BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Domain Wall Formation from Level Crossing in the Axiverse DTSTART;VALUE=DATE-TIME:20151026T055100Z DTEND;VALUE=DATE-TIME:20151026T060800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-820@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ryuji Daido (Tohoku university)\nWe point out that d omain wall formation is a more common phenomenon in the Axiverse than prev iously thought. Level crossing could take place if there is a mixing betwe en axions\, and if some of the axions acquire a non-zero mass through non- perturbative effects as the corresponding gauge interactions become strong . The axion potential changes significantly during the level crossing\, wh ich affects the axion dynamics in various ways. We find that\, if there is a mild hierarchy in the decay constants\, the axion starts to run along t he valley of the potential\, passing through many crests and troughs\, unt il it gets trapped in one of the minima\; the axion roulette. The axion dy namics exhibits a chaotic behavior during the oscillations\, and which min imum the axion is finally stabilized is highly sensitive to the initial mi salignment angle. Therefore\, the axion roulette is considered to be accom panied by domain wall formation. The cosmological domain wall problem can be avoided by introducing a small bias between the vacua. We discuss cosmo logical implications of the domain wall annihilation.\n\nhttps://indico.ic rr.u-tokyo.ac.jp/event/23/contributions/820/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/820/ END:VEVENT 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:20260417T115702Z UID:indico-contribution-23-821@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:MAGIC detection of very-high-energy gamma-ray emission from the z = 0.94 blazar PKS 1441+25 DTSTART;VALUE=DATE-TIME:20151026T061500Z DTEND;VALUE=DATE-TIME:20151026T063000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-822@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Miguel Nievas-Rosillo (Universidad Complutense de Ma drid\, Grupo de Altas Energías)\nVery-high-energy (VHE\, E > 100 GeV) gam ma-ray emission from the very distant flat spectrum radio quasar PKS 1441+ 25 (z = 0.940) was detected in April 2015 with the MAGIC telescopes. Aside from the gravitationally lensed VHE blazar QSO B0218+357 (z = 0.944)\, al so detected by MAGIC\, PKS 1441+25 is the most distant VHE blazar detected to date. The VHE detection occurred in April 2015 during enhanced activit y of the source at high energy (HE\, 0.1 GeV \n\nhttps://indico.icrr.u-tok yo.ac.jp/event/23/contributions/822/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/822/ END:VEVENT BEGIN:VEVENT SUMMARY:Highlights from VERITAS studies of TeV astroparticle physics DTSTART;VALUE=DATE-TIME:20151027T061300Z DTEND;VALUE=DATE-TIME:20151027T063600Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-823@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Nahee Park (University of Chicago)\nVERITAS is an ar ray of four imaging atmospheric Cherenkov telescopes designed to observe g amma-ray emission from astrophysical objects in the energy range from 85 G eV to > 30 TeV. Located at the Fred Lawrence Whipple Observatory in Arizon a\, VERITAS has operated successfully over seven years with two major upgr ades that improved the performance of the array. The scientific goals of V ERITAS include understanding the acceleration\, interactions\, and propaga tion of TeV particles by observing very high energy gamma rays from extrem e environments in both Galactic and extragalactic sources. VERITAS also co nducts searches for dark matter in the TeV energy range and performs studi es of cosmic rays. In this presentation\, we will summarize the current st atus of VERITAS and highlight recent scientific results.\n\nhttps://indico .icrr.u-tokyo.ac.jp/event/23/contributions/823/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/823/ 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:20260417T115702Z UID:indico-contribution-23-824@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:Particle acceleration and nonthermal emission from fast winds in a ctive galactic nuclei DTSTART;VALUE=DATE-TIME:20151026T063000Z DTEND;VALUE=DATE-TIME:20151026T064500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-825@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Susumu Inoue (RIKEN)\nX-ray observations of active g alactic nuclei (AGN) are revealing the widespread existence of powerful\, baryonic outflows reaching mildly relativistic velocities\, seen as variab le\, blue-shifted absorption lines of ionized heavy elements\, in both rad io-quiet and radio-loud objects. Sometimes called ultra-fast outflows (UFO s)\, they are plausibly interpreted as winds driven by the accretion disk and may be the key agents for AGN feedback onto their host galaxies\, alth ough their formation mechanism is not yet clear. We discuss the possibilit y of acceleration of electrons and hadrons in collisionless shocks that ar e likely to form at different locations in such fast winds\, together with expectations for the consequent nonthermal emission from the radio band u p to high-energy gamma-rays. We find that: 1) For some radio-quiet AGN wit h known outflows\, synchrotron emission from electrons can account for the ir radio emission whose origin is not yet clear. 2) For radio-quiet AGN wi th known outflows and tentative GeV associations such as ESO 323-G77\, ext ernal inverse Compton emission provide a potential explanation of the gamm a-rays. 3) For radio galaxies with known outflows and tentative GeV associ ations such as 3C111 and 3C120\, external inverse Compton emission provide an explanation of the gamma-rays (and partially of the X-rays) that is un related to jets. 4) For radio-quiet AGN with known outflows and GeV upper limits such as NGC 4151\, lower limits on magnetic fields can be inferred and may point to magnetically driven outflows. We conclude with a discussi on of future prospects.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/cont ributions/825/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/825/ END:VEVENT BEGIN:VEVENT SUMMARY:MAGIC detection of the the most distant AGN observed in TeV\, grav itationally lensed blazar B0218+357 DTSTART;VALUE=DATE-TIME:20151026T054500Z DTEND;VALUE=DATE-TIME:20151026T060000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-826@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Dijana Dominis Prester (University of Rijeka / The U niversity of Tokyo)\nThe blazar QSO B0218+357 is the most distant AGN (z=0 .944) detected so far in the TeV range. It is gravitationally lensed by th e galaxy B0218+357G (z=0.68). Very-high-energy (VHE) gamma-ray emission fr om QSO B0218+357 was detected in July 2014 with the MAGIC telescopes\, by measuring the time-delayed image of the flare\, detected earlier by FERMI in the GeV range. Its emission enables the study of the EBL properties whe n the Universe was only half of its present age.\nIn addition\, some featu res in the observed gamma-ray light curves hint that on the top of the tim e-delay caused by the mass of the lens galaxy\, the gravitational microlen sing effect may have occurred as well in the case of this system. The grav itational microlensing effect is very sensitive on the sizes of emitting r egions at different wavelenghts. Ideas for future MWL observations of B021 8+357 and similar systems will be discussed.\n\nhttps://indico.icrr.u-toky o.ac.jp/event/23/contributions/826/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/826/ END:VEVENT BEGIN:VEVENT SUMMARY:The Fermi GeV excess: testing the point source interpretation DTSTART;VALUE=DATE-TIME:20151027T085000Z DTEND;VALUE=DATE-TIME:20151027T090500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-828@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Francesca Calore (University of Amsterdam)\nA spatia lly extended excess of gamma rays collected by the Fermi-LAT from the inne r region of the Milky Way has been discovered by different groups and with increasingly sophisticated techniques of data analysis. I will review the characterization of spectral and morphological properties of the excess w hen variations of the Galactic diffuse emission are properly taken into ac count. Recently\, there has been strong support for a population of dim mi llisecond-pulsar-like sources being the dominant component of the excess e mission. However\, further evidence is needed. \nI will discuss how it is possible to probe the contribution from unresolved point sources with curr ent multi-wavelength observations\, in particular at radio frequencies\, a nd I will present prospects for future observatories [1].\n[1] F. Calore\, M. Di Mauro\, F. Donato\, F. Massaro and C. Weniger\, In preparation.\n\n https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/828/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/828/ END:VEVENT BEGIN:VEVENT SUMMARY:The Galactic Center region imaged with MAGIC and variability searc hes during the G2 pericenter passage DTSTART;VALUE=DATE-TIME:20151029T053500Z DTEND;VALUE=DATE-TIME:20151029T055000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-829@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Christian Fruck (Max-Planck-Institut für Physik\, M ünchen)\nWe present the results from the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) telescope of the search for TeV variability in the very high energy (VHE) gamma ray regime performed in the years 2012-2015 during the pericenter passage of the G2 gas cloud. This gas cloud orbits the Gal actic Center (GC) on a highly eccentric trajectory with a pericenter dista nce of only a few thousand Schwarzschild radii\, The GC has been monitored by MAGIC for over three years. Due to its location in the northern hemisp here\, MAGIC observes the GC at large zenith angles (58-70 deg)\, resultin g in a higher energy threshold\, but an enhanced effective collection area at multi-TeV energies.\nNo variability was detected in the TeV regime\, b ut these observations also gave us the opportunity to study the overall mo rphology of the TeV sources in the vicinity of the GC in great detail. We will discuss possible source counterparts in other wavelengths and various scenarios for the production of VHE emission in this complex region.\n\nh ttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/829/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/829/ 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:20260417T115702Z UID:indico-contribution-23-830@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:Cartan's Supersymmetry and the Universe DTSTART;VALUE=DATE-TIME:20151026T064200Z DTEND;VALUE=DATE-TIME:20151026T065900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-831@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sadataka Furui (Graduate School of Science and Engin eering\, Teikyo University)\nCartan has proposed a model of number systems given by octonions and a pair of 4 dimensional vector system. Octonions c ontains 2 quaternions or a pair of Dirac particles\nand by the transformat ion G_{23}\, particle-antiparticle transformation occurs\, and by the tran sformations G_{12}\,G_{123}\,G_{13} and G_{132}\, supersymmetric transform ation occur.\nWe extend the model to the system in which quark\, leptons\, gauge fields and Higgs particles are interacting\, and the construct a pi cture of the universe.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contr ibutions/831/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/831/ END:VEVENT BEGIN:VEVENT SUMMARY:Charged Q-balls in gauge mediated SUSY breaking models DTSTART;VALUE=DATE-TIME:20151026T053400Z DTEND;VALUE=DATE-TIME:20151026T055100Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-832@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Jeong-Pyong Hong (Institute for Cosmic Ray Research University of Tokyo)\nIt is known that after Affleck-Dine baryogenesis\, s patial inhomogeneities of Affleck-Dine field grow into non-topological sol itons called Q-balls. In gauge mediated SUSY breaking models\, sufficientl y large Q-balls with baryon charge are stable while Q-balls with lepton ch arge can always decay into leptons. For a Q-ball that carries nonzero $B$ and $L$ charges\, the difference between the baryonic component and the le ptonic component in decay rate may induce nonzero electric charge on the Q -ball. This implies that charged Q-ball\, also called gauged Q-ball\, may emerge in our universe. We investigate two complex scalar fields\, a baryo nic scalar field and a leptonic one\, in an Abelian gauge theory\, and we find stable solutions of gauged Q-balls for different baryon and lepton ch arges. Those solutions shows that a Coulomb potential arises and the Q-bal l becomes electrically charged as expected. It is energetically favored th at some amount of leptonic component decays\, but there is an upper bound on its amount due to the Coulomb force. The baryonic decay also becomes po ssible by virtue of electrical repulsion and we find the condition to supp ress it so that the charged Q-balls can survive in the universe.\n\nhttps: //indico.icrr.u-tokyo.ac.jp/event/23/contributions/832/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/832/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Galactic Sources of Very High Energy Gamma-Ray Emiss ion: Highlights from Ground-Based Experiments DTSTART;VALUE=DATE-TIME:20151027T023000Z DTEND;VALUE=DATE-TIME:20151027T030000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-833@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Reshmi Mukherjee (Barnard College\, Columbia Univers ity)\nThe three major ground-based gamma-ray experiments\, H.E.S.S.\, MAGI C\nand VERITAS have carried out an extensive program of very high energy\n (VHE) observations of the Universe and revolutionized our view of the\nVHE gamma-ray sky. Studies at TeV energies are valuable for exploring\nthe un derlying energetic particle populations in Galactic systems.\nGalactic gam ma-ray sources include shell-type supernova remnants\n(SNRs)\, pulsar wind nebulae (PWN)\, X-ray binary systems\, pulsars\, and\nthe Galactic Center region and its halo\, with PWN in particular\,\ncomprising the bulk of kn own galactic TeV gamma-ray emitting objects.\nH.E.S.S. has also carried ou t an unprecedented survey of the Milky Way\nGalaxy\, revealing several Gal actic VHE sources\, and VERITAS has\ncarried out a survey of the Cygnus re gion\, covering targets previously\nstudied by Milagro. The study of the G alactic VHE sky by ground-based\nIACTs is complemented by the recently-com missioned HAWC array in\nMexico. We will report on some of the highlights of the VHE sky as\nrevealed by ground-based atmospheric Cherenkov telescop es.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/833/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/833/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Future of ground gamma-ray astrophysics DTSTART;VALUE=DATE-TIME:20151030T024500Z DTEND;VALUE=DATE-TIME:20151030T031500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-834@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masahiro Teshima ()\nhttps://indico.icrr.u-tokyo.ac. jp/event/23/contributions/834/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/834/ 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:20260417T115702Z UID:indico-contribution-23-836@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:Radiative Higgs Lepton-Flavor-Violating Decay Mediated by Leptophl ic Dark Matter DTSTART;VALUE=DATE-TIME:20151029T094700Z DTEND;VALUE=DATE-TIME:20151029T100000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-837@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: zhaofeng kang (KIAS)\nIn the standard model (SM)\, H iggs lepton-flavor-violating (LFV) decay is absent and thus it is a good p robe to new physics. In this article we study a type of new physics that c ould lead to large Higgs LFV decay\, i.e.\, leptophlic dark matter (DM) sp ecified by the particle property of DM (a Majorana fermion) and DM-SM medi ators (scalar leptons). Different than other similar setups\, here we intr oduce both the left-handed and right-handed scalar leptons. They allow for large LFV in Higgs decay and thus may explain the tentative Br$(h\\ra\\ta u\\mu)\\sim1\\%$. In particular\, we find that the stringent bound from $\ \tau\\ra\\mu\\gamma$ can be naturally avoided. Aspects of relic density an d especially radiative direct detection of the leptonic DM are also invest igated.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/837/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/837/ END:VEVENT BEGIN:VEVENT SUMMARY:Higgs Portal Dark Matter and GeV Gamma-ray Excess DTSTART;VALUE=DATE-TIME:20151029T085600Z DTEND;VALUE=DATE-TIME:20151029T091300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-838@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yong Tang (Korea Institute for Advanced Study)\nThe recent claim that gamma-ray excess exists in FERMI data has triggerred man y interesting discussions. Here we propose several simple higgs-portal dar k matter models for explaining the excess. We also compare various channel s using global fit.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribu tions/838/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/838/ END:VEVENT BEGIN:VEVENT SUMMARY:Pulsations from the Vela Pulsar down to 20GeV with H.E.S.S. II DTSTART;VALUE=DATE-TIME:20151029T052000Z DTEND;VALUE=DATE-TIME:20151029T053500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-839@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Bronislaw Rudak (Nicolaus Copernicus Astronomical Ce nter\, Warsaw)\nThe Vela pulsar (PSR J0835 − 4510) is the brightest pers istent source in the high-energy γ-ray sky. It is a relatively near\, you ng and energetic rotation-powered pulsar. Vela was a key target for the Hi gh Energy Stereoscopic System phase II array (H.E.S.S. II). Observations w ere carried out following a hint of pulsed emission above 20GeV seen using Fermi-LAT data. In this talk we present detailed results from the analysi s of data only from the new 28m telescope in monoscopic mode. A high-signi ficance pulsed emission is detected. The low-energy performance of the H.E .S.S. II instrument in monoscopic mode is clearly demonstrated given a dis tinct pulsed excess down to energies of 20GeV. The H.E.S.S. II data provid e a thorough insight into the general phase profile of the Vela pulsar and reveal the specific pulse shape at these energies.\n\nhttps://indico.icrr .u-tokyo.ac.jp/event/23/contributions/839/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/839/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: High energy neutrino astrophysics DTSTART;VALUE=DATE-TIME:20151026T010000Z DTEND;VALUE=DATE-TIME:20151026T013000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-840@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Aya Ishihara (Chiba University)\nFollowing the first observation of PeV neutrino events and successful measurements of high en ergy extraterrestrial neutrino flux in the energy region between a few ten s of TeV and PeV significantly above the atmospheric neutrino background f lux by IceCube\, the field of neutrino astrophysics is becoming more and m ore active. In this contribution\, I summarize the recent experimental res ults from cosmic neutrino observatories\, such as IceCube and ANTARES. The oretical interpretations and their challenges are briefly discussed follow ed by future prospects of the neutrino astronomy.\n\nhttps://indico.icrr.u -tokyo.ac.jp/event/23/contributions/840/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/840/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Recent cosmic-ray anomalies and their interpretation DTSTART;VALUE=DATE-TIME:20151026T023000Z DTEND;VALUE=DATE-TIME:20151026T030000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-841@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Antje Putze (LAPTH\, Universite de Savoie)\nIn recen t years\, direct cosmic-ray detectors reached an unprecedented level of pr ecision\, allowing to measure new spectral features deviating from longsta nding expectations and extrapolations. In this talk\, I will review some m ain theories trying to explain the latest observations of charged cosmic r ays. These ideas range from acceleration and propagation effects to additi onal contributions from local sources or dark-matter annihilation. I will then discuss the implications for indirect dark-matter searches.