Quoi de neuf en astroparticules? Damien Dornic 22/10/07

ICRC program: ~1100 contributions SH: Solar and Heliospheric Phenomena (~250 papers) SH 1: Sun and Corona SH 2: Transient Phenomena in the Heliosphere SH 3: Galactic Cosmic Rays in the Heliosphere SH 4: Anomalous component in the heliosphere SH 5: Cosmic Rays at the Termination Shock and in the Heliosheath OG: Cosmic Ray Origin and Galactic Phenomena (~400 papers) OG 1: Cosmic Ray Origin OG 2: X-ray, Gamma-ray and Neutrino Astronomy and Astrophysics HE: High Energy Phenomena (~450 papers) HE 1: Extensive Air Showers and UHE Cosmic Rays HE 2: Muons and Neutrinos HE 3: Interactions, Particle Physics Aspects, Astroparticle Physics and Cosmology

Main topics Gamma-ray Astrophysics: theoretical aspects, latest observational results from ground based experiments (H.E.S.S., MAGIC, VERITAS), prospects for AGILE and GLAST, future plans for a large gamma-ray infrastructure Neutrino telescopes: Status and future plans for Antares, Baikal, IceCube, Nemo, ANITA and future plans for a large km3 experiment Ultra-High Energy Cosmic rays: update on acceleration and propagation, latest observational results from AUGER, prospect on R&D detection Dark Matter: new strategies for indirect detection, present and future of direct searches, first results from the anti-matter space detector PAMELA

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Galactic sources & Diffuse emission

RX J1713-3946 Close correlation with X-rays Spectral shape IC implies very low magnetic field No correlation with molecular clouds

MILAGRO

Cygnus Region Mrk 421 Crab Nebula

X-ray filaments large magnetic field

Extended gamma-ray emission covering (but offset from) Westerlund 2 Due to collective effects of stellar winds in the clusters? A new source class? See also model of

Extragalactic sources - AGNs - GRBs

(M. Lemoine-Goumard)

No spectral variability compared to the low state => Causality arguments give to limit in the radius of emission

Summary

Under ground Optical: Deep- ice Deep-water Air-showers radio accoustics

MINOS Charge Ratio Model Results Charge Ratio Model Results First high-statistics measurement of muon charge ratio in TeV energy range x 1.37 1.27 x MINOS measure µ+ / µ - and fit to formulas best fit values: f π+ = A π+ /A π - = 0.55; f K+ = A K+ /A K - = 0.67

MINOS Implications for > TeV atm ν f K+ = 0.67 A N K + / A N K - = 2 Substantial contribution of associated production ( p Λ K + ) Effect is amplified for ν s: ν µ / ν µ 2 Important for atmospheric neutrino background in neutrino telescopes MINOS measurement will lead to improved calculation of >TeV φ ν

Super-Kamiokande and status of neutrino oscillations SK-III operating since July 12, 2006 Hardware and software upgrades Full complement of >11 thousand 20 PMTs plus outer (veto) detector Recalibration finished and first year data in good agreement with SK-I + SK-II Potential for lower threshold for solar neutrino analysis

Number of Events 400 300 200 100 Zenith Angle Distributions (SK-I + SK-II) Sub-GeV e-like P<400MeV/c P < SK-I + SK-II 400 300 200 100 Sub-GeV µ-like P<400MeV/cP < 200 150 100 50 ν µ ν τ oscillation (best fit) null oscillation SK-I + SK-II multi-ring e-like 0 0 0 0-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1 600 150 Multi-GeV e-like Multi-GeV µ-like Upward stopping µ Upward through-going 200 200 150 non-showering µ 400 100 150 150 100 100 100 200 50 50 50 50 0-1 -0.8-0.6-0.4-0.2 0 cosθ 300 200 100 multi-ring µ-like 0 0 0 0-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1-1 -0.5 0 0.5 1 Sub-GeV e-like 600 Sub-GeV µ-like PC stop PC through 400 300 P>400MeV/c P > P>400MeV/cP > 40 300 400 200 200 200 20 100 100 0-1 -0.5 0 0.5 1 cosθ 0-1 -0.5 0 0.5 1 cosθ 0-1 -0.8-0.6-0.4-0.2 0 cosθ All distributions agree with oscillated expectations Livetime SK-I SK-I + SK-II 1489d (FCPC) 1646d (Upmu) SK-II 804d (FCPC) 828d(Upmu) µ-like e-like Upward through-going showering µ 0-1 -0.8-0.6-0.4-0.2 0 cosθ

Neutrino oscillation status L/E dip seen at first oscillation minimum No evidence yet for any non-standard oscillations, only upper limits for sterile neutrinos oscillations increasing with energy No sign yet of possible second-order oscillation effects three-neutrino effects θ 13 MINOS in NuMi beam results consistent with SK

S-K Summary (SN burst search) 3 methods of supernova searches with newly installed criteria was conducted. Data set : from May 1996 to Oct 2005 :Total livetime: 2589.3 days (Livetime for 3rd analysis : 2381.3 days) No candidate was observed 100% detection probability up to 100 kpc SN rate within 100kpc(LMC,SMC,our Galaxy) is estimated < 0.32 SN/yr @ 90% C.L. Detection probability is maintained at a level of 7% for SN at Andromeda. No candidate of neutronization burst observed

HE neutrinos

IceCube IceTop Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV 2006-2007: 13 strings deployed Current configuration - 22 strings - 52 surface tanks 2005-2006: 8 strings InIce Planned 80 strings of 60 optical modules each 1450m 2004-2005 : 1 string AMANDA-II 19 strings 677 modules 17 m between modules 125 m string separation 2450m 2007/08: add 14 to 18 strings and tank stations AMANDA now operating as part of IceCube -talk of A. Gross Completion by 2011.

