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

Production: Decay chains of mesons ν e : ν µ : ν τ 1 : 2 2 : 0 (at generic source) 1 pp  π  µ ν µ  e ν e ν µ ν µ 1 : 1 : 1 ( at earth) max.mixing Other mesons like Kaons are also involved to certain degree and all decay chains are very well known  But HOW the mesons are produced ? Andrea Santangelo, Kepler Center-Tü

Sources of Neutrinos? We have an accelerator of protons to generate a proton beam Fermi mechanisms can accelerate protons We need a gas (well nuclei) or ambient photons target • Jets in AGN • Supernova ejecta • Accretion disks • Microquasars, Binaries • Galactic disk • GRB • Molecular clouds • CMB Andrea Santangelo, Kepler Center-Tü • …

Berezinsky & Zatsepin, (1969, 1970) Cosmogenic Neutrinos Berezinsky (2005) I ν /Ip Maximal Energy, Composition, Evolution of sources Andrea Santangelo, Kepler Center-Tü

AGN Mannheim (1995) B)high – A)low GZK(B) Kalashek, Speculative Kuzmin, Semokov, models Sigl (2002) GZK(A) Protheroe (1995) Astrophysical models Cosmogenic Neutrinos Andrea Santangelo, Kepler Center-Tü

UHE Neutrinos P+ 1700 g/cm2 55% ν Rejection > 10 -5 Andrea Santangelo, Kepler Center-Tü

Discrimination of Neutrinos vs Protons Rejection > 10 -5 ν P+ Xmax X1 initial point Andrea Santangelo, Kepler Center-Tü

Neutrino shower simulation • Gamma ray showers – CONEX with....  Horizontally incident neutrinos • Neutrino showers for pilot studies − Survival prob. to come in FOV – Horizontally incident  Neutrino: ~exp(-0.001)  Proton: ~exp(-1000) for 10 20 eV – PYTHIA interaction code for neutrino-nucleon interaction  CONEX code used for – CONEX code connected shower simulation in atmosphere for shower in atmosphere Andrea Santangelo, Kepler Center-Tü

The probability of neutrino interaction in atmosphere is proportional to the atmospheric density. P+ ν NEUTRINOS CC INTERACTIONS Andrea Santangelo, Kepler Center-Tü (LPM effect included)

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

AGN Mannheim (1995) B)high – A)low GZK(B) Kalashek, Speculative Kuzmin, Semokov, models Sigl (2002) GZK(A) Protheroe (1995) Astrophysical models Cosmogenic Neutrinos Andrea Santangelo, Kepler Center-Tü

Top-down models Bhatacharjee & Sigl, 2000 Particles are produced from the top, from the decay of some supermassive unstable particle 1.) particles released from topological defects, left over from the cosmological phase transitions (cosmic strings, magnetic Berezinsly, Blasi, Vilenkin 1999 monopoles, domain walls…) 2.) long-lived massive free particles 12 X q q , m 10 GeV � + X > (“WIMPZILLA” dark matter, mirror matter) 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 Auger Collaboration, 2009 SHDM models are strongly constrained by the absence of identified photon candidates in the Auger data Andrea Santangelo, Kepler Center-Tü

Neutrino Cross sections Fargion et al., 1999 Neutrino Cross Sections can be Bottai & Giurgola, 2003 measured from the ratio of Horizonthal to Upward showers Palomarez-Ruiz, Irimia and Weiler, 2006 Fargion, 1997, 2002, 2004 Yoshida et al., 2004 Andrea Santangelo, Kepler Center-Tü

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

Kifune 1997 EHE γ -rays travel > Gpc only in Quantum Gavity or C-G vacuum • E ( γ ) ε (10 -3 K) • 4 ε E - ξ ≥ 4m e c 4 Andrea Santangelo, Kepler Center-Tü

Scientific Requirements Number of Events: > 1000 (at E> 7x10 19 eV) Arrival direction: < 2.5° Point
Source Point
Source Energy determination: < 30% Energy
spectrum Energy
spectrum Xmax determination: < 120 g/cm 2 LPM
EAS LPM
EAS Neutrino
EAS Neutrino
EAS They have been confirmed by end to end simulations performed with two independent Frameworks (ESAF in Europe) Andrea Santangelo, Kepler Center-Tü

A naïve science objective: exploration of 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 outstanding 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 X max 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