\n\nhttps: //indico.icrr.u-tokyo.ac.jp/event/23/contributions/841/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/841/ 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:20260417T115702Z UID:indico-contribution-23-842@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:20260417T115702Z UID:indico-contribution-23-843@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:Multi-Messenger Tests for the Origin of Cosmic High-Energy Neutrin os DTSTART;VALUE=DATE-TIME:20151026T054000Z DTEND;VALUE=DATE-TIME:20151026T060000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-844@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kohta Murase (Penn State University)\nI review vario us scenarios for the origin of high-energy cosmic neutrinos\, and show how multi-messenger data can be utilized to constrain the models. I discuss t he present implications and prospects for the future observation.\n\nhttps ://indico.icrr.u-tokyo.ac.jp/event/23/contributions/844/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/844/ END:VEVENT BEGIN:VEVENT SUMMARY:Blazars as Cosmic-Ray Sources DTSTART;VALUE=DATE-TIME:20151026T050000Z DTEND;VALUE=DATE-TIME:20151026T052500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-845@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kohta Murase (Penn State University)\nActive galacti c nuclei\, including blazars\, have been considered as cosmic-ray source c andidates\, and GeV-TeV gamma rays can be used as a powerful probe. I will discuss signatures of secondary gamma rays and their multi-messenger conn ection.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/845/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/845/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic Center excess by two Higgs doublet portal scalar dark mat ter DTSTART;VALUE=DATE-TIME:20151029T091300Z DTEND;VALUE=DATE-TIME:20151029T093000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-846@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Osamu Seto (Hokkai-Gakuen University)\nWe consider a simple extension of the Higgs sector in a Higgs portal dark matter where a real scalar is a candidate for dark matter in the present Universe. This Higgs sector extension allows that its dark matter annihilation suitably explains the observed excess of the gamma-ray flux from the Galactic Cente r. We identify the parameter region of the model that can fit the gamma-ra y excess and satisfy phenomenological constraints\, such as the observed d ark matter relic density and the null results of direct dark matter search experiments.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/ 846/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/846/ END:VEVENT BEGIN:VEVENT SUMMARY:Searches for high energy neutrinos and gravitational waves: recent results in data from the LIGO and Virgo detectors and expectations for th e Advanced Detector Era DTSTART;VALUE=DATE-TIME:20151029T092500Z DTEND;VALUE=DATE-TIME:20151029T094000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-847@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Di Palma Irene (University of Rome\, "La Sapienza")\ nMany of the astrophysical sources and violent phenomena observed in our U niverse are potential emitters of gravitational waves and high energy neut rinos. Both these probes are\ncosmic messengers that may escape much dense r media than photons. LIGO and Virgo scientific collaborations have carrie d out joint searches for gravitational waves and high energy neutrinos fro m IceCube and ANTARES neutrino detectors. I report the results of these co incident analyses and present plans and expectations for the Advanced Dete ctor Era.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/847/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/847/ 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:20260417T115702Z UID:indico-contribution-23-848@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:20260417T115702Z UID:indico-contribution-23-849@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:New Results from the CRESST Experiment DTSTART;VALUE=DATE-TIME:20151029T062500Z DTEND;VALUE=DATE-TIME:20151029T064200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-850@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Raimund Strauss (MPI für Physik München)\nThe CRES ST (Cryogenic Rare Event Search with Superconducting Thermometers) experim ent aims at the direct detection of WIMPs. The recent Dark Matter run was operated for 2 years with a total target mass of 5kg. With respect to prev ious measuring campaigns the intrinsic radiopurity of CaWO4 crystals and t he capability to reject recoil events from alpha surface contamination has been significantly improved. We analyzed the data acquired by two CaWO4 d etectors which combine an unprecedented background level with a trigger th reshold as low as 300eV. In this talk\, we present a new detector design a nd the results of a low-threshold analysis which set stringent limits for the spin-independent WIMP-nucleon cross section\, in particular for low-ma ss WIMPs. The status of the currently ongoing preparations towards the nex t phase of CRESST and the strategy beyond will be discussed.\n\nhttps://in dico.icrr.u-tokyo.ac.jp/event/23/contributions/850/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/850/ 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:20260417T115702Z UID:indico-contribution-23-865@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:20260417T115702Z UID:indico-contribution-23-851@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:Multi-band variability and correlation study of the extraordinary Mrk421 flare in April 2013 DTSTART;VALUE=DATE-TIME:20151026T084300Z DTEND;VALUE=DATE-TIME:20151026T085800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-853@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Francesco Borracci (Max Planck Institute for Physics (MAGIC Telescopes))\nThe blazar Mrk 421 is one of the closest and brighte st extragalactic very high energy (VHE\, >100 GeV) gamma-ray emitters\, an d hence one of the VHE objects that we can study best. Since 2009\, Mrk 42 1 is yearly observed during 6 months with more than 25 instruments in the framework of broadband multifrequency campaigns. During April 2013\, Mrk42 1 underwent unprecedented flaring activity in many wavelengths\, which w as densely monitored at VHE by MAGIC and VERITAS (up to fluxes of the orde r of ~18 Crab Units above 800 GeV)\, in the hard X-rays by NuSTAR\, in the soft X-rays by Swift-XRT\, and by numerous optical facilities. The high s ensitivity of the instruments involved\, together with the ~45 hours of st rictly simultaneous observations in the VHE and X-ray energy bands during the entire period of the flare (i.e. 10 consecutive days)\, make this data set an unique opportunity for unveiling the highly energetic emission on s ub-hour timescales. Here we perform detailed correlations studies and an e xquisite characterization of the multi-band flux variability of the source . We will also discuss the origin of the VHE emission with our new results .\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/853/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/853/ END:VEVENT BEGIN:VEVENT SUMMARY:Results of the ARAcalTA experiment: measurement of the coherent ra dio emission from an electron excess in ice. DTSTART;VALUE=DATE-TIME:20151026T063000Z DTEND;VALUE=DATE-TIME:20151026T064500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-854@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Romain Gaior (Chiba University)\nThe Askaryan Radio Array is a neutrino radio detector array being\nbuilt at the south p ole. It aims at the observation of cosmic ultra\nhigh energy neutrino (E > 10PeV) via the coherent radio waves emitted\nfrom the charge excess in the cascade induced after the interaction of\nthe neutrinos in ice. The radio signal expected by ARA rely mostly on\nthe simulation of the emissi on process\, the Askaryan radiation\, and\nthe detector response. In or der to verify both of these aspects\, we\nset up a replica of ARA ex periment\, ARAcalTA\, using the 40 MeV\nelectron beam of the Electron Light Source facility at Telescope Array\nsite. Electron bunches were s hot in a block of ice to produce an\nelectromagnetic shower and the re sulting radiation was collected with\nARA sensors. Parameters such as c oherence\, polarization ratio and\nangular distribution were measured. The difficulty in this experiment\ncomes from the estimation of the possible background such as\ntransition radiation and the radiation from the beam appearance.\nAfter describing the experimental setup a nd the presentation of the\nmain measurements\, we will interpret our r esults in the light of the\nsimulation of the various emission process.\n \nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/854/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/854/ END:VEVENT BEGIN:VEVENT SUMMARY:Electroweak physics and Dark Matter: colliders vs sky DTSTART;VALUE=DATE-TIME:20151026T083900Z DTEND;VALUE=DATE-TIME:20151026T085600Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-855@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Filippo Sala (IPhT\, CEA/Saclay)\nProbing the therma l WIMP paradigm for Dark Matter is one of the primary goals of the high en ergy physics community. To study the interplay of the LHC with direct and indirect detection experiments\, it is necessary to study benchmark WIMP m odels. I will do so by adding to the Standard Model an electroweak multipl et\, which is arguably the simplest way to realise such a study. Besides t hat\, these DM candidates are also motivated by Supersymmetry\, Minimal Da rk Matter\, and strongly-coupled constructions. I will overview\nthe inter play of several different constraints\, commenting also on the impact of e lectroweak corrections\, in particular at a futuristic 100 TeV pp collider .\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/855/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/855/ END:VEVENT BEGIN:VEVENT SUMMARY:On muon->electron+photon and (g-2)_muon in Non-Sterile Electroweak Scale Right-Handed Neutrino Models DTSTART;VALUE=DATE-TIME:20151026T062500Z DTEND;VALUE=DATE-TIME:20151026T064200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-856@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Tzu-Chiang Yuan (Institute of Physics\, Academia Sin ica\, Taiwan)\nAn updated analysis on the mu --> e + gamma was performed i n a new class of non-sterile electroweak scale right-handed neutrino model s with a A_4 symmetry in the neutrino sector. This class of models provide an interesting link between charged lepton flavor violating processes to the physics of neutrino sector. Constraints from the current limit and pro jected sensitivity from MEG experiment are studied in details. Finally\, t he anomalous magnetic moment of the muon will be discussed.\n\nhttps://ind ico.icrr.u-tokyo.ac.jp/event/23/contributions/856/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/856/ END:VEVENT BEGIN:VEVENT SUMMARY:Distinguishing WIMP-nucleon interactions with directional dark mat ter experiments DTSTART;VALUE=DATE-TIME:20151027T053400Z DTEND;VALUE=DATE-TIME:20151027T055100Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-857@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Bradley Kavanagh (IPhT - CEA/Saclay)\nThe framework of non-relativistic effective field theory (NREFT) aims to generalise the standard analysis of direct detection experiments\, which is typically fra med in terms of spin-dependent (SD) and spin-independent (SI) interactions . I will show that a number of these more general NREFT operators lead to distinctive new directional signatures\, such as prominent ring-like featu res in the directional recoil rate\, even for relatively low mass WIMPs. I will focus on how well different operators can be distinguished in direct ional and non-directional direct detection experiments. In particular\, I will show that for certain NREFT operators\, directional sensitivity provi des the only method of distinguishing them from the standard SI/SD operato rs\, highlighting the importance of directional detectors in probing the p article physics of dark matter.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event /23/contributions/857/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/857/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent observations of Active Galactic Nuclei with H.E.S.S. DTSTART;VALUE=DATE-TIME:20151026T052500Z DTEND;VALUE=DATE-TIME:20151026T054500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-858@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Robert Wagner (University of Stockholm)\nBy upgradin g the H.E.S.S. array of Imaging Atmospheric Cherenkov Telescopes with a fi fth\, 28-m diameter telescope\, the sensitivity of H.E.S.S. towards low ga mma-ray energies has been extended to energies below 100 GeV. This allows studies particularly of distant Active Galactic Nuclei (AGN) with soft gam ma-ray spectra. Results of observations with the five-telescope array will be discussed\, including the low-energy view of H.E.S.S. on the blazar-ty pe AGN PKS 2155-304 and PG 1553+113. We also will discuss how low-energy A GN observations will improve our insights on radiation mechanisms in blaza rs\, on the extragalactic background light\, but also on fundamental physi cs topics.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/858 / LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/858/ END:VEVENT BEGIN:VEVENT SUMMARY:The Mopra Southern Galactic Plane Molecular Gas Survey - why the C TA needs it DTSTART;VALUE=DATE-TIME:20151029T085500Z DTEND;VALUE=DATE-TIME:20151029T091000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-859@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Michael Burton (University of New South Wales)\nThe Mopra Southern Galactic Plane molecular gas survey is the next generation CO survey of the distribution and dynamics of the molecular gas along the southern galactic plane. Being conducted with 0.6 arcmin and 0.1 km/s res olution\, it provides an order of magnitude improvement in both spatial an d spectral resolution over the Dame et al 2001 survey\, currently our stan dard source of reference on the distribution of the molecular gas in our G alaxy. It is also being conducted in three isotopologues of the molecule\ , not just one\, so providing information on the optical depth (and hence the column density). Knowledge of the distribution of the molecular gas a s a function of distance from the Sun is a key input for the interpretatio n of TeV gamma ray images\, for molecules provide the greatest column dens ities of nuclei that high energy cosmic rays might collide with\, in the h adronic scenario for TeV gamma ray production. With CTA's resolution appr oaching an arcminute\, an order of magnitude improvement on the HESS\, it will be essential to know the distribution of the gas on this scale in ord er to be able to fully interpret the gamma ray images it will produce. Th e Mopra CO survey is being conducted with the CTA's needs as a primary dri ver. This talk will describe the status of the Mopra CO survey\, and illu strate the difference that the order of magnitude improvement in spatial r esolution brings to the cartographic charting of the Galaxy's interstellar medium.\n\nFurther details at the project website: www.phys.unsw.edu.au/m opraco\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/859/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/859/ END:VEVENT BEGIN:VEVENT SUMMARY:Multiwavelength properties of gamma-ray binary systems DTSTART;VALUE=DATE-TIME:20151029T061000Z DTEND;VALUE=DATE-TIME:20151029T063000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-860@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Dmitriy Khangulyan (Rikkyo University)\nSeveral comp act binary systems appeared to have spectral energy\ndistributions that pe ak is gamma-ray energy band. Almost all these\nsources have been detected in the high energy and very high energy\nregimes with Fermi/LAT and ground based Cherenkov detectors\,\nrespectively. Detection of very high energy photons from these compact\nsources implies operation of a very efficient particle accelerator in\nthere. Moreover\, comparison of the spectra and l ightcurves collected\nwith these instruments suggests that there should be present several\ndistinct production sites for gamma-ray emission. Proper implications\nof these striking facts on particle acceleration theories d emands\naccurate modelling of the physical processes taking place in gamma -ray\nbinary systems. This includes hydrodynamic simulations\, calculation s\nof the production and transport of non-thermal emission. In this talk\n I will present these simulations for two binary systems: LS 5039 and\n1FGL J1018.65856.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/ 860/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/860/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Status of the CALorimetric Electron Telescope on the International Space Station DTSTART;VALUE=DATE-TIME:20151030T021500Z DTEND;VALUE=DATE-TIME:20151030T024500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-862@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shoji Torii (Waseda University)\nThe CALorimetric El ectron Telescope (CALET) space experiment\, which had been developed by Ja pan in collaboration with Italy and the United States\, is a high-energy a stroparticle physics mission on the International Space Station (ISS). The primary goals of the CALET mission include investigating possible nearby sources of high energy electrons\, studying the details of galactic partic le propagation and searching for dark matter signatures. During a two-year mission\, extendable to five years\, the CALET experiment will measure th e flux of cosmic-ray electrons (including positrons) to 20 TeV\, gamma-ray s to 10 TeV and nuclei with Z=1 to 40 to 1000 TeV.\nThe instrument consis ts of two layers of segmented plastic scintillators for the cosmic-ray cha rge identification (CHD)\, a 3 radiation length thick tungsten-scintillati ng fiber imaging calorimeter(IMC) and a 27 radiation length thick lead-tun gstate calorimeter (TASC). CALET has sufficient depth\, imaging capabiliti es and excellent energy resolution to allow for a clear separation between hadrons and electrons and between charged particles and gamma rays. The p ayload is being prepared for launch on Aug. 16th\, 2015 to the ISS with HTV-5 (H-II Transfer Vehicle5) and installed on the Japanese Experiment Mo dule-Exposed Facility (JEM-EF). \nWe will have the first report of the CAL ET observations on the ISS.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/ contributions/862/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/862/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma ray tests of Minimal Dark Matter DTSTART;VALUE=DATE-TIME:20151029T093000Z DTEND;VALUE=DATE-TIME:20151029T094700Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-863@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Paolo Panci (Institut d'Astrophysique de Paris (IAP) )\nWe reconsider the model of Minimal Dark Matter (a fermionic\, hyperchar ge-less quintuplet of the EW interactions) and precisely compute its gamma ray signals. We compare them with a number of gamma-ray probes: the galac tic halo diffuse measurements\, the galactic center line searches and rece nt dwarf galaxies observations. We find that the original minimal model\, whose mass is fixed at 9.4 TeV by the relic abundance requirement\, is par ticularly constrained by the line searches: it is ruled out if the Milky W ay possesses a cuspy profile such as NFW but it is still allowed if it has a cored one. Searches of gamma-ray lines from dwarf spheroidal galaxies a re also particularly relevant\, and ongoing astrophysical progresses have the potential to eventually rule out the model. We also explore a wider ma ss range. Furthermore\, most of our results can be safely extended to the larger class of multi-TeV WIMP DM annihilating into massive gauge bosons.