BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:High Energy Gamma Ray Instruments for Dark Matter Searches DTSTART;VALUE=DATE-TIME:20191113T010000Z DTEND;VALUE=DATE-TIME:20191113T013000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1505@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masahiro Teshima (ICRR\, the University of Tokyo)\nh ttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1505/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1505/ END:VEVENT BEGIN:VEVENT SUMMARY:The Dark Matter distribution of the Milky Way (its astrophysical u ncertainties and effects on determination of physics beyond the standard m odel) DTSTART;VALUE=DATE-TIME:20191112T050000Z DTEND;VALUE=DATE-TIME:20191112T053000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1525@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Fabio Iocco (Imperial College / Università di Napol i)\nThe distribution of Dark Matter in galaxies is one remarkable output o f structure formation in a cosmological context\, and an important input f or the searches of the nature of Dark Matter. In this talk I will present the results of recent\, fully data-driven analysis of the determination of the Dark Matter content and distribution in the Milky Way. \nI will also highlight the current uncertainties of empirical (and astrophysical) natur e\, and how they affect the interpretation of direct and indirect searches \, and eventually the searches for the very nature of the Dark Matter.\n\n https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1525/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1525/ END:VEVENT BEGIN:VEVENT SUMMARY:Current and Future WIMP Searches with Fermi-LAT\, HAWC\, and SWGO DTSTART;VALUE=DATE-TIME:20191113T030000Z DTEND;VALUE=DATE-TIME:20191113T033000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1523@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Andrea Albert (Los Alamos National Lab)\nEvidence su ggests ~85% of the mass in the Universe is dark matter (DM). Several promi sing DM theories predict that it is a fundamental particle. The most famou s of which is the Weakly Interacting Massive Particle (WIMP). WIMPs that a nnihilate at a weak-scale cross section that were in thermal equilibrium i n the Universe produce the observed DM abundance today. DM particles are t heorized to interact and produce standard model particles\, like gamma ray s. So far\, no definitive gamma-ray signal has been detected\, but current experiments have started excluding several thermal WIMP models. I will di scuss the current status of DM searches with gamma-ray observatories like the Fermi LAT and HAWC. I will also discuss how both future analysis with current observatories and future observatories like CTA and SWGO will prob e thermal WIMP models for masses from 5 GeV to ~100 TeV.\n\nhttps://indico .icrr.u-tokyo.ac.jp/event/259/contributions/1523/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1523/ END:VEVENT BEGIN:VEVENT SUMMARY:Higgsino Dark Matter DTSTART;VALUE=DATE-TIME:20191111T041500Z DTEND;VALUE=DATE-TIME:20191111T044500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1526@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Takeo Moroi ()\nI will discuss phenomenology of Higg sino dark matter. First\, I will briefly overview theoretical issues relat ed to Higgsino dark matter. Then\, I will summarize present status and fu ture prospects of Higgsino dark matter search using colliers and direct de tection experiments.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contri butions/1526/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1526/ END:VEVENT BEGIN:VEVENT SUMMARY:Discussion of experimental approach to go beyond the neutrino floo r in the WIMP search DTSTART;VALUE=DATE-TIME:20191111T083000Z DTEND;VALUE=DATE-TIME:20191111T090000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1534@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Tatsuhiro Naka (Toho University )\nIn the standard m ethodology for the WIMP search detect recoiled nuclei due to elastic scatt ering with that\, the neutrino should become background to be not able to avoid. If not detect significant signals or just few events detected befor e neutrino floor\, more reliable search to confirm those are the signals d ue to WIMP or new information to distinguish the WIMP signals from neutrin o backgrounds will be required. For example\, one of the promising informa tion in current studies is to use “direction” or signals attributed to that. In this talk\, I will report current experimental approach about d irection sensitive search\, and discuss about the issues to go beyond neut rino floor.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1 534/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1534/ END:VEVENT BEGIN:VEVENT SUMMARY:The Neutrino Floor DTSTART;VALUE=DATE-TIME:20191111T073000Z DTEND;VALUE=DATE-TIME:20191111T080000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1527@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kate Scholberg (Duke University)\nWIMP detectors in the 2020's will approach the sensitivity at which\nscatters of natural neu trinos will create a background sufficient to\nobscure the WIMP recoil sig nal. This is the so-called "Neutrino\nFloor". This talk will discuss the nature of the neutrino floor and\nthe motivations to get to it\, and to p otentially go beyond it.