Space Based observation of the UHE Universe Andrea Santangelo - - PowerPoint PPT Presentation

Andrea Santangelo, Kepler Center-Tü Vulcano 2010, May 25

“Space Based observation of the UHE Universe” Andrea Santangelo

Kepler Center for Astro and Particle Physics, Eberhard-Karls-Universität , Tübingen

Andrea Santangelo, Kepler Center-Tü

Outline of the presentation

• Science case, and the requirements for the “next

generation” UHE Observatories

• Main Science objective: Particle Astronomy
• Other UHE messengers: Neutrinos, Photons
• Fundamental Physics
• (status of) The JEM-EUSO Mission
• How from space?
• Why from space?
• Performances

Andrea Santangelo, Kepler Center-Tü Erice, September 16-24, 2005

E > (5-6)×1019 eV (~1016 keV)

Their origin, nature and even their route to Earth presents an extraordinary puzzle

UHE

Andrea Santangelo, Kepler Center-Tü

Cosmic Ray propagation in our Galaxy

Largely unknown local extragalactic and galactic magnetic field limits proton astronomy to higher energies

Andrea Santangelo, Kepler Center-Tü

The GZK Effekt

Kenneth Greisen George Zatsepin Vadim Kuzmin Greisen (1966) and, independently Zatsepin & Kuz’min (1966) γCMB p Δ+ π+ n

Δ-resonance multi-pion production

Andrea Santangelo, Kepler Center-Tü

Attenuation length, a limited horizon

A + hν → (A-1) + N A + hν → (A-2) + 2N A + hν → A+ e++e-

Photodisintegration (Puget et al., 1976) Pair production (Blumenthal, 1970)

E ~ 2*1020 eV (nuclei) Nagano & Watson, Rev. Mod. Phys, Vol. 72, N°3 (2000)

Andrea Santangelo, Kepler Center-Tü

A key result of Auger South and HiRes

The Auger Collaboration (2008a), Abbasi et al. (2008), Bergman (2008)

Observation of a “flux suppression” in the spectrum: GZK feature (?)

3 = 4.3± 0.2

2 = 2.59 ± 0.02 1 = 3.26 ± 0.04

Andrea Santangelo, Kepler Center-Tü

Open Questions remain

– 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?

• Requirement: A high precision measurement of

the UHECR spectrum around and beyond the „GZK“ feature

Andrea Santangelo, Kepler Center-Tü

Relevance of Auger's result:

• (Good news) It limits the horizon and gives us

the possibility to find local sources:

– Large angular separation – Smaller magnetic deflections

• (Bad news for current observatories) it implies

a very low flux:

1particle/km2 /sr/century

E > 6 1019eV

1particle/km2 /sr/millennium?

E >1020eV

Sources?

Andrea Santangelo, Kepler Center-Tü

A second key result from Auger

Observation anisotropy of UHE particles at E>5x1019 eV

The Auger Collaboration (2007)

• Ang. Sep. ψ < 3.1°, z < 0.018 (75 Mpc)

and E > 56 EeV

Enables Particle Astronomy

Andrea Santangelo, Kepler Center-Tü

Auger South latest results

Pdata =k/N binomial parameter It indicates the degree of correlation For isotropy Piso=0.21

PAuger09=0.38±0.07 More than 2σ

58 events for E> 55 EeV 2004-2009 Cen A interesting region

Hague & PAO collaboration, 2009

And HiRes? No clear evidence...

Andrea Santangelo, Kepler Center-Tü Tuebingen, October 19th, 2005 Fakultaets Kolloquium

« Compact » Sources of CR ?

AGASA Arrival Direction Distribution 1 Triplets 6 Doublets

Andrea Santangelo, Kepler Center-Tü

A clear message from the Pierre Auger Observatory and HiRes is that they are too small: Need NEXT GENERATION! Rate of events that seem to be anisotropically distributed is only ~ 2 per month

Andrea Santangelo, Kepler Center-Tü

Mean Xmax and RMS from 3754 events Auger: iron nuclei?