\ n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/863/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/863/ END:VEVENT BEGIN:VEVENT SUMMARY:KM3NeT: Neutrino astronomy and oscillation research in the Mediter ranean Sea DTSTART;VALUE=DATE-TIME:20151026T050000Z DTEND;VALUE=DATE-TIME:20151026T052000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-866@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Veronique Van Elewyck (APC)\nThe KM3NeT Collaboratio n is currently constructing the first phase of a\nnext-generation neutrino telescope on two sites in the Mediterranean\nSea: KM3NeT-FR near Toulon ( France)\, and KM3NeT-IT near Capo Passero in\nSicily (Italy). Each site wi ll host a three-dimensional array of\nthousands of photosensors that will detect the Cherenkov light resulting\nfrom neutrino interactions in the vi cinity of the detector. The KM3NeT\ndetector relies on a novel design for its Digital Optical Modules\,\nhousing 31 three-inch photomultiplier tubes enclosed in a glass sphere\,\nwhich provide enhanced photon counting and directionality performances.\n\nTwo configurations have been defined that are optimised for studies in\ndifferent ranges of energy. KM3NeT-FR will be mainly dedicated to the\nstudy of oscillation effects and the measureme nt of the neutrino mass\nhierarchy with ~GeV atmospheric neutrinos (ORCA). KM3NeT-IT will focus\non high-energy (TeV-PeV) neutrino astronomy\, aimin g at the exploration\nof the all-flavour neutrino sky with unprecedented r esolution (ARCA).\n\nThis contribution will present the status of the firs t phase of the\nKM3NeT detector implementation\, and survey the physics po tentialities of the telescope with respect to its twofold aim.\n\nhttps:// indico.icrr.u-tokyo.ac.jp/event/23/contributions/866/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/866/ END:VEVENT BEGIN:VEVENT SUMMARY:The Electron Spectrum with MAGIC DTSTART;VALUE=DATE-TIME:20151027T060000Z DTEND;VALUE=DATE-TIME:20151027T061500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-867@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:Strong support for a millisecond pulsar origin of the galactic cen ter GeV excess DTSTART;VALUE=DATE-TIME:20151027T073000Z DTEND;VALUE=DATE-TIME:20151027T074700Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-868@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Richard Bartels (University of Amsterdam\, GRAPPA)\n Using gamma-ray data from the Fermi Large Area Telescope\, various groups have identified an excess emission in the inner Galaxy centred around ener gies of a few GeV. This excess resembles remarkably well a signal from dar k matter annihilation. One of the most plausible astrophysical interpretat ions is in terms of the combined emission from an undetected population of dim gamma-ray sources. In particular\, millisecond pulsars are the best c andidates due to their spectral similarity to the excess emission. We sear ch for this hypothetical source population using a novel approach based on a wavelet decomposition of the gamma-ray sky and using the latest pass 8 data. Assuming a spatial distribution compatible with the GeV excess emiss ion\, we find evidence for the existence of such a population of dim sourc es in the inner galaxy at high significance. For plausible values of the l uminosity function\, this component can explain 100% of the observed exces s emission.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/86 8/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/868/ 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:20260417T115702Z UID:indico-contribution-23-869@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:Gamma-ray emission from the recently discovered dwarf galaxy Retic ulum II DTSTART;VALUE=DATE-TIME:20151027T083800Z DTEND;VALUE=DATE-TIME:20151027T085500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-870@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Savvas Koushiappas (Brown University)\nI will presen t results on the analysis of gamma-ray emission from the recently discover ed dwarf galaxy Reticulum II. Using Fermi-LAT data and a suite of backgro und models we quantify the probability that the observed gamma-ray emissi on is due to background. Taking into account trials factors\, we find emi ssion p-values in the range between 9.8x10^-5 and 9.7x10^-3 and conclude t hat Reticulum II has the most significant gamma-ray emission from any othe r known dwarf galaxy. I will also discuss the dark matter content of Retic ulum II as derived from kinematic studies of its member stellar population and show that Reticulum II has a dark matter halo similar to other nearby dwarf galaxies. If the gamma ray emission is due to dark matter annihilat ion\, the annihilation cross section is consistent with the s-wave relic a bundance cross section. I will conclude by discussing further tests that a re needed in order to ascertain the likelihood of this emission to be due to a conventional astrophysical interpretation.\n\nhttps://indico.icrr.u-t okyo.ac.jp/event/23/contributions/870/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/870/ END:VEVENT BEGIN:VEVENT SUMMARY:Radio Detection of Cosmic Rays DTSTART;VALUE=DATE-TIME:20151029T061000Z DTEND;VALUE=DATE-TIME:20151029T063000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-871@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:20260417T115702Z UID:indico-contribution-23-872@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:Determination of the extragalactic background light spectral energ y distribution with H.E.S.S. DTSTART;VALUE=DATE-TIME:20151026T081300Z DTEND;VALUE=DATE-TIME:20151026T082800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-873@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Fabian Schüssler (CEA-Saclay / Irfu)\nWhen very hig h-energy photons (VHE\, E>100 GeV) propagate over cosmological distances\, they interact with background light by pair production. Observations of s pectral features in the VHE band of extragalactic sources related to this energy-dependent absorption process with the H.E.S.S. array of Cherenkov t elescopes allow measuring the spectral energy distribution (SED) of the ex tragalactic background light (EBL)\, otherwise very difficult to determine . Preliminary results on the determination of the SED of the EBL will be p resented\, based on the measurements of the energy spectra of blazars with H.E.S.S. . This model independent approach shows that the shape and overa ll normalization of the EBL SED is accessible.\n\nhttps://indico.icrr.u-to kyo.ac.jp/event/23/contributions/873/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/873/ END:VEVENT BEGIN:VEVENT SUMMARY:Spying on the next-door blazar Markarian 501 during multiple years DTSTART;VALUE=DATE-TIME:20151026T085800Z DTEND;VALUE=DATE-TIME:20151026T091300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-876@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Marlene Doert (Ruhr-Universität Bochum)\nWe present recent results on the high-frequency-peaked BL Lac object Markarian 501 d erived from extensive multi-wavelength campaigns in the years 2009\, 2012 and 2013. The blazar is located in our extragalactic neighborhood (z=0.034 )\, which reduces spectral uncertainties due to absorption effects of the Extragalactic Background Light and allows for significant detections on su b-hour timescales\, thus permitting precise studies of its multi-band flux variability and evolution of its broadband spectral energy distribution. \nWe will present the first broadband SED that includes the sensitive hard X-ray data from NuSTAR\, the first light curves with FACT compared to tho se of MAGIC and VERITAS\, and we will report about the first physics resul t obtained with Cherenkov telescope data taken under challenging atmospher ic conditions and corrected with information from the MAGIC LIDAR. We will show that also in the HBL Mrk 501 a rotation of the optical polarisation vector can be measured coinciding with gamma-ray flares\, as it was observ ed in LBLs and FSRQs. We will also discuss the finding that the X-ray and gamma-ray spectra of Mrk 501 can be harder than those of many known extrem e blazars\, suggesting that being "extreme" may be a temporal state rather than an intrinsic characteristic of a blazar. A novel technique to model broadband SEDs with a substantially smaller bias in terms of assumptions w ill also be presented\, leading to the conclusions that some SSC model par ameters can be strongly constrained by the data\, while others not\, and t hat the broadband SED of Mrk 501 during a flaring state can also be succes sfully modelled with Doppler factors one order of magnitude smaller than t hose typically used in the literature.\n\nhttps://indico.icrr.u-tokyo.ac.j p/event/23/contributions/876/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/876/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: The Extragalactic Gamma-ray sky DTSTART;VALUE=DATE-TIME:20151027T010000Z DTEND;VALUE=DATE-TIME:20151027T013000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-918@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Paolo Giommi (ASI Science Data Center\, INAF\, Italy )\nOur knowledge of the extragalactic gamma-ray sky is evolving very rapid ly as new data becomes available.\nI will present recent results on the ga mma-ray emission from extragalactic sources based on the latest Fermi-LAT catalogs (3FGL-3LAC and 2FHL)\, on new large samples of multi-frequency se lected gamma-ray and VHE emitting blazars (1WHSP and 2WHSP)\, and from ext ensive Monte-Carlo simulations of gamma-ray surveys of blazars. Specific p redictions for the present generation of Cherenkov telescopes and for the upcoming CTA will be presented. This will include the number of detectable sources\, their redshift distribution\, and the contribution of blazars t o the extragalactic gamma-ray and VHE background.\n\nhttps://indico.icrr.u -tokyo.ac.jp/event/23/contributions/918/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/918/ 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:20260417T115702Z UID:indico-contribution-23-878@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:MAGIC VHE gamma-ray observations of transient and variable stella r objects DTSTART;VALUE=DATE-TIME:20151029T055000Z DTEND;VALUE=DATE-TIME:20151029T061000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-879@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daniela Hadasch ()\nThere are several types of Galac tic sources that can potentially accelerate charged particles up to GeV an d TeV energies. These accelerated particles can produce Very High Energy ( VHE) gamma-ray emission through different processes\, for example inverse Compton scattering of ambient photon fields by accelerated electrons.\nWe study various transient and variable stellar objects in the VHE regime usi ng observations made with the MAGIC telescopes.\nIn this talk we will pres ent data from four sources: LS I +61 303\, Cygnus X-1\, MWC 656 and SS433. \nThe two binary systems LS I +61º 303 and Cygnus X-1 were observed in long-term monitoring campaigns\, eight and seven years\, respectively.\nFo r LS I +61 303 we will present the latest results of our search for supero rbital variability combined with contemporaneous optical observations.\nTh e microquasar Cygnus X-1\, one of the brightest X-ray sources\, has been w ell studied along a broad range of wavelengths.\nHere we present a search for steady and variable signal using combined X-ray and MAGIC observations .\nMWC 656 is a unique high-mass X-ray binary system as it is the only kno wn binary to be composed of a Be star and a black hole.\nFinally\, we will present our observations of the only super-critical accretion system know n in our galaxy: SS433.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/cont ributions/879/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/879/ END:VEVENT BEGIN:VEVENT SUMMARY:Towards a refined understanding of the Galactic Center excess DTSTART;VALUE=DATE-TIME:20151027T074700Z DTEND;VALUE=DATE-TIME:20151027T080400Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-880@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Mauro Valli (SISSA)\nThere is a striking evidence fo r a roughly spherical-symmetric diffuse gamma-ray signal peaked in the Gal actic Center (GC) region\, extended up to several degrees off the GC. \nHe re we critically review the main points regarding the derivation of this s ignal\, characterized by means of the template-fitting method. In particul ar we focus our attention on the usual Inverse Compton (IC) component adop ted for the background emission\, finding that it does not provide a reali stic description of the complex GC environment. Driven by the evidence of a large gas density in the inner kpc of the Galaxy correlated with an impr essive Supernova rate (2 order of magnitude larger than the Galactic avera ge)\, and therefore with ongoing CR acceleration\, we are able to show tha t no clear evidence of the aforementioned excess comes out when a possibly more realistic diffuse CR source term is taken into account.\n\nhttps://i ndico.icrr.u-tokyo.ac.jp/event/23/contributions/880/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/880/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Neutrino physics DTSTART;VALUE=DATE-TIME:20151026T030000Z DTEND;VALUE=DATE-TIME:20151026T033000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-881@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masato Shiozawa (The University of Tokyo\, Institute for Cosmic Ray Research\, Kamioka Observatory)\nhttps://indico.icrr.u-tok yo.ac.jp/event/23/contributions/881/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/881/ END:VEVENT BEGIN:VEVENT SUMMARY:Opening Address of TeVPA by Dr. Gianfranco Bertone DTSTART;VALUE=DATE-TIME:20151026T004000Z DTEND;VALUE=DATE-TIME:20151026T005000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-882@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Gianfranco Bertone (University of Amsterdam)\nhttps: //indico.icrr.u-tokyo.ac.jp/event/23/contributions/882/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/882/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Theories of VHE emission from pulsar magnetospheres DTSTART;VALUE=DATE-TIME:20151027T020000Z DTEND;VALUE=DATE-TIME:20151027T023000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-883@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kouichi Hirotani (Academia Sinica\, Taiwan)\nThe Cra b pulsar is one of the youngest pulsars in our galaxy. It exhibits the hig hest spin-down luminosity among the galactic neutron stars and has been ob served from radio to VHE. Fermi/LAT reported a detailed phase-resolved spe ctrum in 0.1-10 GeV\, while VERITAS and MAGIC detected pulsed photons in t he double peak and the bridge phases in 25GeV-2TeV. In this talk\, I will solve the particle accelerator in the Crab pulsar’s magnetosphere from t he Poisson equation for the electrostatic potential and the Boltzmann equa tions for electrons\, positrons and photons\, and demonstrate that these m ulti-wavelength observations can be reproduced by this outer-magnetospheri c model from IR to VHE. I will briefly show that exactly the same method c an also be applied to black-hole magnetospheres and that the recent MAGIC detection of the TeV flare from the radio galaxy IC 310 can be reproduced if the supermassive black hole is extremely rotating.\n\nhttps://indico.ic rr.u-tokyo.ac.jp/event/23/contributions/883/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/883/ END:VEVENT BEGIN:VEVENT SUMMARY:Update on scalar singlet dark matter from GAMBIT DTSTART;VALUE=DATE-TIME:20151029T082200Z DTEND;VALUE=DATE-TIME:20151029T083900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-884@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Christoph Weniger (University of Amsterdam)\nThe arg uably most simple model for WIMP dark matter is a scalar singlet that coup les to the Standard Model sector via the Higgs portal. It is a simple exa mple for beyond-the-Standard Model (BSM) physics\, and can be tested with collider\, direct\, indirect and cosmological probes. In this talk\, I wi ll present the first analysis results for the scalar singlet dark matter m odel that we obtained with GAMBIT (Global And Modular BSM Inference Tool). GAMBIT is a new code that provides an extensive and flexible framework f or global scans. Already now\, it integrates accurate likelihood function s for a number of direct detection (like XENON and LUX) and indirect detec tion (like Fermi LAT and IceCube) experiments. It is easily extensible an d allows a seamless integration of popular existing theory codes like Dark SUSY and MicrOmegas. Besides presenting results that we obtain for scalar singlet dark matter and generic WIMP models\, this talk will provide an o verview over the existing and planned dark matter functionality of GAMBIT. \n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/884/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/884/ END:VEVENT BEGIN:VEVENT SUMMARY:Separation of Electron\, Proton and Gamma-ray induced Air Showers with Imaging Atmospheric Cherenkov Telescopes DTSTART;VALUE=DATE-TIME:20151026T091300Z DTEND;VALUE=DATE-TIME:20151026T092800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-885@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Tanya Edwards (Max-Planck-Institut für Kernphysik)\ nGround-based gamma-ray astronomy is still tackling a major problem: backg round. Reconstruction techniques exist to distinguish most of the backgrou nd of hadrons but an irreducible background of electrons and gamma-like pr otons still remain. I present here a new technique making use of direct Ch erenkov light and air shower development that provides a way to efficientl y distinguish between electrons and gamma-rays for the first time. In addi tion to this\, the remaining proton background can also be identified. Thi s analysis increases the sensitivity of Imaging Atmospheric Cherenkov Tele scopes and allows an improved measurement of the cosmic electron spectrum. I also discuss further applications of this approach to the studies on di ffuse emissions\, extended sources and cosmic ray composition.\n\nhttps:// indico.icrr.u-tokyo.ac.jp/event/23/contributions/885/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/885/ END:VEVENT BEGIN:VEVENT SUMMARY:Prospects on the indirect dark matter detection and a future spect roscopic survey of dwarf spheroidal galaxies DTSTART;VALUE=DATE-TIME:20151027T082100Z DTEND;VALUE=DATE-TIME:20151027T083800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-886@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Koji Ichikawa (Kavli IPMU)\nOne of the most promisin g way to detect dark matter is to look for its annihilation or decay produ cts among cosmic-rays. Recently\, more and more interesting results are re ported by measurements of cosmic-rays from various kinds of targets such a s the milky way galaxy\, dwarf spheroidal galaxies\, cluster galaxies\, et c. Among them\, dwarf spheroidal galaxy is one of the nearest\, dark matte r dominated galaxies and therefore one can expect that a large number of d ark matter annihilation/decay signals reach the earth from its halo. In th is presentation\, we will discuss robustness of the gamma-ray search from the dwarf spheroidal galaxies and give prospects of the dark matter halo s urvey by the Prime Focus Spectroscopy (PFS) of SuMIRe project.\n\nhttps:// indico.icrr.u-tokyo.ac.jp/event/23/contributions/886/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/886/ END:VEVENT BEGIN:VEVENT SUMMARY:Low-mass WIMP results and prospects with the EDELWEISS-III experim ent DTSTART;VALUE=DATE-TIME:20151029T051700Z DTEND;VALUE=DATE-TIME:20151029T053400Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-888@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Eric Armengaud (CEA Saclay)\nThe EDELWEISS-III colla boration is operating an experiment for the direct detection of WIMP dark matter in the low radioactivity environment of the Modane Underground Labo ratory. It consists of 36 advanced "FID" germanium detectors operating at 18 mK in a dilution refrigerator in order to identify eventual rare nuclea r recoils induced by elastic scattering of WIMPs from our Galactic halo.\n After a brief discussion on the backgrounds and rejection method with the FID detectors\, a first low-mass WIMP search using data acquired in a long -term campaign will be presented. I will also present the prospects for th ese detectors to explore uncharted parameter space for WIMPs in the GeV - 10 GeV domain.