BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:The calibration of the photo-detector module of the EUSO telescope DTSTART;VALUE=DATE-TIME:20151029T054000Z DTEND;VALUE=DATE-TIME:20151029T055500Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-821@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yoshiya Kawasaki (RIKEN)\nThe photo-detector module (PDM) of the EUSO is composed of 36 Hamamatsu multi-anode photomultiplier s (64 channels per tube)\, and 36 photon counting readout ASICs\, for a to tal of 2304 channels.\nWe present the calibration of the detection efficie ncy of the PDM.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribution s/821/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/821/ END:VEVENT BEGIN:VEVENT SUMMARY:Fast winds in active galactic nuclei as sources of ultra-high-ener gy cosmic rays DTSTART;VALUE=DATE-TIME:20151026T091000Z DTEND;VALUE=DATE-TIME:20151026T093000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-824@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Susumu Inoue (RIKEN)\nWe discuss the possible produc tion of ultra-high-energy cosmic rays (UHECRs) in fast winds of active gal actic nuclei (AGN). Recent X-ray observations of AGN are revealing the wid espread presence of powerful outflows of baryonic material reaching mildly relativistic velocities\, in the form of variable\, blue-shifted absorpti on lines of ionized heavy elements.\nBeing discerned in both radio-quiet a nd radio-loud AGN\, they are distinct from radio jets and likely subtend m uch broader opening angles\, and have been plausibly interpreted as winds driven by the accretion disk. In such winds\, strong shocks can plausibly form at different locations\, either external shocks due to interaction wi th the ambient medium or internal shocks due to inhomogeneities within the flow\, wherein hadrons can be potentially accelerated up to UHE. This sce nario has some clear advantages compared to the better studied picture of UHECR production in AGN jets: i) the sources can be much more numerous and nearer than radio-loud AGN and hence in better accord with the observed i sotropy\; ii) the elemental composition of the winds is not only clearly b aryonic but also guaranteed to contain heavy nuclei including iron\, and h ence can more readily account for a mixed composition as indicated by rece nt measurements. We discuss further implications of this scenario\, includ ing expectations for multi-messenger signatures.\n\nhttps://indico.icrr.u- tokyo.ac.jp/event/23/contributions/824/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/824/ END:VEVENT BEGIN:VEVENT SUMMARY:Precision research of cosmic rays from space with PAMELA detector : Results and perspectives DTSTART;VALUE=DATE-TIME:20151027T054000Z DTEND;VALUE=DATE-TIME:20151027T060000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-830@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Marco Casolino (Riken)\nThe Pamela spectrometer was launched in 2006 from the cosmodrome of Baikonur\, Kazakistan\, on board t he Russian satellite Resurs-DK1. Since then\, it has been collecting cosmi c rays from its 70 degrees inclination\, 600 km altitude polar orbit. Thi s orbit allows to sample particles of trapped\, semi-trapped nature in the Earth geomagnetosphere\, of solar origin (emitted in solar particle event s)\, of galactic origin (modulated by solar activity). Antiparticles of ga lactic origin can constrain and provide information on the dark matter c omponent in the galaxy. Furthermore the Proton and Helium spectra provide detail information on the acceleration and propagation processes in the ga laxy. At lower enegy\, particles of solar and trapped nature provide cruc ial clues on the acceleration and propagation processes in the Heliopshere . In this talk we will discuss some of these recent results of Pamela and the implication for various fields of research.\n\nhttps://indico.icrr.u- tokyo.ac.jp/event/23/contributions/830/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/830/ END:VEVENT BEGIN:VEVENT SUMMARY:Study of Ultra-High-Energy Cosmic Rays from space with K-EUSO dete ctor: status and perspectives DTSTART;VALUE=DATE-TIME:20151029T050000Z DTEND;VALUE=DATE-TIME:20151029T052000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-836@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Marco Casolino (Riken)\nKLYPVE/K-EUSO is a detector designed to detect and study Ultra-High-Energy Cosmic Rays (UHECR) from sp ace. It is Russian mission to be located on the International Space Statio n. It consists of a 3.6m diameter mirror which reflects UV light from UHEC R on a Fresnel lens\, in turn focusing the signal on a 1.4m focal surface. The focal surface is made up of 1872\, 64 channel Hamamatsu PMTs for a to tal of about 120kchannels. The Fresnel lens and the PMTs of the Focal sur face will be provided by the Japanese part of the collaboration\, with el ectronics and other parts built in Europe and other countries. In this p resentation we will discuss the status of the mission in light also of the results of the ground- and balloon-based precursors.