Who is who… Back-up slides 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) φ 2552 Lid JEM-EUSO Fresnel Lenses Deploy Mechanism Telescope (See Next Page) Focal Surface klkdflsk:lkdsf Electronics φ 2175 EUSO Launch (Stowed) Configuration EUSO On -Orbit (Deployed) Configuration Andrea Santangelo, Folded config. Expanded config. Kepler Center-Tü EUSO Telescope Configuration (Truss Concept)

Succesfull Launch of HTV September 11, 2009 Andrea Santangelo, Kepler Center-Tü

JEM-EUSO Optics Precision
Fresnel
lens Op#cs
Requirements – FoV

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

~0.1 ° 
(5mmΦ) – Spectral
range
330‐400
nm Focal
Surface Fresnel
lenses Precision optics cancels New
Material
CYTOP chromatic aberration 
within
5mm
dia. Encircled
Energy Surface
of
the
Precision
Fresnel
lens 0.7 ~50%
up PMMA 0 Field
of
View
(deg) 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

Mirror area is 2 m 2 TUS exposure factor 3000 km2 sr per A pathfinder year (orbit height 500 km). several Events per year TUS launch date: Nov. Andrea Santangelo, 2011, Prototypes of JEM-EUSO Kepler Center-Tü

Signal for a p shower (60 deg, 10 20 eV) Mernik et al. , 2009 Andrea Santangelo, Kepler Center-Tü

500 counts/ (ns sr m 2) 31st Course of Andrea Santangelo, International School of Nuclear Physics 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

Atmospheric Monitoring System ISS motion JEM-EUSO ・ 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 ・ Cloud amount, cloud top altitude: (IR cam., Lidar, slow-data) ・ Airglow ： (slow-data) ・ Calibration of telescope ： (Lidar) Andrea Santangelo, Kepler Center-Tü

Calibration and Monitor by Onboard LIDAR, Ground LIDAR & Xe flasher JEM-EUSO Onboard LIDAR 50mJ Nd:YAG 3 rd Xe Flasher 10~20 x LIDAR station 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 Submitted to ESA in response of “A Space Observatory for next the AO for the first cycle of generation studies of the missions of the Programme Universe at Ultra High energies” “Cosmic Vision 2015-2020” Maximize the Statistics in the 10 19 -10 21 eV energy range DESY, Zeuthen February 26, 2010 Astroteilchenphysik in Deutschland: Andrea Santangelo, Status und Perspektiven Kepler Center-Tü

The scientific requirements Effective Aperture  E>10 6 km 2 sr yr (Nadir Mode) Low energy threshold  ~E ≤ 10 19 eV Average angular resolution  Δα ∼ 1° -3° @ E ≤ 10 20 eV Energy resolution  Δ E/E ≤ 0.1 @ E ≤ 10 19 eV EAS maximum determination  Δ X MAX ≤ 20 g cm -2 Orbit height  variable 800 (goal 500) -1200 km Operational life  5 yr on-orbit operational life (goal is 10 years) Andrea Santangelo, Long term view of the community 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. Andrea Santangelo, DESY, Zeuthen February 26, 2010 Astroteilchenphysik in Deutschland: Kepler Center-Tü Status und Perspektiven

Andrea Santangelo, Kepler Center-Tü

Comparison of the Cumulative Exposures Relative Accepta Observat. CumulativeEx Relative Experiment / Period Operational Exposure nce Efficiency posure Exposure Observatory Year [years] to Auger [%] [km 2 sr year] to AGASA [km 2 sr] South 2.2x10 3 AGASA 160 1990-2004 14 100 1 6.4x10 3 HiRes-I 8,000 1997-2005 8 10 2.9 5,000 1999-2004 4 10 2.0x10 3 0.9 HiRes-II Auger South SD 7,000 2006-2020 12 100 10 × 10 4 38 1 Auger North SD 50,000 2015-2020 5 100 30.0x10 4 114 3 TA-SD 1,400 11 100 1.4 × 10 4 6.4 0.2 2007-2017 TA-FD 6,700 11 10 7 × 10 3 3.2 0.1 JEM-EUSO 2.2 × 10 5 Nadir 580,000 2015-2016 2 19 100 3 (>10 20 eV) 2,900,000 2017-2020 3 19 8.3 × 10 5 380 11 Tilt(in 38) (>10 20 eV) Total 1.1 × 10 6 500 14 Andrea Santangelo, Kepler Center-Tü