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/co ntributions/1527/ LOCATION:Remote talk URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1527/ END:VEVENT BEGIN:VEVENT SUMMARY:Recent Results and Dark Matter Search with CALET on the ISS DTSTART;VALUE=DATE-TIME:20191113T043000Z DTEND;VALUE=DATE-TIME:20191113T050000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1535@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yoichi Asaoka (WISE\, Waseda University)\nThe CALori metric Electron Telescope (CALET)\, which is currently conducting direct c osmic-ray observations onboard the International Space Station (ISS)\, use s an all-calorimetric instrument with total vertical thickness of 30 radia tion lengths and fine imaging capability. The instrument is optimized for cosmic-ray electron measurements by achieving large proton rejection and e xcellent energy resolution well into the TeV energy region. In addition\, very wide dynamic range of energy measurements and absolute charge identif ication capability of the instrument enable us to measure proton and nucle i spectra as well as electron and gamma-ray spectra. The CALET mission goa ls include the investigation of acceleration and propagation of galactic c osmic rays\, of possible nearby sources\, and of potential signature of da rk matter. Since the start of observation in October 2015\, smooth and con tinuous operations have taken place. In this talk\, we will give a brief s ummary of the recent results obtained with CALET and discuss about the dar k matter search using the CALET all-electron spectrum.\n\nhttps://indico.i crr.u-tokyo.ac.jp/event/259/contributions/1535/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1535/ END:VEVENT BEGIN:VEVENT SUMMARY:Varieties of DM density profile in Galactic dwarf spheroidal galax ies and the gamma-ray search of the annihilation signature DTSTART;VALUE=DATE-TIME:20191112T053000Z DTEND;VALUE=DATE-TIME:20191112T060000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1538@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Nagisa Hiroshima (Riken)\nDwarf spheroidal galaxies (dSph) are good targets to search for dark matter annihilation signals thr ough gamma-ray observations. Currently\, the most strong constraints on th e cross-section at mDM\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/cont ributions/1538/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1538/ END:VEVENT BEGIN:VEVENT SUMMARY:CTA Dark Matter searches in dwarf galaxies\, dark halos\, and gala xy clusters DTSTART;VALUE=DATE-TIME:20191113T023000Z DTEND;VALUE=DATE-TIME:20191113T030000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1539@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Moritz Hütten (Max Planck Institute for Physics)\nT he Cherenkov Telescope Array (CTA) represents the next-generation ground-b ased gamma-ray observatory in the energy range between 30 GeV and 300 TeV. It will open the window to gamma-ray searches for annihilation or decay o f heavy (TeV) Weakly Interacting Massive Particles (WIMPs) in astrophysica l Dark Matter (DM) budgets with unprecedented sensitivity. In this talk\, I will review the current prospects for WIMP searches with CTA in dwarf sp heroidal galaxies orbiting our Milky Way\, enhanced annihilation in close- by dark halos\, and galaxy clusters of the local Universe. I will also out line the current knowledge of the DM targets and foreseen observation stra tegies\, on which the success of the searches crucially depends.\n\nhttps: //indico.icrr.u-tokyo.ac.jp/event/259/contributions/1539/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1539/ END:VEVENT BEGIN:VEVENT SUMMARY:The GAPS experiment: sensitive survey of cosmic-ray antinuclei to search dark matter DTSTART;VALUE=DATE-TIME:20191112T030000Z DTEND;VALUE=DATE-TIME:20191112T030100Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1540@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Takuya Wada on behalf of the GAPS collaboration (Aoy ama Gakuin University)\nThe General Antiparticle Spectrometer (GAPS) is an international balloon-borne project for indirect dark matter (DM) searche s that investigates low-energy antinuclei in cosmic-ray\, especially undis covered antideuterons. Cosmic-ray antideuterons can be produced by self-an nihilation or decay of WIMP DM. The flux of DM-originated antideuterons ca n be orders of magnitude higher than that of the secondary (or background) component. Therefore\, antideuterons are considered to be a background-fr ee probe to search for DM. GAPS uses a unique concept to identify antinucl ei by applying the physics of exotic atom creation and decay. The GAPS ins trument is composed of lithium-drifted silicon (Si(Li)) detectors surround ed by a double-layered plastic scintillation-counter time-of-flight system . An incoming antinucleus forms an exotic atom in the Si(Li) detectors. Th rough the deexcitation and nuclear annihilation processes of the exotic at om\, characteristic X-rays and charged particles are emitted. By detecting and tracking those X-rays and particles\, GAPS has strong particle identi fication\, resulting in a high sensitivity for rare antinuclei. The first GAPS flight is scheduled for late 2021. We are currently developing all di fferent subsystems\, such as the Si(Li) tracker\, time-of-flight system\, cooling system\, and detailed simulation code of the instrument. We will r eport the scientific motivation\, detection concept\, and development stat us of GAPS.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1 540/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1540/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraint on the nature of annihilating dark matter with Low Surf ace Brightness Galaxies DTSTART;VALUE=DATE-TIME:20191112T030600Z DTEND;VALUE=DATE-TIME:20191112T030700Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1541@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daiki Hashimoto (Nagoya University)\nIn the context of the high energy astrophysics\, the nature of dark matter annihilation e xpected to emit gamma rays have been probed utilizing observed gamma-ray f lux in a direction of a high matter-density region. Recently\, some studie s have been performed with nearby dwarf galaxies or the Galactic center an d then the cross section for dark matter annihilation have been constraine d.\nIn our study\, we focus on Low Surface Brightness Galaxies (LSBGs) cat aloged by the observation data of Hyper Suprime-Cam (HSC). LSBGs can be us ed as novel tracers of dark matter annihilation signals because of being m ore massive than dwarf spheroids and having less astronomical contaminatio ns due to relatively quiescent states of those\, which can perform robuste r research for dark matter annihilation signals. \nWe model the gamma-ray flux from LSBGs using the 8 HSC-LSBGs measured each redshift\, and comperi ng with observed gamma-ray flux by Fermi Large Area Telescope\, provide th e upper limit of the cross section for dark matter annihilation. \nMoreove r\, we prospect the future constraint with soon-to-be-detected LSBGs by fu ture observation. In our poster presentation\, we report our method and re sults\, and also discuss the prospects for the future constraint.