\n\nhttps://indico.ic rr.u-tokyo.ac.jp/event/23/contributions/836/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/836/ END:VEVENT BEGIN:VEVENT SUMMARY:Energy spectrum measured by the Telescope Array experiment in 10^1 5.6 eV to 10^20.3 eV range DTSTART;VALUE=DATE-TIME:20151026T073000Z DTEND;VALUE=DATE-TIME:20151026T075000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-842@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Toshihiro FUJII (KICP University of Chicago\, ICRR U niversity of Tokyo)\nThe Telescope Array (TA) experiment is the largest co smic ray detector in the Northern Hemisphere. The TA surface detector (SD ) array is deployed on a square grid of 1.2 km spacing\, covering an effec tive area of 700 km^2. The TA SD is overlooked by three fluorescence dete ctor (FD) stations: Black Rock Mesa (BRM)\, Long Ridge (LR)\, and Middle D rum (MD). The TA BRM and LR stations cover 3 to 33 degrees in elevation\, while the TA MD\, together with the TA low energy extension (TALE) FD\, c over 3 to 57 degrees. In addition\, there is a TALE infill array\, which consists of 400 and 600 m spaced counters placed in front of the TA MD sit e at distances ranging from 1.5 to 3 km.\nThe TA SD observes cosmic rays a bove 10^18.2 eV with the most statistics. The TA FD stand alone measureme nt\, on the other hand\, is sensitive to cosmic rays above 10^17.2 eV. Bec ause of a 10% duty cycle\, it provides the best statistics in 10^17.2 eV t o 10^18.5 eV range. Together with the TALE\, the TA FD observes cosmic ra ys down to 10^15.6 eV. We report the energy spectrum of cosmic rays obtai ned by a combination of TA SD\, TA FD and TALE measurements.\n\nhttps://in dico.icrr.u-tokyo.ac.jp/event/23/contributions/842/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/842/ END:VEVENT BEGIN:VEVENT SUMMARY:Fluorescence detector Array of Single-pixel Telescopes (FAST) proj ect DTSTART;VALUE=DATE-TIME:20151029T063000Z DTEND;VALUE=DATE-TIME:20151029T064500Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-843@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Toshihiro FUJII (KICP University of Chicago\, ICRR U niversity of Tokyo)\nWe present a concept for large-area\, low-cost detect ion of ultra-high energy cosmic rays (UHECRs) with a Fluorescence detector Array of Single-pixel Telescopes (FAST)\, addressing the requirements for the next generation of UHECR experiments. In the FAST design\, a large fi eld of view is covered by a few pixels at the focal plane of a mirror or F resnel lens. We report first results of a FAST prototype installed at the Telescope Array site\, consisting of a single 200 mm photomultiplier tube (PMT) at the focal plane of a 1 m^2 Fresnel lens system taken from the pro totype of the JEM-EUSO experiment. The FAST prototype took data for 19 nig hts\, demonstrating remarkable operational stability. We detected laser sh ots at distances of several kilometres as well as 16 highly significant UH ECR shower candidates. Moreover\, we show a full-scale FAST prototype unde r construction which consists of a 2x2 PMT camera and a segmented shperica l mirror of 1.6 m diameter.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/ contributions/843/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/843/ END:VEVENT BEGIN:VEVENT SUMMARY:Mini-EUSO: Measurement of the Earth's UV background emission from the ISS as a pathfinder for the JEM-EUSO mission DTSTART;VALUE=DATE-TIME:20151029T064500Z DTEND;VALUE=DATE-TIME:20151029T070000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-848@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Oscar Larsson (Riken)\nThe key measurement for any e xperiment which aims to the observe the elusive Ultra High Energy Cosmic R ays (UHECR) from space is related to the UV background in Earth's atmosphe re and at the surface. In view of the planned missions (KLYPVE/K-EUSO\, JE M-EUSO) bound for the International Space Station (ISS)\, a small\, compac t UV telescope\, Mini-EUSO\, with the aim to the study the UV night emissi ons from the Earth\, is currently being developed by the JEM-EUSO Internat ional Collaboration. The Mini-EUSO detector will be placed at the UV trans parent\, nadir looking window of the Russian Zvezda module of the ISS. The Mini-EUSO mission has been approved by the Italian Space Agency (ASI) and \, under the name "UV atmosphere"\, also by the Russian Space Agency Rosco smos. Scientific\, technical and programmatic aspects of this project wil l be presented.