%0 Electronic Article
%A Tak, Donggeun
%A Pueschel, E.
%A Baumgart, M.
%A Rodd, N. L.
%A Acharyya, A.
%A Archer, A.
%A Bangale, P.
%A Bartkoske, J. T.
%A Batista, P.
%A Benbow, W.
%A Buckley, J. H.
%A Falcone, A.
%A Feng, Q.
%A Finley, J. P.
%A Foote, G. M.
%A Fortson, L.
%A Furniss, A.
%A Gallagher, G.
%A Hanlon, W. F.
%A Hervet, O.
%A Hoang, J.
%A Holder, J.
%A Humensky, T. B.
%A Jin, W.
%A Kaaret, P.
%A Kertzman, M.
%A Kherlakian, M.
%A Kieda, D.
%A Kleiner, T. K.
%A Korzoun, N.
%A Krennrich, F.
%A Lang, M. J.
%A Lundy, M.
%A Maier, G.
%A McGrath, C. E.
%A Moriarty, P.
%A O'Brien, S.
%A Ong, R. A.
%A Pfrang, K.
%A Pohl, Martin
%A Quinn, J.
%A Ragan, K.
%A Reynolds, P. T.
%A Roache, E.
%A Ryan, J. L.
%A Sadeh, I.
%A Saha, L.
%A Santander, M.
%A Sembroski, G. H.
%A Shang, R.
%A Splettstoesser, M.
%A Tucci, J. V.
%A Vassiliev, V. V.
%A Williams, D. A.
%T Search for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS
%N arXiv:2302.08784
%M PUBDB-2023-00876
%M arXiv:2302.08784
%D 2023
%Z 10 pages, 7 figures
%X Dark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV  <~M<sub>χ</sub>  <~ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; M<sub>χ</sub>  >~ 100 TeV) has been suggested as an under-explored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS gamma-ray observatory. With 216 hours of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a γ-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle.
%K dark matter, annihilation (INSPIRE)
%K background, fluctuation (INSPIRE)
%K cross section, annihilation (INSPIRE)
%K WIMP (INSPIRE)
%K galaxy (INSPIRE)
%K TeV (INSPIRE)
%K VERITAS (INSPIRE)
%K observatory (INSPIRE)
%K GeV (INSPIRE)
%K composite (INSPIRE)
%K Cherenkov counter (INSPIRE)
%K imaging (INSPIRE)
%K gamma ray (INSPIRE)
%F PUB:(DE-HGF)25
%9 Preprint
%U https://bib-pubdb1.desy.de/record/576705