Composition?

Andrea Santangelo, Kepler Center-Tü

HiRes, 2010 HiRes: protons?

Composition?

Andrea Santangelo, Kepler Center-Tü

Science Objectives for Particle Astronomy

• Identification of the sources of UHE particles

– Localize the sources (Multi-messengers study) – Understand the nature of the sources

• Measurement of the spectra of individual sources

– Spectral shape, Maximum Energy – Flux, Power

Understand the

• rigin!

High Statistics

Andrea Santangelo, Kepler Center-Tü

Bottom-up: Acceleration Mechanisms?

1st Order Fermi Shock Acceleration

The fractional energy gain per shock crossing depends on the velocity jump at the shock. Spectrum E-q with q > 2 typically

When the gyroradius becomes comparable to the region size, the spectrum cuts off.

Hillas’ limit

To accelerate a particle efficiently it must cross the shocks several times.

Andrea Santangelo, Kepler Center-Tü

Possible Sources

Unknown sources

Andrea Santangelo, Kepler Center-Tü Tuebingen, October 19th, 2005 Fakultaets Kolloquium

Pulsar SNR A.G.N. GRB Radio Galaxy Lobe

All Astrophysical models are limited to

Torres & Anchordoqui, 2004 Ptytsina & Troitsky, 2008 Hillas plot

Andrea Santangelo, Kepler Center-Tü

Why “from space”? How “from space”? The ways to go... Ground (Auger North) vs. Space

Andrea Santangelo, Kepler Center-Tü

hadrons N ) NC ( hadrons l N ) CC (

l l l

+

• +
• A. Bunner, 1967;

Nagano, 2009;

Y ph /cm

( ) = N E0,t ( )q z ( )

i

• E i

( )

1+ P z

( )

P' T0 T z

( )

• 1 2

i

• 10-1

100 101 102 320 330 340 350 360 370 380 390 400 Relative Spectral Radiance (A.U.)

Wavelengths in nm

Fluorescence Lines in Air 600 Torr by 50-KeV electrons G.Davidson and R. O'neil

• Jour. Chem. Phys. 41,12(1964)3946

q=2.2 MeV/(g/cm2) ε = # of photons of wavelength λi per MeV

Kakimoto et al., 1996

p, 1020eV, 60 deg

GTU time units

Andrea Santangelo, Kepler Center-Tü

JEM-EUSO

The JEM-EUSO Collaboration, led by RIKEN- Japan, brings together 150 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

Andrea Santangelo, Kepler Center-Tü Madrid, September 17, 2007, 5th FW

ISS Flight direction

51.6°

Japanese Experiment Module (KIBO)

• nboard the International Space Station

Candidate positions for JEM-EUSO

Andrea Santangelo, Kepler Center-Tü

Vertical Mode (2 years) Tilted Mode (3 years)

Larger effective area (×5) with ~35°tilt

JEM-EUSO Telescope on ISS

Andrea Santangelo, Kepler Center-Tü

The UV Telescope

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Fresnel lens prototype Dec. 09 Toshi Ebisuzaki, JEM-EUSO PI

Andrea Santangelo, Kepler Center-Tü

JEM-EUSO Focal Surface Detector

(156PDMs = 0.2M pixels)

2.6 m max MAPMT (6x6 pixels) QE 25-30% 26.2 mm

Andrea Santangelo, Kepler Center-Tü

Baseline: M36 (Hamamatsu) Advanced Options: MAPMT M64 SiPM (Germany)

Alternative: SiPM (MPI-HLL)

Andrea Santangelo, Kepler Center-Tü

Proton Shower (60 deg, 1020eV)

PDM GTU= 2.5 µsec

Andrea Santangelo, Kepler Center-Tü

Result of end-to-end simulation

Andrea Santangelo, Kepler Center-Tü 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

Andrea Santangelo, Kepler Center-Tü

Aexp (2 4.5)10

5 km 2 sr yr

Life 5yr

Atilted

exp 106km2sr yr

Andrea Santangelo, Kepler Center-Tü Erice, September 16-24, 2009 31st Course of International School of Nuclear Physics

Why JEM-EUSO?