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribution s/848/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/848/ END:VEVENT BEGIN:VEVENT SUMMARY:The EUSO-TA telescope for observing UHECR DTSTART;VALUE=DATE-TIME:20151029T052000Z DTEND;VALUE=DATE-TIME:20151029T054000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-849@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Lech Piotrowsi (RIKEN)\nEUSO-TA is an on-ground prot otype of an orbital Ultra High Energy Cosmic Rays detection mission - JEM- EUSO. It consists of two 1 m2 Fresnel lenses and a 2304 pixel focal surfac e\, with resulting field of view of about 10.5x10.5 degrees\, and has been working on Telescope Array site in Black Rock Mesa\, Utah\, USA since the end of February 2015. We show here first observations of calibration sour ces such as stars\, lasers and LEDs\, as well as first results from detect ion of cosmic rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribu tions/849/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/849/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent results from the Tibet ASγ experiment DTSTART;VALUE=DATE-TIME:20151026T085000Z DTEND;VALUE=DATE-TIME:20151026T091000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-865@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Takashi SAKO (Institute for Cosmic Ray Research\, Un iversity of Tokyo)\nRecent results from the Tibet ASγ experiment will be reported.\nThe presentation will be focused mainly on\nthe high-energy cos mic-ray anisotropy and\nthe research on the Sun’s magnetic field by mea ns of the Sun’s shadow observed by the Tibet air shower array.\n\nhttps: //indico.icrr.u-tokyo.ac.jp/event/23/contributions/865/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/865/ END:VEVENT BEGIN:VEVENT SUMMARY:Lens manufacturing for the near future missions of ultra high ener gy cosmic rays DTSTART;VALUE=DATE-TIME:20151029T055500Z DTEND;VALUE=DATE-TIME:20151029T061000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-851@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yoshiyuki Takizawa (RIKEN)\nWe present the lens manu facturing for the near future missions of ultra high energy cosmic rays. T he EUSO ultra long duration balloon flight mission and the K-EUSO project have been planed. The balloon optics is compose of two Fresnel lenses and a diffractive lens. The K-EUSO optics is composed of a primary aspherical mirror and a Fresnel lens as a corrector lens. RIKEN will provide Fresnel lenses for both projects.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/co ntributions/851/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/851/ END:VEVENT BEGIN:VEVENT SUMMARY:The Electron Spectrum with MAGIC DTSTART;VALUE=DATE-TIME:20151027T060000Z DTEND;VALUE=DATE-TIME:20151027T061500Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-867@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kathrin Mallot (DESY)\nVery high energy (E>100 GeV) cosmic electrons and positrons reaching Earth from beyond the solar system are important tracers of recent energetic events in our galactic neighbou rhood. Rapid energy losses due to synchrotron radiation and inverse Compto n processes result in typical lifetimes of these energetic particles of le ss than 10^5 years. Their mean free path in the Galaxy is O(1-2) Kpc. Meas urements of the flux distribution of this radiation therefore provide valu able checks in our galaxy for pulsars physics and some of the more exotic dark matter models.\n The MAGIC experiment\, a stereoscopic system of t wo Cherenkov telescopes\, can measure the total flux of cosmic electrons a nd positrons at very high energies between a few 100GeV and a few TeV.\n Such a measurement will allow to confirm the results provided by other e xperiments such as Fermi-LAT\, AMS2 as well as give a first cross-check of the results from H.E.S.S..\n We have analyzed ~60h of MAGIC observation s with a field of view of 3.5degrees with improved MC statistics. We appli ed a dedicated\, more aggressive\, image cleaning and have improved the qu ality selection as well as the background normalization. This results in t he measurement of the electron-positron flux measurement between 200GeV an d 2TeV.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/867/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/867/ END:VEVENT BEGIN:VEVENT SUMMARY:Summary of UHECR Composition Measurements by the Telescope Array E xperiment DTSTART;VALUE=DATE-TIME:20151026T075000Z DTEND;VALUE=DATE-TIME:20151026T081000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-869@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daisuke Ikeda (Institute for Cosmic Ray Research\, U niversity of Tokyo)\nWe study the chemical composition of Ultra-High Energ y Cosmic Rays (UHECRs) primarily using the Xmax technique. The reconstruct ion techniques use events either seen by two of the TA fluorescence detect ors (stereo mode)\, or by one fluorescence detector\, and one fluorescence detector and the TA surface detector (hybrid mode). We compare the obser ved Xmax distributions to those of shower Monte Carlo simulations\, by gen erating events and analyzing them with exactly the same programs as the da ta. The results of all analysis are consistent with a light composition. In this talk\, a summary of TA chemical composition analysis using the Xma x technique will be presented.