\n\nhttps ://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1541/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1541/ END:VEVENT BEGIN:VEVENT SUMMARY:Breaking through the neutrino floor DTSTART;VALUE=DATE-TIME:20191111T080000Z DTEND;VALUE=DATE-TIME:20191111T083000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1549@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ciaran O'Hare ()\nI will explain why the neutrino fl oor exists from a statistical perspective and then discuss what kind of in formation we need from an experimental search to be able to subtract the n eutrino background.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contrib utions/1549/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1549/ END:VEVENT BEGIN:VEVENT SUMMARY:Improved search for Dark Matter annihilation with a combined ana lysis of data from Fermi-LAT\, HAWC\, H.E.S.S.\, MAGIC and VERITAS: a fr amework for future DM analyses DTSTART;VALUE=DATE-TIME:20191113T063000Z DTEND;VALUE=DATE-TIME:20191113T065000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1550@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Daniel Kerszberg (IFAE-BIST)\nThe next generation of gamma-ray experiments are expected to improve significantly the current r esults in the search for Dark Matter (DM). Before these next-generation in struments start operating at their nominal design\, one possibility to imp rove the current results is to combine data from existing experiments. Thi s technique allows to increase energy coverage by combining data from ins truments with better sensitivity in different energy ranges and also to ma ximize the sensitivity by combining individual data sets from all the expe riments for which the energy ranges overlap. We will report on such an ini tiative aiming at combining data from dwarf spheroidal galaxies (dSphs)  from the Fermi-LAT\, HAWC\, H.E.S.S.\, MAGIC\, and VERITAS experiments. Be ing among the most DM dominated objects with negligible expected astrophys ical gamma-ray emission\, dSphs are ideal targets for DM indirect searches and thus will be also primary targets for the next generation of experime nts. Preliminary results of the combination constraining the DM annihi lation cross section will be presented spanning a range of DM masses f rom 10 GeV to 100 TeV. The potential of extending this analysis framework to more experiments as well as to future experiments will also be discusse d.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1550/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1550/ END:VEVENT BEGIN:VEVENT SUMMARY:Status and Prospect of PandaX experiment DTSTART;VALUE=DATE-TIME:20191112T070500Z DTEND;VALUE=DATE-TIME:20191112T072500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1552@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Pengwei Xie (Tsung-Dao Lee Institute)\nPandaX is a d ark matter search experiment located at China Jin Ping Underground Lab usi ng xenon time projection chamber.\nIn this talk\, I will present the lates t result from PandaX-II experiment and the current status of PandaX-4T exp eriment.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1552 / LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1552/ END:VEVENT BEGIN:VEVENT SUMMARY:Dark Matter Heating vs. Rotochemical Heating in Old Neutron Stars DTSTART;VALUE=DATE-TIME:20191112T082000Z DTEND;VALUE=DATE-TIME:20191112T084000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1551@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Keisuke Yanagi (University of Tokyo)\nWIMP DMs in th e Universe accumulate in neutron stars (NSs) through their interactions wi th nucleons. It has been known that their annihilation inside the NS core causes late-time heating\, with which the surface temperature becomes $T_s \\simeq (2-3) \\times 10^3$ K for the NS age $t > 10^{6-7}$ years. Thus t he measurement of NS surface temperature can be used as a new probe of WIM P DMs. Because of the strong gravity of NSs\, DM heating has several advan tages compared to the direct detection experiments on the earth.\n\nDespit e such advantages\, the background on the DM heating is rarely discussed i n the particle physics community. In particular\, the rotochemical heating \, internal heating caused by the out-of-equilibrium beta reactions in a N S\, should be considered because it does not assume any exotic physics. In fact\, if the rotochemical heating operates in a NS\, it may conceal the DM heating effects.\n\nIn this work\, we reevaluate the significance of th e DM heating in NSs\, including the effect of the rotochemical heating. We show that the signature of DM heating can still be detected in old ordina ry pulsars\, and discuss what is necessary to confirm the evidence for the DM heating.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/ 1551/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1551/ END:VEVENT BEGIN:VEVENT SUMMARY:Search for dark matter TeV spectral lines around the Galactic Cent re with the MAGIC telescopes DTSTART;VALUE=DATE-TIME:20191113T065000Z DTEND;VALUE=DATE-TIME:20191113T071000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1555@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Tomohiro Inada (ICRR\, UTokyo)\nIn this talk\, we wi ll present a status report on the search for dark matter spectral lines ar ound the Galactic centre (GC) with the MAGIC telescope system located on t he Canary island of La Palma\, Spain. MAGIC is sensitive to gamma rays fro m 50 GeV to 50 TeV. So far\, MAGIC has produced groundbreaking results in the field of indirect DM searches observing a variety of targets\, such as the Galactic halo\, dwarf spheroidal galaxies and clusters of galaxies. W e are now aiming to add the GC region as an observational target to search for line signatures from DM annihilation. MAGIC has observed the GC regio n for hundreds of hours at high zenith angles\, at which the collection ar ea for TeV gamma rays is significantly increased. This allows us to probe promising SUSY models of heavy DM candidates\, and to set limits on the DM annihilation cross section competitive to those obtained from observation s in the Southern hemisphere. We will also discuss how we exploit the data from a complex sky region to analise for line-like gamma-ray signatures.