Welcome

• Rolf Heuer (CERN)

Room: 500/1-001 - Main Auditorium

Introduction to the AMS Experiment

• Samuel Ting (Massachusetts Inst. of Technology (US))

Room: 500/1-001 - Main Auditorium Following the pioneering experiments (ATIC, BESS, CREAM, HEAT, PAMELA, …), using a magnetic spectrometer (AMS) on ISS is a unique way to provide precision long term measurements of primordial high energy charged cosmic rays. AMS was installed on the Station in May 2011. Up to now, 60 billion events have been collected. 40 billion events have been partially analysed. AMS is scheduled to be on the Station until at least 2024. By then AMS will have collected close to 200 billion events. The detector properties and the analysis methods will be introduced.

Latest AMS Results: The Positron Fraction and the p-bar/p Ratio

• Andrei KOUNINE (MIT)

Room: 500/1-001 - Main Auditorium A precision measurement by AMS of the positron fraction in primary cosmic rays is presented. The results show that at 275±32 GeV the positron fraction no longer increases with energy. The current status of the anti-proton analysis is also presented.

The e− Spectrum and e+ Spectrum from AMS

• Stefan SCHAEL (RWTH-Aachen)

Room: 500/1-001 - Main Auditorium Precision measurements by AMS on the ISS of the primary cosmic-ray electron flux in the range 0.5 to 700 GeV and the positron flux in the range 0.5 to 500 GeV are presented. The electron flux and the positron flux each require a description beyond a single power-law spectrum. Both the electron flux and the positron flux change their behavior at ∼30 GeV but the fluxes are significantly different in their magnitude and energy dependence. Between 20 and 200 GeV the positron spectral index is significantly harder than the electron spectral index.

New Physics, Dark Matter and the LHC

• Fabio ZWIRNER (University of Padova and CERN)

Room: 500/1-001 - Main Auditorium

Complementarity of Indirect Dark Matter Detection

• Jonathan L. FENG (University of California, Irvine)

Room: 500/1-001 - Main Auditorium

Cosmic Rays in the Milky Way and Other Galaxies

• Igor MOSKALENKO (Stanford University)

Room: 500/1-001 - Main Auditorium

It's About Time: Interpreting AMS Antimatter Data in Terms of Cosmic Ray Propagation

• Kfir BLUM (Institute for Advanced Study, Princeton)

Room: 500/1-001 - Main Auditorium If cosmic ray positrons come from a secondary origin, then their production spectrum is correlated with the production spectrum of other secondary particles such as boron and antiprotons through scattering cross sections measured in the laboratory. This allows to define a first-principle upper bound on the positron flux at the Earth, independent of propagation model assumptions. Using currently available B/C and antiproton/proton data, we show that the positron flux reported by AMS is consistent with the bound and saturates it at high energies. This coincidence is a compelling indication for a secondary source. We explain how improved AMS measurements of the high energy boron, antiproton, and secondary radioactive nuclei fluxes can corroborate or falsify the secondary source hypothesis. Assuming that the positrons are secondary, we show that AMS data imply a propagation time in the Galaxy of order 1Myr or less for cosmic rays with magnetic rigidity > 300 GV. This corresponds to an average traversed interstellar matter density of ∼ 1 particle/cc, comparable to the density of the Milky Way gaseous disk.

Acceleration and Transport of Galactic Cosmic Rays

• Vladimir PTUSKIN (IZMIRAN, Moscow)

Room: 500/1-001 - Main Auditorium

Public Lecture: Human Space Exploration

• William H. GERSTENMAIER (NASA)

Room: 500/1-001 - Main Auditorium Public Lecture in English only. Should you wish to attend to this lecture only (and not the full colloquium), please register here: https://indico.cern.ch/event/386996/registration/ Participants to the full colloquium are automatically registered to the public lectures.

The (e− plus e+) Spectrum from AMS

• Bruna BERTUCCI (INFN and University of Perugia)

Room: 500/1-001 - Main Auditorium We present a measurement of the cosmic ray e+ + e− flux in the range 0.5 GeV to 1 TeV based on the analysis of 10.6 million (e+ + e−) events. The statistics and the resolution of AMS provide a precision measurement of the flux. The flux is smooth and reveals new and distinct information.

The Proton Spectrum from AMS

• Vitaly CHOUTKO (MIT)

Room: 500/1-001 - Main Auditorium A precise measurement of the proton flux in primary cosmic rays with rigidity 1GV to 1.8TV is presented. At rigidities above 50 GV the flux requires a description beyond a single power law.

The Helium Spectrum from AMS

• Sadakazu HAINO (Academia Sinica, Taiwan)

Room: 500/1-001 - Main Auditorium

Indirect Detection: Enhanced Density Models and Antideuteron Searches

• Lisa RANDALL (Harvard University)

Room: 500/1-001 - Main Auditorium

Background to Dark Matter Searches from Galactic Cosmic Rays

• Subir SARKAR (Oxford, Niels Bohr Institute)

Room: 500/1-001 - Main Auditorium Just as searches for BSM physics at the LHC necessitate a careful audit of SM backgrounds, the search for signals of dark matter in cosmic rays must contend with production of secondaries like e+ and pbar through cosmic ray propagation in the Galaxy. The theoretical framework for calculating this has however not been directly calibrated at the high energies being explored by AMS-02 and there may be surprises in store. In particular a nearby source where cosmic rays are being accelerated stochastically can naturally generate a e+ fraction rising with energy as is observed. The test of this is the expected correlated rise in other secondary/primary ratios e.g. B/C and pbar/p. Such a nearby cosmic accelerator should also be detectable through the concomitant flux of neutrinos and its discovery would be (nearly!) as exciting as that of dark matter.

