kosice, april 13, 2011
DESCRIPTION
JEM-EUSO in Poland. Jacek Szabelski Cosmic Ray Laboratory The Andrzej Sołtan Institute for Nuclear Studies Łódź http: //ipj.u.lodz.pl. Kosice, April 13, 2011. JEM-EUSO JEM – Japan Experiment Module EUSO – Extreme Universe Space Observatory. Main scientific target: - PowerPoint PPT PresentationTRANSCRIPT
Kosice, April 13, 2011
JEM-EUSO in Poland
Jacek SzabelskiCosmic Ray LaboratoryThe Andrzej Sołtan Institute for Nuclear StudiesŁódźhttp: //ipj.u.lodz.pl
JEM-EUSOJEM – Japan Experiment Module
EUSO – Extreme Universe Space Observatory
Main scientific target:
Measurements of ultra high energy
cosmic rays (UHE CR)Japan – 62USA – 27France – 19Germany – 25Italy – 46Mexico - 11Korea – 15Russia – 6Switzerland – 6Spain – 11Poland - 13Slovakia – 4Bulgaria - 7
plan to launch at 2016http: //jemeuso.riken.jp
Cosmic rays
Astrophysics (primary cosmic rays):energetic stable particlesenergetic – non-thermal energy distributionenergy range up to about 1e20 eV (is there a
limit ?)
stable particles:protons, nuclei, electrons, gammas,
neutrinos,anti-protons, positrons
Secondary cosmic rays:secondary energetic particles in atmospheregenerated by primary cosmic rayscoherent events: EAS (extensive air showers)
cascades of gammas, electrons/positrons, muons
and hadronsmuons
Cosmic rays: main scientific problems/questions
Cosmic ray sources:●Astrophysical sources●Physical/astrophysical mechanism of acceleration
High energy interaction properties(physics at energies above accelerator energies)
Ultra high energy cosmic rays studies●Measurements of energy spectrum●Measurements of primary particle masses●Measurements of direction of the events●(search for point-like sources,● isotropy/anisotropy)●Measurements of temporal variations
Cosmic ray energy spectrum
Direct measurementson balloons and satellitesup to 1e15eV(limited by:
exposure,energy
estimation )
Above 1e14 eVEAS measurements(problems with:
mass determination
energy estimation)
Knee
AnkleAnkle
LHC beam
How to accelerate particles ?
at CERN
now:3.5·1012 eV
from 2013 (?):7.0·1012 eV
JEM-EUSO would measureone particle with 7·1019 eV per day
The nature provides particles107 times more energetic than CERN
ground level observationsof EAS(extensive air showers)
animation: T.Wibig
Particles in EAS:photons (10 x Ne)electrons + positron (Ne)muons (0.1 x Ne)hadrons (0.01 x Ne)neutrinos
EAS particles goes with a speednearly c – light speed in vacuum(i.e. might be faster than light in the atmosphere)
typical EAS last about 30 microseconds (e.g. 10 km/c)
EAS Arrays for 1015 – 1018 eV
KASCADE
KASCADE-Grande
FzKarlsruhe
PAO – Pierre Auger Observatory(South hemisphere)
3000 km2
7000 km2 sr yr (θ<60°)
Expected 25 EAS/ year(E > 5.5 1019eV)
FD – fluorescence detectorsSA – surface array
FD & SA measurements
FD – only during clear dark nights
Auger North20500 km2
ECR > 3 1019eV
Expected 175 EAS/ year(E > 5.5 1019eV)
J.L.Harton, 31st ICRC
Starts 2011/2012
Northern hemisphere
Auger North20500 km2
ECR > 3 1019eV
Expected 175 EAS/ year(E > 5.5 1019eV)
J.L.Harton, 31st ICRC
Starts 2011/2012
Northern hemisphere
EAS longitudinal development vs. ground observation levels
VR – Volcano RanchYa – YakutskPAO – P.Auger Observatory
EAS array observationsat constantbut zenith angle dependentdepth (EAS development stage)
Figure shows an averageNe distribution;In real EAS development●fluctuates●depends on primary particle mass●interpretation depends●on the interaction models
The GZK Effect
Kenneth Greisen
George Zatsepin
Vadim Kuz'min
Greisen (1966) and, independently Zatsepin & Kuz’min (1966)
CMB
p +
+
n-resonance
multi-pion production
eepp
pp
np0
Energy spectrum: problems at the highest energies
Existence of GZK effectTest of Lorentz transformation
range of CR < 50 Mpc(ECR > EGZK)
Anisotropy / “sources” problems
POA: 27 events with ECR > 4 1019eV
Wibig + Wolfendale: mass of CR from „source” CEN-A ~ A=12(i.e. no protons, no iron nuclei)
●Measurements of energy spectrum (GZK cut-off)●Measurements of primary particle masses●(sources and GZK cut-off)●Measurements of direction of the events●(search for point-like sources,● isotropy/anisotropy)
Larger exposure (statistics) is neededto enable experimental solution
Observations from space !!