\ n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1555/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1555/ END:VEVENT BEGIN:VEVENT SUMMARY:Scalar dark matter interacting through an extra U (1) gauge intera ction DTSTART;VALUE=DATE-TIME:20191112T030300Z DTEND;VALUE=DATE-TIME:20191112T030400Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1561@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Osamu Seto (Hokkaido University)\nWe propose models of a thermal relic DM with the present annihilation cross-section being ve ry suppressed. This property can be realized in an extra U(1) gauge intera cting complex scalar DM. We consider scalar dark matter in U(1)B−L\,U(1) (B−L)3 and U(1)Lμ−Lτ extended models and identify viable parameter r egions. We also discuss various implication to future DM detection experim ents\, the DM interpretation of the gamma ray excess in the globular clust er 47 Tucanae\, the muon anomalous magnetic moment\, the Hubble Tension an d others.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/156 1/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1561/ END:VEVENT BEGIN:VEVENT SUMMARY:Probing heavy dark matter decays with multi-messenger astrophysica l data DTSTART;VALUE=DATE-TIME:20191112T031200Z DTEND;VALUE=DATE-TIME:20191112T031300Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1560@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Oscar Macias ()\nWe set conservative constraints on decaying dark matter particles with masses spanning a very wide range ($10 ^4-10^{16}$ GeV). For this we use multimessenger observations of cosmic-ra y (CR) protons/antiprotons\, electrons/positrons\, neutrinos/antineutrinos and gamma rays. Focusing on decays into the $b\\bar{b}$ channel\, we simu late the spectra of dark matter yields by using the Dokshitzer-Gribov-Lipa tov-Altarelli-Parisi equations and the Pythia package. We then propagate t he CRs of dark matter origin till Earth by using the state-of-the-art nume rical frameworks CRPropa\, GALPROP and HelMod for the solution of the CR t ransport equation in the extragalactic\, Galactic region and the heliosphe re\, respectively. Conservative limits are obtained by requiring that the predicted dark matter spectra at Earth be less than the observed CR spectr a. Overall\, we exclude dark matter lifetimes of $10^{28}$ s or shorter fo r all the masses investigated in this work. The most stringent constraints reach $10^{30}$ s for very heavy dark matter particles with masses in the range $10^{11}−10^{14}$ GeV.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event /259/contributions/1560/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1560/ END:VEVENT BEGIN:VEVENT SUMMARY:TeV dark matter search at the Galactic center with the CTA DTSTART;VALUE=DATE-TIME:20191113T013000Z DTEND;VALUE=DATE-TIME:20191113T020000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1562@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Gabrijela Zaharijas (University of Nova Gorica)\nHig h-energy gamma rays are among the most promising tools to constrain or rev eal the nature of dark matter (DM)\, in particular the Weakly Interacting Massive Particles models. The Cherenkov Telescope Array (CTA) is well int o its pre-construction phase and will soon probe the high-energy gamma-ray sky in the 20 GeV - 300 TeV energy range. Thanks to its improved energy and angular resolutions as well as significantly larger effective area\, t he CTA will probe a parameter space of heavier dark matter (above 100 GeV) \, with unprecedented sensitivity\, reaching the DM thermal annihilation r ate at the TeV regime. \n\nThis talk will summarise the planned DM search strategies with CTA\, focusing on the signal of DM in the centre of our Ga laxy. As observed with the Fermi LAT at lower energies\, this region exhib its complex large-scale gamma-ray emission and the CTA is expected to be t he first ground based observatory able to detect it. In this talk we repor t on the collaboration effort to study the impact of extended astrophysica l backgrounds on DM search\, based on the astrophysical emission observed with the Fermi LAT at lower energies and to suggest the promising data ana lysis and observational strategies for the upcoming CTA data.\n\nhttps://i ndico.icrr.u-tokyo.ac.jp/event/259/contributions/1562/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1562/ END:VEVENT BEGIN:VEVENT SUMMARY:SUSY Dark matter Search at LHC and future colliders DTSTART;VALUE=DATE-TIME:20191112T013000Z DTEND;VALUE=DATE-TIME:20191112T020000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1567@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Koji Terashi (University of Tokyo\, ICEPP)\nThe exis tence of dark matter (DM) is a cornerstone of extensive search programs at colliders. The ATLAS and CMS experiments at the LHC have performed a wide range of searches for DM particles predicted in SUSY\, in particular for the lightest neutralino in R-parity conserving scenarios. The event topolo gy and final states containing the neutralino DMs depend on the mass eigen states of the gauginos and their compositions. In this talk\, I will prese nt the current status of neutralino DM searches at the LHC\, putting some emphasis on DMs with Wino and Higgsino components. Prospects for the Wino/ Higgsino DM searches at future colliders are also discussed.