1 MLinsley

Andrea Santangelo, Kepler Center-Tü

ISS Orbit Uniform Exposure

http://www.nlsa.com/

Inclination: 51.6° Height: ~400km JEM-EUSO can observe the arrival direction of EECR very uniformly

• wing to the nature of the ISS
• rbit.

Full-Sky Coverage

Andrea Santangelo, Kepler Center-Tü

Trigger Efficiency (May 2010 baseline)

50% 5×1019eV

Andrea Santangelo, Kepler Center-Tü

Trigger efficiency in the inner part: important for Cross-Calibration

Andrea Santangelo, Kepler Center-Tü

JEM-EUSO sky

• More than 1,000 events: E>7x1019eV
• We expect to discover several dozens of clusters
• Can observe the whole sky

Takami 2008 Forecast in case of 1,000 events

Brightness of particles ∝ X ray （AGN）

Andrea Santangelo, Kepler Center-Tü

Test of the GZK effect

Spectra as function of the distance of the source we can study the GZK effect

Andrea Santangelo, Kepler Center-Tü

General “Mission” of JEM-EUSO Exploring the Universe at Ultra-High Energies Main Science Objective: Particle Astronomy

Andrea Santangelo, Kepler Center-Tü

Exploratory Science Objectives:

• Neutrinos at UHE
• Photons at UHE
• Fundamental Physics

From Particle Astronomy:

• Galactic and local intergalactic

Magnetic Fields Other exploratory objectives

Andrea Santangelo, Kepler Center-Tü

Understanding Magnetic fields

Medina Tanco et al., 2009 A Source appears like a spot due to magnetic spreading (magnetic PSF)

Andrea Santangelo, Kepler Center-Tü

Astrophysical Neutrinos... (at UHE)

neutrinos Astrophysical source Low energy protons deflected High energy gammas 10 Mpc

νs not affected by cosmic radiation νs not bent by magnetic fields

Migneco, (2004)

Andrea Santangelo, Kepler Center-Tü

Production: Decay chains of mesons

Other mesons like Kaons are also involved to certain degree and all decay chains are very well known But HOW the mesons are produced ?

νe : νµ : ντ

1 1 : 2 2 : 0 (at generic source) pp π  µ νµ e νeνµνµ 1 : 1 : 1 (at earth) max.mixing

Andrea Santangelo, Kepler Center-Tü

Sources of Neutrinos?

We have an accelerator of protons to generate a proton beam We need a gas (well nuclei) or ambient photons target

• Supernova ejecta
• Accretion disks
• Galactic disk
• Molecular clouds
• …

Fermi mechanisms can accelerate protons

• Jets in AGN
• Microquasars, Binaries
• GRB
• CMB

Andrea Santangelo, Kepler Center-Tü

Cosmogenic Neutrinos

Berezinsky & Zatsepin, (1969, 1970) Berezinsky (2005)

Maximal Energy, Composition, Evolution of sources

Iν/Ip

Andrea Santangelo, Kepler Center-Tü

Cosmogenic Neutrinos

Speculative models

Astrophysical models

GZK(A) Protheroe (1995) GZK(B) Kalashek, Kuzmin, Semokov, Sigl (2002) AGN Mannheim (1995) B)high – A)low

Andrea Santangelo, Kepler Center-Tü

UHE Neutrinos

Rejection > 10-5

1700 g/cm2 55%

P+ ν

Andrea Santangelo, Kepler Center-Tü

Discrimination of Neutrinos vs Protons P+ ν

Rejection > 10-5 Xmax X1 initial point

Andrea Santangelo, Kepler Center-Tü

Neutrino shower simulation

• Gamma ray showers

– CONEX with....

