BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:CRPropa Workshop: opening and introduction DTSTART;VALUE=DATE-TIME:20220914T090000Z DTEND;VALUE=DATE-TIME:20220914T093000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-87@indico.ift.uam-csic.es DESCRIPTION:Speakers: Rafael Alves Batista (Instituto de Física Teórica\ , Universidad Autónoma de Madrid (IFT UAM-CSIC))\nhttps://indico.ift.uam- csic.es/event/11/contributions/87/ LOCATION: URL:https://indico.ift.uam-csic.es/event/11/contributions/87/ END:VEVENT BEGIN:VEVENT SUMMARY:Neutrinos and gamma rays from clusters of galaxies DTSTART;VALUE=DATE-TIME:20220915T081000Z DTEND;VALUE=DATE-TIME:20220915T084500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-84@indico.ift.uam-csic.es DESCRIPTION:Speakers: Rafael Alves Batista (Instituto de Física Teórica\ , Universidad Autónoma de Madrid (IFT UAM-CSIC))\nCosmic rays can be acce lerated to high energies by astrophysical objects embedded in clusters of galaxies or by shocks taking place in the intracluster medium. These cosmi c rays are trapped within clusters\, interacting with the gas and radiatio n permeating this environment\, producing high-energy non-thermal messenge rs including neutrinos and gamma rays. These messengers can be observed ei ther from individual clusters or as diffuse fluxes resulting from the whol e population of these objects. While their fluxes depend on properties of the cosmic-ray emission\, this contribution is guaranteed to exist\, conse quently constraining the parameter space available for other components th at could generate them\, such as some populations of astrophysical objects and the elusive dark matter. In this talk I will describe the propagation of high-energy cosmic rays in galaxy clusters considering a sample of the se objects obtained from cosmological magnetohydrodynamical simulations of structure formation. I will then present estimates for the neutrino and g amma-ray fluxes from individual clusters\, followed by estimates of the as sociated diffuse neutrino and gamma-ray fluxes. Finally\, I will discuss t hese results within a broader astrophysical context\, focusing on their im portance for high-energy multi-messenger astronomy.\n\nhttps://indico.ift. uam-csic.es/event/11/contributions/84/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/84/ END:VEVENT BEGIN:VEVENT SUMMARY:CRPropa high statistic simulations for UHECR anisotropy studies DTSTART;VALUE=DATE-TIME:20220915T073000Z DTEND;VALUE=DATE-TIME:20220915T081000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-82@indico.ift.uam-csic.es DESCRIPTION:Speakers: Simone Rossoni (University of Hamburg)\nDespite the great progress made by modern cosmic ray observatories\, the origin and ac celeration mechanism of ultra-high-energy cosmic rays (UHECRs) remains an unsolved problem to this day. However\, there is experimental evidence for an anisotropic component in the UHECR arrival direction greater then few EeV. The search for UHECR sources is further complicated by two main facto rs: during extragalactic propagation UHECRs interact with background photo n fields (like the CMB and the EBL) and\, since they are electrically char ged\, they are deflected by extragalactic and galactic magnetic fields (EG MF and GMF). Moreover\, the strength\, structure and origin of the EGMF ar e still not well known\, causing reconstructing the deflection of UHECRs a non-trivial task. In this work we consider several EGMF models obtained f rom constrained MagnetoHydroDynamics (MHD) simulations of our local Univer se to study the propagation of UHECRs through such a structured environmen t. We simulate propagation\, interactions and observation of UHECRs by usi ng the Monte Carlo code CRPropa3. We also take into account the effect of the GMF by adopting a lensing procedure of the arrival UHECR sky map. We e xplore several combination of source distribution\, EGMF structure and mas s composition. As a reference\, we also simulate scenarios without the EGM F and with a statistically homogeneous field. We use our simulation result s to compute UHECR observables\, such as the energy spectrum\, the angular power spectrum and the arrival direction map (before and after the GMF) i n order to obtain constraints on possible combinations of source distribut ions and EGMF models.\n\nhttps://indico.ift.uam-csic.es/event/11/contribut ions/82/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/82/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic propagation of GCRs and EGCRs in the shin region with CRP ropa DTSTART;VALUE=DATE-TIME:20220915T101500Z DTEND;VALUE=DATE-TIME:20220915T104500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-83@indico.ift.uam-csic.es DESCRIPTION:Speakers: Alex Kääpä (Ruhr Universität Bochum)\nThe energy range pertaining to the shin region of the cosmic ray (CR) energy spectru m is noteworthy in that propagation shifts from diffusive to ballistic wit h increasing energy. At the same time\, the transition from Galactic cosmi c rays (GCRs) to extragalactic cosmic rays (EGCRs) in this energy range\, the details of which hitherto not certain.