\n\nhttps://in dico.icrr.u-tokyo.ac.jp/event/259/contributions/1567/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1567/ END:VEVENT BEGIN:VEVENT SUMMARY:Current status of Dark matter searches at LHC DTSTART;VALUE=DATE-TIME:20191112T010000Z DTEND;VALUE=DATE-TIME:20191112T013000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1563@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Priscilla Pani (DESY)\nThis talk aims to provide an overview of the theoretical framework\, the search strategies and the curr ent status of the results of Dark Matter searches at the LHC. The focus wi ll be restricted to mediator-based Dark Matter models (non-SUSY). Experim ental analyses and results will be presented on a selection of the models\ , using up to 150 ifb of $\\sqrt{s} = 13$ TeV $pp$ collision data collecte d by the ATLAS and CMS experiments at the LHC.\n\nhttps://indico.icrr.u-to kyo.ac.jp/event/259/contributions/1563/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1563/ END:VEVENT BEGIN:VEVENT SUMMARY:Overview on thermal DM models with emphasis on Electroweak charges DTSTART;VALUE=DATE-TIME:20191111T034500Z DTEND;VALUE=DATE-TIME:20191111T041500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1568@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shigeki Matsumoto (Kavli IPMU)\nDark matter (DM) pro blem is now one of the most important problems in many fields of physics. DM mass is\, however\, currently predicted to be in a range between 10^– 55 g and 10^40 g\; uncertainty of a hundred orders of magnitude. A certain diversity of research is thus required to solve the DM problem and many D M candidates are now being proposed and discussed. Among various candidate s\, TeV-scale thermal DM candidates now attract attention as they are pred icted by new physics models intensively discussed after the Higgs discover y at LHC and they also have a certain reason why current DM search experim ents/observations do not detect their signals. I will summarize above inte resting discussions of the TeV scale thermal DM candidates in this talk.\n \nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1568/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1568/ END:VEVENT BEGIN:VEVENT SUMMARY:Galaxy collisions and the missing satellite problem in the cold da rk matter model DTSTART;VALUE=DATE-TIME:20191112T031500Z DTEND;VALUE=DATE-TIME:20191112T031600Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1564@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masao Mori (University of Tsukuba)\nCold dark matter (CDM) cosmology is the standard paradigm of structure formation in the un iverse. However\, it has several unsolved severe problems. The missing sat ellites problem refers to the overabundance of theoretically predicted CDM subhalos compared to observed satellite galaxies in the Local Group. The most popular interpretation is that the small dark matter halos have extre mely inefficient star-forming history. In this study\, we investigate the possible existence of the stellar deficient CDM halos using large scale nu merical simulations for galaxy collisions between a CDM subhalo and a dwar f galaxy in the Local Group.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/25 9/contributions/1564/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1564/ END:VEVENT BEGIN:VEVENT SUMMARY:DM searches with LAr DTSTART;VALUE=DATE-TIME:20191111T061500Z DTEND;VALUE=DATE-TIME:20191111T064500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1548@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Cristiano Galbiati (Princeton University)\nExperimen ters from four different argon dark matter searches have joined their forc es in the the “Global Argon Dark Matter Collaboration” to carry out a unified program for dark matter direct detection.\n The next step at the s cale of a few tens of tonnes is the DarkSide-20k experiment\, a 20-tonne f iducial volume dual-phase TPC to be operated at LNGS with an underground a rgon fill\, designed to collect an exposure of 100 tonne×years\, complete ly free of neutron-induced nuclear recoil background and all electron reco il background. DarkSide-20k is set to start operating by 2023 and will ha ve sensitivity to WIMP-nucleon spin-independent cross sections of 7.4×10 −48 cm2 for WIMPs of 1 TeV/c2 mass\, to be achieved during a 10 year run with an exposure of 200 tonne×years. DarkSide-20k will explore the WIMP -nucleon cross-section down to the edge of the ’neutrino floor’\, wher e coherent neutrino-nucleus scattering from environmental neutrinos induce nuclear recoils in the detector.\n A second step in the program is the co nstruction and operation of Argo\, a detector with a fiducial mass of a fe w hundred tonnes\, capable of collecting an exposure of several thousands of tonne×years\, completely free of all backgrounds on top of CNNS\, slat ed for a 2030 start.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contri butions/1548/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1548/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraints on cosmic ray propagation and magnetic fields using ga mma-ray observations DTSTART;VALUE=DATE-TIME:20191113T053000Z DTEND;VALUE=DATE-TIME:20191113T060000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1661@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Rubén López-Coto (INFN Padova)\nThe origin and pro pagation of cosmic rays is one of the most important questions in astropar ticle physics nowadays. To perform Indirect searches of Dark Matter search ing for their products in the local cosmic ray spectra\, we first need to comprehend what is the background coming from astrophysical sources. We ca n only model this background by achieving a deep understanding of cosmic r ay propagation. Although the transport of these cosmic rays through the ga laxy make them lose the information about their origin due to interstellar magnetic fields\, we can directly study the properties of their propagati on using gamma rays. In this talk\, I will give a review of current measur ements of magnetic fields and cosmic ray propagation parameters using gamm a rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1661/ LOCATION:Remote talk URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1661/ END:VEVENT BEGIN:VEVENT SUMMARY:DM searches with LXe DTSTART;VALUE=DATE-TIME:20191111T054500Z DTEND;VALUE=DATE-TIME:20191111T061500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1572@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masaki Yamashita (ICRR\, The University of Tokyo)\nD irect dark matter searches have been conducted for more than 30 years in t he underground laboratories to look for signals via dark matter-nucleus el astic scattering of its target materials. Weakly interacting massive part icles as dark matter candidates arise naturally in various theories\, s uch as Supersymmetry\, Extra Dimensions. WIMPs interact through the weak interaction and can efficiently transfer kinetic energy by the scattering from atomic nuclei\, the WIMP model can be tested by searching for nuclear recoils in a sensitive\, low-radioactivity detector. This review talk wi ll focus on a liquid xenon base detectors among those searches which incl ude current bounds and future prospects.