The JEM-EUSO Mission to Explore the The JEM-EUSO Mission to Explore - - PowerPoint PPT Presentation

E Extreme U Universe S Space O Observatory The JEM-EUSO Mission to Explore the

The JEM-EUSO Mission to Explore the Extreme Universe Extreme Universe

Piergiorgio Picozza INFN e Università di Roma Tor Vergata

Commissione II INFN

31 Gennaio 2011

JEM-EUSO

The JEM-EUSO Collaboration, brings together 250 scientists from 12 Countries: Japan, Europe, US, Korea, Mexico and Russia

The Extreme Universe Space Observatory (EUSO)

• nboard the Japan Experiment Module (JEM) of

the International Space Station

Science Objectives

• Main Objective：

Astronomy and astrophysics through particle channel with extreme energies

– Are there differences between and North and South of the galactic plane? – Identification of the energy sources based on the analysis of the arrival direction of the particles. – Identification of the acceleration and radiation mechanisms with the measurement of energy spectrum from individual sources

• Exploratory objective：

– Measurement of extreme energy gamma rays – Detection of extreme energy neutrinos – Estimation of the structure of galactic magnetic field and its intensity – Identification of relativity and quantum gravitational effect – Study of atmospheric luminous phenomena

Other Open Questions

– Is this the GZK suppression? Or are the sources running out of fuel… – Do we see a recovery of the spectrum ? – Has the spectrum an end? Which is the maximum energy Do we have a high statistics description of the spectrum?

ESA AWG meeting#139, May 11. 2010

Success criteria

Full success： detect about 1000 events with energy higher than 5×1019 eV Success： 500 events (minimum to identify sources)

• Analysis of the arrival

direction of particles

– Accuracy of the determination

• f the arrival direction：less

than 2.5 °

• Analysis of spectrum

– Accuracy of the energy determination： less than 30%

• Identification of Hadron/

photon/ neutrino：

– Accuracy of the Xmax determination: <120 g /cm2

JEM-EUSO sky simulated with 1,000 events

Brightness of UHECR∝? X ray （AGN）

Open problems:

• What is the nuclear

composition of UHECR?

• Are the sources

isotropic or not? What is the role of CenA region?

Auger
2010 HiRes
2010

Auger (07,08): excess correlation of UHECR arrival directions with nearby (weak) AGN 99% c.l. rejection

• f isotropy of arrival directions

HiRes rejects correlation with galaxy and AGN catalogs at 95% cl...

Light composition Heavier composition above ankle

Extreme Energetic Cosmic Neutrinos

Neutrino production by the GZK process Air showers initiated by different kind

• f neutrinos

Neutrino fluxes for various models and detection capability of JEM-EUSO Exploratory Objectives

Expected sensitivity

• n gamma ray fraction

M-I M-II

Ideal case

• Ideal case (only statistics): Xmax strong discriminator for gamma ray
• More realistic estimate (assumed experimental errors in Xmax)

using 2 different approaches to evaluate flux limit → New and stringent limit expected @ the highest energies (~1020eV)‏

– Possible detection of GZK photons during the Mission

Expected limit by 5 year mission compared with upper limits set by existing experiments (95%CL)‏ Exploratory Objectives

Atmospheric Luminous Phenomena

Various trangent airglows OH airglow observed from ground Leonid meteor swarm in 2001 taken by Hivison camera Lightning picture observed from ISS Exploratory Objectives

Erice, September 16-24, 2009

Large distance > 400 km Large FOV Large Target Mass of the atmosphere Full sky coverage looking at both North and South sky Large Distance R but small proximity effect

• International Space Station-aboard EECR
• bservatory

– Orbiting at ~400 km in ±51.6 degrees latitudes – Covers both nordern and southern hemisphere – Flight in varying geomagnetic field (~0.6 gauss) around orbit

• Viewing night atmosphere

in ~500 x 400 km area (nadir mode)‏ – Wide FOV allows to measure entire slowly developing showers – Target volume exceeding an order of 1012 tons

FOV above Okayama Tilt mode(~30o)‏

JEM-EUSO Field of view in Nadir and Tilt Mode

Nadir mode

Erice, September 16-24, 2009 31st Course of International School of Nuclear Physics

JEM-EUSO Exposure

1 MLinsley

Pre‐Phase
A Phase
A Phase
B Phase
C Phase
D Phase
E

Early Study Concept Studies Concept Development Project Formulation Preliminary Design Final Design Production Testing Launch Operations Initial Mission Operation Nominal Mission Operation

SRR (System
Requirements
Review) PDR (Preliminary
Design
Review) CDR (Critical
Design
Review)

[Safety
Review]

MDR (Mission
Definition
Review) QR (Qualification
Review) FAR (Flight
Acceptance
Review)

[Safety
Review] [Safety
Review] [Safety
Review]

JEM‐EUSO

TARGET
PHASES

4 – 9 December 2010 JEM EUSO Collaboration meeting (Tokyo)

At around end of fiscal year 2010, SRR (System Requirement Review) might be held by

• JAXA. We have some issues solved before SRR below.