\n\nThis talk details the approa ch I employed in the study of the propagation effects of the GMF on GCRs a nd EGCRs. We begin with a brief comparison of the two numerical approaches utilisable in this energy range (the Transport Equation approach and the Equation of Motion approach)\, followed by an outline of the simulation se tup and a brief discussion of necessary considerations pertaining to it. A fter this\, the arising propagation effects are presented\, along with the ir effects on CR observables\, and finally the physical implications for t he shin region are drawn.\n\nhttps://indico.ift.uam-csic.es/event/11/contr ibutions/83/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/83/ END:VEVENT BEGIN:VEVENT SUMMARY:Hadronic interactions with CRPropa DTSTART;VALUE=DATE-TIME:20220916T073000Z DTEND;VALUE=DATE-TIME:20220916T080000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-85@indico.ift.uam-csic.es DESCRIPTION:Speakers: Leonel Morejon (Wuppertal University)\n.\n\nhttps:// indico.ift.uam-csic.es/event/11/contributions/85/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/85/ END:VEVENT BEGIN:VEVENT SUMMARY:Momentum diffusion DTSTART;VALUE=DATE-TIME:20220916T083000Z DTEND;VALUE=DATE-TIME:20220916T090000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-86@indico.ift.uam-csic.es DESCRIPTION:https://indico.ift.uam-csic.es/event/11/contributions/86/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/86/ END:VEVENT BEGIN:VEVENT SUMMARY:Modelling Diffusive Shock Acceleration with CRPropa DTSTART;VALUE=DATE-TIME:20220916T080000Z DTEND;VALUE=DATE-TIME:20220916T083000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-81@indico.ift.uam-csic.es DESCRIPTION:Speakers: Lukas Merten (Ruhr University Bochum)\, Sophie Aerdk er (Ruhr-University Bochum)\nCosmic ray particles reach energies as high a s $10^{21}\\\,$eV\, and most likely they are accelerated in varying electr omagnetic fields present in astrophysical sources and the interstellar med ium. Most promising acceleration mechanisms are the First and Second Order Fermi acceleration: Cosmic ray particles repeatedly scatter on moving mag netic field turbulences and on average they gain energy from these collisi ons. \nI present how the First order mechanism\, also referred to as Diffu sive Shock Acceleration\, can be modelled with CRPropa using the Diffusion SDE Module. Particles are accelerated when they diffuse over the shock and experience a changing flow velocity. Changes in the advective field and t he diffusion coefficient over the shock are approximated by differentiable functions that can be handled by DiffusionSDE. With this approach\, the r esulting CR spectrum highly depends on the choice of the "shock width" and the step length of the simulation. \nIn addition\, I give an outlook how the Second order mechanism\, also referred to as Momentum Diffusion\, can be modelled by stochastic differential equations. The modelling of Diffusi ve Shock Acceleration and Momentum Diffusion extend CRPropa's Acceleration Module to diffusive transport.\n\nhttps://indico.ift.uam-csic.es/event/11 /contributions/81/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/81/ END:VEVENT BEGIN:VEVENT SUMMARY:Deriving Constraints on Intergalactic Magnetic Fields DTSTART;VALUE=DATE-TIME:20220915T141500Z DTEND;VALUE=DATE-TIME:20220915T150000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-80@indico.ift.uam-csic.es DESCRIPTION:Speakers: Andrey Saveliev ()\nIntergalactic Magnetic Fields (I GMFs) are one of the most important phenomena in astrophysics and cosmolog y\, as a lot of information concerning the evolution and the present state of the Universe may be derived using them. In order to put constraints on IGMFs\, one needs to consider a variety of their interactions with differ ent environments: On the one hand\, they influence the propagation of char ged particles\, of which Ultra High Energy Cosmic Rays (UHECRs) and electr omagnetic cascades initiated by TeV-gamma rays are of particular interest since their trajectories are highly sensitive to IGMF parameters (such as their average field strength\, correlation length\, spectrum and helicity) . On the other hand\, IGMFs directly interact with the Intergalactic Mediu m (IGM)\, the understanding of which requires numerical and (semi-)analyti cal large-scale simulations. In case one assumes that they have been creat ed in the Early Universe\, one has also to consider cosmological aspects s uch as their impact on the Cosmic Microwave Background (CMB)\, which might be used to derive further constraints. In this talk we will discuss all t hese different methods for a coherent and comprehensive view on IGMFs.