\n\nhttps://indico.icrr.u-tokyo.ac .jp/event/259/contributions/1572/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1572/ END:VEVENT BEGIN:VEVENT SUMMARY:Disappearing track searches at LHC and future colliders DTSTART;VALUE=DATE-TIME:20191112T023000Z DTEND;VALUE=DATE-TIME:20191112T030000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1664@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ryu Sawada (U. Tokyo)\nThe neutral wino and the ligh test neutral higgsino are dark-matter candidates. If those are the lightes t SUSY particles\, the lightest chargino can be long-lived and can travel macroscopic distances then decay in detectors. In such scenarios\, dark ma tter particles can be searched for using a "disappearing track" signature. Such searches have been done at the LHC giving lower limits on their mass es. Much higher sensitivities are expected in future analyses at the LHC a nd at future colliders. With an optimal detector layout at the Future Circ ular Collider\, the sensitivity can cover the entire mass range compatible to the thermal relic abundance.\n\nhttps://indico.icrr.u-tokyo.ac.jp/even t/259/contributions/1664/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1664/ END:VEVENT BEGIN:VEVENT SUMMARY:N-body self-consistent stars-halo modelling of the Fornax dwarf ga laxy DTSTART;VALUE=DATE-TIME:20191112T072500Z DTEND;VALUE=DATE-TIME:20191112T074500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1557@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Galina Shchelkanova (NRC "Kurchatov institute" - ITE P)\nWe present nearly self-consistent stellar-halo models of the dwarf sph eroidal Fornax galaxy the satellite of the Milky Way galaxy. Such galaxies are dark matter dominated objects with almost no gas in them so they are excellent objects for N-body modelling that takes into account visible and dark matter(DM) halo components. Three models are self-consistent realiza tions containing a truncated King or Plummer models bulge (it stands for t he stellar component of the galaxy) and the lowered Evans dark halo model. These components are given by the distribution functions which are the fu nctions of $E$ and $L_z$ only. And four models with the King and Plummer v isible components are made by the AGAMA code based on the calculation of o rbits. To guess the parameters which make the N-body models close to the v isible object we use hydrodynamic stellar-dark model of the Fornax galaxy taking into account the velocity anisotropy parameter. The AGAMA models sh ow better agreement of the resulting velocity dispersion profiles with the observed data. We also traced the evolution of all these models and found them rather stable during several typical dynamical times.\n\nhttps://ind ico.icrr.u-tokyo.ac.jp/event/259/contributions/1557/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1557/ END:VEVENT BEGIN:VEVENT SUMMARY:Propagation processes of cosmic rays DTSTART;VALUE=DATE-TIME:20191113T050000Z DTEND;VALUE=DATE-TIME:20191113T053000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1574@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yutaka Ohira (The university of Tokyo)\nIn this talk \, I'll review recent theoretical studies and observational results about propagation processes of cosmic rays in our galaxy.\n\nhttps://indico.icrr .u-tokyo.ac.jp/event/259/contributions/1574/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1574/ END:VEVENT BEGIN:VEVENT SUMMARY:Wino theory and future prospects DTSTART;VALUE=DATE-TIME:20191111T044500Z DTEND;VALUE=DATE-TIME:20191111T051500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1573@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Satoshi Shirai ()\nWino is one of the most attractiv e candidates of the dark matter.\nThe Wino is a natural prediction of SUSY models and provides very rich signatures in collider\, direct and indirec t search for the dark matter.\nI will talk about the current experimental and theoretical status of the Wino dark matter and the future prospects.\n \nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1573/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1573/ END:VEVENT BEGIN:VEVENT SUMMARY:SMILE project: all-sky MeV gamma-ray observation and dark matter s urvey DTSTART;VALUE=DATE-TIME:20191112T080000Z DTEND;VALUE=DATE-TIME:20191112T082000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1554@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yuta Nakamura (Kyoto University)\nIn the MeV gamma-r ay band\, the observed Galactic diffuse gamma-rays has the excessive compo nent cannot be explained by the current standard model of the Galaxy. This excess might be gamma-rays due to annihilation of MeV scale WIMP dark mat ter or evaporations of primordial black holes. The MeV band has the advant age over the GeV band because there is less diffuse gamma-ray background d ue to no $\\pi ^0$ bump.\nIn 2018 April 7\, we carried out the campaign\, sub-MeV and MeV gamma-ray imaging loaded-on balloon experiment 2+ (SMILE-2 +)\, in order to demonstrate the imaging performance of the gaseous electr on tracking Compton camera (ETCC). Unlike conventional Compton cameras suc h as COMPTEL\, ETCC uniquely reconstructs the directions of gamma-rays and realizes the noiseless gamma-ray observation even in the space environmen t by the particle identification and Compton kinematical test. This detect or has the energy range from $200\\\,\\mathrm{keV}$ to $5\\\,\\mathrm{MeV} $ and the wide field of view ($3\\\,\\mathrm{str}$). We observed the Gala ctic center for 8 hours and detect it with the significances of $5\\\,\\si gma$ ($511\\\,\\mathrm{keV}$) and $10\\\,\\sigma$ (continuum). The sensiti vity of the satellite with ETCC will reach $1\\\,\\mathrm{mCrab}$ ($10^6\\ \,\\mathrm{sec}$\, $3\\\,\\sigma$) and the HPR of its PSF will be $5\\\,\\ mathrm{degree}$.