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:20250110T182817Z UID:indico-contribution-259-36@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Teshima\, Masahiro (ICRR\, the University of Tokyo)\ nhttps://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:20250110T182817Z UID:indico-contribution-259-46@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Iocco\, Fabio (Imperial College / Università di Nap oli)\nThe distribution of Dark Matter in galaxies is one remarkable output of structure formation in a cosmological context\, and an important input for the searches of the nature of Dark Matter. In this talk I will presen t the results of recent\, fully data-driven analysis of the determination of the Dark Matter content and distribution in the Milky Way. \nI will als o highlight the current uncertainties of empirical (and astrophysical) nat ure\, and how they affect the interpretation of direct and indirect search es\, and eventually the searches for the very nature of the Dark Matter.\n \nhttps://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:20250110T182817Z UID:indico-contribution-259-27@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Albert\, Andrea (Los Alamos National Lab)\nEvidence suggests ~85% of the mass in the Universe is dark matter (DM). Several pro mising DM theories predict that it is a fundamental particle. The most fam ous of which is the Weakly Interacting Massive Particle (WIMP). WIMPs that annihilate at a weak-scale cross section that were in thermal equilibrium in the Universe produce the observed DM abundance today. DM particles are theorized to interact and produce standard model particles\, like gamma r ays. So far\, no definitive gamma-ray signal has been detected\, but curre nt experiments have started excluding several thermal WIMP models. I will discuss the current status of DM searches with gamma-ray observatories lik e the Fermi LAT and HAWC. I will also discuss how both future analysis wit h current observatories and future observatories like CTA and SWGO will pr obe thermal WIMP models for masses from 5 GeV to ~100 TeV.\n\nhttps://indi co.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:20250110T182817Z UID:indico-contribution-259-25@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Moroi\, Takeo ()\nI will discuss phenomenology of Hi ggsino dark matter. First\, I will briefly overview theoretical issues rel ated to Higgsino dark matter. Then\, I will summarize present status and future prospects of Higgsino dark matter search using colliers and direct detection experiments.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/cont ributions/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:20250110T182817Z UID:indico-contribution-259-58@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Naka\, Tatsuhiro (Toho University )\nIn the standard methodology for the WIMP search detect recoiled nuclei due to elastic sca ttering with that\, the neutrino should become background to be not able t o avoid. If not detect significant signals or just few events detected bef ore neutrino floor\, more reliable search to confirm those are the signals due to WIMP or new information to distinguish the WIMP signals from neutr ino backgrounds will be required. For example\, one of the promising infor mation in current studies is to use “direction” or signals attributed to that. In this talk\, I will report current experimental approach about direction sensitive search\, and discuss about the issues to go beyond ne utrino floor.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions /1534/ 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:20250110T182817Z UID:indico-contribution-259-47@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Scholberg\, Kate (Duke University)\nWIMP detectors i n the 2020's will approach the sensitivity at which\nscatters of natural n eutrinos will create a background sufficient to\nobscure the WIMP recoil s ignal. This is the so-called "Neutrino\nFloor". This talk will discuss t he nature of the neutrino floor and\nthe motivations to get to it\, and to potentially go beyond it.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/ contributions/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:20250110T182817Z UID:indico-contribution-259-55@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Asaoka\, Yoichi (WISE\, Waseda University)\nThe CALo rimetric Electron Telescope (CALET)\, which is currently conducting direct cosmic-ray observations onboard the International Space Station (ISS)\, u ses an all-calorimetric instrument with total vertical thickness of 30 rad iation lengths and fine imaging capability. The instrument is optimized fo r cosmic-ray electron measurements by achieving large proton rejection and excellent energy resolution well into the TeV energy region. In addition\ , very wide dynamic range of energy measurements and absolute charge ident ification capability of the instrument enable us to measure proton and nuc lei spectra as well as electron and gamma-ray spectra. The CALET mission g oals include the investigation of acceleration and propagation of galactic cosmic rays\, of possible nearby sources\, and of potential signature of dark matter. Since the start of observation in October 2015\, smooth and c ontinuous operations have taken place. In this talk\, we will give a brief summary of the recent results obtained with CALET and discuss about the d ark matter search using the CALET all-electron spectrum.