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions /888/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/888/ END:VEVENT BEGIN:VEVENT SUMMARY:Update on GAMBIT DTSTART;VALUE=DATE-TIME:20151029T080500Z DTEND;VALUE=DATE-TIME:20151029T082200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-889@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Pat Scott\, on behalf of the GAMBIT Collaboration (I mperial College London)\nI will give an update on GAMBIT\, the Global And Modular BSM Inference Tool. GAMBIT is a flexible\, modular\, massively pa rallel new framework for carrying out global fits to essentially any BSM t heory. First results from GAMBIT will incorporate direct\, indirect\, sol ar and relic density searches for dark matter\, limits on production of ne w particles from the LHC and LEP\, complete flavour constraints from LHCb\ , LHC Higgs production and decay\, and various electroweak precision obser vables. In many cases\, the likelihoods in GAMBIT are new\, updated or co mputed in significantly more detail than in previous scans. GAMBIT also f eatures interfaces to a range of sampling algorithms\, including different ial evolution and nested sampling\, and the ability to produce both Bayesi an and profile likelihood results.\n\nhttps://indico.icrr.u-tokyo.ac.jp/ev ent/23/contributions/889/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/889/ END:VEVENT BEGIN:VEVENT SUMMARY:Resolving the blazar gamma-ray emission regions with gravitational microlensing DTSTART;VALUE=DATE-TIME:20151026T060000Z DTEND;VALUE=DATE-TIME:20151026T061500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-890@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ievgen Vovk (Max Planck Institute for Physics)\nThe blazars high-energy emission is believed to be produced in the jets\, powe red by their central supermassive black holes. At the same time the locati on of the emission region within the jet is presently uncertain - mainly d ue to its extremely small angular size\, far beyond the capabilities of th e existing gamma-ray instruments. However\, in the rare case of the gravit ationally lensed blazars\, it is possible to use the natural "magnifying l ens" to assist the situation. I will report on the detection of the gravit ational microlensing effect for two gamma-ray loud blazars - PKS 1830-211 and B0218+357\,- which allowed for the first time to resolve their emissio n regions\, providing strong arguments for their connection with the direc t vicinities of the corresponding central black holes.\n\nhttps://indico.i crr.u-tokyo.ac.jp/event/23/contributions/890/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/890/ END:VEVENT BEGIN:VEVENT SUMMARY:A New Method for Determining the Local Dark Matter Density DTSTART;VALUE=DATE-TIME:20151027T051700Z DTEND;VALUE=DATE-TIME:20151027T053400Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-891@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hamish Silverwood (GRAPPA\, University of Amsterdam) \nDetermination of the Dark Matter (DM) density at the solar position is c ritical to direct and indirect dark matter searches. Additionally\, it is important to make this determination with as few assumptions as possible\, as results from direct detection searches are used to explore a wide vari ety of theoretical models\, and hidden astrophysical assumptions could bia s theoretical searches. Here we present a Jeans analysis based method for the determination of the local DM density which allows us to limit the num ber of assumptions we need to make. We fit vertical profiles of baryon and DM density to tracer density and velocity dispersion data via integrated Jeans equations\, and from these derive the local DM density. We present t ests on mock data\, demonstrate the importance of the 'tilt term' which li nks radial and vertical motions\, and also present initial investigations using SDSS and RAVE data.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/co ntributions/891/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/891/ END:VEVENT BEGIN:VEVENT SUMMARY:High performance MeV-GeV gamma-ray astronomy with a time projectio n chamber DTSTART;VALUE=DATE-TIME:20151029T092500Z DTEND;VALUE=DATE-TIME:20151029T094000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-892@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Denis Bernard (LLR\, Ecole Polytechnique & CNRS/IN2P 3.)\ngamma-ray astronomy suffers from the sensitivity gap between the\nene rgy ranges for which Compton telescopes and pair telescopes are\nefficient . \nThis blank part of the SED of the cosmic sources that are active at\nh igh energy hinders the understanding of their nature. In particular\nthe p i0 bump that is dreamt to be signing the hadronic interactions in\nthe cos mic accelerators that produce the highest energy cosmic rays is\nnot easil y observed.\n\nWe will describe the development in progress of a thin gase ous active\ntarget\, a time projection chamber\, as a high performance pai r\ntelescope for gamma-ray astronomy and polarimetry in the MeV - GeV\nene rgy range. \nIn particular the characterization of a prototype in a data-t aking\ncampaign performed recently on the 1.7 - 74 MeV gamma-ray beam at\n LASTI (U. of Hyôgo) will be described.\n\nhttps://indico.icrr.u-tokyo.ac. jp/event/23/contributions/892/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/892/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: HAWC Results DTSTART;VALUE=DATE-TIME:20151029T000000Z DTEND;VALUE=DATE-TIME:20151029T003000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-893@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Andrew Smith (University of Maryland\, College Park) \nThe High Altitude Water Cherenkov Observatory (HAWC) is a new and novel TeV gamma-ray detector that was recently completed and began full operatio n in March 2015. Located on the Sierra Negra volcano\, Puebla\, Mexico\, a t an elevation of 4\,100m\, HAWC is optimized for the detection of gamma r ays in the 0.1 - 100~TeV range. It's 2sr field-of-view and >90% duty cycle make HAWC an ideal instrument for surveying the high-energy sky\, searchi ng for new sources\, studying extended emission from diffuse sources and m onitoring transient and variable sources such as GRBs and AGN. I will desc ribe the HAWC detector and its performance characteristics and report init ial results from the first months of operation.\n\nhttps://indico.icrr.u-t okyo.ac.jp/event/23/contributions/893/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/893/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray production in millisecond pulsar binary systems DTSTART;VALUE=DATE-TIME:20151029T083500Z DTEND;VALUE=DATE-TIME:20151029T085500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-894@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Wlodek Bednarek (University of Lodz)\nWe discuss sce narios which turn to production of gamma-ray emission\nwithin the redback type binary systems containing millisecond pulsar\nand a low mass stellar companion. The millisecond pulsar can eject relativistic leptons from the inner magnetosphere in the rotation powered stage. These leptons\, or afte r additional re-acceleration\, can interact with radiation of companion s tar.\nIn the accretion stage\, the accretion disk penetrates the inner pul sar magnetosphere. Leptons from the inner pulsar magnetosphere can interac t with the disk radiation. We propose that in both stages gamma-rays can b e produced not only in the pulsar mechanism but also in other processes wh ich involve the presence of the companion star.\n\nhttps://indico.icrr.u-t okyo.ac.jp/event/23/contributions/894/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/894/ END:VEVENT BEGIN:VEVENT SUMMARY:Test of Self-interacting dark matter and its thermal transport in the Sun DTSTART;VALUE=DATE-TIME:20151027T062500Z DTEND;VALUE=DATE-TIME:20151027T064200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-895@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Chian-Shu Chen (National Center for Theoretical Scie nces)\nThe halo dark matter (DM) can be gravitationally captured by the Su n. For\nself-interacting DM (SIDM)\, we show that the number of DM trapped inside\nthe Sun remains unsuppressed even if the DM-nucleon cross section is\nnegligible. We consider a SIDM model where *U*(1) gauge symmetry is i ntroduced\nto account for the DM self-interaction. Such a model naturally leads to\nisospin violation for DM-nucleon interaction\, although isospin symmetry is\nstill allowed as a special case. We show that the indirect de tection of\nDM-induced neutrinos from the Sun can probe those SIDM paramet er ranges not\nreachable by direct detections. Those parameter ranges are either the\nregion with a very small *m* or the region opened up due to is ospin\nviolations. The energy flows in and out of the system include the\n gravitational capture via DM-nucleon and DM-DM scatterings\, the energy\nd issipation via DM annihilation\,\nand the heat exchange between DM and sol ar nucleus are studied. The DM\ntemperature can be higher than the core te mperature of the Sun. We further\nexplore its impact on the DM indirect se arch signal.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/8 95/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/895/ END:VEVENT BEGIN:VEVENT SUMMARY:Status and prospects for the Askaryan Radio Array (ARA) cosmogenic neutrino detector DTSTART;VALUE=DATE-TIME:20151026T061500Z DTEND;VALUE=DATE-TIME:20151026T063000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-896@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Michael DuVernois (University of Wisconsin-Madison)\ nThe Askaryan Radio Array (ARA) is an ultra-high energy (>100 PeV) cosmic neutrino detector which is in phased construction near the South Pole. ARA searches for radio Cherenkov-like emission from particle cascades induced by neutrino interactions in the ice using radio frequency antennas (~150- 800MHz) deployed at a design depth of 200m in the Antarctic ice. A prototy pe ARA Testbed station was deployed at ~30m depth in the 2010-2011 season and the first three full ARA stations were deployed in the 2011-2012 and 2 012-2013 seasons. We present the status of the array and plans for the nea r-term construction of a full ARA-37 detector with profound discovery pote ntial for most models of cosmogenic neutrinos from 100 PeV to 100 EeV in e nergy.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/896/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/896/ END:VEVENT BEGIN:VEVENT SUMMARY:Ultra High Energy Cosmic Rays at the Pierre AugerObservatory after 10 years : results and future DTSTART;VALUE=DATE-TIME:20151029T030000Z DTEND;VALUE=DATE-TIME:20151029T033000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-897@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: isabelle Lhenry-Yvon (Institut de Physique Nucléair e d'Orsay\, CNRS/IN2P3)\nThe Pierre Auger Observatory has been designed to investigate the origin and nature of Ultra High Energy Cosmic rays with e nergies from 1017 to 1020 eV. We will review some seletected recent result s obtained from data of the Pierre Auger Observatory and discuss the impli cation of these results for assembling a consistent description of the com position\, origin and propagation of cosmic rays. We will discuss the open questions that will be adressed by the foreseen upgrade of the Observator y.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/897/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/897/ END:VEVENT BEGIN:VEVENT SUMMARY:Implications of simulated Milky Way-like haloes for dark matter di rect detection DTSTART;VALUE=DATE-TIME:20151027T050000Z DTEND;VALUE=DATE-TIME:20151027T051700Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-898@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Nassim Bozorgnia (University of Amsterdam)\nThere is significant astrophysical uncertainty in the interpretation of data from dark matter direct detection experiments\, due to the poorly known dark ma tter distribution at the position of the Sun. I will discuss the local dar k matter density and velocity distribution of Milky Way-like galaxies obta ined from the high-resolution EAGLE hydrodynamical simulations. To make re liable predictions for direct detection searches\, we identify simulated h aloes which satisfy the Milky Way observational constraints. Using the dar k matter distribution obtained for the selected Milky Way-like simulated h aloes\, I will present an analysis of current direct detection data.\n\nht tps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/898/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/898/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray emission from the Galactic center and implications of it s past activities DTSTART;VALUE=DATE-TIME:20151029T075500Z DTEND;VALUE=DATE-TIME:20151029T081500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-899@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yutaka Fujita (Osaka University)\nRadiatively ineffi cient accretion flows (RIAFs) in low-luminosity active galactic nuclei (LL AGNs) have been suggested as cosmic-ray and neutrino sources\, which may l argely contribute to the observed diffuse neutrino intensity. We show that this scenario naturally predicts hadronic multi-TeV gamma-ray excesses ar ound galactic centers. The protons accelerated in the RIAF in Sagittarius A* (Sgr A*) escape and interact with dense molecular gas surrounding Sgr A*\, which is known as the Central Molecular Zone (CMZ)\, and produce gamm a rays as well as neutrinos. Based on a theoretical model that is compatib le with the IceCube data\, we calculate gamma-ray spectra of the CMZ and f ind that the gamma rays with ~\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 23/contributions/899/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/899/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrino Flavor Ratios Modified by Cosmic Ray Secondary-accelerati on DTSTART;VALUE=DATE-TIME:20151029T084000Z DTEND;VALUE=DATE-TIME:20151029T085500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-900@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Norita Kawanaka (The University of Tokyo)\nAccelerat ion of 's and 's modies the flavor ratio at Earth (at astrophysical source s) of\nneutrinos produced by pion decay\, nu_e : nu_mu : nu_tau \, from 1 : 1 : 1 (1 : 2 : 0) to 1 : 1:8 : 1:8 (0 : 1 : 0) at high energy\, because pions decay more than muons during secondary-acceleration. The neutrino s pectrum accompanies a flat excess\, differently from the case of energy lo sses. With the flavor spectra\, we can probe timescales of cosmic-ray acce leration and shock dynamics. We obtain general solutions of convection-dif fusion equations and apply to gamma-ray bursts\, which may have the flavor modication at around PeV - EeV detectable by IceCube and next-generation experiments.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/9 00/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/900/ END:VEVENT BEGIN:VEVENT SUMMARY:A reconstruction scheme for f(T) gravity based on QCD ghost dark e nergy DTSTART;VALUE=DATE-TIME:20151026T060800Z DTEND;VALUE=DATE-TIME:20151026T062500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-901@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Surajit Chattopadhyay (Pailan College of Management and Technology\, Kolkata)\nAccelerated expansion of our universe\, as evid enced by Supernovae Ia (SNeIa)\, Cosmic Microwave Background (CMB) radiati on anisotropies\, Large Scale Structure (LSS) and X-ray experiments\, is w ell documented in literature. A missing energy component\, also known as D ark Energy (DE) with negative pressure\, is widely considered by scientist s as the responsible of this accelerated expansion. DE model\, so-called V eneziano ghost DE (GDE)\, has been proposed in [1]. The key ingredient of this new model is that the Veneziano ghost\, which is unphysical in the us ual Minkowski spacetime quantum field theory (QFT)\, exhibits important ph ysical effects in dynamical spacetime or spacetime with non-trivial topolo gy. Veneziano ghost is supposed to exist for solving the U(1) problem in t he low-energy effective theory of QCD [2]. The present paper reports a rec onstruction scheme for f(T) gravity based on QCD ghost dark energy. Two mo dels of f(T) have been generated and the pressure and density contribution s due to torsion have been reconstructed. Two realistic models have been o btained and the effective equations of state have been studied. Also\, the squared speed of sound has been studied to examine the stability of the m odels.\n\nReferences:\n[1] F.R. Urban\, A.R. Zhitnitsky\, Phys. Lett. B 68 8\, 9 (2010).\n[2] R.-G. Cai\, Z.-L. Tuo\, H.-B. Zhang\, Q. Su\, Phys. Rev . D 84\, 123501 (2011).\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/cont ributions/901/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/901/ END:VEVENT BEGIN:VEVENT SUMMARY:High-Energy Neutrinos from Fast-spinning Newborn Pulsars DTSTART;VALUE=DATE-TIME:20151029T091000Z DTEND;VALUE=DATE-TIME:20151029T092500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-902@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ke Fang (University of Chicago)\nFast-spinning newbo rn pulsars are promising sources of ultrahigh energy cosmic rays (UHECRs). With proper injection abundances\, integrated cosmic rays from the extrag alactic pulsar population can match UHE observation in all aspects - energ y spectrum\, chemical composition\, and anisotropy. High-energy neutrinos would be produced unavoidably\, when accelerated UHECRs travel through the supernova envelope surrounding the pulsar. In this talk\, we will invest igate this neutrino production process\, including the hadronuclear intera ction between cosmic rays and the background\, and possible suppression du e to the pion interaction. We will report the spectrum\, flux and flavor r atio of the high-energy neutrinos from pulsars\, and compare their detect ability to sensitivities of current and future experiments. Finally\, we w ill discuss our model dependence on the source emissivity\, the distribut ion of pulsar population at birth\, as well as the injection composition o f cosmic rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions /902/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/902/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter search from DarkSide DTSTART;VALUE=DATE-TIME:20151029T055100Z DTEND;VALUE=DATE-TIME:20151029T060800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-903@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masayuki Wada (Princeton University)\nDarkSide-50 (D S-50) at Gran Sasso underground laboratory\, Italy\, is a\ndirect dark mat ter search experiment based on a TPC with liquid argon\nfrom underground s ources. The DS-50 TPC\, with 50 kg of active argon\nand a fiducial mass of ~37 kg\, is installed inside an active neutron\nveto based on a boron-loa ded organic scintillator. The neutron veto is\nbuilt inside a water cheren kov muon veto.\nDS-50 has been taking data since Nov 2013\, collecting 47 days livetime\nof data with atmospheric argon. Also\, recently DS-50 commi ssioned\nliquid Ar from underground and measured the level of radioactive 39Ar.\nThe first physics result from DarkSide as well as underground argon \nperformance will be presented. This is the most sensitive dark matter\ns earch preformed with an argon target.\n\nhttps://indico.icrr.u-tokyo.ac.jp /event/23/contributions/903/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/903/ END:VEVENT BEGIN:VEVENT SUMMARY:Radial gradients in cosmic-ray transport: Implications for TeV gam ma and neutrino astronomy. DTSTART;VALUE=DATE-TIME:20151027T082000Z DTEND;VALUE=DATE-TIME:20151027T083500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-904@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daniele Gaggero (SISSA)\nThe Fermi-LAT measurements of the diffuse Galactic gamma-ray emission reveal a hardening of the cosmi c-ray (CR) spectrum with decreasing Galactocentric radius. This result can be the signature of different CR trasport properties in the inner Galaxy \, and in particular a harder rigidity scaling of the diffusion coefficien t.\nWe model this effect with DRAGON and we provide a good description of both Fermi-LAT gamma-ray data in the most relevant sky windows and local c osmic-ray measurements by PAMELA\, AMS-02 and CREAM. \n\nOur model is in remarkably good agreement with the gamma-ray flux measured by MILAGRO at 1 5 TeV from the inner Galactic plane region\, and with H.E.S.S. data from t he Galactic ridge.\n\nOn the neutrino side\, we show that our scenario pro vides an explanation for a significant fraction of the astrophysical flux measured by IceCube above 25 TeV\; moreover\, we discuss how the neutrino telescopes in the Northern hemisphere (ANTARES and the future KM3NeT)\, be tter positioned for the observation of the Galactic Ridge\, will be able t o confirm or constrain our picture.