BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Progresses in γ–ray Astronomy and Cosmic-ray ResearchProgresses in γ–ray Astronomy and Cosmic-ray Research DTSTART:20241015T144500Z DTEND:20241015T153000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10465@events.icecube.wisc.edu DESCRIPTION:Speakers: Zhen Cao (Institute of High Energy Physics)\n\nhttps ://events.icecube.wisc.edu/event/183/contributions/10465/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10465/ END:VEVENT BEGIN:VEVENT SUMMARY:The Unexpected TeV Emitters in the Galactic Plane DTSTART:20241016T190000Z DTEND:20241016T194500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10597@events.icecube.wisc.edu DESCRIPTION:Speakers: Ke Fang (University of Wisconsin–Madison)\n\nRecen t multi-messenger observations of the Galactic plane have revealed new cla sses of gamma-ray emitters at energies reaching into the multi-tens of TeV range\, challenging our previous understanding based on lower-energy data . These unexpected sources include TeV halos—extended gamma-ray emission s around isolated pulsars that cannot be explained as traditional pulsar w ind nebulae—as well as X-ray binaries and supernova remnants exhibiting emissions up to 100 TeV. In this talk\, we will present recent findings fr om studies utilizing data from HAWC\, Fermi-LAT and IceCube. Furthermore\, we will discuss theoretical interpretations that shed light on these obse rvations and explore their implications for high-energy astrophysical proc esses.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10597/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10597/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube: Status of the Search for Cosmic Ray Sources DTSTART:20241016T144500Z DTEND:20241016T153000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10598@events.icecube.wisc.edu DESCRIPTION:Speakers: Francis Halzen (UW-Madison)\n\nBelow the geographic South Pole\, the IceCube project has transformed one cubic kilometer of na tural Antarctic ice into a neutrino detector. IceCube detects more than 10 0\,000 neutrinos per year in the GeV to 10 PeV energy range. Among those\, we have isolated a flux of high-energy neutrinos originating beyond our G alaxy\, with an energy flux that is comparable to that of the extragalacti c high-energy photon flux observed by the NASA Fermi satellite. With a dec ade of data\, we have identified their first sources\, which point to the obscured dense cores associated with the supermassive black holes at the c enters of active galaxies as the origin of high-energy neutrinos and high- energy cosmic rays. We recently also observed neutrinos originating in our own Milky Way which is\, interestingly\, not a prominent feature in the n eutrino sky.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10 598/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10598/ END:VEVENT BEGIN:VEVENT SUMMARY:Science Results of 9 Years of Measurements from CALET Operation on the International Space Station DTSTART:20241014T160000Z DTEND:20241014T164500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10622@events.icecube.wisc.edu DESCRIPTION:Speakers: John Krizmanic (NASA/GSFC)\n\nOperating nearly flawl essly for nine years from October 2015\, the Calorimetric Electron Telesco pe (CALET) has been measuring the properties of the cosmic radiation. CA LET was designed to achieve the primary objectives of measuring the spectr a of electrons/positrons through the TeV energy decade to search for nearb y sources and/or signatures of dark matter processes and measure the spect ra of the hadronic components up to a PeV. Combined with secondary science goals of measuring the relative abundances of the ultra-heavy galactic co smic ray (UHGRC) component above Z=28 (nickel) and past Z=40 (zirconium) a nd of measuring gamma-rays potentially in the TeV region\, CALET’s measu rements are designed to provide detailed investigations of the processes i nvolved in cosmic-ray acceleration\, including understand the relationship between volatile and refractory material in this process\, as well as the subsequent propagation in the galaxy. CALET also monitors the sky for X- ray and soft gamma-ray transients using the CALET Gamma-Ray Burst Monitor (CGBM). Additionally\, CALET has demonstrated exceptional sensitivity to s pace weather events vis-à-vis the observation of variability in the flux of geomagnetically trapped particles\, especially using on-board measureme nts of precipitating electrons. The science results obtained during the f irst 9 years of CALET operation\, including the breaks in spectral indices observed in the all-electron and hadronic spectra\, will be presented and discussed.