\n\nhttps://indico .icrr.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:20250110T182817Z UID:indico-contribution-259-64@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hiroshima\, Nagisa (Riken)\nDwarf spheroidal galaxie s (dSph) are good targets to search for dark matter annihilation signals t hrough gamma-ray observations. Currently\, the most strong constraints on the cross-section at mDM\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/co ntributions/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:20250110T182817Z UID:indico-contribution-259-65@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hütten\, Moritz (Max Planck Institute for Physics)\ nThe Cherenkov Telescope Array (CTA) represents the next-generation ground -based gamma-ray observatory in the energy range between 30 GeV and 300 Te V. It will open the window to gamma-ray searches for annihilation or decay of heavy (TeV) Weakly Interacting Massive Particles (WIMPs) in astrophysi cal Dark Matter (DM) budgets with unprecedented sensitivity. In this talk\ , I will review the current prospects for WIMP searches with CTA in dwarf spheroidal galaxies orbiting our Milky Way\, enhanced annihilation in clos e-by dark halos\, and galaxy clusters of the local Universe. I will also o utline the current knowledge of the DM targets and foreseen observation st rategies\, on which the success of the searches crucially depends.\n\nhttp s://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:20250110T182817Z UID:indico-contribution-259-23@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Wada on behalf of the GAPS collaboration\, Takuya (A oyama Gakuin University)\nThe General Antiparticle Spectrometer (GAPS) is an international balloon-borne project for indirect dark matter (DM) searc hes that investigates low-energy antinuclei in cosmic-ray\, especially und iscovered antideuterons. Cosmic-ray antideuterons can be produced by self- annihilation or decay of WIMP DM. The flux of DM-originated antideuterons can be orders of magnitude higher than that of the secondary (or backgroun d) component. Therefore\, antideuterons are considered to be a background- free probe to search for DM. GAPS uses a unique concept to identify antinu clei by applying the physics of exotic atom creation and decay. The GAPS i nstrument is composed of lithium-drifted silicon (Si(Li)) detectors surrou nded by a double-layered plastic scintillation-counter time-of-flight syst em. An incoming antinucleus forms an exotic atom in the Si(Li) detectors. Through the deexcitation and nuclear annihilation processes of the exotic atom\, characteristic X-rays and charged particles are emitted. By detecti ng and tracking those X-rays and particles\, GAPS has strong particle iden tification\, resulting in a high sensitivity for rare antinuclei. The firs t GAPS flight is scheduled for late 2021. We are currently developing all different subsystems\, such as the Si(Li) tracker\, time-of-flight system\ , cooling system\, and detailed simulation code of the instrument. We will report the scientific motivation\, detection concept\, and development st atus of GAPS.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions /1540/ 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:20250110T182817Z UID:indico-contribution-259-51@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hashimoto\, Daiki (Nagoya University)\nIn the contex t of the high energy astrophysics\, the nature of dark matter annihilation expected to emit gamma rays have been probed utilizing observed gamma-ray flux in a direction of a high matter-density region. Recently\, some stud ies have been performed with nearby dwarf galaxies or the Galactic center and then the cross section for dark matter annihilation have been constrai ned.