BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN 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:20250110T182630Z UID:indico-contribution-462-26@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: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:20250110T182630Z UID:indico-contribution-462-56@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:Constraining Secluded Dark Matter Scenarios with HAWC DTSTART;VALUE=DATE-TIME:20191113T071000Z DTEND;VALUE=DATE-TIME:20191113T073000Z DTSTAMP;VALUE=DATE-TIME:20250110T182630Z UID:indico-contribution-462-54@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:Status and Prospect of PandaX experiment DTSTART;VALUE=DATE-TIME:20191112T070500Z DTEND;VALUE=DATE-TIME:20191112T072500Z DTSTAMP;VALUE=DATE-TIME:20250110T182630Z UID:indico-contribution-433-24@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: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:20250110T182630Z UID:indico-contribution-433-21@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: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:20250110T182630Z UID:indico-contribution-433-34@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:Dark Matter Heating vs. Rotochemical Heating in Old Neutron Stars DTSTART;VALUE=DATE-TIME:20191112T082000Z DTEND;VALUE=DATE-TIME:20191112T084000Z DTSTAMP;VALUE=DATE-TIME:20250110T182630Z UID:indico-contribution-468-20@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: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:20250110T182630Z UID:indico-contribution-468-50@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 END:VCALENDAR