Search for diffuse ν flux Gary Hill et al.

Search for neutrinos from 32 candidate sources 1ES1959 Cyg-X3 Mk501 Mk421 Cyg-X1 M87 SS433 3C273 crab event selection optimized for both dn/de ~E -2 and E -3 spectra Achterberg et al. astro-ph/0611063 1.2σ equiv. (random maps) source Markarian 421 M87 1ES 1959+650 SS433 Cygnus X-3 Cygnus X-1 Crab Nebula 3C 273 nr. of ν events (5 years) 6 6 5 4 7 8 10 8 expected background (5 years) 7.4 6.1 4.8 6.1 6.5 7.0 6.7 4.72 E -2 flux upper limit (90% c.l.) Φ ν µ +ν τ [10-11 TeV -1 cm -2 s -1 ] 7.4 8.7 13.5 4.8 11.8 13.2 17.8 18.0 No significant excess observed

ANTARES: Conclusions and Outlook Major step forward during the last year Detector working well within design specifications: Junction Box in operation since Dec. 2002 5 lines delivering data on the site All technical problems solved 12 lines detector complete early 2008: Operation for science 5 years Antoine Kouchner Milestone towards a KM 3 underwater detector Candidates for first undersea neutrino!!

Zenith angle distribution number of events After quality cuts 5 lines 2007 data No alignement ANTARES PRELIMINARY µ Indicates good angular resolution cos θ

Present status Down-going µ (jan 2007)

Quest for cosmogenic ν Motivated by indication of GZK feature in UHE cosmic-ray spectrum Cosmogenic ν (from p + γ 2.7 n + π + ν) Probe evolution, composition, spectra of extragalactic cosmic-ray sources Goal: >1000 km 3 sr, > 100 events/yr, E >10 18 ev RICE, AURA, ANITA, ARIANNA at this conference Acoustic detection in Ice another possibility

Model dependence of cosmogenic ν Pure protons (N. Busca) Mixed Cosmic rays Neutrinos

>PeV ν absorbed in the Earth Earth-skimming ν E. Bernardini

Detector was tested in pulsed electron beam at SLAC J. Kowalski

Jaime Alvarez-Muniz The radio technique Conditions for coherent radio emission 1. Net excess charge MOON REGOLITH 2. λ obs > shower dimensions L θ Diffraction by a slit θ ~ (νl) -1

Status of Auger

Auger reconstruction techniques

Auger: energy calibration

AirFly measurements

1E-27 1E-28 1E-29 1E-30 Auger Combined HiResI HiResII J (m 2 sr s ev) -1 1E-31 1E-32 1E-33 1E-34 1E-35 1E-36 1E-37 1E-38 17.0 17.5 18.0 18.5 19.0 19.5 20.0 20.5 Auger Aperture is INDEPENDENT of models, mass or assumptions about Γ log E (ev) This is NOT the case for HiRes, problem with HiRes aperture?

Analyse : Auger spectrum

Auger: Photon limit Rise time in shower front Curvature of shower front Auger 20years operation will reach to GZK gamma flux of ~0.1%

Xmax Auger and HiRes Auger Xmax suggests mixed composition HiRes claimed proton dominance above10 18 ev

2 Spectrum Residuals vs. < ln A > 4 Fe ((J/J s ) - 1: (the residual)) 1 0 Spectrum Mass 2 < ln A > -1 17.5 18.0 18.5 19.0 19.5 20.0 log E (ev) 0 proton

Auger: Galactic Center

HiRes Anisotropy Negative excess at Anti-G.C. Significance plot for 10 17.5 < E < 10 18.5 ev. Akeno/AGASA result

Many open questions Energy scale problem 1.2~1.5 factor between Auger and other experiments FD energy (FY) SD energy (MC energy calibration) What is ankle? Pair creation dip V.Berezinsky Transition from galactic to extragalactic Chemical composition at UHE Proton dominance? support pair creation dip hypothesis Mixed composition photodisintegration energy (Eth ~A) Support Auger Xmax? Break in energy spectrum at 4x10 19 ev GZK Cutoff? Acceleration limit? Drop off of lighter elements? Medium scale anisotropy Relating with large scale structure? Deflected images of point sources (North-South asymmetry)

14 antennas (612 x 473 m) + 13 scintillators

Near futur Telescope Array: 512 scintillators + 3 FD sites ~95% construit + en phase de commissionning + Tale (exetension à basse énergie) Jem-EUSO: sur l ISS vers 2013

Résumé Foisonnement d activités expérimentales Amélioration très impressionnant de la qualité des mesures Analyse multi-messagers GLAST CTA 71 2000 UHECR 2010 Neutrinos GW

Thèmes non abordés, mais pourtant au combien intéressants!!! CR: from knee to ankle Tibet-AS, KASCADE-Grande Understanding of cosmic ray interactions Reliability of interpretation of air shower data, cross section measurements, simulation tools and related questions, accelerator data... Matter and anti-matter in CR CREAM, ATIC, PAMELA Dark matter direct searches Liquid noble gases experiments have shown dramatic progress during the last year (XENON10 )