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

Extreme U Universe S Space O Observatory E 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 Extreme Universe Space Observatory (EUSO) onboard the Japan Experiment Module (JEM) of the International Space Station The JEM-EUSO Collaboration, brings together 250 scientists from 12 Countries: Japan, Europe, US, Korea, Mexico and Russia

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 JEM-EUSO sky simulated Full success ： with 1,000 events d etect about 1000 events with energy higher than 5 × 10 19 eV Success ： 5 00 events (minimum to identify sources) • Analysis of the arrival direction of particles – Accuracy of the determination of the arrival direction ：l ess Brightness of UHECR ∝? X ray （ AGN ） 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 /cm 2

Open problems: HiRes
2010 • What is the nuclear Auger
2010 composition of UHECR? Light composition Heavier composition above ankle • Are the sources isotropic or not? What is the role of CenA region? Auger (07,08): excess correlation of UHECR arrival directions with nearby (weak) AGN 99% c.l. rejection of isotropy of arrival directions HiRes rejects correlation with galaxy and AGN catalogs at 95% cl...

Exploratory Objectives Extreme Energetic Cosmic Neutrinos Neutrino production by the GZK process Air showers initiated by different kind Neutrino fluxes for various models of neutrinos and detection capability of JEM-EUSO

Expected sensitivity Exploratory Objectives on gamma ray fraction Expected limit by 5 year mission compared with upper limits set by M-I existing experiments (95%CL) ‏ M-II Ideal case • Ideal case (only statistics): Xmax strong discriminator for gamma ray • More realistic estimate (assumed experimental errors in X max) using 2 different approaches to evaluate flux limit → New and stringent limit expected @ the highest energies (~10 20 eV) ‏ – Possible detection of GZK photons during the Mission

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

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 Erice, September 16-24, 2009 proximity effect

JEM-EUSO Field of view FOV above Okayama in Nadir and Tilt Mode • International Space Station-aboard EECR observatory – Orbiting at ~400 km Nadir mode 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 10 12 tons Tilt mode(~30 o ) ‏

JEM-EUSO Exposure 1 MLinsley Erice, September 16-24, 2009 31st Course of International School of Nuclear Physics

JEM‐EUSO

TARGET
PHASES Pre‐Phase
A Phase
A Phase
B Phase
C Phase
D Phase
E Early Concept Concept Project Preliminary Final Production Launch Initial Nominal Study Studies Development Formulation Design Design Testing Operations Mission Mission Operation Operation MDR (Mission
Definition
Review) SRR [Safety
Review] (System
Requirements
Review) PDR (Preliminary
Design
Review) [Safety
Review] CDR [Safety
Review] (Critical
Design
Review) QR (Qualification
Review) FAR (Flight
Acceptance
Review) [Safety
Review]

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

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

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










 JEM‐EUSO
Focal
Surface
needs
 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.

PDM Structure prototype (manufactured in LNF) M36 Multi Anode PMT 64 channels 1 PDM = 36 MAPMT = 2304 channels

Mechanical Ground Support Equipment PDM TEST SYSTEM Manual PDM COMPLETE SOLUTION: rotation - CLOSED BOX - 1 MANUAL ROTATION for PDM (for inspection), - 3 AXES MOTORIZED LINEAR POSITIONER for the light source -2 MOTORIZED ROTATION POSITIONER for the Motorized light light source. source movements • 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

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