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributi ons/1554/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1554/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining Secluded Dark Matter Scenarios with HAWC DTSTART;VALUE=DATE-TIME:20191113T071000Z DTEND;VALUE=DATE-TIME:20191113T073000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1558@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sergio Hernandez Cadena (Instituto de Física\, UNAM )\nIt is possible that DM particles are secluded to their own dark sector\ , where the interactions are carried by one or several dark mediators. If this dark sector exists\, DM particles do not couple directly to the stand ard model (SM) particles\, as in the case of WIMP scenarios. However\, ind irect DM searches are still possible if we assume that dark mediators are coupled to SM particles through a kinetic mixing parameter. The HAWC Obser vatory is a wide-field-of-view gamma-ray experiment with a high duty cycle (>95%) and looking for gamma rays with energies between 1 and 100 TeV. So \, for secluded DM candidates in the TeV range\, the HAWC Observatory is able to explore and constrain the parameter space of dark sector scenarios by searching for gamma-ray signals of dark mediator decays in nearby astr ophysical targets. Here\, we present preliminary results of these indirect searches using HAWC data.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/ contributions/1558/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1558/ END:VEVENT BEGIN:VEVENT SUMMARY:Particle and halo model uncertainties in direct dark matter detect ion DTSTART;VALUE=DATE-TIME:20191111T064500Z DTEND;VALUE=DATE-TIME:20191111T071500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1659@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Graciela Gelmini (UCLA)\nAfter briefly reviewing the WIMP status as dark matter (DM) candidate\, I will mention how the impact of the neutrino floor on the direct detection (DD) reach depends on the type of WIMP-nucleus interaction and mass\, and then how a DD signal woul d translate into properties of the DM local velocity distribution\, allowi ng to compare different DD data sets through these predictions (in a “ halo-independent” analysis complementary to the usual halo-dependent met hod).\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1659/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1659/ END:VEVENT BEGIN:VEVENT SUMMARY:Rapid bound-state formation of Dark Matter in the Early Universe DTSTART;VALUE=DATE-TIME:20191112T064500Z DTEND;VALUE=DATE-TIME:20191112T070500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1553@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Tobias Binder ()\nThe thermal decoupling description of multi-TeV scale dark matter (DM) and co-annihilating partners is recon sidered. In such a high-mass region\, even the electroweak force carriers could act as long-range forces\, leading to the existence of meta-stable D M bound states. The formation and subsequent decay of the latter further d epletes the relic density on top of the Sommerfeld enhancement\, allowing for heavier DM masses. So far\, only the on-shell mediator emission (W\, Z \, H\, g\, photon or exotic) was considered as the formation process of th e bound states. In this talk\, I show that bound-state formation via bath particle scattering\, i.e. the mediator instead in the t-channel and conne cted to the SM plasma\, can be the dominant conversion process. For a simp lified setup we find that bound-state formation via bath particle scatteri ng exceeds the single mediator bound-state formation cross-section by seve ral orders of magnitude at the freeze-out temperature. The implications of these findings are that bound-state effects become more pronounced during chemical decoupling and consequently DM could be heavier than previously expected\, eventually informing indirect and collider searches.\n\nhttps:/ /indico.icrr.u-tokyo.ac.jp/event/259/contributions/1553/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1553/ END:VEVENT BEGIN:VEVENT SUMMARY:J-factor estimation of Draco\, Sculptor and Ursa Minor dSphs with the member/foreground mixture model DTSTART;VALUE=DATE-TIME:20191112T030900Z DTEND;VALUE=DATE-TIME:20191112T031000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1559@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shunichi Horigome (Kavli IPMU)\nDwarf spheroidal gal axies (dSphs) are promising targets for indirect detection experiments sin ce they contain a large amount of dark matter (DM). For the precise calcul ation of the amount of annihilation signal flux from dSph\, we must know t he DM mass density distribution of target dSphs\, estimated from the obser vation of the stellar motion.\nIn the DM profile estimation\, the major un certainty of DM profile comes from the foreground contamination of the Mil ky Way stars in front of dSph. In the conventional analyses\, the contamin ated stars are partially removed based on their membership probability est imated by a clustering technique called EM algorithm. However\, even if we use this technique\, some contaminated stars still remain in the data set \, which leads to the incorrect sensitivity of indirect detection experime nts.\nIn this work\, we adopt a new method to deal with the contamination effect based on the mixture model of the dSph member and foreground stars. \nUsing this method\, we estimate the DM density profile of Draco\, Sculpt or\, and Ursa Minor\, the top three DM rich dSphs\, with reliable errorbar s properly including the uncertainty of the contamination effect.