• Neutrino showers for pilot studies

– Horizontally incident – PYTHIA interaction code for neutrino-nucleon interaction – CONEX code connected for shower in atmosphere

 Horizontally incident neutrinos

− Survival prob. to come in FOV

 Neutrino: ~exp(-0.001)  Proton: ~exp(-1000) for 1020 eV  CONEX code used for

shower simulation in atmosphere

Andrea Santangelo, Kepler Center-Tü

The probability of neutrino interaction in atmosphere is proportional to the atmospheric density.

NEUTRINOS CC INTERACTIONS (LPM effect included)

P+ ν

Andrea Santangelo, Kepler Center-Tü

Profile of neutrino induced showers

• First peak resulted from hadronic

part of shower

• Second and following peaks from

electromagnetic part – LPM effect more significant at lower altitudes

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

New Physics?

Andrea Santangelo, Kepler Center-Tü

Cosmogenic Neutrinos

Speculative models

Astrophysical models

GZK(A) Protheroe (1995) GZK(B) Kalashek, Kuzmin, Semokov, Sigl (2002) AGN Mannheim (1995) B)high – A)low

Andrea Santangelo, Kepler Center-Tü

Particles are produced from the top, from the decay of some supermassive unstable particle

Top-down models

GeV 10 m , q q X

12 X >

+

• 1.) particles released from topological defects,

left over from the cosmological phase transitions (cosmic strings, magnetic monopoles, domain walls…) 2.) long-lived massive free particles (“WIMPZILLA” dark matter, mirror matter) Bhatacharjee & Sigl, 2000 Berezinsly, Blasi, Vilenkin 1999

The X particle decay into quarks that hadronize, generating pions and a small fraction of protons and neutrons. At the production most of UHE particles are γ-rays and Neutrinos.

Andrea Santangelo, Kepler Center-Tü

Constrains from Auger

SHDM models are strongly constrained by the absence of identified photon candidates in the Auger data

Auger Collaboration, 2009

Andrea Santangelo, Kepler Center-Tü

Neutrino Cross sections

Palomarez-Ruiz, Irimia and Weiler, 2006

Neutrino Cross Sections can be measured from the ratio of Horizonthal to Upward showers Fargion, 1997, 2002, 2004 Fargion et al., 1999 Bottai & Giurgola, 2003 Yoshida et al., 2004

Andrea Santangelo, Kepler Center-Tü

Neutrino cross sections

Black Hole production p-brane production EW instanton effects Exchange of KK modes Feng & Shapere, 2002 Kachelriess & Plümacher, 2000 Anchordoqui, Feng and Goldberg, 2002 Han & Hooper, 2004 Ringwald, 2003 Bezrukov et al., 2003a, 2003b

Andrea Santangelo, Kepler Center-Tü

EHE γ-rays travel > Gpc only in Quantum Gavity or C-G vacuum

• E (γ)

ε (10-3K)

• 4εE - ξ ≥ 4mec4

Kifune 1997

Andrea Santangelo, Kepler Center-Tü

Number of Events: > 1000 (at E> 7x1019eV) Arrival direction: < 2.5° Energy determination: < 30% Xmax determination: < 120 g/cm2 They have been confirmed by end to end simulations performed with two independent Frameworks (ESAF in Europe)

Point
Source Point
Source Energy
spectrum Energy
spectrum LPM
EAS LPM
EAS Neutrino
EAS Neutrino
EAS

Scientific Requirements

Andrea Santangelo, Kepler Center-Tü

A naïve science objective: exploration

• f the Unknown!

Andrea Santangelo, Kepler Center-Tü

Serendipity or Vision?

Updated from

• F. Halzen, 2002

Andrea Santangelo, Kepler Center-Tü

Conclusions

• Results from Auger South suggests:

– Evidence for the GZK & Anisotropy of distribution – Sources exist but cannot be found by the current generation of UHE Observatories

• A new generation of observatories is required:

– High Statistics – Uniform coverage of the sky

• Breakthrough will come from space:

– Enormous exposures, uniform exposures – JEM-EUSO is the pathfinder with potentially

• utstanding science output

– It’s feasible! As Phase A/B confirms

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Thanks for listening!

