component a factor 10 Russian Klypve with advanced lens and PMT technology.
Fraction of the cost of JEM-EUSO
In one year from launch Address several fundamental physics issues, N/S, hotspot
Next year we will have balloon flight and Mini-EUSO flight
Need to prepare for JEM-EUSO