The JEM-EUSO Program

• Piergiorgio PICOZZA (University of Rome Tor Vergata)

Room: 500/1-001 - Main Auditorium JEM-EUSO on board the International Space Station is a mission that aims at unveiling the nature and the origin of the ultra high energy cosmic rays (UHECRs), and to address basic problems of fundamental physics at extreme energies.  The instrument is designed to measure the arrival direction, the energy and, possibly, the nature of these particles. It basically consists of a wide-field of view telescope that looks down from the International Space Station during night-time to detect UV photons  emitted from air showers generated by UHECRs in the atmosphere, in order to identify their individual sources and their association with known nearby astronomical objects. An infrared camera and an atmosphere monitoring system improve the performance of the instrument. The program is proceeding in different steps. At present, K-EUSO attached at the Russian module of the ISS, an improvement of KLYPVE experiment already approved by Roscosmos, is in the stage of final definition. Two pathfinders have already been developed, the first, EUSO-Balloon flew on board a stratospheric balloon in August 2014, a second, EUSO-TA on ground, is in operation at the Telescope Array site. A third, Mini-EUSO, approved by Roscosmos, will be installed inside the ISS. More short and long duration balloon flights are envisaged. 17 Countries, and about 300 researchers are collaborating in JEM-EUSO.

Latest Results from Ice Cube

• Francis HALZEN (University of Wisconsin-Madison)

Room: 500/1-001 - Main Auditorium

Latest Results from the Pierre Auger Observatory and Future Prospects in Particle Physics and High Energy Astrophysics with Cosmic Rays

• Alan A. WATSON (University of Leeds)

Room: 500/1-001 - Main Auditorium

Latest Results from Fermi-LAT

• Peter MICHELSON (Stanford University)

Room: 500/1-001 - Main Auditorium

Public Lecture: The Odyssey of Voyager

• Edward C. STONE (CALTECH)

Room: 500/1-001 - Main Auditorium Public Lecture in English only. Should you wish to attend to this lecture only (and not the full colloquium), please register here: https://indico.cern.ch/event/387001/registration/ Participants to the full colloquium are automatically registered to the public lectures.

Scrutinizing Possible Dark Matter Signatures with AMS, Fermi and Planck

• Tracy SLATYER (MIT)

Room: 500/1-001 - Main Auditorium

Super-Symmetric Dark Matter

• Jonathan R. ELLIS (CERN and King's College, London)

Room: 500/1-001 - Main Auditorium

AMS Results on Light Nuclei -B/C

• Alberto OLIVA (CIEMAT)

Room: 500/1-001 - Main Auditorium

AMS Results on Light Nuclei - Li

• Laurent M. DEROME (LPSC Grenoble)

Room: 500/1-001 - Main Auditorium

AMS Results on Light Nuclei - C/He

• Melanie HEIL (MIT)

Room: 500/1-001 - Main Auditorium

Implications of AMS-02 Experiment

• Yue-Liang WU (University of Chinese Academy of Sciences)

Room: 500/1-001 - Main Auditorium

The Highest Energy Cosmic Particles

• Angela OLINTO (University of Chicago)

Room: 500/1-001 - Main Auditorium

Recent Results on Ultra-High Energy Cosmic Rays from the Telescope Array

• Masaki FUKUSHIMA (University of Tokyo)

Room: 500/1-001 - Main Auditorium TA's recent results on Ultra-High Energy Cosmic Rays (UHECRs) are reported. The energy spectrum based on 20k events above 10^18.2 eV demonstrates a clear dip at 10^18.7 eV and a cutoff at 10^19.7 eV , the shape and the energies of which are well described by the GZK process: energy loss of extra-galactic protons by the interaction with the CMB and IR background. The primary composition obtained from the shower maximum analysis using the hybrid technique is consistent with 100% proton or light nuclei, and inconsistent with 100% iron up to 10^19.3 eV. Above the GZK cutoff energy, a large flux enhancement of medium size (radius=20deg) is observed in the direction of Ursa-Major. The chance probability of this hotspot appearing from the isotropic flux is 4.0sigma. The center of the hotspot is 19 deg off from the Super-Galactic Plane, and no obvious candidate of UHECRs is known in this direction.

Cosmic Ray Energetics and Mass: From Balloons to the ISS

• Eun-Suk SEO (University of Maryland)

Room: 500/1-001 - Main Auditorium

Latest Results from HESS and the Progress of CTA

• Werner HOFMANN (Max-Planck Institut Heidelberg)

Room: 500/1-001 - Main Auditorium

Are there currently well motivated and phenomenologically allowed dark matter candidates (besides axions)

• Gordon KANE (University of Michigan)

Room: 500/1-001 - Main Auditorium

The Cosmic Fronter at DOE

• Michael SALAMON (Department of Energy)

Room: 500/1-001 - Main Auditorium

What Next in Fundamental and Particle Physics in Space ?

• Roberto BATTISTON (ASI - Italian Space Agency and Univ. Trento)

Room: 500/1-001 - Main Auditorium

Summary

• Samuel TING (CERN and MIT)

Room: 500/1-001 - Main Auditorium