Andrea Santangelo, Kepler Center-Tü

Back-up slides

Andrea Santangelo, Kepler Center-Tü

Mean Xmax from 3754 events

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

JEM-EUSO vs. Auger North

• Let’s consider the exposure: JEM-EUSO will reach

at the end of the decade 10^6 Linsley. Auger North will reach the same exposure in the most optimistic case after 2035.

• Full sky coverage with uniform exposure is a unique

capability of JEM-EUSO.

• In any case to fully explore Particle Astronomy a

space-based mission is essential: this is widely considered the real next experimental breakthrough. JEM-EUSO is the breakthrough within this decade.

• Neutrino physics and associated science is a JEM-

EUSO unique capability.

Andrea Santangelo, Kepler Center-Tü

Status of Auger North

• Auger North is not approved yet
• Site is in Colorado  US is the driver
• Recommendations (and prioritization) from the

Particle Astrophysics Scientific Assessment Group (PASAG) to the High Energy Physics Advisory Panel (HEPAP) of NSF and DOE

• Auger North is recommended in scenario C:

doubling of funding over 10 years (6.5% per year)

• Funding are not approved in other countries.
• Waiting Decadal review outcome: funds from

Astronomy and Astrophysics?

Andrea Santangelo, Kepler Center-Tü

Other Remarks on Auger North

• Auger North will reach JEM-EUSO exposure in

2030-2040 (but problems with uniformity!)

• To increase statistics an experimental breakthrough

is necessary  Go to space  JEM-EUSO is the challenge! (Pathfinder and outstanding science) and then S-EUSO

• My personal opinion: the deployment of Auger North

at crossroads of US state roads is not so easy!

Andrea Santangelo, Kepler Center-Tü

Back-up slides

Who is who…

Andrea Santangelo, Kepler Center-Tü

Involvement of Europe (Sept. 09)

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Transfer to the ISS: H-IIB Transfer Vehicle (HTV)

klkdflsk:lkdsf

EUSO Launch (Stowed) Configuration EUSO On -Orbit (Deployed) Configuration φ2175 φ2552 EUSO Telescope Configuration (Truss Concept) Deploy Mechanism (See Next Page) Fresnel Lenses Focal Surface Electronics Lid

Folded config. Expanded config. JEM-EUSO Telescope

Andrea Santangelo, Kepler Center-Tü

Succesfull Launch of HTV September 11, 2009

Andrea Santangelo, Kepler Center-Tü

Op#cs
Requirements

– FoV

±
30° – Pupil
entrance
pupil
≥
2
m – F/#
≤
1.0 – Spot
dimension

~0.1°
(5mmΦ) – Spectral
range
330‐400
nm

JEM-EUSO Optics

Fresnel
lenses Focal
Surface

Precision
Fresnel
lens

New
Material
CYTOP

PMMA ~50%
up Field
of
View
(deg)

Encircled
Energy 
within
5mm
dia.

Surface
of
the
Precision
Fresnel
lens

0.7

Precision optics cancels chromatic aberration

Andrea Santangelo, Kepler Center-Tü

ESA Science Directorate

Fundamental Physics Roadmap Advisory Team (FPRAT) established in 2009

Andrea Santangelo, Kepler Center-Tü

FPRAT

• A Report, which contains the roadmap, is

being prepared (draft1.0 already issued)

• Workshop on the 21-22 January at ESA in

ESTEC (Noordwjik)

Andrea Santangelo, Kepler Center-Tü

Recommendation of FPRAT

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

recommendation has been given

Andrea Santangelo, Kepler Center-Tü

AO-2009-Phys-BIOSR (ELIPS) by ESA HSR

• Letter of Intent

submitted on the 15th June 2009

• Full Proposal

submitted on the 14th of September

• Main requests to

ESA: resources on the ISS

Andrea Santangelo, Kepler Center-Tü

Proposal Submitted

• Outcome ?