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/106 22/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10622/ END:VEVENT BEGIN:VEVENT SUMMARY:Are Supernova Remnants as Cosmic Ray Factories? Yes\, but… DTSTART:20241016T210000Z DTEND:20241016T214500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10595@events.icecube.wisc.edu DESCRIPTION:Speakers: Damiano Caprioli (University of Chicago)\n\nFirst-pr inciples plasma simulations have been pivotal in helping developing a theo ry of ion and electron acceleration at shocks\, and in particular in SNRs. I discuss what we have learned about particle acceleration efficiency\, s pectra\, and maximum energy\, and contrast these results with multi-wavele ngth emission from SNRs. Despite compelling evidence of hadron acceleratio n in these sources\, there are both theoretical and observational open que stions that prevent us from claiming that SNRs can accelerate CRs up to th e knee.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10595/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10595/ END:VEVENT BEGIN:VEVENT SUMMARY:A Multi-Messenger View of the Milky Way DTSTART:20241017T140000Z DTEND:20241017T144500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10623@events.icecube.wisc.edu DESCRIPTION:Speakers: Dan Hooper\n\nI will discuss the origin of the high- energy neutrino observed from the Galactic Plane by IceCube in a multi-mes senger context. Observations of diffuse gamma-ray emission\, resolved gamm a-ray sources (in particular\, TeV halos)\, and the cosmic ray spectrum ea ch bear on this question. IceCube data\, in turn\, can be used to test cos mic-ray transport models\, and models of origin of the Galactic cosmic ray s.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10623/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10623/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic Cosmic Rays: loose ends or shaking pillars? (remote) DTSTART:20241014T140000Z DTEND:20241014T144500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10624@events.icecube.wisc.edu DESCRIPTION:Speakers: Pasquale Blasi (GSSI)\n\nI will discuss some of the open problems related to the origin of Galactic cosmic rays\, in terms of both acceleration and transport.\n\nhttps://events.icecube.wisc.edu/event/ 183/contributions/10624/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10624/ END:VEVENT BEGIN:VEVENT SUMMARY:Multi-messenger modeling of Galactic cosmic-ray acceleration and t ransport DTSTART:20241014T210000Z DTEND:20241014T214500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10535@events.icecube.wisc.edu DESCRIPTION:Speakers: Lukas Merten (RUB)\n\nRecent observation of LHAASO's detection of several ultrahigh energy gamma ray sources and IceCube's obs ervation of the Galactic plane in neutrinos are clear a indication of Gala ctic cosmic ray sources with energies in the PeV range. However\, up to no w the exact acceleration processes are still unknown. Therefore\, modeling the acceleration and propagation of those particles in the source and on their way to Earth can help to understand their origin.\n\nIn this talk\, I will show recent improvements of CRPropa's\, an open source simulation f ramework\, ensemble averaged approach to model the diffusive propagation o f charged cosmic rays in arbitrary magnetic fields. This includes more sop histicated models of spatial diffusion\, allowing for changing Eigenvalues of the diffusion tensor and anomalous diffusion. Besides diffusive shock acceleration\, also momentum diffusion can now be taken into account. Furt hermore\, our advances to model hadron-hadron interactions with CRPropa wi ll be shown. Combining the two will allow us to build a more consistent mo del of the complete cosmic-ray lifetime\, from acceleration to arrival at Earth.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10535/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10535/ END:VEVENT BEGIN:VEVENT SUMMARY:Introduction DTSTART:20241014T134500Z DTEND:20241014T140000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10625@events.icecube.wisc.edu DESCRIPTION:Speakers: Paolo Desiati (University of Wisconsin–Madison)\n\ nhttps://events.icecube.wisc.edu/event/183/contributions/10625/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10625/ END:VEVENT BEGIN:VEVENT SUMMARY:Spectral Signatures of Local Cosmic Ray Sources DTSTART:20241014T190000Z DTEND:20241014T194500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10596@events.icecube.wisc.edu DESCRIPTION:Speakers: Igor Moskalenko (Stanford University)\n\nI will disc uss possible origins of spectral features observed at low and high energie s.