\nIn our study\, we focus on Low Surface Brightness Galaxies (LSBGs) c ataloged by the observation data of Hyper Suprime-Cam (HSC). LSBGs can be used as novel tracers of dark matter annihilation signals because of being more massive than dwarf spheroids and having less astronomical contaminat ions due to relatively quiescent states of those\, which can perform robus ter research for dark matter annihilation signals. \nWe model the gamma-ra y flux from LSBGs using the 8 HSC-LSBGs measured each redshift\, and compe ring with observed gamma-ray flux by Fermi Large Area Telescope\, provide the upper limit of the cross section for dark matter annihilation. \nMoreo ver\, we prospect the future constraint with soon-to-be-detected LSBGs by future observation. In our poster presentation\, we report our method and results\, and also discuss the prospects for the future constraint.\n\nhtt ps://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:20250110T182817Z UID:indico-contribution-259-68@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: O'Hare\, Ciaran ()\nI will explain why the neutrino floor exists from a statistical perspective and then discuss what kind of information we need from an experimental search to be able to subtract the neutrino background.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contr ibutions/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:20250110T182817Z UID:indico-contribution-259-26@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kerszberg\, Daniel (IFAE-BIST)\nThe next generation of gamma-ray experiments are expected to improve significantly the current results in the search for Dark Matter (DM). Before these next-generation instruments start operating at their nominal design\, one possibility to i mprove the current results is to combine data from existing experiments. T his technique allows to increase energy coverage by combining data from i nstruments with better sensitivity in different energy ranges and also to maximize the sensitivity by combining individual data sets from all the ex periments for which the energy ranges overlap. We will report on such an i nitiative aiming at combining data from dwarf spheroidal galaxies (dSphs)  from the Fermi-LAT\, HAWC\, H.E.S.S.\, MAGIC\, and VERITAS experiments. Being among the most DM dominated objects with negligible expected astroph ysical gamma-ray emission\, dSphs are ideal targets for DM indirect search es and thus will be also primary targets for the next generation of experi ments. Preliminary results of the combination constraining the DM anni hilation cross section will be presented spanning a range of DM masses from 10 GeV to 100 TeV. The potential of extending this analysis framewor k to more experiments as well as to future experiments will also be discus sed.\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:20250110T182817Z UID:indico-contribution-259-24@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Xie\, Pengwei (Tsung-Dao Lee Institute)\nPandaX is a dark matter search experiment located at China Jin Ping Underground Lab u sing xenon time projection chamber.\nIn this talk\, I will present the lat est result from PandaX-II experiment and the current status of PandaX-4T e xperiment.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/15 52/ 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:20250110T182817Z UID:indico-contribution-259-20@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yanagi\, Keisuke (University of Tokyo)\nWIMP DMs in the Universe accumulate in neutron stars (NSs) through their interactions with nucleons. It has been known that their annihilation inside the NS cor e 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 the measurement of NS surface temperature can be used as a new probe of W IMP DMs. Because of the strong gravity of NSs\, DM heating has several adv antages compared to the direct detection experiments on the earth.\n\nDesp ite such advantages\, the background on the DM heating is rarely discussed in the particle physics community. In particular\, the rotochemical heati ng\, internal heating caused by the out-of-equilibrium beta reactions in a NS\, should be considered because it does not assume any exotic physics. In fact\, if the rotochemical heating operates in a NS\, it may conceal th e DM heating effects.\n\nIn this work\, we reevaluate the significance of the 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 ordi nary pulsars\, and discuss what is necessary to confirm the evidence for t he DM heating.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contribution s/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:20250110T182817Z UID:indico-contribution-259-56@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Inada\, Tomohiro (ICRR\, UTokyo)\nIn this talk\, we will present a status report on the search for dark matter spectral lines around the Galactic centre (GC) with the MAGIC telescope system located on the Canary island of La Palma\, Spain. MAGIC is sensitive to gamma rays f rom 50 GeV to 50 TeV. So far\, MAGIC has produced groundbreaking results i n the field of indirect DM searches observing a variety of targets\, such as the Galactic halo\, dwarf spheroidal galaxies and clusters of galaxies. We are now aiming to add the