1)Strengthening of System integration function.

• At present, roll sharing of each country (12 countries) who expresses participation in

JEM-EUSO is becoming clear. However, in the project phase, organization that more effectively coordinates and integrates the roll sharing for each country becomes strongly necessary at least in Science Instrument System side.

• Corresponding this issue, Advanced Science Institute, RIKEN as host laboratory, is

secured a scientist of ripe space experience and an engineer of space instrument manufacturing experience. By this action, organization is being constructed to response the above issue.

Organizzazione

• PI Piergiorgio Picozza
• Deputy PI Toshikazu Ebisuzaki
• Global Coordinator Andrea Santangelo
• PI Team:
• Fumiyoshi Kajino
• Marco Casolino
• Guido Castellini
• Katsuhiko Tsuno
• Mario Bertaina

Executive Board

• PI
• Deputy PI
• Global Coordinator
• US representative
• European Representative
• Science Working Group Chairman
• RIKEN JEM-EUSO Team Leader
• Instrument manager
• Masahiro Teshima (Cosmic Ray specialist)
• Invited Mario Bertaina

Componente Italiana

• 48 ricercatori
• 5 tecnologi
• +10 non associati INFN
• 7 Sezioni (BA CT FI LNF NA RM2 TO)

The UV Telescope

Prototypes: Structure, 1.5m Bread Board Model

Lens Frame Metering Structure

Optics is officialy responsability of RIKEN. NASA/MSFC + UAH are in charge of optical testings. Contributions from Italy for: 1.Design and simulations

• Storically, all the designs have been produced by AZM.
• Optimizations of baseline (“PPP”) and advanced (“CPP”) designs.
• Contributions to performance analysis with realistic simulations.
• Assessments on thermal, mechanical, FS issues.
• Manufacturability of lenses w.r.t. designs.

2.Support to optical tests

• Verification of optical quality for the 1.5 m Ø PPP design:

illumination of regions and of the whole system.

• Use of this feedback to retrieve new information on design.

OPTICS Alessandro Zuccaro Marchi CNR-INO, INFN-Firenze (DTZ)

Hamamatsu Ultra Bialkali high efficiency MAPMT M64 64 channels in 8*8 grid Arranged in 6*6 in PDM structure M36

New M64

Hamamatsu
Photonics

MAPMT
characterization













JEM‐EUSO
Focal
Surface
needs


JEM‐EUSO
Focal
Surface
needs
≈ ≈
5000
MAPMT
calibrated 
5000
MAPMT
calibrated

Development
 and
 implementation
 of
 a
 MAPMT
 Relative and
absolute
calibration

procedure
to
support
and
verify the
France
activities
on
the
calibration
task:

‐Lab.
Measurement
using
UVscope
unit
(64
channels
Single


Photon Counting
 Front‐end
 and
 read_out)
 developed
 at
 IASF‐Pa
 coupled with
 an
 integrating
 sphere
equipped
 with
 a
NIST
 calibrated
 photo‐ diode
and
a
light
source
(LED). ‐Comparison,
verification
and
validation
of
the
calibration
procedure and
results
on
a
sample
of
MAPMTs
using
the
calibration
facilities
of the
Astrophysical
Observatory
of
Catania.

M36

PDM Structure prototype

(manufactured in LNF)

Multi Anode PMT 64 channels

1 PDM = 36 MAPMT = 2304 channels

PDM TEST SYSTEM

COMPLETE SOLUTION:

• CLOSED BOX
• 1 MANUAL ROTATION for PDM (for inspection),
• 3 AXES MOTORIZED LINEAR POSITIONER for

the light source

• 2 MOTORIZED ROTATION POSITIONER for the

light source.

Motorized light source movements Manual PDM rotation

• CLOSED BOX
• MOVABLE PDM,
• 3 AXES (Horizontal and vertical) - 30 cm full range MOTORIZED

LINEAR POSITIONER for the light source

• 2 MOTORIZED ROTATION POSITIONER for the light source.
• UV led
• 1 Sphere

Mechanical Ground Support Equipment

In-flight mechanical components

Chassis that host: CCB (trigger boards), HV and House-Keeping boards ( 4 chassis foreseen for the flight model) Realization of the prototype chassis: year 2013 MAPMT base: plastic base to insulate the PMT from the mechanical structure

Volume for Electronics Volume for Electronics (167 x 128 x 130) (167 x 128 x 130) PDM Frame PDM Frame EC Base EC Base 64 channel 64 channel MAPMT MAPMT

FS Structure: 137 PDMs 315 kchannels Three element support, (note sphericity) (LNF) Photo Detector Module 2304 channels