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10596/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10596/ END:VEVENT BEGIN:VEVENT SUMMARY:Excesses in Cosmic-Ray Antinuclei DTSTART:20241017T181500Z DTEND:20241017T190000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10626@events.icecube.wisc.edu DESCRIPTION:Speakers: Tim Linden (Stockholm University)\n\nObservations by AMS-02 on the International Space Station have tentatively detected appro ximately 10 events that are consistent with antihelium nuclei. Such a dete ction would be of significant theoretical interest due to the difficulty i n producing any detectable antihelium flux through standard model interact ions. In this talk\, I will discuss the state of these observations\, the state of models that are capable of producing such observations -- and the possibility that dark matter may first be detected due to its exceedingly rare annihilations into heavy antinuclei states\, compared to more standa rd processes that produce gamma rays\, positrons\, or antiprotons.\n\nhttp s://events.icecube.wisc.edu/event/183/contributions/10626/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10626/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic CR sources: Insights from the diffuse emission\, TeV halo s\, and the CR anisotropy (remote) DTSTART:20241016T214500Z DTEND:20241016T223000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10517@events.icecube.wisc.edu DESCRIPTION:Speakers: Gwenael Giacinti (Tsung-Dao Lee Institute\, SJTU)\n\ nWe present two models of CR transport in the Galaxy. One with isotropic d iffusion\, and another one with anisotropic diffusion\, where CRs are prop agated in Galactic magnetic field models. In both models\, CRs are injecte d at discrete transient sources in the disc. We calculate the correspondin g diffuse Galactic gamma-ray emissions. We find that the emission at >~ 10 0 TeV is very clumpy\, and does not correlate with the gas density along t he line of sight. It is substantially different from the relatively smooth er emission detected by Fermi at ~ GeV energies. We then discuss how many PeVatrons would be detectable in our simulations (hadronic and leptonic)\, and compare our predictions with LHAASO data. We show that this allows to place interesting constraints on the nature and properties of PeVatrons.\ nMoreover\, we suggest that extended gamma-ray sources of a hadronic origi n should exist in the data. We show that such a source may exist in the AS -gamma data at 398-1000 TeV. We also discuss the case of another type of extended sources\, TeV halos\, and show that some may lead to the appearan ce of spurious “mirage” gamma-ray sources with no counterparts.\nFinal ly\, we discuss the implications of the observed TeV-PeV cosmic-ray anisot ropies\, and present a new calculation of their expected angular power spe ctrum.\n\nhttps://events.icecube.wisc.edu/event/183/contributions/10517/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10517/ END:VEVENT BEGIN:VEVENT SUMMARY:Investigating the CREDIT history of supernova remnants as cosmic-r ay sources DTSTART:20241014T201500Z DTEND:20241014T210000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10599@events.icecube.wisc.edu DESCRIPTION:Speakers: Anton Stall (TTK\, RWTH Aachen University)\, Philipp Mertsch\, Chun Khai Loo (TTK\, RWTH Aachen University)\n\nSupernova remna nts (SNRs) have long been suspected to be the primary sources of Galactic cosmic rays. Over the past decades\, great strides have been made in the m odelling of particle acceleration\, magnetic field amplification\, and esc ape from SNRs. Yet\, while many SNRs have been observed in non-thermal emi ssion in radio\, X-rays\, and gamma-rays\, there is no evidence for any in dividual object contributing to the locally observed flux. Here\, we propo se a particular spectral signature from individual remnants that is due to the energy-dependent escape from SNRs. For young and nearby sources\, we predict fluxes enhanced by tens of percent in narrow rigidity intervals\; given the percent-level flux uncertainties of contemporary cosmic-ray data \, such features should be readily detectable. We model the spatial and te mporal distribution of sources and the resulting distribution of fluxes wi th a Monte Carlo approach. The decision tree that we have trained on simul ated data is able to discriminate with very high significance between the null hypothesis of a smooth distribution of sources and the scenario with a stochastic distribution of individual sources. We suggest that this cosm ic-ray energy-dependent injection time (CREDIT) scenario be considered in experimental searches to identify individual SNRs as cosmic-ray sources.