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 23/contributions/869/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/869/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio Detection of Cosmic Rays DTSTART;VALUE=DATE-TIME:20151029T061000Z DTEND;VALUE=DATE-TIME:20151029T063000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-871@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Frank Schröder (Karlsruhe Institute of Technology ( KIT))\nIn the last decade significant progress was made regarding the radi o detection of cosmic-ray air showers. Mainly at MHz frequencies\, air sho wers emit a coherent radio pulse in the forward direction\, which exceeds the galactic radio background at an energy threshold of roughly 100 PeV. T he dominant emission mechanism is the deflection of electrons and positron s in the shower by the geomagnetic field\, but also sub-dominant processes as the time variation of the charge excess in the shower play a role. Usi ng digital techniques\, the detection method was successfully revived by t he LOPES and CODALEMA experiments starting 2003. Nowadays a second generat ion of digital antenna arrays\, like AERA\, LOFAR and Tunka-Rex\, starts t o become competitive with traditional air-shower techniques regarding the precision for the shower direction\, energy\, and position of the shower m aximum. Moreover\, the signal properties meanwhile are understood\, since recent simulation codes for the radio signal agree with experiments within the current measurement accuracy of the radio amplitude of less than 20 % . This talk will provide an overview on the current status of the radio te chnique and its future prospects at very dense arrays like SKA\, and spars er arrays aiming at the highest energies. In particular the combination of particle detectors and radio antennas seems promising\, because their com bination provides highest accuracy for the primary energy and mass composi tion with almost 100 % duty cycle around the clock.\n\nhttps://indico.icrr .u-tokyo.ac.jp/event/23/contributions/871/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/871/ END:VEVENT BEGIN:VEVENT SUMMARY:TA Anisotropy Summary DTSTART;VALUE=DATE-TIME:20151026T081000Z DTEND;VALUE=DATE-TIME:20151026T083000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-872@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Eiji Kido (Institute for Cosmic Ray Research\, Unive rsity of Tokyo)\nWe present the results of searching for large- and small- scale anisotropy of ultra-high energy cosmic rays (UHECRs) observed for 7 years by the surface detectors of the Telescope Array experiment. The Tele scope Array experiment accumulated the largest UHECR data set in the North ern hemisphere. At small angular scales we examine the data for clustering of events and correlations with various classes of astrophysical sources. At large angular scales we published an excess last year -- the "hot spot " -- at the highest energies by oversampling using a radius of 20 degrees\ , centered in the constellation Ursa Major. We present the estimation of t he statistical significance of this excess using the results of 7 years of observation and show how it manifests itself in various other tests. Fina lly\, we show the result of searching for correlations with the large-scal e structures in the nearby Universe.\n\nhttps://indico.icrr.u-tokyo.ac.jp/ event/23/contributions/872/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/872/ END:VEVENT BEGIN:VEVENT SUMMARY:Can we explain AMS-02 antiproton and positron excesses simultaneou sly? DTSTART;VALUE=DATE-TIME:20151027T063000Z DTEND;VALUE=DATE-TIME:20151027T064500Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-878@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kazunori Kohri (KEK)\nI explain the excess of the an tiproton fraction recently reported by the AMS-02 experiment by\nconsideri ng collisions between cosmic-ray protons accelerated by a local supernova remnant (SNR) and the surrounding dense cloud. The same "pp collisions" pr ovide the right branching fraction to fit the observed positron excess sim ultaneously without a fine tuning. The supernova happened in relatively lo wer metalicity than the majorcosmic-ray sources. The cutoff energy of elec trons marks the supernova age of ~10^5 years\, while the antiproton excess may extend to higher energy. Both antiproton and positron fluxes are comp letely consistent with our predictions in Fujita\, Kohri\, Yamazaki and Io ka (2009).\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/878 / LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/878/ END:VEVENT BEGIN:VEVENT SUMMARY:The knee of the proton spectrum DTSTART;VALUE=DATE-TIME:20151027T050000Z DTEND;VALUE=DATE-TIME:20151027T052000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-908@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Zhen Cao (IHEP\, Chinese Academy of Sciences)\nUsing a LHAASO wide field of view Cherenkov telescope and the ARGO-YBJ resistiv e plate chamber array as 4300m a.s.l.\, the energy spectrum of cosmic hydr ogen and helium nuclei (H&He) between 100 TeV and 3 PeV is measured. A cle ar knee feature is observed around 630 TeV in the spectrum with an energy resolution of about 25%. Below 300 TeV\, the data from direct charge measu rements provide rather precise measurements of fluxes of H\, He and other heavier nuclei. In this paper\, we discuss the knee feature of the pure pr oton spectrum indicated by the newly published H&He spectrum. We also esti mate the systematic errors of the spectrum measurement with a mixture of n uclei. We propose a way to minimize the systematic error in measurement of the knee feature of the cosmic ray spectrum.