GC region as an observational target to sear ch for line signatures from DM annihilation. MAGIC has observed the GC reg ion for hundreds of hours at high zenith angles\, at which the collection area for TeV gamma rays is significantly increased. This allows us to prob e promising SUSY models of heavy DM candidates\, and to set limits on the DM annihilation cross section competitive to those obtained from observati ons in the Southern hemisphere. We will also discuss how we exploit the da ta 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:20250110T182817Z UID:indico-contribution-259-35@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Seto\, Osamu (Hokkaido University)\nWe propose model s of a thermal relic DM with the present annihilation cross-section being very suppressed. This property can be realized in an extra U(1) gauge inte racting 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 regions. We also discuss various implication to future DM detection exper iments\, the DM interpretation of the gamma ray excess in the globular clu ster 47 Tucanae\, the muon anomalous magnetic moment\, the Hubble Tension and others.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1 561/ 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:20250110T182817Z UID:indico-contribution-259-63@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Macias\, Oscar ()\nWe set conservative constraints o n decaying dark matter particles with masses spanning a very wide range ($ 10^4-10^{16}$ GeV). For this we use multimessenger observations of cosmic- ray (CR) protons/antiprotons\, electrons/positrons\, neutrinos/antineutrin os and gamma rays. Focusing on decays into the $b\\bar{b}$ channel\, we si mulate the spectra of dark matter yields by using the Dokshitzer-Gribov-Li patov-Altarelli-Parisi equations and the Pythia package. We then propagate the CRs of dark matter origin till Earth by using the state-of-the-art nu merical frameworks CRPropa\, GALPROP and HelMod for the solution of the CR transport equation in the extragalactic\, Galactic region and the heliosp here\, respectively. Conservative limits are obtained by requiring that th e predicted dark matter spectra at Earth be less than the observed CR spec tra. Overall\, we exclude dark matter lifetimes of $10^{28}$ s or shorter for all the masses investigated in this work. The most stringent constrain ts reach $10^{30}$ s for very heavy dark matter particles with masses in t he range $10^{11}−10^{14}$ GeV.\n\nhttps://indico.icrr.u-tokyo.ac.jp/eve nt/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:20250110T182817Z UID:indico-contribution-259-69@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Zaharijas\, Gabrijela (University of Nova Gorica)\nH igh-energy gamma rays are among the most promising tools to constrain or r eveal the nature of dark matter (DM)\, in particular the Weakly Interactin g Massive Particles models. The Cherenkov Telescope Array (CTA) is well i nto its pre-construction phase and will soon probe the high-energy gamma-r ay sky in the 20 GeV - 300 TeV energy range. Thanks to its improved energ y and angular resolutions as well as significantly larger effective area\, the CTA will probe a parameter space of heavier dark matter (above 100 Ge V)\, with unprecedented sensitivity\, reaching the DM thermal annihilation rate at the TeV regime. \n\nThis talk will summarise the planned DM searc h strategies with CTA\, focusing on the signal of DM in the centre of our Galaxy. As observed with the Fermi LAT at lower energies\, this region exh ibits complex large-scale gamma-ray emission and the CTA is expected to be the first ground based observatory able to detect it. In this talk we rep ort on the collaboration effort to study the impact of extended astrophysi cal backgrounds on DM search\, based on the astrophysical emission observe d with the Fermi LAT at lower energies and to suggest the promising data a nalysis and observational strategies for the upcoming CTA data.\n\nhttps:/ /indico.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:20250110T182817Z UID:indico-contribution-259-72@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Terashi\, Koji (University of Tokyo\, ICEPP)\nThe ex istence of dark matter (DM) is a cornerstone of extensive search programs at colliders. The ATLAS and CMS experiments at the LHC have performed a wi de range of searches for DM particles predicted in SUSY\, in particular fo r the lightest neutralino in R-parity conserving scenarios. The event topo logy and final states containing the neutralino DMs depend on the mass eig enstates of the gauginos and their compositions. In this talk\, I will pre sent the current status of neutralino DM searches at the LHC\, putting som e emphasis on DMs with Wino and Higgsino components. Prospects for the Win o/Higgsino DM searches at future colliders are also discussed.