\n \nhttps://events.icecube.wisc.edu/event/183/contributions/10599/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10599/ END:VEVENT BEGIN:VEVENT SUMMARY:Multi-messenger search for the hadronic accelerators in our Galaxy DTSTART:20241015T210000Z DTEND:20241015T214500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10627@events.icecube.wisc.edu DESCRIPTION:Speakers: Nahee Park (Queen's University)\n\nThe origin of cos mic rays has been a century-old question. As it is challenging to utilize the directional information of cosmic rays to learn about their origin\, o bserving the gamma rays and neutrinos generated by the interactions of cos mic rays around the source regions has been considered to be the best way to study the origin of cosmic rays. In the last decades\, there have been remarkable improvements in the measurements of cosmic rays\, gamma rays an d neutrinos. This rich multi-messenger data should provide a consistent pi cture of the hadronic accelerators in our Galaxy. I will summarize current observations of multi-messenger observations focusing on the hadronic acc elerators in our Galaxy and discuss what near-future observations may adva nce our current understanding.\n\nhttps://events.icecube.wisc.edu/event/18 3/contributions/10627/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10627/ END:VEVENT BEGIN:VEVENT SUMMARY:Turbulent tales of stellar collapse and rebirth DTSTART:20241016T181500Z DTEND:20241016T190000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10628@events.icecube.wisc.edu DESCRIPTION:Speakers: Sarah Gossan (Hofstra University)\n\nThe next Galact ic core-collapse supernova will offer an unparalleled opportunity to probe the explosive rebirth of massive star to compact object across all cosmic messengers. In this talk\, I will outline what multi-messenger observatio ns can tell us about stellar evolution\, the nascent compact object popula tion\, and fundamental physics. I will discuss the current prospects for d etection of gravitational waves from core-collapse supernovae\, and before outlining how we can seek to improve them through experimental and analyt ical techniques over the next twenty years. To conclude\, I will muse on t he impact of these topics on our understanding of the central engines driv ing sources of Galactic cosmic rays.\n\nhttps://events.icecube.wisc.edu/ev ent/183/contributions/10628/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10628/ END:VEVENT BEGIN:VEVENT SUMMARY:Young stellar cluster as cosmic ray sources DTSTART:20241015T201500Z DTEND:20241015T210000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10618@events.icecube.wisc.edu DESCRIPTION:Speakers: Giovanni Morlino (INAF/Osservatorio Astrofisico di A rcetri)\n\nIn the last decade or so\, several young stellar clusters in po ur Galaxy have been associated with diffuse gamma-ray sources detected fro m GeV to multi-TeV enegy band\, supporting the idea that efficient particl e acceleration is taking place in those objects. Particle acceleration may occur through different mechanisms: i) at the termination shock of stella r winds produced by massive stars\, ii) at the shock of supernove explodin g inside the cluster or iii) due to the second order Fermi acceleration in the highly turbulente environment generated by winds and SN explotions. W hich mechanism dominate remains to be understood.\nIn this talk I will rev iew the acceleration models applied to stellar clusters\, highlighting the prediction for the resulting gamma-ray emission.\n\nhttps://events.icecub e.wisc.edu/event/183/contributions/10618/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10618/ END:VEVENT BEGIN:VEVENT SUMMARY:IceCube's Galactic Neutrinos: Diffuse Emission or Hidden Sources? DTSTART:20241017T144500Z DTEND:20241017T153000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10619@events.icecube.wisc.edu DESCRIPTION:Speakers: Markus Ahlers (Niels Bohr Institute - University of Copenhagen)\n\nThe IceCube Neutrino Observatory has recently reported stro ng evidence for neutrino emission from the Galactic plane. The signal is c onsistent with model predictions of diffuse emission from cosmic ray propa gation in the interstellar medium. However\, due to IceCube's limited pote ntial of identifying individual neutrino sources\, it is also feasible tha t unresolved Galactic sources could contribute to the signal. I will discu ss the contribution of this quasi-diffuse emission and examine whether thi s hypothesis can be tested by the upcoming KM3NeT detector or the planned future facility IceCube-Gen2.\n\nhttps://events.icecube.wisc.edu/event/183 /contributions/10619/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10619/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic Gamma Ray Sources as seen by HAWC DTSTART:20241015T190000Z DTEND:20241015T194500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10468@events.icecube.wisc.edu DESCRIPTION:Speakers: Jordan Goodman (UMD)\n\nhttps://events.icecube.wisc. edu/event/183/contributions/10468/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10468/ END:VEVENT BEGIN:VEVENT SUMMARY:Symposium's Summary DTSTART:20241017T190000Z DTEND:20241017T193000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10482@events.icecube.wisc.edu DESCRIPTION:Speakers: Simona Toscano (Université Libre de Bruxelles)\n\nh