\n\nhttps ://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1559/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1559/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamics of the cusp-to-core transformation in the cold dark matte r halos DTSTART;VALUE=DATE-TIME:20191112T031800Z DTEND;VALUE=DATE-TIME:20191112T031900Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1569@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kazuki Kato (University of Tsukuba)\nThe lambda cold dark matter model is the standard paradigm of structure formation in the universe. However\, there is a discrepancy known as the “cusp–core pro blem” in the mass–density distribution of a dark matter halo (DMH) bet ween theory and observation. We investigate the dynamical response of DMHs to recurrent starbursts on the formation of less massive galaxies to solv e this issue. In the early epoch of the galaxy formation\, the cycle of ex pansion and contraction of the interstellar gas driven by the stellar feed backs leads to a recursive change in the gravitational potential of the ga s. The eccentricity of the DMH particles around the centre becomes large b y this change. Then\, the system expands\, and the core scale increases du e to the oscillation process. Finally\, the DMH then reaches the new quasi -equilibrium state. Our simulation shows that the energy transport by the overtone components contained in the periodic oscillation of the potential change strongly influences the inner slope of the mass–density profile of the DMH. We conclude that the resonance between DMH particles and the d ensity wave excited by the oscillating potential plays a crucial role in u nderstanding the physical mechanism of the cusp–to–core transition of DMHs.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1569/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1569/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of new photo-detectors for the future dark matter experiments with liquid xenon DTSTART;VALUE=DATE-TIME:20191112T032100Z DTEND;VALUE=DATE-TIME:20191112T032200Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1571@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kosuke Ozaki (Nagoya University)\nIn the last three decades\, numerous terrestrial experiments have been built to detect the f aint interactions between WIMP dark matter and ordinary matter. Among them \, experiments using dual-phase xenon time projection chambers (TPCs) are leading the search especially for high mass WIMPs. In these experiments\, photomultipliers (PMTs) are used to detect the prompt primary scintillatio n and secondary electro-luminescence of ionized electrons. However\, PMTs have several important shortcomings: the residual radioactivity levels\, c ost\, bulkiness\, and stability at cryogenic conditions. Therefore\, sever al alternative technologies are under consideration toward the future dark matter experiments using ~50 tons of liquid xenon (LXe). One of the such technologies is silicon photomultipliers (SiPMs). SiPM has very low radioa ctivity\, compact geometry\, low operation voltages and reasonable photo-d etection efficiency for VUV light. However\, current SiPM still has ~two o rder of magnitude higher dark count rate compared with PMT\, which signifi cantly increases accidental coincidence background. In order to solve thes e problems\, we are currently developing a new SiPM with the help of Hamam atsu and FBK. In this poster\, we will report the current status of the p erformance measurements of the Hamamatsu VUV4 SiPMs (3mm×3mm)\, new SiPMs with less dark count and FBK VUV SiPMs (6mm×6mm).\n\nhttps://indico.icrr .u-tokyo.ac.jp/event/259/contributions/1571/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1571/ END:VEVENT BEGIN:VEVENT SUMMARY:Paradigms and Scenarios for the Dark Matter DTSTART;VALUE=DATE-TIME:20191112T043000Z DTEND;VALUE=DATE-TIME:20191112T050000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1668@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Paolo Salucci (SISSA)\nThe deeper we go into the kno wledge of the dark component that embeds the stellar component of galaxies \, the more we realize the profound interconnection which is present betw een the two of them. The scaling laws among the structural properties of t he dark and luminous matter in disc systems are too complex to be arisen b y two inert components that just share the same gravitational field. This brings us to critically focus on the 30 years old paradigm\, that\, resti ng on a priori knowledge of the nature of dark matter (DM)\, has led us to a restricted number of scenarios for dark matter. The galaxies's structur al properties show strong indications that the dark and luminous component s have interacted in a direct way over the Hubble time. We propose to brea k the dark matter mystery by taking a step back and start following a new paradigm: the Nature of dark matter can be guessed/derived only from deep analyzing the properties of the dark and luminous mass distribution at gal actic scales. As first result in Spirals\, the quantity $\\rho_{DM}(r\,L\, R_D) \\rho_\\star (r\,L\,R_D)$\, the (macroscopic) kernel of a dark-to-lum inous interaction\, shows specific properties that call for a collisional nature of the dark particle.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/25 9/contributions/1668/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1668/ END:VEVENT BEGIN:VEVENT SUMMARY:Closing remarks DTSTART;VALUE=DATE-TIME:20191113T073000Z DTEND;VALUE=DATE-TIME:20191113T074000Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1670@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ryu Sawada (U. Tokyo)\nhttps://indico.icrr.u-tokyo.a c.jp/event/259/contributions/1670/ LOCATION:The University of Tokyo\, Kashiwa Campus URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1670/ END:VEVENT BEGIN:VEVENT SUMMARY:Opening remarks DTSTART;VALUE=DATE-TIME:20191111T033000Z DTEND;VALUE=DATE-TIME:20191111T034500Z DTSTAMP;VALUE=DATE-TIME:20260509T164708Z UID:indico-contribution-259-1669@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Masahiro Teshima ()\nhttps://indico.icrr.u-tokyo.ac. jp/event/259/contributions/1669/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1669/ END:VEVENT END:VCALENDAR