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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:20250110T182827Z
UID:indico-contribution-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/
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