\n\nhttps://indico.icrr.u-tokyo.ac.jp/e vent/23/contributions/904/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/904/ END:VEVENT BEGIN:VEVENT SUMMARY:The electron plus positron spectrum from annihilation of Kaluza-Kl ein dark matter and comparison with recent measurements DTSTART;VALUE=DATE-TIME:20151029T083900Z DTEND;VALUE=DATE-TIME:20151029T085600Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-905@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Satoshi Tsuchida (Ritsumeikan University)\nOne of th e good candidates for cold dark matter is the lightest Kaluza-Klein partic le (LKP)\,which produce electrons and positrons by pair annihilation in th e Galactic halo. The directions of electrons and positrons are randomized by the Galactic magnetic field\, and the energy is reduced by some energy loss mechanisms\, when the charged particles propagate in the Universe.\n We calculate the observed electron and positron spectra expected from the LKP annihilation taking account of propagation effect\, such as brems strahlung. The spectra include the electron-positron component from two-bo dy decays and ``continuum'' emission\, which is produced by LKP annihilati on via muon pair\, tauon pair\, quark pair\, and gauge bosons. We compare the spectra with recent observational data\, and we can set some constrain ts on the boost factor\, which indicates the dark matter concentration in the Galactic halo. In addition\, we will discuss the recent results of pos itron excess in high energy region based on our calculation.\n\nhttps://in dico.icrr.u-tokyo.ac.jp/event/23/contributions/905/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/905/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy Particle Emission and Cumulative Background from Low- Luminosity Active Galactic Nuclei DTSTART;VALUE=DATE-TIME:20151029T085500Z DTEND;VALUE=DATE-TIME:20151029T091000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-906@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shigeo KIMURA (Tohoku University)\nThe origin of hig h-energy neutrinos detected by the IceCube neutrino telescope is a big mys tery of high-energy astrophysics. We propose low-luminosity active galacti c nuclei (LLAGNs) as a novel source of the high-energy neutrinos. The radi ation inefficient accretion flows (RIAFs) are believed to exist in LLAGNs. The Coulomb collisions inside RIAFs is so inefficient that plasmas natura lly have high-energy protons through the stochastic particle acceleration. We calculate spectra of escaping neutrinos and cosmic-ray (CR) protons\, and find that the RIAFs in LLAGNs can accelerate protons up to ~ PeVs and emit TeV–PeV neutrinos via pp and/or pγ reactions. If ~ 1% of the accre tion luminosity is carried away by non-thermal protons\, the diffuse neutr ino intensity from the RIAFs in LLAGN can be compatible with the observed IceCube data (Kimura\, Murase & Toma 2015\, ApJ\, 806\, 159). This result does not contradict either of the diffuse gamma-ray background observed by Fermi or observed diffuse CR flux. This model can be tested by gamma-ray observations around the cores of LLAGNs (e.g.\, Fujita\, Kimura\, Murase 2015\, PRD\, 92\, 023001).\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/c ontributions/906/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/906/ END:VEVENT BEGIN:VEVENT SUMMARY:Testing the Millisecond Pulsar Scenario of the Galactic Center Gam ma-Ray Excess With Very High Energy Gamma-Rays DTSTART;VALUE=DATE-TIME:20151029T081500Z DTEND;VALUE=DATE-TIME:20151029T083500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-907@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kunihito Ioka (KEK)\nRecent analyses of Fermi Large Area Telescope data show an extended GeV γ-ray excess on top of the expec ted diffuse background in the Galactic center region\, which can be explai ned by annihilating dark matter (DM) or a population of millisecond pulsar s (MSPs). We propose observations of very high energy (VHE) γ-rays to dis tinguish the MSP scenario from the DM scenario. GeV γ-ray MSPs should rel ease most of their energy to the relativistic e± wind\, which will diffus e into the Galaxy and radiate TeV γ-rays through inverse Compton scatteri ng and bremsstrahlung processes. By calculating the spectrum and spatial d istribution\, we show that such emission is detectable with the next gener ation VHE γ-ray observatory\, the Cherenkov Telescope Array (CTA)\, under reasonable model parameters. It is essential to search for multi-waveleng th counterparts to the GeV γ-ray excess in order to solve this mystery in the high-energy universe.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/c ontributions/907/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/907/ 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:20260417T115702Z UID:indico-contribution-23-908@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:Prospect for indirect Dark Matter searches with the Cherenkov Tele scope Array DTSTART;VALUE=DATE-TIME:20151027T092900Z DTEND;VALUE=DATE-TIME:20151027T094600Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-910@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Saverio Lombardi (OAR-INAF\, ASDC)\nThe nature of da rk matter (DM) is an open issue of modern physics. Cosmological considerat ions and observational evidences indicate a behaviour beyond the Standard Model for optimal dark matter particle candidates. The non-baryonic dark m atter is compatible with a gas of cold and weakly interacting massive part icles (WIMPs) expected to have a mass in the range between O(10)GeV and O( 100)TeV. Indirect DM searches with imaging atmospheric Cherenkov telescope s (IACTs) may play a crucial role in constraining the nature of the DM par ticle(s) through the study of their annihilation in very high energy (VHE) gamma rays from promising targets\, such as the Galactic Center (GC) and the dwarf spheroidal galaxies (dSphs) of the Milky Way. In this contributi on\, we focus on indirect DM searches prospects for the next-generation ga mma-ray Cherenkov Telescope Array (CTA) observatory.\n\nhttps://indico.icr r.u-tokyo.ac.jp/event/23/contributions/910/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/910/ END:VEVENT BEGIN:VEVENT SUMMARY:Welcome Address by Prof. Takaaki Kajita DTSTART;VALUE=DATE-TIME:20151026T003000Z DTEND;VALUE=DATE-TIME:20151026T004000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-911@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Takaaki Kajita ()\nhttps://indico.icrr.u-tokyo.ac.jp /event/23/contributions/911/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/911/ END:VEVENT BEGIN:VEVENT SUMMARY:Welcome Address and Local Information DTSTART;VALUE=DATE-TIME:20151026T005000Z DTEND;VALUE=DATE-TIME:20151026T010000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-912@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masahiro Teshima ()\nWelcome to TeV Particle Astroph ysics 2015.\nThis is the 10th edition of TeVPA in Kashiwa\, near Tokyo.\nT his 5-day conference aims to provide the stage for the most recent advance s in the booming field of Astroparticle Physics\, bringing leading members of the scientific communities that are contributing to its success.\n\nht tps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/912/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/912/ END:VEVENT BEGIN:VEVENT SUMMARY:The ASTRI mini-array and its scientific prospects in the framework of the Cherenkov Telescope Array DTSTART;VALUE=DATE-TIME:20151026T092800Z DTEND;VALUE=DATE-TIME:20151026T094300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-913@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Saverio Lombardi (OAR-INAF\, ASDC)\nIn the framework of the international Cherenkov Telescope Array (CTA) observatory\, the It alian National Institute for Astrophysics (INAF) has developed a large fie ld-of-view (9.6 degrees)\, dual-mirror\, small-sized\, end-to-end telescop e (ASTRI SST-2M). This prototype has been installed at Mt. Etna (Italy) on September 2014\, and it is currently undergoing engineering tests. Soon a fter the scientific validation of the ASTRI SST-2M prototype\, INAF will b e ready to lead\, in synergy with the Universidade de Sao Paulo (Brazil) a nd the North-West University (South Africa)\, the deployment at the final CTA southern site of the ASTRI mini-array composed of nine ASTRI SST-2M te lescopes that are proposed to be a precursor to CTA. The ASTRI mini-array will overtake the sensitivity of current IACTs above few TeVs up to about 100 TeV\, and will be well suited to perform unprecedented scientific obse rvations of known and predicted bright TeV emitters\, both Galactic and ex tra-Galactic. In addition\, it will also allow us to address problems in f undamental physics such as the particle nature of Dark Matter. In this con tribution\, we review the main ASTRI mini-array scientific prospects.\n\nh ttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/913/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/913/ END:VEVENT BEGIN:VEVENT SUMMARY:X-ray and Gamma-ray Study of Supernova Remnants DTSTART;VALUE=DATE-TIME:20151029T073000Z DTEND;VALUE=DATE-TIME:20151029T075500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-914@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yasunobu Uchiyama (Rikkyo University)\nDiffusive sho ck acceleration (DSA)\, a well-developed theory of the acceleration proces s at work in supernova remnants (SNRs)\, lays the foundation for the SNR p aradigm of the CR origin\, though key problems are yet to be solved. Dete rmining the acceleration efficiency is one of the key issues\, where the t erm “acceleration efficiency” carries two different meanings\; one is related to the maximum attainable energy\, and the other is the energy con tent of CRs. Synchrotron X-ray emission produced by highest energy electro ns with energies of tens of TeV\, and gamma-ray emissions either by relati vistic electrons via IC scattering or by high-energy protons via pion-deca y can provide information about the acceleration efficiencies at SNR shock s. We will report on our recent work on X-ray and GeV gamma-ray observatio ns of some supernova remnants. Also we will discuss prospect for the upcom ing X-ray observatory\, ASTRO-H\, which allows us to perform X-ray spectro scopy of extended objects with unprecedented spectral resolution (7 eV).\n \nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/914/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/914/ END:VEVENT BEGIN:VEVENT SUMMARY:Pulsars and pulsar wind nebulae at high energies DTSTART;VALUE=DATE-TIME:20151027T052500Z DTEND;VALUE=DATE-TIME:20151027T055000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-915@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Roberta ZAnin (MPIK-Heidelberg)\nPulsars and their s ynchrotron nebulae have been extensively observed in the gamma-ray energy band only in the last 10 years. With the advent of the Fermi satellite the number of known gamma-ray emitting pulsars has increased by one order of magnitude\, touching the 150 mark. On the other hand\, the last generation of imaging Cherenkov telescopes proved that the pulsar wind nebulae are t he most populous class of sources radiating in the VHE (>100 GeV) sky.\nTh e now feasible population studies\, together with the available high-preci sion spectral and morphological measurements led to important developments in understanding the physics of the neutron star magnetosphere and their surroundings. In addition a long-term monitor of the gamma-ray sky has rev ealed evidence of flux variability from the Crab nebula and the PSR J2021+ 41 pulsar\, challenging the constant-emission paradigm.\nA couple of more unexpected discoveries moves even forward this ongoing "pulsar revolution" . On the one hand\, a new spectral component emerging above the expected s ynchro-curvature cutoff was observed in two young pulsars\, the Crab and t he Vela pulsars. In the case of the Crab\, this new component reaches the TeV energies\, requesting an extreme particle acceleration up to a 5x10^6 Lorentz factor. On the other hand\, the old and recycled millisecond pulsa rs\, with 10^-4 weaker magnetic fields with respect to the young pulsars\, were established as a new class of gamma-ray emitters.\n\nhttps://indico. icrr.u-tokyo.ac.jp/event/23/contributions/915/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/915/ END:VEVENT BEGIN:VEVENT SUMMARY:Highlights from the H.E.S.S. telescope array: gamma-ray astronomy from 20 GeV to hundreds of TeV's DTSTART;VALUE=DATE-TIME:20151027T063600Z DTEND;VALUE=DATE-TIME:20151027T065900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-916@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Aion Viana (Max-Planck-Institut für Kernphysik (MPI K))\nH.E.S.S. is an array of Imaging Atmospheric Cherenkov Telescopes obse rving the gamma-ray sky beyond ~20 GeV. In the course of the first 10 year s of operation\, this experiment significantly contributed to the field of ground-based gamma-ray astronomy. In 2012\, a fifth telescope was added a t the centre of the original array. This large telescope of 28 meters diam eter improves the performance of the array\, including a lowering of the e nergy threshold down to a few tens of GeV. This new phase of the experimen t provides the first hybrid array of Cherenkov telescopes. In this talk\, I will highlight new results obtained with the newest hybrid array and obs ervations with the fifth\, large telescope\, of Galactic and Extragalactic sources\, such as the Vela pulsar\, the Crab nebula and a handful of impo rtant Active Galactic Nuclei. I will also present striking new findings fr om the accelerator of ultrarelativistic cosmic-rays located in the Galacti c Centre region\, the Large Magellanic Cloud\, new VHE source discoveries from the upcoming H.E.S.S. Galactic Plane Survey\, indirect dark matter se arches\, among other results from the legacy of H.E.S.S. observations.\n\n https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/916/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/916/ 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:20260417T115702Z UID:indico-contribution-23-917@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:Invited Talk: Searching for sharp gamma-ray spectral features from dark matter annihilation DTSTART;VALUE=DATE-TIME:20151030T004500Z DTEND;VALUE=DATE-TIME:20151030T011500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-936@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Alejandro Ibarra (Technische Universität München)\ nThe search for sharp features in the gamma-ray spectrum is a promising ap proach to identify a signal from dark matter annihilation over the astroph ysical backgrounds. In this talk we review different scenarios leading to sharp gamma-ray spectral features and we discuss the current experiments l imits as well as the prospects for detection with future instruments.\n\nh ttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/936/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/936/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Direct Detection at the Ton Scale with the XENON Exper iment DTSTART;VALUE=DATE-TIME:20151029T064200Z DTEND;VALUE=DATE-TIME:20151029T065900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-919@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daniel Coderre (Albert Einstein Center for Fundament al Physics\, University of Bern)\nFor over a decade the XENON Collaboratio n has been a pioneer in the field of dark matter direct detection. The col laboration has achieved world-leading sensitivities in WIMP-nucleon intera ctions using liquid xenon time projection chambers (TPCs)\, first with the XENON10 and later with the XENON100 experiments. This year the next phase \, XENON1T\, will begin data-taking with an unprecedented one ton fiducial (three tons total) volume of ultra pure liquid xenon as both target and d etection medium\, and should reach sensitivities down to 10-47 cm2 after t wo ton years of exposure. The upgrade to the ton scale is only possible du e to a massive research and development program encompassing every aspect of the detector. This program is ongoing and will enable a seamless upgrad e from XENON1T to a true multi-ton detector\, XENONnT\, with the goal of a n order of magnitude increase in sensitivity. XENONnT will reuse the XENON 1T infrastructure but feature a 7 ton active volume. It will be the penult imate iteration leading to the DARWIN experiment\, a 30 ton liquid xenon W IMP detector designed to reach sensitivities down to 10-49 cm2. This talk will discuss the current and future stages of the XENON experiment in the context of the global dark matter search.\n\nhttps://indico.icrr.u-tokyo.a c.jp/event/23/contributions/919/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/919/ END:VEVENT BEGIN:VEVENT SUMMARY:The VERITAS Dark Matter and Astroparticle Program DTSTART;VALUE=DATE-TIME:20151027T091200Z DTEND;VALUE=DATE-TIME:20151027T092900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-920@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ben Zitzer (McGill University)\nVERITAS\, an array o f atmospheric Cherenkov telescopes is sensitive to VHE gamma rays in the 8 5 GeV-30 TeV energy range. VERITAS has a wide scientific reach including o bservations of supernova remnants\, pulsars\, pulsar wind nebulae\, active galactic nuclei\, among others. This presentation will focus on recent de velopments of the various astroparticle science topics by members of the V ERITAS collaboration\, including the search for dark matter (DM). The poss ible astrophysical objects considered to be candidates for indirect DM det ection are dwarf spheroidal galaxies (dSphs) of the Local Group and the Ga lactic Center among others. Results of a combined search for DM of four dS phs will be reported along with a spectrum cosmic-ray electrons\, constrai nts on the inter-galactic magnetic field and other astroparticle physics t opics.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/920/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/920/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Next Steps in Experimental High-energy Neutrino Astr ophysics DTSTART;VALUE=DATE-TIME:20151030T044500Z DTEND;VALUE=DATE-TIME:20151030T051500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-921@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: John Kelley (University of Wisconsin)\nIceCube's dis covery of a diffuse flux of high-energy astrophysical neutrinos has vitali zed the emerging field of neutrino astronomy\, but many questions remain u nanswered. The source populations remain unidentified\, and other expecte d astrophysical high-energy neutrinos\, such as those from the GZK process \, remain undetected. Details of the energy spectrum and flavor compositi on also are yet to be understood. The next generation of neutrino observa tories will shed light on these and other questions. Large-scale ice and w ater arrays will instrument from 10 to 100 square kilometers with optical and/or radio detector elements to detect the Cherenkov and Askaryan radiat ion from neutrino interactions. Other novel approaches include large ball oon-borne detectors\, or searching for tau neutrino conversion in adjacent mountains. I will survey the status and prospects for a number of these experiments and detail how each aims to further the field in the coming ye ars.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/921/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/921/ END:VEVENT BEGIN:VEVENT SUMMARY:Summary & Conclusion DTSTART;VALUE=DATE-TIME:20151030T051500Z DTEND;VALUE=DATE-TIME:20151030T060000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-922@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Alex Kusenko (UCLA Physics & Astronomy)\nhttps://ind ico.icrr.u-tokyo.ac.jp/event/23/contributions/922/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/922/ END:VEVENT BEGIN:VEVENT SUMMARY:Complementarity of direct detection and collider searches for Higg s portal DM DTSTART;VALUE=DATE-TIME:20151026T085600Z DTEND;VALUE=DATE-TIME:20151026T091300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-923@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Pyugwon KO (KIAS)\nIn this talk\, I will describe co mplementarity of direct detection and collider searches for Higgs portal D M models\, and show that it is essential to work in renormalizable and gau ge invariant DM models for collider searches (both the invisible Higgs dec ay and the monojet (or dijet) + missing ET). In particular we derive the b ounds on new physics scale within a UV model\, and show that it is complet ely different from those presented by ATLAS and CMS Collaborations based o n simple mediator models.