ttps://events.icecube.wisc.edu/event/183/contributions/10482/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10482/ END:VEVENT BEGIN:VEVENT SUMMARY:The Fermi view of the Galactic diffuse gamma-ray emission DTSTART:20241015T160000Z DTEND:20241015T164500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10620@events.icecube.wisc.edu DESCRIPTION:Speakers: Michela Negro\n\nIn our pursuit of understanding the origins and mechanisms of Galactic cosmic rays\, diffuse gamma-ray emissi on serves as a vital indirect probe of cosmic ray propagation within the M ilky Way. This presentation will provide an overview of the diffuse gamma- ray emissions observed by the Fermi Large Area Telescope (Fermi-LAT)\, emp hasizing the intricate connections with cosmic ray interaction and propaga tion through the interstellar medium.\n\nhttps://events.icecube.wisc.edu/e vent/183/contributions/10620/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10620/ END:VEVENT BEGIN:VEVENT SUMMARY:Interaction of Cosmic Rays at Mesoscopic Scales DTSTART:20241016T201500Z DTEND:20241016T210000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10621@events.icecube.wisc.edu DESCRIPTION:Speakers: ELLEN GOULD ZWEIBEL (Univ. Wisconsin-Madison)\, Elle n Zweibel (Univ. Wisconsin-Madison)\n\nI will discuss some recent work on the interaction of cosmic rays with turbulent\, diffuse\, multiphase gas i n the interstellar medium and beyond. Our work focuses on spatial scales w hich are typically not resolved by global simulations but are large compar ed to kinetic scales\, and to the cosmic ray mean free path\, so the fluid approximation holds. Phenomena at these scales are potentially observable and provide tests of the underlying models. These results were obtained i n collaboration with Roark Habegger\, Hanjue Zhu\, Ka Ho Yuen\, Ka Wai Ho\ , and Nick Gnedin\, and were funded by DoE\, NASA and the NSF.\n\nhttps:// events.icecube.wisc.edu/event/183/contributions/10621/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10621/ END:VEVENT BEGIN:VEVENT SUMMARY:Results from the DAMPE space mission (remote) DTSTART:20241014T181500Z DTEND:20241014T190000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10592@events.icecube.wisc.edu DESCRIPTION:Speakers: Ivan De Mitri (GSSI and INFN)\n\nThe space-based DAM PE (DArk Matter Particle Explorer) detector has been taking data since its successful launch in December 2015. Its main scientific goals include the indirect search for dark matter signatures in the cosmic electron and gam ma-ray spectra\, the measurements of galactic cosmic ray fluxes from tens of GeV up to hundreds of TeV and high energy gamma ray astronomy above a f ew GeV.\nA review of the detector features and the main mission results wi ll be given.\nIn particular\, results on proton and helium\, which reveale d new spectral features\, will be described. Ongoing analyses on light\, m edium\, and heavy mass nuclei will be outlined\, together with results on secondary-to-primary flux ratios.\n\nhttps://events.icecube.wisc.edu/event /183/contributions/10592/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10592/ END:VEVENT BEGIN:VEVENT SUMMARY:AMS-02 results and perspectives for future measurements with a mag netic spectrometer DTSTART:20241014T144500Z DTEND:20241014T153000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10460@events.icecube.wisc.edu DESCRIPTION:Speakers: Paolo Zuccon (Trento University and INFN-TIFPA)\n\nh ttps://events.icecube.wisc.edu/event/183/contributions/10460/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10460/ END:VEVENT BEGIN:VEVENT SUMMARY:Galactic gamma-ray PeVatron observations and non-thermal processes in galactic sources (remote) DTSTART:20241016T140000Z DTEND:20241016T144500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10519@events.icecube.wisc.edu DESCRIPTION:Speakers: Rubén López-Coto (IAA-CSIC)\n\nCosmic rays are ult rarelativistic particles that permeate the Milky Way\, propagating through the Galactic turbulent magnetic fields. The mechanisms under which these particles increase their energy can be reasonably described by current the ories of acceleration and propagation of cosmic rays. There are\, however\ , still many open questions as to how to reach petaelectronvolt (PeV) ener gies\, the maximum energy believed to be attained in our Galaxy\, and in w hich astrophysical sources (dubbed PeVatrons) this ultra-high energy accel eration happens. In this contribution\, I will present the theoretical con ditions for plasma acceleration to these energies\, and the Galactic sourc es in which these conditions are possible. These theoretical predictions a re then confronted with the latest experimental results\, summarising the state-of-the-art of our current knowledge of PeVatrons. I finally describe future prospects to keep advancing the understanding of these elusive obj ects\, still unidentified more than one hundred years after the discovery of cosmic rays.