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Cosmic Rays in the Multi-Messenger Era

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APC Laboratory (Paris)

APC Laboratory

Paris

Amphithéâtre Pierre-Gilles de Gennes (floor -1), 10 rue Alice Domon et Leonid Duquet, 75013 Paris
Description

The 'Cosmic Rays  in the Multi-Messenger Era' conference aims to bring together the scientific communities working on high-energy cosmic rays, from an experimental point of view as well as from a theoretical and phenomenological sides. In addition to detailed presentations of theoretical models dealing with the production of cosmic rays and secondary neutrinos and gamma-rays, the conference will include reviews of the latest experimental results as well as prospects for the next decade.

The workshop will be divided into two parts: the first part focusing on neutrinos will be organized from November 29th to December 2nd, 2022 in Louvain-la-Neuve, Belgium:  https://agenda.irmp.ucl.ac.be/event/4681/

The second part focusing on cosmic rays will be organized the week after, from December 5th to December 7th.  2022, in Paris, France.  Each session will end with general discussion of presented results. Additionally we organize poster session for PhD students and young researchers.

Organizing Committee:

Organizing committee: 

G. de Wasseige, co-chair
S. Gabici
M. Kachelriess, co-chair 
A.Kouchner

A. Neronov
D. Semikoz, chair
S.Vydelingum, secretary

Participants
  • Alexander Korochkin
  • Anatoly Spitkovsky
  • Andrii Neronov
  • Björn Eichmann
  • Bruno Khélifi
  • Carmelo Evoli
  • Dmitri Semikoz
  • Enrico Peretti
  • Felix Aharonian
  • Fiorenza Donato
  • Foteini Oikonomou
  • Francesco Villante
  • Grigory Rubtsov
  • Gwenael Giacinti
  • Gwenhaël de Wasseige
  • Ievgen Vovk
  • Igor Tkachev
  • Indira Vergara-Quispe
  • Jean-Marco Alameddine
  • Joaquín de Jesús
  • John Matthews
  • Juan Carlos Díaz Vélez
  • Juan Manuel González
  • Klaus Dolag
  • Konstantin Dolgikh
  • Mathieu Lamoureux
  • Michael Kachelriess
  • Michael Unger
  • Niccolo' Bucciantini
  • Ottavio Fornieri
  • Paolo Zuccon
  • Pascal Gutjahr
  • Pasquale Blasi
  • Qiang Yuan
  • Ralph Engel
  • Rogerio de Almeida
  • rosine lallement
  • Sergey Koldobskiy
  • Sergey Ostapchenko
  • Shoushan Zhang
  • Stefano Gabici
  • Théophile Cartraud
  • Vincent Tatischeff
  • +6
  • lundi 5 décembre
    • 08:00 → 09:00
      registration
    • 09:00 → 09:10
      Wellcome
      Président de session: Dmitri Semikoz (APC, Paris)
    • 09:10 → 10:40
      Summary of neutrino workshop
    • 10:40 → 11:00
      Coffee 20m
    • 11:00 → 13:00
      Cosmic rays at knee
    • 13:00 → 14:30
      Lunch 1h 30m
    • 14:30 → 16:30
      Low energy cosmic rays
      • 14:30
        Results from AMS-02 30m
        Orateur: Paolo Zuccon (Università degli Studi di Trento and TIFPA)
        PZ_CRMME22.pdf
      • 15:00
        Interpretation of the antinuclei data 30m
        Orateur: Michael Kachelriess (Department of Physics, NTNU)
        kachelriess.pdf
      • 15:30
        Making sense of recent results on electrons and positrons from cosmic ray experiments 30m
        Orateur: Carmelo Evoli (n Gran Sasso Science Institute)
        Evoli_Paris2022.pdf
        slides
    • 16:30 → 17:00
      coffee 30m
    • 17:00 → 18:30
      Low energy cosmic rays
      • 17:00
        Secondary particles in the Galaxy, the role of cross sections 30m
        Orateur: Fiorenza Donato (Dept. Theoretical Physics)
        Donato.pdf
      • 17:30
        Cosmic Ray abundances 30m
        Orateur: Vincent Tatischeff (CSNSM)
        VTatischeff_GCR_Composition_2022.pdf
      • 18:00
        Discussion: low energy cosmic rays 30m
    • 18:30 → 20:00
      Wine and cheese 1h 30m
  • mardi 6 décembre
    • 09:00 → 10:30
      UHECR
    • 10:30 → 11:00
      coffee 30m
    • 11:00 → 12:35
      UHECR
      • 11:05
        Ultra-high energy cosmic rays from a population of source 30m
        Orateur: Foteni Oikonomou (Norwegian University of Science and Technology)
        paris-oikonomou.pdf
      • 11:35
        Radio Galaxies as UHECR sources 30m
        Orateur: Björn Eichmann
        Eichmann_Paris2022.pdf
      • 12:05
        Discussion: UHECR 30m
    • 12:35 → 14:00
      Lunch 1h 25m
    • 14:00 → 15:30
      UHECR
    • 15:30 → 16:00
      Coffee 30m
    • 16:00 → 18:00
      Poster session
      • 16:05
        Ideas to measure the prompt component of the atmospheric muon flux 12m