Andrea Santangelo, Kepler Center-Tü

TUS launch date: Nov.

2011, Prototypes of JEM-EUSO several Events per year

Mirror area is 2 m2 exposure factor 3000 km2 sr per year (orbit height 500 km).

TUS A pathfinder

Andrea Santangelo, Kepler Center-Tü

Signal for a p shower (60 deg, 1020eV)

Mernik et al. , 2009

Andrea Santangelo, Kepler Center-Tü 31st Course of International School of Nuclear Physics

500 counts/ (ns sr m2)

Andrea Santangelo, Kepler Center-Tü

What is the expected background of the mission?

• Dark Sky Background

– Estimated from balloon flight data collected by Italian and US balloon experiments and from Russian satellite measurements (Tatiana). The additional light seen from space was checked against upper atmosphere models for the Hertzberg emission in the UV. Simulations show that the EAS signals an be seen above this background.

• The Moon

– We have used measurements of lunar emissions in the UV to determine the addition of reflected moonlight to the dark sky background. Since the moon is very non-Lambertian, it adds little below half-moon. Nearer full moon the threshold must be raised to accommodate the background.

• Background light from Cities

– This was measured by balloon flights and satellites. Extrapolations were made to cities not measured, scaling by population. Avoiding cities results in a rather small reduction in collection time.

• Auroral light:

– This was estimated from satellite measurements and estimated from historical patterns of auroral activity. Aurora will cause a small decrease in collection time.

• Other Sources:

– Lightening: We have found that all known forms of lightening longer duration pulses of light. These should not be confused with the EAS signal. – Xenon flash lamps on aircraft, tall towers, etc. These are too fast to satisfy the EAS trigger criterion.

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü

What will be the impact of clouds in the efficiency of the mission?

• In rough numbers:

– 1/3 of the time the sky is clear, – 1/3 of the time there are only low altitude clouds (<1 km), and – 1/3 of the time there clouds at higher altitudes, interfering with measurements.

• The cloud interference will be assessed by:

– IR imagery calibrated by nadir-pointing LIDAR measurements – Auto-detection using the forward directed Cherenkov emission from the EAS events themselves.

Andrea Santangelo, Kepler Center-Tü

・ Cloud amount, cloud top altitude: (IR cam., Lidar, slow-data) ・ Airglow： (slow-data) ・ Calibration of telescope： (Lidar)

ISS motion

JEM-EUSO

Atmospheric Monitoring System ・IR Camera

Imaging observation of cloud temperature

inside FOV of JEM-EUSO

・Lidar

Ranging observation using UV laser

・JEM-EUSO “slow-data”

Continuous background photon counting

Andrea Santangelo, Kepler Center-Tü

Calibration and Monitor by Onboard LIDAR, Ground LIDAR & Xe flasher

10~20 x LIDAR station Xe Flasher 50mJ Nd:YAG 3rd JEM-EUSO Onboard LIDAR

Andrea Santangelo, Kepler Center-Tü

How is JEM-EUSO calibrated?

• Ground based calibration:

– MAPMTs and front-end electronics are calibrated before integration in focal plane – Throughput of optics as a function of incident angle and wavelength is measured using a large collimator (USA) – Spot-size as a function of incident angle and wavelength is measured using a large collimator (USA) – Scattered light as a function of incident angle and wavelength is measured using a large collimator (needed due to background sources in the FOV near candidate EAS events) (USA) – Performance test of fully integrated instrument (Japan) – Potentially a full performance test in the flight thermal/vacuum environment (Japan or USA)

• On-orbit calibration/performance monitoring:

– Electronics performance monitored with built-in testing capabilities – MAPMT/EM performance monitored during day-light time with strategically placed LEDS within the telescope volume or on the lid – Ground Light Sources (GLS)

• ~30 GLS units strategically placed around the world, candidate sites are remote areas with

little manmade background, over-flights occur once per day on average,

• GLS are calibrated before deployment, monitored during operations and re-

calibrated/replaced as warranted

• During over-flight, the GLS flashes repeatedly and triggers the telescope and the

atmospheric monitoring system (AMS).