ISS – altitude about 400 km
neutrino shower
EAS
particles excite N2, N2 emits UV light
JEM-EUSO: fast camera400 000 frames per secondto measure events lasting about 30 μs
Vertical Mode Tilted Mode
Larger effective area (×5) with ~35°tilt
JEM-EUSO Telescope on ISS
JEM-EUSO observation areas (nadir and tilt)
Comparison of exposures
Optical system
Fresnel lens
Optical system – diameter about 2.4 m
Mutli-anode photomultipliers arrangement in FS
FC – Focal Surface = 137 PDMPDM – Photo-Detector Module = 36 MAPMTMAMPT – multi-anode photomultiplier
= 64 pixels1 pixel = 500m x 500m at ground level
new MAPMT – M64 – 64 anodes (pixels)M36
Photomultiplier (PMT)Multianode photomultiplier (MAPMT)
36 anodes MAMPT
photon → photo-electron →106 electrons (anode)
Background
●Reflection from sky●(Moon, stars, planets)●Man made light (cities)●Lightnings●Meteorites etc.
background estimation(per PMT):25 millions p-e per second
camera if very fast:GTU – gate time unit= 2.5 microsec
background:1 p-e per pixel per GTU
JEM-EUSO – Polish hardware contribution: 900V DC-DC suppliers for photomultipliers
Input power: 30-50 mW/PDM(preliminary)(400 times smaller than for standard solution)
HV suppliers:Cockcroft-Waltonand with transformer
Standard load due to light background:about 70 p-e per GTU per PMT
GTU – gate time unit = 2.5 microsec
TLE – Transient Luminous Events
TLE – transient luminous eventsdischarges to outer atmosphere
Such events last 0.5 – 100 millisec(1 millisec = 400 GTU)are extremely long and bright for JEM-EUSO detectorsPolish group from Space Research Centerand Slovak group from Space Physics Centerwould collaborate on TLEs
Neutrino S
hower
K. B
ittermann, K
C-T
ü
Movie real time:1/30000 of second
Simulations assuming that AGNs are CR sources
3000 eventsE > 5 1019eV
1000 eventsE > 7 1019eV
particle astronomy ?
JEM-EUSO status (March/April 2011)
ISS status
Japan:●Accepted for further preparation to lunch in 2016 by JAXA●Rocket is under development●Transportation module is under development●No government decisionEurope (8 countries):●Approved by ESA Programme Board for Human Spaceflights, Microgravity and Exploration,●Selected for inclusion in ELIPS research pool (ELIPS – European Programme for Life and Physical sciences and applications utilising the International Space Station),●Positively reviewed by EAS Astronomy Working Group (AWG)●JEM-EUSO is strongly supported by the ESA-appointed Fundamental Physics Roadmap Advisory Team (FPR-AT) in the document “A Roadmap for Fundamental Physics in Space (July, 26, 2010)
●Formally accepted till 2015●Recommendation to continue at least until 2020●No decision sign on government level (USA, Japan, Europe-ESA)
USA/NASA:Formal talks are in progress
JEM-EUSO in Poland
The formal status: Letter of Invitation from RIKEN addressed to:T.Batsch, Jkarczmarczyk, B.Szabelska, J.Szabelski (as Polish coordinator), T.Wibig – IPJT.Tymieniecka – Podlasie UniversityJ.Błęcki, P.Orleański, H.Rothkaehl, K. Słomińska – CBK PANM.Rybczyński, Z.Włodarczyk – Kielce UniversityG.Siemieniec-Oziebło – OA Jagiellonian Universityand accepted with pleasureNew formal body will be created: the consortium to●apply for funds in Poland (Poland is not ESA memeber, so far)●sign Memorandum of Understanding with RIKEN
Poland is going to join ESA – European Space Agencywe found the electronic manufacture suitable to produce (assemble)electronics for space,but there are no such enterprise with space certificates in Poland.