\n\nRefs: \n(1) arXiv:1405.3530 (Phys.Rev. D90 (2 014) 5\, 055014)\n(2) arXiv:1506.06556\, and works in preparation\n\nhttps ://indico.icrr.u-tokyo.ac.jp/event/23/contributions/923/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/923/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter density profiles in dwarf satellites DTSTART;VALUE=DATE-TIME:20151027T080400Z DTEND;VALUE=DATE-TIME:20151027T082100Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-924@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Piero Ullio (SISSA)\nDwarf spheroidal satellites of the Milky Way are a prime target for dark matter indirect searches. E.g.\, upper limits on gamma-ray fluxes in their directions\, obtained with the Fermi Large Area Telescope\, have been recently used to update constraints on weakly interacting massive particles (WIMPs)\, excluding pair annihila ting cross sections at the level of WIMP thermal relic cross sections for WIMP masses lighter than about 100 GeV. The mapping of a limit on the flux onto a limit on particle dark matter properties stems from the knowledge one has regarding the distribution of dark matter in each dwarf. Such dark matter density profiles are usually derived assuming that dwarfs are equi librium\, pressure-supported\, spherical systems\, and implementing the sp herical Jeans equation to link mass profiles to stellar velocity dispersio ns. This link requires assumptions regarding quantities like the stellar a nisotropy profiles\, which are not measurable and are usually treated as n uisance parameters over which to marginalize. We propose here a novel appr oach to infer the dark matter mass profiles\, based on the analytical inve rsion of the spherical Jeans equation. This methods allows us revisit the so-called mass-anisotropy degeneracy problem\, and more direct assessment s of the uncertainties on line-of-sight integrals of dark matter halo dens ity profiles. Implications for dark matter indirect detection limits are discussed.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/924 / LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/924/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Mapping dark matter in the Milky Way DTSTART;VALUE=DATE-TIME:20151030T014500Z DTEND;VALUE=DATE-TIME:20151030T021500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-925@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Miguel Pato (The Oskar Klein Centre for Cosmoparticl e Physics\, Stockholm University)\nThe presence of dark matter in spiral g alaxies was inferred long ago by measuring the rotational speed of the gas across each galaxy. Applying the same technique to the Milky Way\, a spir al itself\, is much more challenging due to our peculiar position and thus the Galactic distribution of dark matter remains poorly constrained to th is day. In this talk\, I shall introduce two important developments for dy namical studies of the Milky Way. First\, a new compilation of kinematic m easurements is presented and used to pinpoint with unprecedented precision the rotation curve of our Galaxy. Second\, an exhaustive array of observa tion-based baryonic models is constructed to set the contribution of stell ar bulge\, stellar disc and gas to the total gravitational potential. I wi ll then quantify the discrepancy between these two components and derive t he latest constraints on the dark matter distribution. The implications fo r modified Newtonian dynamics are also briefly examined. I shall end with a discussion of future directions to improve our mapping of the dark matte r distribution in the Milky Way.\n\nhttps://indico.icrr.u-tokyo.ac.jp/even t/23/contributions/925/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/925/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent results from the ANTARES deep-sea neutrino telescope DTSTART;VALUE=DATE-TIME:20151029T075000Z DTEND;VALUE=DATE-TIME:20151029T081000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-926@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Rodrigo Gracia Ruiz (APC)\nThe ANTARES detector\, lo cated in the deep Mediterranean sea off the coast of Toulon (France)\, is the first deep-sea neutrino telescope and has been running in its final co nfiguration since 2008. It consists of a 3D array of 885 photomultipliers distributed on 12 lines anchored on the sea bed\, that detect the Cherenko v light induced by upward-going charged leptons produced by neutrino inter actions in and around the detector.\n\nThe primary goal of ANTARES is to s earch for astrophysical neutrinos in the TeV-PeV range. This comprises gen eric searches for any diffuse cosmic neutrino flux as well as more specifi c searches for astrophysical sources such as active galactic nuclei or Gal actic sources. The search program also includes multi-messenger analyses r equiring time and/or space coincidences with other cosmic probes (cosmic r ays\, gamma rays or gravitational waves).\n\nThanks to its location in the Northern hemisphere and its excellent pointing accuracy\, ANTARES is a pr ivileged observer of the central part of our galaxy. This allows it to pu t interesting constraints on the origin of the signal reported by the IceC ube collaboration. The ANTARES sensitivity is also high enough to study a wide-range of other phenomena\, from atmospheric neutrino oscillations to dark matter annihilation or potential exotics such as nuclearites and magn etic monopoles. \n\nThis contribution will present the most recent results obtained by the collaboration in the fields mentioned above.\n\nhttps://i ndico.icrr.u-tokyo.ac.jp/event/23/contributions/926/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/926/ END:VEVENT BEGIN:VEVENT SUMMARY:Observations of the diffuse astrophysical neutrino flux with IceCu be DTSTART;VALUE=DATE-TIME:20151029T073000Z DTEND;VALUE=DATE-TIME:20151029T075000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-928@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Jakob van Santen (DESY Zeuthen)\nIceCube is a cubic- kilometer neutrino observatory buried deep in the ice sheet\nat the geogra phic South Pole. The data from its first few years of operation\nhave reve aled an excess of high-energy neutrino events in multiple detection\nchann els that is incompatible with purely atmospheric origins\, which we\ninter pret as evidence for a flux of neutrinos from unresolved astrophysical\nso urces. At the same time\, no point sources of neutrinos have been detected .\nThis talk will provide an overview of IceCube's constraints on the ener gy\nspectrum and neutrino flavor composition of the diffuse astrophysical neutrino\nflux.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribution s/928/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/928/ END:VEVENT BEGIN:VEVENT SUMMARY:H.E.S.S. multi-messenger and real-time follow-up observations DTSTART;VALUE=DATE-TIME:20151029T065000Z DTEND;VALUE=DATE-TIME:20151029T070500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-929@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Fabian Schüssler (CEA-Saclay / Irfu)\nIn this contr ibution the H.E.S.S. programs to follow up on multi-wavelength and multi-m essenger observations and alerts will be presented.\nOngoing activities se arching for high-energy gamma-ray emission in coincidence with Gamma Ray B ursts\, recent extensions to Fast Radio Bursts and (in the future) gravita tional waves are going to be discussed. Furthermore the newly installed H. E.S.S. multi-messenger program will be introduced\, showing for example fi rst results on the combination of high-energy neutrinos and high-energy ga mma rays and discussing possible future extensions.\n\nhttps://indico.icrr .u-tokyo.ac.jp/event/23/contributions/929/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/929/ END:VEVENT BEGIN:VEVENT SUMMARY:Modelling the flux distribution function of the extragalactic gamm a-ray background from dark matter annihilation DTSTART;VALUE=DATE-TIME:20151027T085500Z DTEND;VALUE=DATE-TIME:20151027T091200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-930@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Michael Feyereisen (University of Amsterdam)\nThe on e-point function (i.e.\, the isotropic flux distribution) is a complementa ry method to (anisotropic) two-point correlations in searches for a gamma- ray dark matter annihilation signature. Using analytical models of structu re formation and dark matter halo properties\, we compute the gamma-ray fl ux distribution due to annihilations in extragalactic dark matter halos\, as it would be observed by the Fermi Large Area Telescope. Combining the c entral limit theorem and Monte Carlo sampling\, we show that the flux dist ribution takes the form of a narrow Gaussian of ‘diffuse’ light\, with an ‘unresolved point source’ power-law tail as a result of bright hal os. We argue that this background due to dark matter constitutes an irredu cible and significant background component for point-source annihilation s earches with galaxy clusters and dwarf spheroidal galaxies\, modifying the predicted signal-to-noise ratio. A study of astrophysical backgrounds to this signal reveals that the shape of the total gamma-ray flux distributio n is very sensitive to the contribution of a dark matter component\, allow ing us to forecast promising one-point upper limits on the annihilation cr oss section. We show that by using the flux distribution at only one energ y bin\, one can probe the canonical cross section required for explaining the relic density\, for dark matter of masses around tens of GeV.\n\nhttps ://indico.icrr.u-tokyo.ac.jp/event/23/contributions/930/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/930/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Indirect DM searches DTSTART;VALUE=DATE-TIME:20151029T003000Z DTEND;VALUE=DATE-TIME:20151029T010000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-931@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Keith Bechtol (University of Wisconsin-Madison)\nMan y dark matter (DM) models predict that DM in a broad range of astrophysica l settings could annihilate or decay into Standard Model particles at rate s that would be detectable by contemporary telescopes and cosmic-ray exper iments. I will review the status of indirect DM searches with a special fo cus on recent experimental and theoretical developments. I will also consi der future observations that might resolve some of the current anomalies\, and generally increase the reach of indirect DM searches.\n\nhttps://indi co.icrr.u-tokyo.ac.jp/event/23/contributions/931/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/931/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Future direct search for various types of dark matte r DTSTART;VALUE=DATE-TIME:20151029T020000Z DTEND;VALUE=DATE-TIME:20151029T023000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-932@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shigetaka Moriyama (ICRR)\nModern cosmology requires dark matter (DM) to explain the structure of the visible universe. The na ture of DM is totally unknown. One attractive candidate put forward by the ory is a weakly interacting massive particle (WIMP)\, which could be a the rmal relic of the Big Bang. The supersymmetric extension of the standard m odel provides one of the major candidates for DM. With this consideration\ , worldwide experimental efforts to detect WIMPs have been made and future large-scale projects are currently planned. However\, no positive evidenc e of supersymmetric particles was observed in the large hadron collider ex periments so far. This strengthens the interest in investigating a broad r ange of DM candidate. In this talk\, future projects to search for standar d WIMPs and experimental approaches to study various types of dark matter candidates are discussed.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/co ntributions/932/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/932/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Status of Direct dark Matter Search DTSTART;VALUE=DATE-TIME:20151029T010000Z DTEND;VALUE=DATE-TIME:20151029T013000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-933@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Bruno Serfass (University of California Berkeley)\nh ttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/933/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/933/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Gravitational wave status of searches DTSTART;VALUE=DATE-TIME:20151030T001500Z DTEND;VALUE=DATE-TIME:20151030T004500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-934@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Samaya Nissanke (Radboud University\, Nijmegen)\nhtt ps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/934/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/934/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Particle physics beyond Higgs DTSTART;VALUE=DATE-TIME:20151029T234500Z DTEND;VALUE=DATE-TIME:20151030T001500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-935@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hitoshi Murayama (Institute for the Physics and Math ematics of the Universe\, University of Tokyo)\nhttps://indico.icrr.u-toky o.ac.jp/event/23/contributions/935/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/935/ END:VEVENT BEGIN:VEVENT SUMMARY:The impact of the Calorimeter-only photons in the Fermi-LAT analys is of VHE sources DTSTART;VALUE=DATE-TIME:20151029T094000Z DTEND;VALUE=DATE-TIME:20151029T095500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-937@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Mitsunari Takahashi (ICRR)\nAbove tens of GeV\, gamm a-ray observations with the Fermi Large Area Telescope (LAT) are often dom inated by statistical uncertainties due to the low source flux and the lim ited acceptance. The newly released Pass 8 analysis extended the acceptanc e of Fermi-LAT to ~ 2.5 m^2 sr over 100 GeV\, and made effective an event class that can improve the acceptance at these very high gamma-ray energie s: the “Calorimeter-only (CalOnly)” event class. While the conventiona l event classes require information from the LAT tracker\, the CalOnly eve nt class\, which is still under development\, can recover ~40-50% of event s above 50 GeV without usable tracker information\, at the expense of a wo rse angular resolution and larger cosmic-ray background. In the conference we will describe the working principle\, and report on the performance of this new event class using Monte Carlo simulations and real data from ast rophysical VHE sources from the recently-released catalog of LAT sources a bove 50 GeV (2FHL).\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribu tions/937/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/937/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Results from the Telescope Array experiment\, Hot sp ots and anisotropy DTSTART;VALUE=DATE-TIME:20151029T023000Z DTEND;VALUE=DATE-TIME:20151029T030000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-938@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Toshiyuki Nonaka (Institute for Cosmic Ray Reseach U niversity of Tokyo)\nThe Telescope Array (TA) experiment is located in the western desert of Utah\, USA\, and observes ultra high energy cosmic rays in the northern hemisphere. The experiment observes cosmic ray air shower at energies > 1 EeV using the fluorescence telescopes and the surface det ectors. From first 5 year data\, an anisotropy called "Hot spot" in arriva l direction of cosmic ray was found at energy >57EeV. In this talk\, we pr esent updated result of the "Hot spot" and discuss together with studies on cosmic ray spectrum\, chemical composition and other anisotropy studies at highest energy region.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/c ontributions/938/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/938/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic VHE gamma-ray astrophysics with H.E.S.S. DTSTART;VALUE=DATE-TIME:20151029T050000Z DTEND;VALUE=DATE-TIME:20151029T052000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-939@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ryan Chaves (CNRS Montpellier)\nH.E.S.S. is a hybrid array of five imaging atmospheric Cherenkov telescopes operating in the v ery-high-energy (VHE) gamma-ray energy range ~20 GeV to 100 TeV. With its unprecedented sensitivity\, broad energy range\, fast slew time\, and Sout hern-hemisphere location in Namibia\, H.E.S.S. provides an unparalleled\, high-quality view of the VHE Galaxy\, in a multi-messenger approach that b uilds on agreements with many collaborations\, including in particular Fer mi-LAT\, IceCube\, ANTARES and VIRGO/LIGO. H.E.S.S. has conducted deep obs ervations of several key Galactic regions of utmost importance for underst anding the mechanisms at work accelerating cosmic rays and producing VHE g amma rays. Among them are the Galactic Center and Ridge\, the Crab Nebula\ , the energetic Vela pulsar\, and several binary systems such as PSR B1259 -63 and LS 5039. To capitalize on these observations\, recent years have s een a tremendous effort in the design\, implementation\, and optimization of analysis techniques for both monoscopic and stereoscopic events\, as we ll as standardized analysis pipelines for processing large datasets like t hat of the Galactic Plane Survey. The comprehensive Survey is the culminat ion of a decade-long\, ~2800-hr observation program and is the first high- resolution (~0.1 deg) and sensitive (~2% Crab Nebula point-source sensitiv ity) survey of the Milky Way in TeV gamma rays. A public release of this l egacy H.E.S.S. data\, including a source catalog and source population stu dies\, is also on schedule for 2015 and will be presented. This presentati on will highlight the newest hybrid data and observations utilizing the fi fth\, large telescope\, as well as spectacular new findings from the Large Magellanic Cloud\, the powerful particle accelerator situated in the inne r region of the Galactic Center\, high-precision measurements of the iconi c supernova remnant RX J1713.7-3946\, and a handful of brand-new VHE sourc e discoveries from the Survey.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 23/contributions/939/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/939/ END:VEVENT BEGIN:VEVENT SUMMARY:Prospects for dark matter discovery with inelastic transitions of xenon DTSTART;VALUE=DATE-TIME:20151027T055100Z DTEND;VALUE=DATE-TIME:20151027T060800Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-940@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Christopher McCabe (University of Amsterdam)\nDark m atter can excite the xenon isotopes 129Xe and 131Xe through a spin depende nt interaction. The excited isotopes quickly decay giving a 40 keV and 80 keV photon\, respectively. This signal is very distinct from the usual sig nal from elastically scattering dark matter and\, if discovered\, would pr ovide clear evidence against the usual spin independent interaction. I dis cuss the prospects of discovering this inelastic signal with up-coming ton ne-scale two-phase xenon direct detection experiments.\n\nhttps://indico.i crr.u-tokyo.ac.jp/event/23/contributions/940/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/940/ END:VEVENT BEGIN:VEVENT SUMMARY:Natural model for the Fermi bubbles and Galactic haze DTSTART;VALUE=DATE-TIME:20151027T090500Z DTEND;VALUE=DATE-TIME:20151027T092000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-941@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ilya Gurwich (NRCN &\; Weizmann Institute)\nWe sh ow that the Fermi Bubbles and the Galactic haze are naturally interpreted as inverse-Compton and synchrotron emission from the same spectrum of cool ing cosmic ray electrons. This avoids the ad-hoc spectral features and sup erfluous acceleration mechanisms typically assumed. The model implies that the bubbles originated 2-3 Myr ago\, the mean magnetic field in the haze region is ~3\\muG\, and the radiation field in the bubble is dominated by starlight with mean energy density >2eV/cm^3. These parameters imply that the bubbles accelerate cosmic ray protons (iron nuclei) up to energies of ~5·10^{17}eV (~10^{19}eV).