\n\nhttps:// indico.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:20250110T182817Z UID:indico-contribution-259-70@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Pani\, Priscilla (DESY)\nThis talk aims to provide a n overview of the theoretical framework\, the search strategies and the cu rrent status of the results of Dark Matter searches at the LHC. The focus will be restricted to mediator-based Dark Matter models (non-SUSY). Exper imental analyses and results will be presented on a selection of the model s\, using up to 150 ifb of $\\sqrt{s} = 13$ TeV $pp$ collision data collec ted by the ATLAS and CMS experiments at the LHC.\n\nhttps://indico.icrr.u- tokyo.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:20250110T182817Z UID:indico-contribution-259-73@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Matsumoto\, Shigeki (Kavli IPMU)\nDark matter (DM) p roblem 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 cert ain diversity of research is thus required to solve the DM problem and man y DM candidates are now being proposed and discussed. Among various candid ates\, TeV-scale thermal DM candidates now attract attention as they are p redicted by new physics models intensively discussed after the Higgs disco very at LHC and they also have a certain reason why current DM search expe riments/observations do not detect their signals. I will summarize above i nteresting 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:20250110T182817Z UID:indico-contribution-259-71@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Mori\, Masao (University of Tsukuba)\nCold dark matt er (CDM) cosmology is the standard paradigm of structure formation in the universe. However\, it has several unsolved severe problems. The missing s atellites problem refers to the overabundance of theoretically predicted C DM subhalos compared to observed satellite galaxies in the Local Group. Th e most popular interpretation is that the small dark matter halos have ext remely inefficient star-forming history. In this study\, we investigate th e possible existence of the stellar deficient CDM halos using large scale numerical simulations for galaxy collisions between a CDM subhalo and a dw arf galaxy in the Local Group.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 259/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:20250110T182817Z UID:indico-contribution-259-67@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Galbiati\, Cristiano (Princeton University)\nExperim enters from four different argon dark matter searches have joined their fo rces 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 scale of a few tens of tonnes is the DarkSide-20k experiment\, a 20-tonne fiducial volume dual-phase TPC to be operated at LNGS with an underground argon fill\, designed to collect an exposure of 100 tonne×years\, comple tely free of neutron-induced nuclear recoil background and all electron re coil background. DarkSide-20k is set to start operating by 2023 and will have sensitivity to WIMP-nucleon spin-independent cross sections of 7.4×1 0−48 cm2 for WIMPs of 1 TeV/c2 mass\, to be achieved during a 10 year ru n with an exposure of 200 tonne×years. DarkSide-20k will explore the WIM P-nucleon cross-section down to the edge of the ’neutrino floor’\, whe re coherent neutrino-nucleus scattering from environmental neutrinos induc e nuclear recoils in the detector.\n A second step in the program is the c onstruction and operation of Argo\, a detector with a fiducial mass of a f ew hundred tonnes\, capable of collecting an exposure of several thousands of tonne×years\, completely free of all backgrounds on top of CNNS\, sla ted for a 2030 start.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contr ibutions/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:20250110T182817Z UID:indico-contribution-259-80@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: López-Coto\, Rubén (INFN Padova)\nThe origin and p ropagation of cosmic rays is one of the most important questions in astrop article physics nowadays. To perform Indirect searches of Dark Matter sear ching for their products in the local cosmic ray spectra\, we first need t o comprehend what is the background coming from astrophysical sources. We can only model this background by achieving a deep understanding of cosmic ray propagation. Although the transport of these cosmic rays through the galaxy make them lose the information about their origin due to interstell ar magnetic fields\, we can directly study the properties of their propaga tion using gamma rays. In this talk\, I will give a review of current meas urements of magnetic fields and cosmic ray propagation parameters using ga mma rays.