JEMEUSO mission Astronomy with UHECRs

1
JEM-EUSOmissionAstronomy with UHECRs

• Masahiro Teshima
• Max-Planck-Institute for Physics
• For JEM-EUSO collaboration

2
Proposal was submitted to JAXA (Japanese space
agency) AO for second phase ISS utilization
program
Official Proposal to JAXA
Supplements
30 pages
82 pages
3
Physics Objectives of JEM-EUSO

• Origin of Ultra High Energy Cosmic Rays
• Energy Spectrum of cosmic rays above 3x1019eV
• GZK cutoff or extension
• Beyond GZK energy
• Arrival directions of cosmic rays above 1020eV
• Matter/AGN density distribution within 50-100Mpc
• Number of events above 1020eV gt Number of sources
  (10-100)
• To establish sources, we needs at least 10
  events/sources
• Fundamental physics
• Look for exotic origin (gamma rays, neutrinos)
• Neutrino cross-section (extra-dimension, etc)
• Test of Lorentz invariance at ?1011
• Earth Science
• Study of atmospheric night-glow, plasma-discharge
  and lightning

4
Candidates for UHECR accelerator
A.G.N.
GRB
Radio Galaxy Lobe
5
UHECR Propagation in our Galaxy

• Deflection angle 1 degree at 1020eV
• Astronomy by hadronic particles?

6
Full sky map of deflection angles
By K.Dolag, D.Grasso, V.Springel, and I.Tkachev
7
Matter (90Mpc) and Galaxies(45Mpc)
By A.Kravtsov
8
Cosmic Ray Energy Spectrum
9
(No Transcript)
10
JEM-EUSO Telescope on ISS
JEM-EUSO Telescope will be attached to Exposure
Facility of Japanese Experiment Module (JEM/EF)
of ISS in 2012- 2013
Vertical Mode
Tilted Mode
Larger effective area (x5) with 35tilt
11
EUSO 300 x AGASA 10-50 x Auger EUSO
(Instantaneous) 3000-15000 x AGASA 100-500 x
Auger
JEM-EUSO tilt-mode
AGASA
12
Astronomy with UHECRs JEM-EUSO
Matter (lt90Mpc), Galaxies (lt45Mpc) by A.Kravtsov
X30 Auger South UHECRs 2x106km2sr year UHE ? 20
T-Ton year
13
Configurations of JEM-EUSO in Launch and Deployed
phases
14
JEM-EUSO in HTV
15
Acceptance and Exposure
PMMA ? CYTOP (X1.5) UBA MAPMT (X1.5) Line
integration trigger (x2.0)
16
Sensitivity for UHE Neutrino
17
EUSO Instrument
18
JEM-EUSO Focal Surface
19
QE Measurement for R7600U-200 UBA PMT (by
C.C.Hsu, MPI-Munich)
Q.E. peak 41
Q.E. peak 38
UBA(Ultra-Bialkali) photocathode
20
Air shower imaged data
simulation
20 events of 1020eV proton showers are
superimposed on the EUSO focal surface with 192
k pixels.
4
21
JEM-EUSO Level-0 Specification 1

• Science Requirements
• More than 1000 events above 71019 eV
• Determine arrival direction to a few degrees or
  less, and identify the source
• Clarify the entire structure of the trans-GZK(5 x
  1019lt E lt 1021 eV)
• Observational Requirements(e.g. E1020eV, Zenith
  angle 60?)
• Observational area ? 7105 (H/400 km)2 km2 sr
• Accuracy of arrival direction ? 2.5
• Energy resolution ? 30
• Xmax Resolution ? 120 g cm2
• Requirements of the Instruments
• Detection Efficiency ? 10
• Loss of efficiency ? 30 than specification
  during operations
• Lifetime ? 2 yrs (and 2 yrs storage time before
  launch)
• Accuracy of attitude control ? 0.05?, allowing
  off-line correction)
• (absolute) clock and timing accuracy ? 1 ms

22
JEM-EUSO Level-0 Specification 2

• Spec of the Instruments
• Field of View Wide-field 30 degree
• Aperture Diameter 2.5m
• Optical bandwidth 330-400nm
• Angular Resolution 0.1 degree
• Pixel Size ? 4.5mm
• Number of Pixels 2.0105
• Pixel Size at the ground 750m
• Duty Cycle 20
• Observational Area 1.9105 km2 and x 3 - 5
  larger by tilt
• Parameters of Mission
• Time of launch 2012-13
• Operation Period 3 years (2 - 5) years
• Launching Rocket H2B
• Transportation to ISS non pressurized
  Cargo-Carrier of H2 Transfer Vehicle
• Site to Attach Japanese
  Experiment Module/ Exposure Facility E2
• Mass 1880 kg
• Power 1031 W (operative) 344 W (non-operative)
• Data Transfer Rate 360 kpbs

23
H-II, HTV (H-II Transfer Vehicle)
24
HTV, HTV prototype
25
(No Transcript)
26
(No Transcript)
27
Time schedule and etc.

• Time schedule
• We will hear the judgment from JAXA this May we
  are very optimistic
• After two years of Phase-A study, there is a
  critical review of the mission
• In 2009-2012, JEM-EUSO will be build
• Launch is expected in 2012 or 2013, as a program
  in the second phase of ISS utilization
• Physics
• More focus on the Astronomy with UHECRs
  (gt1000events above GZK cutoff, 1020eV)
• Deliver the skymap of UHECRs with 100010,000
  events above 1020eV

28
Thanks