        Extensive air showers arise due to particles coming from the Universe interacting with the atmosphere. In these high-energetic interactions, many particles of different types
        are produced.
        Since muons have a long lifetime and thus a long range compared to other particles in the air shower, they are abundant even on the Earth's surface. These muons are detected with air shower detectors and also underground muon experiments.
        The resulting muon flux is divided into a conventional and a prompt component. The prompt muons come from parent particles with a very short lifetime, causing the spectrum of the prompt
        component nearly to follow the primary spectrum. Particles with lifetimes larger than picoseconds such as pions and kaons live long enough to interact with the atmosphere which results in energy losses. Muons
        from decays of these particles are called conventional and follow a softer energy spectrum.

        Ideas to measure the prompt muon flux using the IceCube Neutrino Observatory are presented based on previous analyses. New CORSIKA simulations will be performed in the future and re-weighting should be used to
        create several datasets with different scalings of the prompt component. At the end, an unfolding as well as a fit of the normalization will be performed.

      • 16:20
        Observation of Cosmic-Ray Anisotropy with Eleven Years of IceCube Data 12m

        The complete IceCube Observatory has collected over 690 billion cosmic-ray induced muon events from May 2011 to May 2022. These unprecedented statistics make it possible to observe significant structure in in the distribution of cosmic-ray arrival directions at both higher cosmic-ray energies and smaller angular scales. Combined with improved simulation and systematics, we can provide a newly detailed assessment of the energy- and time-dependence of the cosmic-ray anisotropy in the Southern Hemisphere. We present the preliminary results from a study with the extended event
        sample.

        CR Anisotropy MultiMessenger 2022.pdf
      • 16:32
        Anisotropies studies in the arrival directions of Ultrahigh-Energy Cosmic Rays 12m

        The study of ultrahigh-energy cosmic rays contributes to a better understanding of the Universe. In particular, the study of anisotropy in their arrival directions is of key importance to unraveling the sources of such particles. The Pierre Auger Observatory, the largest cosmic ray observatory in the world, collected an unprecedentedly large
        data set over 17 years of operation. In this work, we describe anisotropy-related results obtained by using such events. These are the large-scale searches in the arrival direction of events detected with energies above 4 EeV and the analysis of arrival directions of the highest-energy events, exceeding 32 EeV. A remarkable dipolar modulation in right ascension for energies above 8 EeV is observed, as previously reported, with a statistical significance of 6.6$\sigma$ as well as evidence of anisotropy at intermediate angular scale with $\sim15^{ \circ}$ Gaussian spread at 4$\sigma$ significance level for cosmic-ray energies above $\sim$ 40 EeV.