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/259/contributions/166 1/ 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:20250110T182817Z UID:indico-contribution-259-76@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Yamashita\, Masaki (ICRR\, The University of Tokyo)\ nDirect dark matter searches have been conducted for more than 30 years in the underground laboratories to look for signals via dark matter-nucleus elastic scattering of its target materials. Weakly interacting massive pa rticles as dark matter candidates arise naturally in various theories\, such as Supersymmetry\, Extra Dimensions. WIMPs interact through the wea k interaction and can efficiently transfer kinetic energy by the scatterin g from atomic nuclei\, the WIMP model can be tested by searching for nucle ar recoils in a sensitive\, low-radioactivity detector. This review talk will focus on a liquid xenon base detectors among those searches which in clude 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:20250110T182817Z UID:indico-contribution-259-82@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sawada\, Ryu (U. Tokyo)\nThe neutral wino and the li ghtest neutral higgsino are dark-matter candidates. If those are the light est SUSY particles\, the lightest chargino can be long-lived and can trave l macroscopic distances then decay in detectors. In such scenarios\, dark matter particles can be searched for using a "disappearing track" signatur e. Such searches have been done at the LHC giving lower limits on their ma sses. Much higher sensitivities are expected in future analyses at the LHC and at future colliders. With an optimal detector layout at the Future Ci rcular Collider\, the sensitivity can cover the entire mass range compatib le to the thermal relic abundance.\n\nhttps://indico.icrr.u-tokyo.ac.jp/ev ent/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:20250110T182817Z UID:indico-contribution-259-21@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shchelkanova\, Galina (NRC "Kurchatov institute" - I TEP)\nWe present nearly self-consistent stellar-halo models of the dwarf s pheroidal Fornax galaxy the satellite of the Milky Way galaxy. Such galaxi es are dark matter dominated objects with almost no gas in them so they ar e excellent objects for N-body modelling that takes into account visible a nd dark matter(DM) halo components. Three models are self-consistent reali zations containing a truncated King or Plummer models bulge (it stands for the stellar component of the galaxy) and the lowered Evans dark halo mode l. These components are given by the distribution functions which are the functions of $E$ and $L_z$ only. And four models with the King and Plummer visible components are made by the AGAMA code based on the calculation of orbits. To guess the parameters which make the N-body models close to the visible object we use hydrodynamic stellar-dark model of the Fornax galax y taking into account the velocity anisotropy parameter. The AGAMA models show better agreement of the resulting velocity dispersion profiles with t he observed data. We also traced the evolution of all these models and fou nd them rather stable during several typical dynamical times.\n\nhttps://i ndico.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:20250110T182817Z UID:indico-contribution-259-78@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ohira\, Yutaka (The university of Tokyo)\nIn this ta lk\, I'll review recent theoretical studies and observational results abou t propagation processes of cosmic rays in our galaxy.\n\nhttps://indico.ic rr.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:20250110T182817Z UID:indico-contribution-259-77@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Shirai\, Satoshi ()\nWino is one of the most attract ive candidates of the dark matter.\nThe Wino is a natural prediction of SU SY models and provides very rich signatures in collider\, direct and indir ect search for the dark matter.\nI will talk about the current experimenta l 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:20250110T182817Z UID:indico-contribution-259-50@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Nakamura\, Yuta (Kyoto University)\nIn the MeV gamma -ray band\, the observed Galactic diffuse gamma-rays has the excessive com ponent cannot be explained by the current standard model of the Galaxy. Th is excess might be gamma-rays due to annihilation of MeV scale WIMP dark m atter or evaporations of primordial black holes. The MeV band has the adva ntage over the GeV band because there is less diffuse gamma-ray background due 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 elec tron tracking Compton camera (ETCC). Unlike conventional Compton cameras s uch as COMPTEL\, ETCC uniquely reconstructs the directions of gamma-rays a nd realizes the noiseless gamma-ray observation even in the space environm ent by the particle identification and Compton kinematical test. This