\n\nIn contrast\, a hadronic model fails to nat urally account for the gamma-ray spectrum of the bubbles\, in particular o nce the haze-emitting electrons are taken into account.\n\nhttps://indico. icrr.u-tokyo.ac.jp/event/23/contributions/941/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/941/ END:VEVENT BEGIN:VEVENT SUMMARY:Particle acceleration observed in gamma-rays DTSTART;VALUE=DATE-TIME:20151027T073000Z DTEND;VALUE=DATE-TIME:20151027T075500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-942@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Rolf Buehler (DESY\,)\nGamma-rays give us a view on the acceleration some of the most energetic particles in the universe. The se particles are usually thought to be accelerated in (relativistic) shock s. However\, with the advances in Particle In Cell simulations over the pa st years it became clear that magnetic reconnection is also a compelling a lternative. In this talk\, I will discuss what gamma-ray observations can tell us about these two options. I will discuss this question for differen t gamma-ray source classes\, as Supernova Remnants\, Jets of Active Galact ic Nuclei and Pulsar Wind Nebulae.\n\nhttps://indico.icrr.u-tokyo.ac.jp/ev ent/23/contributions/942/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/942/ END:VEVENT BEGIN:VEVENT SUMMARY:New physics searches at the LHC: Where do we go with run II DTSTART;VALUE=DATE-TIME:20151026T073000Z DTEND;VALUE=DATE-TIME:20151026T080500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-943@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Osamu Jinnouchi (TokyoTech)\nTwo LHC experiments\, A TLAS and CMS restarted their operations so called\nRun-2 from June this ye ar. The center of mass energy is increased to 13 TeV\,\nwith which the sig nificant enhancement in sensitivity is anticipated for\nthe new physics. T he talk will briefly review the Run-1 results and will discuss\nthe prospe cts for the Run-2. The status and the early results from the Run-2\nwill b e also shown.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/ 943/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/943/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark matter search using fiducial volume analysis in XMASS experim ent DTSTART;VALUE=DATE-TIME:20151029T060800Z DTEND;VALUE=DATE-TIME:20151029T062500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-946@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hiroshi Ogawa (ICRR\, The Univ. of Tokyo)\nAn 800kg liquid xenon detector (XMASS) was constructed at Kamioka Observatory\, Jap an in 2010. XMASS can be made the low background region in center of dete ctor by shield of the liquid xenon which eliminates the background in dete ctor surface. A commissioning run was conducted from November 2010 to Ju ne 2012. We found the unexpected background in detector surface. In order to reduce these backgrounds on detector surface and increase the sensitivi ty for Dark Mater search\, refurbishment of the detector was completed and physics data taking was resumed since Nov 2013. In this presentation\, th e result of dark matter search using fiducial volume analysis is reported. Also expected background events should be evaluated.\n\nhttps://indico.ic rr.u-tokyo.ac.jp/event/23/contributions/946/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/946/ END:VEVENT BEGIN:VEVENT SUMMARY:Star-Jet Interactions and Gamma-Ray Flares DTSTART;VALUE=DATE-TIME:20151026T082800Z DTEND;VALUE=DATE-TIME:20151026T084300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-947@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Maxim Barkov (ABBL RIKEN)\nWe propose a model to exp lain the ultra-bright GeV gamma-ray flares observed from the blazar 3C454. 3. The model is based on the concept of a relativistic jet interacting wit h compact gas condensations produced when a star (red giant) crosses the j et close to the central black hole. The study includes an analytical treat ment of the evolution of the envelop lost by the star within the jet\, and calculations of the related high-energy radiation. \nThe model readily ex plains the day-long\, variable on timescales of hours\, GeV gamma-ray flar e from 3C454.3\, observed during November 2010 on top of a weeks-long plat eau. In the proposed scenario\, the plateau state is caused by a strong wi nd generated by the heating of the star atmosphere by nonthermal particles accelerated at the jet-star interaction region. The flare itself could be produced by a few clouds of matter lost by the red giant after the initia l impact of the jet. In the framework of the proposed scenario\, the obser vations constrain the key model parameters of the source\, including the m ass of the central black hole: M_BH≃10^9M⊙\, the total jet power: L_j ≃10^48 erg s−1\, and the Doppler factor of the gamma-ray emitting clou ds\, δ≃20. Whereas we do not specify the particle acceleration mechanis ms\, the potential gamma-ray production processes are discussed and compar ed in the context of the proposed model. We argue that synchrotron radiati on of protons has certain advantages compared to other radiation channels of directly accelerated electrons.\n\nhttps://indico.icrr.u-tokyo.ac.jp/ev ent/23/contributions/947/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/947/ END:VEVENT BEGIN:VEVENT SUMMARY:The Extragalactic Radio Background from Dark Matter Annihilation a nd the ARCADE-2 Excess DTSTART;VALUE=DATE-TIME:20151027T064200Z DTEND;VALUE=DATE-TIME:20151027T065900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-948@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ke Fang (University of Chicago)\nObservations of the ARCADE-2 and other telescopes have reported a significant isotropic emiss ion spanning from 22 MHz to 10 GHz. The intensity of this signal significa ntly exceeds the expected contribution from known astrophysical sources\, and the distribution of the signal is suggested to be unusually smooth com pared to emission which traces large scale structure. In this talk\, we in vestigate the extragalactic radio background from dark matter annihilation and its possible connection to the ARCADE-2 excess signal. We show that w ith assumptions of strong magnetic fields and extended substructure in mas sive clusters\, dark matter models can explain both intensity and spectrum of the ARCADE-2 excess\, while produce small anisotropies that remain con sistent with observational constraints. We also demonstrate that the above constraints could be significantly relaxed in an alternative scenario whe re electrons from the annihilation could be re-accelerated by turbulence i n the intra-cluster medium.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/ contributions/948/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/948/ END:VEVENT BEGIN:VEVENT SUMMARY:Scalar dark matter with colored partner DTSTART;VALUE=DATE-TIME:20151026T080500Z DTEND;VALUE=DATE-TIME:20151026T082200Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-949@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Laura Lopez Honorez (Vrije Universiteit Brussel)\nIn my talk I will review the case of scalar dark matter model in which case the dark matter candidate couples to the Standard Model (SM) fermions thro ugh Yukawa interactions involving a new vector-like fermion. The latter mo dels are already know to give rise to particularly interesting gamma ray s ignals when the Yukawa coupling is restricted to leptons. In my talk\, I w ill present our latest results associated to a similar Yukawa interactions to SM quarks including constraints and prospects for Direct detection\, c olliders\, and indirect dark matter searches.\n\nhttps://indico.icrr.u-tok yo.ac.jp/event/23/contributions/949/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/949/ END:VEVENT BEGIN:VEVENT SUMMARY:MAGIC observations of the February 2014 flare of 1ES 1011+496 appl ied to the measurement of the Extragalactic Background Light density DTSTART;VALUE=DATE-TIME:20151026T075500Z DTEND;VALUE=DATE-TIME:20151026T081300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-950@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Abelardo Moralejo Olaizola (Institut de Físca d'Alt es Energies\, Barcelona)\n1ES 1011+496 is a blazar located at a redshift z =0.212\, revealed as a very-high-energy gamma-ray emitter by the MAGIC tel escopes in 2007. In February 2014 the source underwent an unprecedented fl aring episode\, reaching a peak flux of almost 14 times the flux measured at the time of discovery\, before returning to its low state. The MAGIC te lescopes observed the source for a total of 17 nights between February 6 a nd March 7\, during which the source displayed a remarkably stable spectra l shape (estimated intrinsic photon index around 2) and significant flux v ariations in timescales of 1 day. The average spectrum during the flare co uld be well measured up to a few TeV\, which makes this an ideal observati on for probing the Extragalactic Background Light (EBL) through its effect on the gamma-ray flux. A maximum likelihood method was applied for the si multaneous estimation of the source intrinsic spectral parameters and of t he optical depth due to the EBL\, using the EBL model by Domínguez et al (2011) as a template to account for the EBL spectrum and evolution. The re sulting measurement of the EBL density is among the most constraining ones obtained with gamma-ray telescopes on a single source\, and is compatible with current EBL models\, strengthening the case for no significant contr ibution of unresolved sources to the EBL.\n\nhttps://indico.icrr.u-tokyo.a c.jp/event/23/contributions/950/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/950/ END:VEVENT BEGIN:VEVENT SUMMARY:A measurement of the diffuse astrophysical muon neutrino flux usin g six years of IceCube data DTSTART;VALUE=DATE-TIME:20151029T082500Z DTEND;VALUE=DATE-TIME:20151029T084000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-951@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sebastian Schoenen (RWTH Aachen\, 3. Physikalisches Institut B)\nThe IceCube Collaboration has observed a high-energy astrophy sical neutrino flux using neutrino candidates with interaction vertices co ntained within the instrumented volume. A complementary measurement can be done with charged current muon neutrinos where the interaction vertex can be outside the instrumented volume. Due to the large muon range the effec tive area is significantly larger but the field of view is limited to the northern hemisphere. IceCube data from 2009 through 2015 have been analyze d by a likelihood approach with reconstructed muon energy and zenith angle as observables. The analyzed data consist of about 340\,000 muon neutrino candidates with a negligible contribution of atmospheric muons. While the majority of these events are atmospheric neutrinos\, the highest energy e vents are incompatible with that interpretation. In this talk we will pres ent the observation of an astrophysical muon neutrino flux and the measure ment of its properties.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/cont ributions/951/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/951/ END:VEVENT BEGIN:VEVENT SUMMARY:The PandaX Dark Matter Experiment DTSTART;VALUE=DATE-TIME:20151029T053400Z DTEND;VALUE=DATE-TIME:20151029T055100Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-952@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Xun Chen (Shanghai Jiao Tong University)\nPandaX is a dark matter direct detection experiment with xenon located in the China Jinping Laboratory. The collaboration was established in 2009. It's first stage\, PandaX-I\, started to take data in May\, 2014 and stopped running in the end of Oct\, 2014. Its first dark matter searching results based on 17.4 live days of data was released in Aug 2014\,and disfavor all previou sly claimed possible dark matter signals by other experiments. The final d ata analysis results of PandaX-I based on 80.1 live days of data were rele ased in this May with many updates in analysis methods\, and verified Pand aX-I first results.The second stage\, PandaX-II\, is being tested and will start operation in this year. The detector will contain 500kg of xenon an d we hope it will set the most stringent limit for dark matter after one y ear of running.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribution s/952/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/952/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Direct measurements of cosmic-rays in GeV-TeV DTSTART;VALUE=DATE-TIME:20151026T020000Z DTEND;VALUE=DATE-TIME:20151026T023000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-953@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sadakazu Haino (Institute of Physics\, Acadmia Sinic a\, Taiwan)\nEnergy spectra of cosmic-rays in GeV-TeV region have been dir ectly measured by balloons and in space. Particularly cosmic-ray antiparti cles can provide unique opportunity to study fundamental physics such as i ndirect searches for Dark Matter and understanding of its nature. More tha n four years after AMS (Alpha Magnetic Spectrometer) start taking data on the ISS (International Space Station)\, the precision has been decreasing to % level.\nIn my talk brief history of direct measurements is summarized and the latest AMS results and their physics implications are discussed.\ n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/953/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/953/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: The Galactic Gamma-ray sky DTSTART;VALUE=DATE-TIME:20151027T003000Z DTEND;VALUE=DATE-TIME:20151027T010000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-954@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Olaf Reimer (University of Innsbruck\, Austria)\nhtt ps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/954/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/954/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited Talk: Extragalactic Sources of Very High Energy Gamma-Ray Emission: Highlights from Imaging Atmospheric Cherenkov Telescopes DTSTART;VALUE=DATE-TIME:20151027T030000Z DTEND;VALUE=DATE-TIME:20151027T033000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-955@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daniel Mazin (ICRR)\nThe very high energy gamma-ray astrophysics with Imaging Atmospheric Cherenkov Telescopes is blooming tha nks to the excellent performance of the experiments H.E.S.S.\, MAGIC and V ERITAS. Large fraction of the scientific program of these experiments is d evoted to observation of active galactic nuclei (such as blazars and radio galaxies) and follow-ups of gamma-ray burst alerts. In this talk I will h ighlight the progress of the field in the recent years revealing new and e xciting phenomena studying of which answered some of long standing questio ns but also opened many new ones.\n\nhttps://indico.icrr.u-tokyo.ac.jp/eve nt/23/contributions/955/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/955/ 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:20260417T115702Z UID:indico-contribution-23-956@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:TeV Gamma rays with ICAL-INO DTSTART;VALUE=DATE-TIME:20151026T064500Z DTEND;VALUE=DATE-TIME:20151026T070000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-957@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: REETANJALI MOHARANA (University of Johannesburg)\nTh e feasibility of the detection of TeV gamma-rays from astrophysical object s has been carried out using the INO-ICAL detector. The detection of very high energy gamma-rays has been followed by the detection of down going m uons produced through the electromagnetic showers initiated by gamma-ray in the atmosphere. As the produced muons through this process are of same charge ratio\, they might be result in the enhancement of mu+ to mu- rati o at very high energy ( above 100 GeV). The ICAL detector is proposed to b e a magnetised calorimeter with an average magnetic field of nearly 1.3 T. So the signature of gamma-rays could be addressed very easily through thi s technique.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/9 57/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/957/ END:VEVENT BEGIN:VEVENT SUMMARY:2FHL The second Catalog of Hard Fermi-LAT Sources DTSTART;VALUE=DATE-TIME:20151026T073000Z DTEND;VALUE=DATE-TIME:20151026T075500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-958@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Alberto Dominguez (Clemson University/UC Madrid)\nTh e Fermi Large Area Telescope (LAT) has been routinely gathering science da ta since August 2008\, surveying the full sky every three hours. The first Fermi-LAT catalog of sources detected above 10 GeV (1FHL) relied on three years of data to characterize the >10 GeV sky. The improved acceptance an d point-spread function of the new Pass 8 event reconstruction and classif ication together with six years of observations now available allow the de tection and characterization of sources directly above 50 GeV. This closes the gap between ground-based Cherenkov telescopes\, which have excellent sensitivity but small fields of view and duty cycles\, and all-sky observa tions at GeV energies from orbit. In this contribution\, we will present the second catalog of hard Fermi-LAT sources detected at >50 GeV. We will discuss the properties of the extragalactic and Galactic source population s with an emphasis on the detection of spatially extended sources in the p lane of our Galaxy.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribu tions/958/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/958/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube Cosmic Neutrino events from Star-forming galaxies. DTSTART;VALUE=DATE-TIME:20151029T081000Z DTEND;VALUE=DATE-TIME:20151029T082500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-959@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: REETANJALI MOHARANA (University of Johannesburg)\nSo urces of the 53 high energy neutrino events detected by IceCube with energ y between 20 TeV and 2.7 PeV is one of the outstanding puzzles in recent y ears. Suggestions range from Galactic to extragalactic sources\, and from standard model interactions to dark matter decay or annihilation. We perfo rm a statistical analysis of the distribution of these neutrino events and astrophysical sources. Our results suggest correlation between the IceCub e neutrino events and star forming galaxies with at least 3-sigma signific ance. We also perform a multi-messenger study of gamma rays and neutrinos from these sources and constrain star formation rate and environment param eters based observations.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/co ntributions/959/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/959/ END:VEVENT BEGIN:VEVENT SUMMARY:The CR-WIMP connection in the Galaxy DTSTART;VALUE=DATE-TIME:20151029T073000Z DTEND;VALUE=DATE-TIME:20151029T080500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-960@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Carmelo Evoli (GSSI\, L'Aquila)\nWhether or not an e xotic component\, as the fugitive Dark Matter\, contributes to the observe d high-energy CR fluxes\, is one of the most important open problem in Cos mology. Charged CRs play a key role in this context\, since Weakly Interac ting Massive Particle annihilations or decays can be a copious source of a ntimatter in our Galaxy\, and the local CR fluxes from conventional astrop hysical sources can be predicted with fair accuracy. \nIn this talk\, I wi ll show the implications of adopting realistic models for the propagation of CRs in the Galaxy and in the Heliosphere on our ability to provide accu rate background predictions. In particular\, I will focus on the antiproto n channel since the recent measurements by AMS-02 can be profitably used t o search for DM contributions or to constrain the DM annihilation cross se ction in the Galactic halo. Remarkably\, this channel has been recently u sed to argue the DM interpretation of the gamma-ray excess observed from t he Galactic Center.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribu tions/960/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/960/ END:VEVENT BEGIN:VEVENT SUMMARY:Propagation of CR in the Galaxy with the DRAGON code DTSTART;VALUE=DATE-TIME:20151027T075500Z DTEND;VALUE=DATE-TIME:20151027T082000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-961@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Carmelo Evoli (GSSI\, L'Aquila)\nDRAGON is a public software package developed to study CR propagation in the Galaxy.