\n\n https://indico.ift.uam-csic.es/event/11/contributions/80/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/80/ END:VEVENT BEGIN:VEVENT SUMMARY:Cosmic Ray Electron transport in the external galaxy M51 DTSTART;VALUE=DATE-TIME:20220915T094500Z DTEND;VALUE=DATE-TIME:20220915T101500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-79@indico.ift.uam-csic.es DESCRIPTION:Speakers: Julien Dörner (Ruhr-University Bochum)\nRecent meas urements of the synchrortron emission of the external galaxy M51 give indi rect implication for the cosmic-ray electron (CRE) transport in the inters tellar medium. \nBy modelling the CRE transport considering all relevant e nergy loss processes we aim to distinguish the contribution of diffusive a nd advective transport. The current measurements give insights in the diff usion coefficient\, the star formation rate and the magnetic field strengt h. \nUsing these information we use the CRPropa module `DiffusionSDE` to s olve the 3D transport equation for isotropic diffusion and the 3D-advectio n profile. Additionally we implement the relevant energy loss processes as a continues loss.\n\nWith our best fit model the data can be described we ll. For the best fit the wind speed followed from the observation of the s tar formation rate must be decreased by a factor 5. We find that the inner galaxy is dominated by advection and the outer by spatial diffusion. \n\n In general leads this approach of modelling face-on galaxies insights of t he only indirect observable advection profile.\n\nhttps://indico.ift.uam-c sic.es/event/11/contributions/79/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/79/ END:VEVENT BEGIN:VEVENT SUMMARY:Inferring the diffusion coefficient in the heliosheath by time spe ctra simulations of GCRs in the HelMod framework DTSTART;VALUE=DATE-TIME:20220915T091500Z DTEND;VALUE=DATE-TIME:20220915T094500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-76@indico.ift.uam-csic.es DESCRIPTION:Speakers: Silvia Salvatore ()\nThe cosmic rays propagation ins ide the heliosphere is a very complex physical process\, well described by the Parker Transport Equation (PTE). When travelling in the heliosphere\, particles undergo convection\, diffusion and energy changes as they move in the irregular magnetic fields originated from the Sun\, and their flux is therefore modulated. The irregularities are due to the outward flowing solar wind plasma\, incapsulating the interplanetary magnetic field within the heliopause. HelMod is a code developed in INFN and Università di Mil ano-Bicocca solving the PTE in terms of stochastic differential equations and returning the modulated energy spectrum of the particles inside the he liosphere. The extremely turbulent region from the termination shock to th e heliopause – the heliosheath - is responsible for a significant part o f the modulation\, particularly for low energy CRs. In this work\, the sol ar modulation for H\, He\, C\, O\, Mg and Si ions is studied in the 2000-2 016 time period and compared with the Voyager 1 data\, in a ~ 0.5 - 2 GV r igidity range. This procedure allows us to infer the diffusion coefficient function inside the heliosheath area\, i.e. a power law with γ=1.4.\n\nh ttps://indico.ift.uam-csic.es/event/11/contributions/76/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/76/ END:VEVENT BEGIN:VEVENT SUMMARY:Fitting an astrophysical model for the UHECR origin DTSTART;VALUE=DATE-TIME:20220914T123000Z DTEND;VALUE=DATE-TIME:20220914T131500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-75@indico.ift.uam-csic.es DESCRIPTION:Speakers: Teresa Bister (RWTH Aachen University)\nThree observ ables of ultra-high-energy cosmic rays can be measured with present-day ob servatories: the energy spectrum\, the distribution of maximum shower dept hs and the arrival directions. We use all three observables for a combined fit\, in which the parameters of possible UHECR sources are constrained. The astrophysical model used in this fit is based on 1-dimensional CRPropa 3 simulations\, taking into account all known interactions. Then\, these 1 -dimensional simulations are reweighted to account for the three-dimension al source setup consisting of homogeneous background sources and a variabl e contribution from nearby source candidates. The signal fraction\, as wel l as the size of a rigidity-dependent local magnetic field blurring\, are part of the fit parameters. The influence of the extragalactic magnetic fi eld is investigated\, considering the low-energy suppression due to diffus ion\, as well as a source-distance-dependent beam-widening of the arrival directions.\n\nhttps://indico.ift.uam-csic.es/event/11/contributions/75/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/75/ END:VEVENT BEGIN:VEVENT SUMMARY:Inverting UHECR propagation with a normalizing flow DTSTART;VALUE=DATE-TIME:20220914T131500Z DTEND;VALUE=DATE-TIME:20220914T134500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-74@indico.ift.uam-csic.es DESCRIPTION:Speakers: Josina Schulte (RWTH Aachen University)\nAs shown by the Pierre Auger Collaboration\, the combined fit of energy spectrum and depth of shower maximum distributions of ultra-high-energy cosmic rays can provide constraints on the parameters their sources. To this end\, a data base describing the connection between the shape of the injected energy sp ectrum and composition at the sources and the observables measured on Eart h is built using 1-dimensional CRPropa3 simulations. Here\, the injection at the source is described by several free model parameters\, namely the s pectral index\, maximum rigidity and five representative mass fractions.Th e inference of the free model parameters can be done with\, e.g.