dete ctor has the energy range from $200\\\,\\mathrm{keV}$ to $5\\\,\\mathrm{Me V}$ and the wide field of view ($3\\\,\\mathrm{str}$). We observed the Ga lactic center for 8 hours and detect it with the significances of $5\\\,\\ sigma$ ($511\\\,\\mathrm{keV}$) and $10\\\,\\sigma$ (continuum). The sensi tivity 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/contribu tions/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:20250110T182817Z UID:indico-contribution-259-54@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Hernandez Cadena\, Sergio (Instituto de Física\, UN AM)\nIt is possible that DM particles are secluded to their own dark secto r\, where the interactions are carried by one or several dark mediators. I f this dark sector exists\, DM particles do not couple directly to the sta ndard model (SM) particles\, as in the case of WIMP scenarios. However\, i ndirect DM searches are still possible if we assume that dark mediators ar e coupled to SM particles through a kinetic mixing parameter. The HAWC Obs ervatory is a wide-field-of-view gamma-ray experiment with a high duty cyc le (>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 i s able to explore and constrain the parameter space of dark sector scenari os by searching for gamma-ray signals of dark mediator decays in nearby as trophysical targets. Here\, we present preliminary results of these indire ct searches using HAWC data.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/25 9/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:20250110T182817Z UID:indico-contribution-259-79@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Gelmini\, Graciela (UCLA)\nAfter briefly reviewing t he WIMP status as dark matter (DM) candidate\, I will mention how the impa ct of the neutrino floor on the direct detection (DD) reach depends on th e type of WIMP-nucleus interaction and mass\, and then how a DD signal wo uld translate into properties of the DM local velocity distribution\, allo wing to compare different DD data sets through these predictions (in a “halo-independent” analysis complementary to the usual halo-dependent method).\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:20250110T182817Z UID:indico-contribution-259-34@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Binder\, Tobias ()\nThe thermal decoupling descripti on of multi-TeV scale dark matter (DM) and co-annihilating partners is rec onsidered. In such a high-mass region\, even the electroweak force carrier s could act as long-range forces\, leading to the existence of meta-stable DM bound states. The formation and subsequent decay of the latter further depletes the relic density on top of the Sommerfeld enhancement\, allowin g 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 the bound states. In this talk\, I show that bound-state formation via bat h particle scattering\, i.e. the mediator instead in the t-channel and con nected to the SM plasma\, can be the dominant conversion process. For a si mplified setup we find that bound-state formation via bath particle scatte ring exceeds the single mediator bound-state formation cross-section by se veral orders of magnitude at the freeze-out temperature. The implications of these findings are that bound-state effects become more pronounced duri ng chemical decoupling and consequently DM could be heavier than previousl y 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:20250110T182817Z UID:indico-contribution-259-59@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Horigome\, Shunichi (Kavli IPMU)\nDwarf spheroidal g alaxies (dSphs) are promising targets for indirect detection experiments s ince they contain a large amount of dark matter (DM). For the precise calc ulation of the amount of annihilation signal flux from dSph\, we must know the DM mass density distribution of target dSphs\, estimated from the obs ervation of the stellar motion.\nIn the DM profile estimation\, the major uncertainty of DM profile comes from the foreground contamination of the M ilky Way stars in front of dSph. In the conventional analyses\, the contam inated stars are partially removed based on their membership probability e stimated by a clustering technique called EM algorithm. However\, even if we use this technique\, some contaminated stars still remain in the data s et\, which leads to the incorrect sensitivity of indirect detection experi ments.\nIn this work\, we adopt a new method to deal with the contaminatio n effect based on the mixture model of the dSph member and foreground star s.\nUsing this method\, we estimate the DM density profile of Draco\, Scul ptor\, and Ursa Minor\, the top three DM rich dSphs\, with reliable errorb ars properly including the uncertainty of the contamination effect.