• The captured image and AMS data are used to reconstruct the luminosity of the GLS signal

and compared with the known luminosity of the GLS. This validates the data analysis of the EAS

• The GLS enables monitoring the spot-size of the optics because it is a point source
• The GLS includes an air-borne unit that is flown at different altitudes on a monthly basis

Altitudes will cover the range of shower maximum depths

Andrea Santangelo, Kepler Center-Tü

S-EUSO and “Cosmic Vision”

Opening Particle Astronomy “A Space Observatory for next generation studies of the Universe at Ultra High energies” Submitted to ESA in response of the AO for the first cycle of missions of the Programme “Cosmic Vision 2015-2020” Maximize the Statistics in the 1019-1021 eV energy range

DESY, Zeuthen February 26, 2010 Astroteilchenphysik in Deutschland: Status und Perspektiven

Andrea Santangelo, Kepler Center-Tü

The scientific requirements

Effective Aperture  E>106 km2 sr yr (Nadir Mode)

Low energy threshold ~E≤1019 eV Average angular resolution  Δα ∼ 1° -3° @ E≤1020 eV Energy resolution  ΔE/E ≤ 0.1 @ E≤1019 eV EAS maximum determination ΔXMAX ≤ 20 g cm-2 Orbit height  variable 800 (goal 500) -1200 km Operational life  5 yr on-orbit operational life (goal is 10 years) Long term view of the community

Andrea Santangelo, Kepler Center-Tü

Conclusions

• Space-Based observation of UHE particles can provide a

breakthrough in Physics and Astrophysics at UHE

• Detection of sources and their spectra, and of nature of

UHE particles is at the core of the science case of the JEM-EUSO Mission (launch in 2015). Phase A/B study is running full speed.

• Our simulation studies indicate that JEM-EUSO is indeed

capable of triggering, reconstructing and discriminating UHE particles: protons & nuclei, neutrinos and photons.

• We are confident that within a decade the UHE

astrophysics will be open and full of surprises.

DESY, Zeuthen February 26, 2010 Astroteilchenphysik in Deutschland: Status und Perspektiven

Andrea Santangelo, Kepler Center-Tü

Andrea Santangelo, Kepler Center-Tü Experiment / Observatory

Accepta nce [km2 sr]

Operational Year

Period [years]

Observat. Efficiency [%] CumulativeEx posure [km2 sr year] Relative Exposure to AGASA Relative Exposure to Auger South

AGASA

160 1990-2004 14 100 2.2x103 1

HiRes-I

8,000 1997-2005 8 10 6.4x103 2.9

HiRes-II

5,000 1999-2004 4 10 2.0x103 0.9

Auger South SD

7,000 2006-2020 12 100 10×104 38 1

Auger North SD

50,000 2015-2020 5 100 30.0x104 114 3

TA-SD

1,400 2007-2017 11 100 1.4×104 6.4 0.2

TA-FD

6,700 11 10 7×103 3.2 0.1

JEM-EUSO Nadir (>1020eV)

580,000 2015-2016 2 19 2.2×105 100 3

Tilt(in 38) (>1020eV)

2,900,000

2017-2020 3 19 8.3×105 380 11

Total

1.1×106 500

14

Comparison of the Cumulative Exposures

Andrea Santangelo, Kepler Center-Tü

Conceptual View of the JEM-EUSO Telescope

Andrea Santangelo, Kepler Center-Tü Tuebingen, October 19th, 2005 Fakultaets Kolloquium

« Compact » Sources of CR ?

AGASA Arrival Direction Distribution 1 Triplets 6 Doublets