\, Markov chain Monte Carlo (MCMC) sampling which allows to reconstruct posterior di stributions. \nIn this work\, we investigate an alternative approach based on normalizing flows\, a conditional invertible neural network. We show t hat the posterior distributions obtained with the network agree with those using MCMC\, for a simulation of energy spectrum and shower depth distrib utions resembling Auger measurements. Additionally\, the mapping of the so urce parameters and the observables as learned by the cINN is investigated . The accuracy of the reconstructed variables on a test dataset is shown t o be very good. For different applications\, the concept may also be explo ited to swiftly generate observables for specific source scenarios after t he initial computing-expensive learning phase.\n\nhttps://indico.ift.uam-c sic.es/event/11/contributions/74/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/74/ END:VEVENT BEGIN:VEVENT SUMMARY:Gamma-ray attenuation from extragalactic background light in the F ermi and CTA era DTSTART;VALUE=DATE-TIME:20220915T124500Z DTEND;VALUE=DATE-TIME:20220915T134500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-78@indico.ift.uam-csic.es DESCRIPTION:Speakers: Alberto Saldana-Lopez (University of Geneva)\nThe di ffuse extragalactic background light (EBL) is formed by ultraviolet (UV)\, optical\, and infrared (IR) photons mainly produced by star formation pro cesses over the history of the Universe and contains essential information about galaxy evolution and cosmology. The EBL also attenuates gamma-ray f luxes that travel cosmological distances through pair-production interacti ons\, leaving a signature in the gamma-ray spectra of extragalactic source s. In this talk\, we present a new determination of the evolving EBL spect ral energy distribution using a novel approach purely based on galaxy data aiming to reduce current uncertainties on the higher redshifts and IR int ensities. Our results are based in one of the most comprehensive and deepe st multi-wavelength galaxy datasets ever obtained\, which allow us to deri ve the overall EBL evolution up to z~6 and its uncertainties. We will also discuss the gamma-ray optical depths that are obtained from our EBL appro ximation\, and how we can measure galaxy evolution and other cosmological properties such as the cosmic star-formation rate and the expansion rate o f the Universe using gamma-ray observations of blazars.\n\nhttps://indico. ift.uam-csic.es/event/11/contributions/78/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/78/ END:VEVENT BEGIN:VEVENT SUMMARY:Efficient UHECR simulations with PriNCe and what they taught us so far DTSTART;VALUE=DATE-TIME:20220914T141500Z DTEND;VALUE=DATE-TIME:20220914T151500Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-73@indico.ift.uam-csic.es DESCRIPTION:Speakers: Xavier Rodrigues (Ruhr University Bochum)\nIn this t alk I will introduce PriNCe (Heinze et al 2019) as a novel open-source Py thon software for UHECR propagation. The computational efficiency of PriNC e allows the user to perform vast scans of the source parameters\, the emi tted spectral shape\, and the mass composition. I then discuss recent appl ications of the code\, such as the first joint fit to Auger and Telescope Array (TA) spectral and composition data. The fit favors the presence of a local source of UHECRs in the Northern Hemisphere at the 5.6$\\sigma$ le vel compared to the scenario where both experiments observe only an isotro pic source population. I comment on possible source candidates based on th e predicted distance and mass composition.\n\nhttps://indico.ift.uam-csic. es/event/11/contributions/73/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/73/ END:VEVENT BEGIN:VEVENT SUMMARY:High-energy particles from astrophysical transients DTSTART;VALUE=DATE-TIME:20220914T093000Z DTEND;VALUE=DATE-TIME:20220914T103000Z DTSTAMP;VALUE=DATE-TIME:20261006T123754Z UID:indico-contribution-11-77@indico.ift.uam-csic.es DESCRIPTION:Speakers: Claire Guepin (University of Maryland\, NASA GSFC\, University of Chicago)\nDecisive advances in the understanding of explosiv e transients have been made possible by the development of multi-messenger astronomy and time-domain astronomy. However\, the origin of high-energy (HE) to ultra-high-energy (UHE) cosmic rays and neutrinos remain unclear. Deciding between the various source candidates requires a precise modeling of the propagation\, acceleration and interactions of cosmic rays\, and t he subsequent multi-messenger and time-dependent emissions. We will descri be the production of HE to UHE particles in the vicinity of transient sour ces\, and highlight some key aspects related to the treatment of multi-mes senger predictions\, time-dependencies and uncertainties.\n\nhttps://indic o.ift.uam-csic.es/event/11/contributions/77/ LOCATION:IFT\, Sala Roja (red room) URL:https://indico.ift.uam-csic.es/event/11/contributions/77/ END:VEVENT END:VCALENDAR