JEM-EUSO in Poland
JEM-EUSO Polish group members (by subject):EAS: B.Szabelska, J.Szabelski, T.Wibig, Z.WłodarczykHigh energy interactions: M.Rybczyński, T.Tymieniecka, T.WibigTLE: J.Błęcki, H.Rothkaehl, K. SłomińskaHardware (High voltage power supply + switches): J. Karczmarczyk, T.Batsch, P. Orleański, J.SzabelskiAstronomy (IG magnetic fields): G.Siemieniec-OziębłoPolish coordinator: J.Szabelski
Main participating institutions and researches (1):
CBK PAN (Warsaw)Space Research Center of the Polish Academy of SciencesDr. Piotr Orleański is the leader of the group of the hardware for space research,The group has made several devices which are currently in space,they have many years experience and expertize in hardware for space research;Prof. Jan Błęcki and Prof. Hanna Rothkaehl are experts in TLEs,they are participating in a few other space experiments for TLEs measurementsOAUJ (Kraków)Astronomical Observatory of the Jagielonian UniversityProf. Grażyna Siemieniec-Oziębło is working on the galactic and extragalacticmagnetic fields,the group is also involved in studies of acceleration mechanisms,and in measurements of Schumann resonance (low frequency radio effect)powered by TLEs and lightnings.
JEM-EUSO in Poland
Main participating institutions and researches (2):
IPJ (Łódź)The Andrzej Sołtan Institute for Nuclear StudiesEAS and Cosmic Ray astrophysics are the main topics studied in our group.The Cosmic Ray group in Łódź was set up in the 1950'sby Prof. A. Zawadzki (in collaboration with Prof. R. Maze),then developed by Prof. J. Wdowczyk (in collaborationwith Prof. Sir A.W. Wolfendale, and Prof. J.N. Capdevielle).The first European Cosmic Ray Symposium was held in Łódź,and in 2009 (together with the University of Łódź) we hosted the 31st International Cosmic Ray Conference.
JEM-EUSO in Poland
ISS - KIBO
Transportation modele H-II is of the bus size
Japanese Experiment Module/ Exposure Facility (JEM/EF)
KIBO – JEM inside
Japanese Experiment Module/ Exposure Facility (JEM/EF)
KIBO – JEM inside
ISS - KIBO
High energy interactionsLHC data , and EAS simulations
LHC data till s1/2 = 7000 GeV
Large differences between models used in EAS simulationsfor energies above LHC
High energy interactions
Large differences between models used in EAS simulations for energies above LHC
p - p
π+ - p
π+ - air
p - air
High energy interactions
Large differences between models used in EAS simulations for energies above LHC
Energy spectrum: problems at the highest energies
Difference between AGASAand others (HiRes, PAO)
J.N.Capdevielle, F.Cohen,B. & J. SzabelscyJ.Phys. G, 36 (2009) 075203:Error in AGASA energy estimation
EAS longitudinal development vs. ground observation levels
VR – Volcano RanchYa – YakutskPAO – P.Auger Observatory
EAS array observationsat constantbut zenith angle dependentdepth (EAS development stage)
Figure shows an averageNe distribution;In real EAS development●fluctuates●depends on primary particle mass●interpretation depends●on the interaction models
Anisotropy / “sources” problems
POA: 27 events with ECR > 4 1019eV
Wibig + Wolfendale: mass of CR from „source” CEN-A ~ A=12(i.e. no protons, no iron nuclei)
On Earth no way to explore UHE…
Knee
AnkleAnkle
JEM-EUSO
330 – 400 nm
144 PDM x 36 PMT/DPM = 5184 PMT 186624 pixels (36 MAPMT) 331776 pixels (64 MAPMT)
1980 kg
200 cm x 260 cm x 200 cm
Obserwacje WPA(Wielkich PękówAtmosferycznych)
K. Shinozaki, RIKEN & KC-Tü