      • 16:44
        Magnetic diffusion and interaction effects on Ultrahigh Energy Cosmic Rays 12m

        Magnetic fields present in the Universe and interactions with the cosmic radiation backgrounds play an important role in shaping the flux of the ultrahigh energy cosmic rays reaching the Earth. To account for these processes we include in the SimProp cosmic ray propagation code the effect of a turbulent magnetic field through a stochastic deflection term in the trajectories. We compute the suppression of the spectrum due to the magnetic horizon effect, both for primary nuclei and for the (secondary) nuclei resulting from the photodisintegration of the primary ones. We provide analytic parameterizations of this effect as a function of the magnetic field parameters, and of the density of cosmic ray sources. This allows us to obtain the expected spectra in the presence of the magnetic fields from the one that would be obtained in their absence. We also discuss how the discreteness of the distribution of sources affects the spectrum of cosmic rays at the highest energies.

      • 16:56
        Search for photons at the Pierre Auger Observatory 12m

        The Pierre Auger Observatory is the largest and most accurate air-shower experiment in the world. An essential characteristic of the Pierre Auger Observatory is the hybrid concept, combining a Surface Detector array (SD) with a Fluorescence Detector (FD), offering a large exposure and unique discrimination capabilities to photons with energy above $10^{17}$ eV. The analysis of data taken over 18 years, in hybrid mode as well as with the SD alone, allows various searches for UHE photons including the search for a diffuse UHE photon flux, a flux from point sources of UHE photons, and UHE photons from sources of Gravitational Wave events.

      • 17:08
        The Underground Muon Detector of the Pierre Auger Observatory 12m

        Ultrahigh-energy cosmic rays are a mystery at the frontier of high-energy particle physics and astronomy. The Pierre Auger Observatory is currently the largest detector for ultrahigh-energy cosmic rays in the world and will continue to search for the origins of cosmic rays at the highest energies in its second phase of operation. We will present the potential and the functionality of the Underground Muon Detector (UMD) that will allow for a direct measurement of the muon component in air showers providing the Pierre Auger Observatory an enhanced sensitivity of the primary mass of ultrahigh-energy cosmic rays. The UMD is being deployed as a part of a greater upgrade named AugerPrime, which will make Auger an event-by-event mass-sensitive observatory for cosmic-ray physics and multi-messenger astronomy. The UMD will be mostly efficient at primary energies above 10^16.5 eV and will primarily be used to directly measure the mass composition in the cosmic ray spectrum below the ankle region and to enhance the capabilities of photon-hadron discrimination at these energies.

      • 17:20
        High-energy lepton and photon simulations with the framework PROPOSAL 12m

        Modern analysis methods in cosmic ray physics rely on precise and efficient simulations of high-energy particles.
        To simulate the propagation of charged leptons and photons, the tool PROPOSAL has been developed.
        It provides a 3D Monte Carlo simulation optimized for high-energy particles, usable in C++ and Python.

        We present the simulation framework PROPOSAL and a selection of its applications in astroparticle physics.
        This includes neutrino observatories like the IceCube Neutrino Observatory, the imaging technique muography, and the usage of PROPOSAL in the new air shower simulation framework CORSIKA 8.
        Additionally, the latest study to estimate the impact of muon deflections on directional reconstructions using PROPOSAL is shown.

    • 20:00 → 20:20
      Conference dinner 20m
  • mercredi 7 décembre
    • 09:00 → 10:30
      Gamma-rays from Galaxy
    • 10:30 → 11:00
      coffee 30m
    • 11:00 → 12:30
      Gamma-rays from Galaxy
      • 11:00
        Gamma-ray measurements by LHAASO experiment 30m
        Orateur: Quiang Yuan (TBC)
        2022_LHAASO_YuanQ.pdf
      • 11:30
        Cosmic ray acceleration and multi-messenger radiation from wind bubbles 30m
        Orateur: Enrico Peretti (Niels Bohr Institute)
        Peretti-Paris-WindBubbles.pdf
      • 12:00
        Pulsar Wind Nebulae: the wondrous machines of High-Energy Astrophysics 30m
        Orateur: Niccolo' Bucciantini (INAF - Arcetri)
        Bucciantini_Paris_2022.pdf
    • 12:30 → 14:00
      Lunch 1h 30m
    • 14:00 → 15:30
      Gamma-rays from Galaxy
    • 15:30 → 16:00
      coffee 30m
    • 16:00 → 16:30
      Summary talk
    • 16:30 → 18:00
      Final discussion
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