\n\nhttps://events.icecube.wisc.edu/event/183/contributions /10519/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10519/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent Results on Cosmic Ray Spectrum and Anisotropy from the GRAP ES-3 Experiment (remote) DTSTART:20241015T140000Z DTEND:20241015T144500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10518@events.icecube.wisc.edu DESCRIPTION:Speakers: Pravata Kumar Mohanty (Tata Institute of Fundamental Research)\n\nThe GRAPES-3 experiment\, situated in Ooty\, India\, uses a dense array of plastic scintillator detectors and a large-area tracking mu on detector to measure all charged particles and the muonic components of cosmic ray showers\, respectively. The experiment has measured the cosmic ray proton spectrum in the energy range of 50 TeV to 1.3 PeV\, and the rel ative proton composition was determined using muon multiplicity distributi ons. A spectral hardening was observed beyond 166 TeV\, challenging the si mple power-law description extending to the knee energy. Furthermore\, two significant small-scale anisotropic structures in the cosmic ray arrival distribution were detected at a median energy of 16 TeV\, consistent with results from the HAWC and ARGO-YBJ experiments. This presentation will hig hlight these findings\, along with updates on the status of the detector u pgrades and future plans.\n\nhttps://events.icecube.wisc.edu/event/183/con tributions/10518/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10518/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for Galactic PeVatrons with the Tibet ASgamma Experiment DTSTART:20241017T160000Z DTEND:20241017T164500Z DTSTAMP:20260311T032100Z UID:indico-contribution-10520@events.icecube.wisc.edu DESCRIPTION:Speakers: Kazumasa Kawata\n\nThe Tibet Air Shower (AS) array a nd the underground water-Cherenkov-type muon detector (MD) array have been operating successfully since 2014 at an altitude of 4\,300 m in Tibet\, C hina. The surface AS array determines the primary energies and arrival di rections\, while the MD array enables us to drastically reject background cosmic rays by counting the number of muons in each air shower. Recently \, using these AS+MD arrays\, we succeeded for the first time in observing sub-PeV gamma rays from the Crab Nebula and sub-PeV diffuse gamma rays fr om the Galactic disk. On the other hand\, it is believed that there are PeVatrons in our Galaxy\, which accelerate PeV cosmic rays. PeV cosmic ray s accelerated by the source interact with surrounding molecular clouds and emit sub-PeV gamma rays through neutral pion decay. Therefore\, sub-PeV g amma-ray observations are crucial for PeVatron searches. In this presentat ion\, we will review sub-PeV gamma-ray observations with the Tibet ASgamma experiment and discuss the most energetic cosmic-ray source “PeVatron ” in our Galaxy.\n\nhttps://events.icecube.wisc.edu/event/183/contributi ons/10520/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10520/ END:VEVENT BEGIN:VEVENT SUMMARY:HAWC Observations of the Spectrum\, Composition and Anisotropy of Cosmic Rays Below the Knee DTSTART:20241015T181500Z DTEND:20241015T190000Z DTSTAMP:20260311T032100Z UID:indico-contribution-10594@events.icecube.wisc.edu DESCRIPTION:Speakers: Juan Carlos Díaz Vélez (University of Wisconsin– Madison)\n\nThe HAWC Gamma-Ray Observatory is an extensive air-shower dete ctor array located at 4100 m a.s.l. on the slopes of Volcán Sierra Negra at 19°N in the state of Puebla\, Mexico. While HAWC is designed to study the sky in gamma-rays between 500 GeV and 100 TeV\, it is also sensitive t o showers from primary cosmic rays in the TeV to to multi-PeV energy range . We report on the latest measurements of the energy spectrum\, mass compo sition and arrival direction distribution of cosmic rays at energies from TeV’s to 1 PeV. The cosmic-ray energy spectrum measured by HAWC covers a range that includes the part of the energy region dominated by direct exp eriments up to just below the knee and shows a cut-off in the total spectr um at tens of TeV’s. We have also estimated the energy spectrum for H+He nuclei\, including the observation of a softening at around 24 TeV. Unfol ding studies in this energy region indicate that this is the result of ind ividual cut-offs in the spectra of H and He\, first observed by direct exp eriments. Our results also indicate the existence of a cut-off between 100 and 300 TeV in the heavy component of cosmic rays and a hardening in the spectra of the light cosmic ray nuclei at around 100 TeV.\n\nhttps://event s.icecube.wisc.edu/event/183/contributions/10594/ LOCATION:Northwoods Room (Union South\, University of Wisconsin–Madison) URL:https://events.icecube.wisc.edu/event/183/contributions/10594/ END:VEVENT END:VCALENDAR