2.5 m

Focal Surface Mechanics: Design + Manufacturing INFN-LNF

JEM-EUSO DAQ – Data reduction block scheme

FEE ASIC+ FPGA Count PDM Control Board FPGA Track Trigger Cluster Control Board DSP Fine Trigger FS Control Board MPU Main+ Spare 137 Boards 10 Boards + 10 Spare 10CCB 8PDM 315kch 9EC LVDS with SpaceWire (ECSS-E-50-12A) 297 kbps 3 Gbyte/day

9.6 GB/s (FS)

PhotoDetector Modules

4*10-3 compression 10-3 compression

Storage on SSD will give factor 3, up to 10 Gbyte/day Return with Soyuz

Design + Manufacturing

PMT Read-out ASIC：SPACIROC

ＬＡＬ/IN2P3: omega-team

System
clock
&
synchronizer
board (requirements)

• Generating
and
distributing
system
clock
(40
MHz)

and
GTU
clock
(400
KHz)

• Absolute
time
measurements

– Interfacing
with
the
JEM
EUSO
GPS
system – Interfacing
with
the
Time
provided
by
ISS/JEM
(to
be
used in
case
of
failure
of
GPS
system)

• Time
synchronization
of
the
event
• Live‐time
and
dead‐time
measurements
• Receiving
the

CCB
2nd
level
trigger
signals
and

registering
the
trigger
pattern

CPU

main

Bus PCI IDAQ: FPGA I/F board DSP #2

TI 6713b

DSP #3

TI 6713b

DSP #21

TI 6713b

………… Data to CPU Memory DSP #1

TI 6713b PDM #3 PDM #5 PDM #1 PDM #4 PDM #6 PDM #2 PDM #7 PDM #8

C

• m

m a n d : d a t a r e q u e s t t

• P

D M b

• a

r d

Intermediate Data AcQuisition board (IDAQ)

IDAQ High-speed interface board responsible for event packing and data transfer beetween CCB and mass memory. It takes care of the data commands between the CPU and the different FPGA boards of the trigger levels.

Development of atmospheric monitoring tools for on board laser

• Implementation of the on board laser simulation

in ESAF

– Work already started with the help of the Tubingen group for the ESAF expertise

• Development of on board laser reconstruction

and analysis algorithms for:

– Cloud top height and optical depth retrieval – Study of the achievable precision in the determination

• f the aerosol profile

– Study of the impact of the atmospheric conditions on the shower reconstruction (energy and Xmax resolution)

Calibration using ground based light sources

• Simulation of ground LIDAR and Xenon Flashers

in ESAF

• Absolute calibration using the ground LIDAR

data (aerosol attenuation is estimated using

backscattered light collected by the ground receiver)

• Study of the performances of the absolute

calibration with the combined use of Xenon Flashers, on board laser and/or observation of reference calibrated stars at the Flasher site

Altri argomenti fondamentali

• Ottimizzazione degli algoritmi di trigger da

implementare sulla FPGA

• Simulazione e ricostruzione degli eventi
• Misure di fluorescenza alla BTF Frascati

Measurement
of
the
diffuse/reflected
Cherenkov
light
from sea
and
ground

Diffuse/reflected
 Diffuse/reflected
Cherenkov
 Cherenkov
light
as
end‐mark
of
the
shower
profile light
as
end‐mark
of
the
shower
profile

70%
of
the
observation
time
spent
on
oceans

Measurement
 of
 the
 efficiency
 of
 the
 diffuse/reflected Cherenkov
 light
 bounced
 back
 at
 the
 impact
 point
 of
 the shower
axis
(earth

and
sea
surface
):

‐
a
small
EAS
array
formed
by
five
scintillators
(using
conventional sampling
technique)
disposed
in
a
centered
parallelogram. 
 ‐a
 binocular
 UV
 optical
 device
 (300‐400
 nm
 interval)
 to
 detect
 the Cherenkov
 light,
 including:
 two
 narrow
 field
 (±4.5°
 FoV)
 detectors equipped
 with
 two
 0.5
 m
 fresnel
 lens
 ,
 pointing
 toward
 the
 array central
station.

*
 The
 first
 measurement
 has
 been
 carried
 out
 in
 2004.
 Needs
 to
 be
 repeated
 (higher statistics) Ref.
: Ref.
:"Extensive
Air
Showers
and
Diffused
Cerenkov
Light
Detection:
the
ULTRA
Experiment“ NIM‐A
,
Vol.570,
pp.22‐35,
2007

Recommendation of FPRAT

• The Roadmap has been presented to the Community
• JEM-EUSO science recognized and a very positive

recommendation has been given

International Role Sharing

• France: ASIC (first chip from foundry)
• Spain: Infrared Camera
• Swiss + France – Lidar
• Germany: Simulations + CCB (third level DH)
• USA: Optic test
• Japan: Lens manufacturing
• Japan+Italy: Lens design
• Poland: HV
• Korea: PDM FPGA board
• Italy: Trigger algorithm, simulations, DAQ (general),

CPU, Mass Memory, on board storage, Mechanics, Focal surface integration