\nIt incl udes diffusive/advective transport\, as well as reacceleration and energy losses\, for most of the nuclear and lepton species. Each species can orig inate from astrophysical sources (e.g.\, SNR\, Pulsars) or from DM annihil ations/decays in the halo\, making the code very suitable both for studyin g Galactic high-energy processes and for DM indirect searches.\nFrom the b eginning\, our goal was to design a inhomogeneous model able to properly t ake into account the different galactic environments. Our model provides a ccurate calculation of CR fluxes both locally\, where they can be directly probed\, and at galactic scale\, where they predominantly contribute to g amma and synchrotron diffuse emissions. \nRemarkably\, this approach alrea dy provided noteworthy improvements in our understanding of FERMI and WMAP signals. \nIn this talk\, we present a new update of the DRAGON code whi ch includes several new features incorporated to describe spatially depend ent and anisotropic diffusion.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 23/contributions/961/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/961/ 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:20260417T115702Z UID:indico-contribution-23-962@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:Asymmetric dark matter and an antineutrino signal DTSTART;VALUE=DATE-TIME:20151026T051700Z DTEND;VALUE=DATE-TIME:20151026T053400Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-963@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hajime Fukuda (Kavli IPMU)\nUnder rather generic ass umptions\, we show that in the asymmetric dark matter (ADM) scenario\, the sign of the B-L asymmetry stored in the dark matter sector and the standa rd model sector are always the same. One particularly striking consequence of this result is that\, when the dark matter decays or annihilates in th e present universe\, the resulting final state always involves an anti-neu trino. As a concrete example of this\, we construct a composite ADM model and explore the feasibility of detecting such an anti-neutrino signal in a tmospheric neutrino detectors.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 23/contributions/963/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/963/ END:VEVENT BEGIN:VEVENT SUMMARY:The landscape of flavor composition of high-energy astrophysical n eutrinos DTSTART;VALUE=DATE-TIME:20151026T052000Z DTEND;VALUE=DATE-TIME:20151026T054000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-964@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Mauricio Bustamante (Center for Cosmology and Astrop article Physics\, The Ohio State University)\nIceCube has confirmed the ex istence of the long-sought high-energy astrophysical neutrinos. Recently\, the flavor composition of the diffuse flux\, that is\, the proportion of electron-\, muon-\, and tau-flavor in it\, was measured for the first time . This rich observable can reveal information about physical conditions in the production\, propagation\, and detection of neutrinos\, including whe ther there is new physics involved. We present theoretical expectations fo r the flavor composition at Earth by exploring all possible flavor composi tions that leave the astrophysical sources. We explicitly show that the re gion of accessible flavor composition at Earth is surprisingly small\, reg ardless of the neutrino mass hierarchy and of the experimental uncertainty on the mixing parameters. This remains true even in the presence of a bro ad class of new physics effects during propagation. Furthermore\, we are a ble to clearly identify what regions of the flavor space can be accessed o nly by new physics\, and of what type. In particular\, in the case of neut rino decay under a normal mass hierarchy\, we demonstrate the usefulness o f the flavor composition by using the present IceCube results to improve t he bounds on neutrino lifetimes by several orders of magnitude. The planne d volume upgrade\, IceCube-Gen2\, would be able to strengthen these claims .\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/964/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/964/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy emission from Gamma-Ray Bursts DTSTART;VALUE=DATE-TIME:20151027T050000Z DTEND;VALUE=DATE-TIME:20151027T052500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-965@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Valerie Connaughton (USRA)\nOur understanding of hig h-energy emission from Gamma-Ray Bursts has greatly advanced with observat ions from the Fermi gamma-ray space telescope. I will review the Fermi ob servations\, with particular emphasis on the surprising detection of both prompt and temporally extended emission at high energies. I will also dis cuss the prospects for detection of GRBs with the High Altitude Water Cher enkov (HAWC) and Cherenkov Telescope Array (CTA) experiments.\n\nhttps://i ndico.icrr.u-tokyo.ac.jp/event/23/contributions/965/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/965/ 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:20260417T115702Z UID:indico-contribution-23-966@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:Stochastic Particle Acceleration and Photon Emission in Blazars DTSTART;VALUE=DATE-TIME:20151026T064500Z DTEND;VALUE=DATE-TIME:20151026T070000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-967@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Katsuaki Asano ()\nMulti-wavelength observations of blazars have revealed curved feature in photon spectrum. Moreover\, in som e cases\, the required electron spectral index at injection becomes harder than 2. In order to reproduce such a curved electron spectrum\, we discus s the second order Fermi acceleration by turbulence in the jet. Here\, we focus on the time-dependent effects of the electron acceleration and injec tion. We numerically follow the temporal evolution of the electron spectru m in the jet. We show that the resultant photon spectra well agree with th e various observed spectra of 1ES 1101\, Mrk 421\, and 3C 279. Especially\ , the light curve and spectrum of the recent intensive flare in 3C 279 are both reproduced by our simple model. Therefore\, this stochastic accelera tion model can be a reasonable explanation for the electron acceleration i n blazars.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/967 / LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/967/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for Singlet Majorana dark matter. DTSTART;VALUE=DATE-TIME:20151026T082200Z DTEND;VALUE=DATE-TIME:20151026T083900Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-968@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: YUE-LIN SMING TSAI (Kavli IPMU)\nWe are searching th e Singlet Majorana dark matter (DM) by using constraints from relic densit y\, colliders (LHC and LEP)\, DM direct detection\, and DM indirect detect ion. By the means of effective field theory (EFT)\, we write down several kinds of higher dimensional operators and show the allowed parameter space by current experiments in DM mass and cut-off scale plane. Furthermore\, we also try to explore the parameter space where EFT is invalid. We propos e a method to fix this problem by connecting the EFT with several simplifi ed models\, which allows us to make a robust prediction on DM collider sig nals.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/968/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/968/ END:VEVENT BEGIN:VEVENT SUMMARY:Extending Fermi-LAT discoveries: Compton-Pair Production Space Tel escope (ComPair) for MeV Gamma-ray Astronomy DTSTART;VALUE=DATE-TIME:20151029T091000Z DTEND;VALUE=DATE-TIME:20151029T092500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-969@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Jeremy Perkins (NASA/GSFC)\nThe gamma-ray energy ran ge from a few hundred keV to a few hundred MeV has remained largely unexpl ored\, mainly due to the challenging nature of the measurements\, since th e pioneering but limited observations by COMPTEL on the Compton Gamma-Ray Observatory (1991-2000). This energy regime encompasses the transition bet ween thermal and nonthermal processes\, and accurate measurements are crit ical for answering a broad range of astrophysical questions. We are develo ping a concept for a discovery mission\, ComPair (Compton-Pair Production Space Telescope)\, to investigate energies from 200 keV to > 500 MeV with high energy and angular resolution and with sensitivity approaching a fact or of 100 better than COMPTEL. This instrument will be capable of detectin g both Compton-scattering events at lower energy and pair-production event s at higher energy. ComPair will build on the heritage of successful space missions including Fermi\, AGILE\, AMS and PAMELA\, and will use well-dev eloped space-qualified detector technologies including Si-strip and CdZnTe -strip detectors\, heavy inorganic scintillators\, and plastic scintillato rs.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/969/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/969/ END:VEVENT BEGIN:VEVENT SUMMARY:Enhanced sensitivity to astrophysical neutrinos with a surface vet o array above IceCube DTSTART;VALUE=DATE-TIME:20151026T060000Z DTEND;VALUE=DATE-TIME:20151026T061500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-970@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Delia Tosi (University of Wisconsin - Madison and WI PAC)\nThe IceCube neutrino observatory features a kilometer-cubed deep det ector and a surface component\, IceTop\, instrumenting the square-kilomete r footprint of the detector. IceTop consists of ice-filled tanks equipped with optical sensors capable of detecting charged particles produced in ai r showers. Besides measuring the cosmic-ray spectrum and composition\, Ice Top can be used as a veto for IceCube. With the discovery of an astrophysi cal flux at high energy\, this role is becoming more important as a pathwa y to the design of a larger surface array. Since the earth is not transpar ent to very-high-energy neutrinos\, searching for a signal from the southe rn hemisphere is a priority. This search\, however\, requires suppressing a large background consisting of penetrating atmospheric muons and neutri nos. A surface array\, such as IceTop\, can reduce the background by ident ifying particles which are generated in the same air shower as the muons i n the deep detector. I will present the capabilities and limitations of I ceTop as a veto for cosmic rays as well as the status of simulations of va rious designs for an upgraded surface array.\n\nhttps://indico.icrr.u-toky o.ac.jp/event/23/contributions/970/ LOCATION: Room 3.4 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/970/ 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:20260417T115702Z UID:indico-contribution-23-971@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 BEGIN:VEVENT SUMMARY:Multimessenger test of hadronic model for Fermi bubbles DTSTART;VALUE=DATE-TIME:20151027T083500Z DTEND;VALUE=DATE-TIME:20151027T085000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-972@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Soebur Razzaque (University of Johannesburg)\nThe Fe rmi bubbles at the Galactic center have been imaged in sub-TeV gamma rays by the Fermi-Large Area Telescope and might have been detected in 0.3-1 Pe V neutrinos by the IceCube Neutrino Observatory. A hadronic model\, involv ing cosmic-ray interactions in the bubble volumes\, can account for both g amma-ray and neutrino observations but is far from being confirmed due to low neutrino statistics. We present a possibility to test the hadronic mod el using 0.1-100 TeV gamma-ray observations by the High Altitude Water Che renkov (HAWC) detector which has recently started its operation. HAWC will either substantiate hadronic model\, establishing Fermi bubbles as the fi rst mulimessenger source\, or will severely constrain hadronic origin of s ub-TeV gamma rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contribut ions/972/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/972/ END:VEVENT BEGIN:VEVENT SUMMARY:The very high energy gamma-ray diffuse emission in the Galactic Ce nter region as seen by H.E.S.S DTSTART;VALUE=DATE-TIME:20151027T092000Z DTEND;VALUE=DATE-TIME:20151027T093500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-973@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Anne Lemière (APC\, CNRS/Université Paris7\, Paris France)\nThe Very High Energy (VHE) emission from the Galactic Center Rid ge was revealed by H.E.S.S. in 2006\, after subtraction of the two bright point sources HESS J1745-290 possibly associated with Sgr A*\, and HESS J1 747-281 associated with the composite supernova remnant G0.9+0.1. The hard spectrum of the Ridge emission and its spatial correlation with the local gas density suggest that the emission is due to collisions of multi-TeV c osmic rays with the dense clouds of interstellar gas present in this regio n. The much larger H.E.S.S. dataset (250 hrs) that is now available from t his region and the improved analysis method dedicated to the detection of faint emission allow us to reconsider the characterization of this gamma-r ay emission through a detailed morphology study and the extraction of the total energy spectrum with much better accuracy. To test the various contr ibutions to the total gamma-ray emission\, we use a 2D maximum likelihood approach that allows to constrain a phenomenological model of the signal. We discuss the nature of the various components\, their implication on the cosmic-ray distribution in the central region of our Galaxy\, and their p ossible connection with HESS J1747-281. Finally\, we reveal an additional source in this region and discuss its potential nature.\n\nhttps://indico. icrr.u-tokyo.ac.jp/event/23/contributions/973/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/973/ END:VEVENT BEGIN:VEVENT SUMMARY:Broadband Emission of Magnetar Wind Nebulae DTSTART;VALUE=DATE-TIME:20151029T063000Z DTEND;VALUE=DATE-TIME:20151029T065000Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-974@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shuta Tanaka (ICRR\, The University of Tokyo)\nRotat ion-powered pulsars release their rotational energy as relativistic magnet ized plasma and create pulsar wind nebulae (PWNe) around them.\nAlthough m agnetars are considered as magnetically powered pulsar\, they also release their rotational energy by the wind.\nThis is obvious from the fact that they are spinning down.\nWe have been detected PWNe around energetic pulsa rs which have spin-down power of more than 10^36 erg/s\, typically.\nIn th is study\, we consider the wind nebula around magnetars (MWN).\nAlthough t hey have relatively small spin-down power\, magnetars would have had a lar ge spin-down power at their birth because they spin down rapidly.\nHere\, we construct an one-zone spectral model of MWN considering spin-down evolu tion of magnetar and apply to some objects which are claimed to have MWN i n X-rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributions/974/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/974/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Sensitivity of CALET DTSTART;VALUE=DATE-TIME:20151027T060800Z DTEND;VALUE=DATE-TIME:20151027T062500Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-975@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Holger Motz (ICSEP Waseda University)\nCALET (Calori metric Electron Telescope)\, launched to the ISS in August\, directly meas ures the electron+positron cosmic rays flux up to 20 TeV.\nWith its proton rejection capability of 1 : 10^5 and an aperture of 1200 cm^2 sr\, it wil l provide good statistics even well above one TeV\, while also featuring a n energy resolution of 2%\, which allows it to detect fine structures in t he spectrum. Such structures may originate from Dark Matter annihilation o r decay\, making indirect Dark Matter search one of CALET's main science o bjectives among others\, such as identification of signatures from nearby supernova remnants by observation of TeV electrons\, and measurement of th e heavy nuclei spectra to study the cosmic ray acceleration and diffusion mechanism.\nThe positron excess in cosmic rays above 10 GeV was initially proposed by the AMS-02 collaboration to originate from an extra power law source with exponential cut-off\, which emits an equal amount of electrons and positrons. The latest results from AMS-02 on positron fraction and to tal electron+positron flux can be fitted with a parametrization including such an extra power law source\, which in general may represent nearby ast rophysical accelerators or annihilation/decay of Dark Matter. Assuming tha t the source is a single pulsar\, this scenario is extrapolated into the T eV-region and the expected CALET data for this case simulated. Based on th is prediction and taking the shape of the Dark Matter annihilation spectru m into account\, the sensitivity of CALET to an additional component from Dark Matter annihilation in the galactic halo has been calculated.\nIt is shown that CALET could significantly improve these limits compared to curr ent data\, especially for those Dark Matter candidates that feature a larg e fraction of annihilation directly into electron+positron\, such as the L KP (Lightest Kaluza-Klein particle).\nThe alternative case of Dark Matter annihilation or decay being the primary cause of the positron excess and t he prospects of CALET detecting the corresponding Dark Matter signature ar e discussed as well.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contrib utions/975/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/975/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for Event Rate Modulation in XENON100 Electronic Recoil Dat a DTSTART;VALUE=DATE-TIME:20151029T050000Z DTEND;VALUE=DATE-TIME:20151029T051700Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-976@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Fei Gao (Shanghai Jiao Tong University)\nXENON100 is currently one of the world leading dark matter direct detection experimen ts using a dual phase Xenon time projection chamber (TPC). The XENON100 ex periment has accumulated more than one year of dark matter search data sin ce February 2011 at a background level of 5.3 events/(keV*tonne*day). This data allows to test the interpretation of the long standing DAMA/LIBRA an nual modulation observations for certain dark matter models producing elec tronic recoils. In this talk\, we present the new analysis results searchi ng for event rate modulations in the XENON100 electronic recoil data. We d emonstrate for the first time that long term stability of dual phase Xenon TPC is sufficient to enable searches for modulation signals in the low en ergy region. We finally present the search results from un-binned profile likelihood analysis and make comparison with the DAMA/LIBRA annual modula tion observation.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/23/contributi ons/976/ LOCATION: Room 2 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/976/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent highlights of the MAGIC telescopes DTSTART;VALUE=DATE-TIME:20151027T055000Z DTEND;VALUE=DATE-TIME:20151027T061300Z DTSTAMP;VALUE=DATE-TIME:20260417T115702Z UID:indico-contribution-23-977@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Julian Sitarek (University of Lodz)\nMAGIC (Major At mospheric Gamma Imaging Cherenkov) is a\nsystem of two imaging atmospheric Cherenkov telescopes located at the\nCanary island of La Palma. The teles copes are performing observations\nof gamma rays with energies between 50 GeV and tens of TeV. In 2014\nMAGIC celebrated its 10th anniversary of sci entific operations. In\nthis talk I will present the recent highlights of the observations\nperformed with the MAGIC telescopes. I will discuss the ultra-fast\nvariability of IC 310\, challenging jet emission models in AGN s.\nI will present the detection of the VHE gamma-ray emission from\ntwo a ctive galaxies located at redshift of ~0.94: gravitationally\nlensed blaza r B0218+357 and FSRQ PKS 1441+25. Finally\, I will also\npresent the newes t measurements of the VHE emission from Crab pulsar.\n\nhttps://indico.icr r.u-tokyo.ac.jp/event/23/contributions/977/ LOCATION: Room 5.6 URL:https://indico.icrr.u-tokyo.ac.jp/event/23/contributions/977/ END:VEVENT END:VCALENDAR