\n\nhtt ps://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:20250110T182817Z UID:indico-contribution-259-74@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Kato\, Kazuki (University of Tsukuba)\nThe lambda co ld dark matter model is the standard paradigm of structure formation in th e universe. However\, there is a discrepancy known as the “cusp–core p roblem” in the mass–density distribution of a dark matter halo (DMH) b etween theory and observation. We investigate the dynamical response of DM Hs to recurrent starbursts on the formation of less massive galaxies to so lve this issue. In the early epoch of the galaxy formation\, the cycle of expansion and contraction of the interstellar gas driven by the stellar fe edbacks leads to a recursive change in the gravitational potential of the gas. The eccentricity of the DMH particles around the centre becomes large by this change. Then\, the system expands\, and the core scale increases due to the oscillation process. Finally\, the DMH then reaches the new qua si-equilibrium state. Our simulation shows that the energy transport by th e overtone components contained in the periodic oscillation of the potenti al change strongly influences the inner slope of the mass–density profil e of the DMH. We conclude that the resonance between DMH particles and the density wave excited by the oscillating potential plays a crucial role in understanding the physical mechanism of the cusp–to–core transition o f 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:20250110T182817Z UID:indico-contribution-259-75@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Ozaki\, Kosuke (Nagoya University)\nIn the last thre e decades\, numerous terrestrial experiments have been built to detect the faint interactions between WIMP dark matter and ordinary matter. Among th em\, experiments using dual-phase xenon time projection chambers (TPCs) ar e leading the search especially for high mass WIMPs. In these experiments\ , photomultipliers (PMTs) are used to detect the prompt primary scintillat ion and secondary electro-luminescence of ionized electrons. However\, PMT s have several important shortcomings: the residual radioactivity levels\, cost\, bulkiness\, and stability at cryogenic conditions. Therefore\, sev eral alternative technologies are under consideration toward the future da rk matter experiments using ~50 tons of liquid xenon (LXe). One of the suc h technologies is silicon photomultipliers (SiPMs). SiPM has very low radi oactivity\, compact geometry\, low operation voltages and reasonable photo -detection efficiency for VUV light. However\, current SiPM still has ~two order of magnitude higher dark count rate compared with PMT\, which signi ficantly increases accidental coincidence background. In order to solve th ese problems\, we are currently developing a new SiPM with the help of Ham amatsu and FBK. In this poster\, we will report the current status of the performance measurements of the Hamamatsu VUV4 SiPMs (3mm×3mm)\, new SiP Ms with less dark count and FBK VUV SiPMs (6mm×6mm).\n\nhttps://indico.ic rr.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:20250110T182817Z UID:indico-contribution-259-83@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Salucci\, Paolo (SISSA)\nThe deeper we go into the k nowledge of the dark component that embeds the stellar component of galaxi es\, the more we realize the profound interconnection which is present be tween the two of them. The scaling laws among the structural properties of the dark and luminous matter in disc systems are too complex to be arisen by two inert components that just share the same gravitational field. Th is brings us to critically focus on the 30 years old paradigm\, that\, res ting 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 struct ural properties show strong indications that the dark and luminous compone nts have interacted in a direct way over the Hubble time. We propose to br eak the dark matter mystery by taking a step back and start following a ne w paradigm: the Nature of dark matter can be guessed/derived only from dee p analyzing the properties of the dark and luminous mass distribution at g alactic 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-l uminous interaction\, shows specific properties that call for a collisiona l nature of the dark particle.\n\nhttps://indico.icrr.u-tokyo.ac.jp/event/ 259/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:20250110T182817Z UID:indico-contribution-259-85@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Sawada\, Ryu (U. Tokyo)\nhttps://indico.icrr.u-tokyo .ac.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:20250110T182817Z UID:indico-contribution-259-84@indico.icrr.u-tokyo.ac.jp DESCRIPTION:Speakers: Teshima\, Masahiro ()\nhttps://indico.icrr.u-tokyo.a c.jp/event/259/contributions/1669/ LOCATION: URL:https://indico.icrr.u-tokyo.ac.jp/event/259/contributions/1669/ END:VEVENT END:VCALENDAR