\n\nhttps://indico.icrr.u-tok yo.ac.jp/event/23/contributions/908/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/908/ END:VEVENT BEGIN:VEVENT SUMMARY:The Large High Altitute Air Shower Observatory by Dr. H. He DTSTART;VALUE=DATE-TIME:20151027T052000Z DTEND;VALUE=DATE-TIME:20151027T054000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-917@indico.icrr.u-tokyo.ac.jp DESCRIPTION:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/917/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/917/ END:VEVENT BEGIN:VEVENT SUMMARY:The Possible Extragalactic Source of Ultra-High-Energy Cosmic Rays at the Telescope Array Hotspot DTSTART;VALUE=DATE-TIME:20151026T093000Z DTEND;VALUE=DATE-TIME:20151026T095000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-956@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shigehiro Nagataki (RIKEN)\nThe Telescope Array (TA) collaboration has reported a hotspot of 19 ultrahigh-energy cosmic rays ( UHECRs)\, offering an opportunity to study their origin. Using a universal model with one source and energy-dependent magnetic deections\, we show t hat the distribution of the TA hotspot events is consistent with a single source hypothesis\, and that the chance probability of this distribution a ppearing from a homogeneous distribution is 0.2%. We describe a Monte Carl o Bayesian (MCB) inference approach\, which can be used to derive paramete rs of the magnetic fields as well as the source coordinates\, and we apply this method to the TA hotspot data\, inferring the location of the likely source. We discuss possible applications of the same approach to future d ata.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/956/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/956/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview and recent results of LHCf DTSTART;VALUE=DATE-TIME:20151026T083000Z DTEND;VALUE=DATE-TIME:20151026T085000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-962@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Takashi Sako (Nagoya University)\nLarge Hadron Colli der forward (LHCf) experiment was motivated to study the hadronic interact ion relevant to the air shower development at the very forward of the LHC interaction point. LHCf has measured particle production at LHC 0.9\, 2. 76\, 7 and 13TeV proton-proton collisions and 5TeV proton-Lead collisions. LHCf has tested existing hadronic interaction models and provides strong constraints to the future model improvements. In this talk\, we will pr esent the major results of LHCf including the recent measurements at LHC 1 3TeV collisions.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributio ns/962/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/962/ END:VEVENT BEGIN:VEVENT SUMMARY:Nonrelativistic shocks of young supernova remnants in kinetic simu lations DTSTART;VALUE=DATE-TIME:20151027T064500Z DTEND;VALUE=DATE-TIME:20151027T070000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-966@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Jacek Niemiec (Institute of Nuclear Physics Polish A cademy of Sciences)\nThe formation\, electromagnetic structure\, and the i njection of suprathermal particles into a Fermi-type acceleration at colli sionless shocks constitute important problems of high-energy astrophysics. We report on recent particle-in-cell studies of high Mach-number nonrelat ivistic perpendicular shocks in applications to young supernova remnants. We discuss a nonlinear shock structure mediated by Weibel-type filamentati on instabilities\, shock reformation and rippling\, and conditions leading to heating and efficient electron and ion pre-acceleration. First results of oblique quasi-perpendicular shock studies will also be presented.\n\nh ttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/966/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/966/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic-ray hardenings in the light of AMS-02 DTSTART;VALUE=DATE-TIME:20151027T061500Z DTEND;VALUE=DATE-TIME:20151027T063000Z DTSTAMP;VALUE=DATE-TIME:20260808T122613Z UID:indico-contribution-231-971@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yutaka Ohira (Aoyama Gakuin University)\nRecent prec ise observations of cosmic rays (CRs) by AMS-02 experiment clearly show (1 ) harder spectra of helium and carbon compared to protons by $¥propto R^{ 0.08}$\, and (2) concave breaks in proton and helium spectra at a rigidity $R ¥sim 300$ GV. In particular the helium and carbon spectra are exactly similar\, pointing to the same acceleration site. We examine possible int erpretations of these features and identify a chemically enriched region\, that is\, superbubbles as the most probable origin of Galactic CRs. We fu rther show that CRs originate primarily from the supernova ejecta in the s uperbubble core\, mixed with negligible interstellar medium\, and predict similar spectra for heavy nuclei.\n\nhttps://indico.icrr.u-tokyo.ac.jp/eve nt/23/contributions/971/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/971/ END:VEVENT END:VCALENDAR