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