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000576705 005__ 20230319000437.0
000576705 0247_ $$2INSPIRETeX$$aVERITAS:2023laq
000576705 0247_ $$2inspire$$ainspire:2634024
000576705 0247_ $$2arXiv$$aarXiv:2302.08784
000576705 0247_ $$2altmetric$$aaltmetric:142723543
000576705 037__ $$aPUBDB-2023-00876
000576705 041__ $$aEnglish
000576705 088__ $$2arXiv$$aarXiv:2302.08784
000576705 1001_ $$0P:(DE-H253)PIP1094637$$aTak, Donggeun$$b0$$eCorresponding author
000576705 245__ $$aSearch for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS
000576705 260__ $$c2023
000576705 3367_ $$0PUB:(DE-HGF)25$$2PUB:(DE-HGF)$$aPreprint$$bpreprint$$mpreprint$$s1677572654_14761
000576705 3367_ $$2ORCID$$aWORKING_PAPER
000576705 3367_ $$028$$2EndNote$$aElectronic Article
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000576705 3367_ $$2BibTeX$$aARTICLE
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000576705 500__ $$a10 pages, 7 figures
000576705 520__ $$aDark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV $\lesssim M_{\chi} \lesssim$ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; $M_{\chi} \gtrsim$ 100 TeV) has been suggested as an under-explored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS gamma-ray observatory. With 216 hours of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a $\gamma$-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle.
000576705 536__ $$0G:(DE-HGF)POF4-613$$a613 - Matter and Radiation from the Universe (POF4-613)$$cPOF4-613$$fPOF IV$$x0
000576705 588__ $$aDataset connected to INSPIRE
000576705 650_7 $$2INSPIRE$$adark matter, annihilation
000576705 650_7 $$2INSPIRE$$abackground, fluctuation
000576705 650_7 $$2INSPIRE$$across section, annihilation
000576705 650_7 $$2INSPIRE$$aWIMP
000576705 650_7 $$2INSPIRE$$agalaxy
000576705 650_7 $$2INSPIRE$$aTeV
000576705 650_7 $$2INSPIRE$$aVERITAS
000576705 650_7 $$2INSPIRE$$aobservatory
000576705 650_7 $$2INSPIRE$$aGeV
000576705 650_7 $$2INSPIRE$$acomposite
000576705 650_7 $$2INSPIRE$$aCherenkov counter
000576705 650_7 $$2INSPIRE$$aimaging
000576705 650_7 $$2INSPIRE$$agamma ray
000576705 693__ $$0EXP:(DE-H253)VERITAS-20170101$$5EXP:(DE-H253)VERITAS-20170101$$eVery Energetic Radiation Imaging Telescope Array System$$x0
000576705 7001_ $$0P:(DE-H253)PIP1031007$$aPueschel, E.$$b1$$eCorresponding author$$udesy
000576705 7001_ $$0M.Baumgart.1$$aBaumgart, M.$$b2
000576705 7001_ $$0N.L.Rodd.1$$aRodd, N. L.$$b3
000576705 7001_ $$aAcharyya, A.$$b4
000576705 7001_ $$0A.Archer.1$$aArcher, A.$$b5
000576705 7001_ $$0P.Bangale.1$$aBangale, P.$$b6
000576705 7001_ $$0J.T.Bartkoske.2$$aBartkoske, J. T.$$b7
000576705 7001_ $$0P.Batista.1$$aBatista, P.$$b8
000576705 7001_ $$0W.Benbow.1$$aBenbow, W.$$b9
000576705 7001_ $$0James.H.Buckley.1$$aBuckley, J. H.$$b10
000576705 7001_ $$0A.Falcone.1$$aFalcone, A.$$b11
000576705 7001_ $$aFeng, Q.$$b12
000576705 7001_ $$0J.P.Finley.1$$aFinley, J. P.$$b13
000576705 7001_ $$0G.M.Foote.1$$aFoote, G. M.$$b14
000576705 7001_ $$0L.F.Fortson.1$$aFortson, L.$$b15
000576705 7001_ $$0A.K.Furniss.1$$aFurniss, A.$$b16
000576705 7001_ $$0G.GallagherDaggitt.1$$aGallagher, G.$$b17
000576705 7001_ $$0W.F.Hanlon.1$$aHanlon, W. F.$$b18
000576705 7001_ $$0O.Hervet.16$$aHervet, O.$$b19
000576705 7001_ $$0J.Hoang.2$$aHoang, J.$$b20
000576705 7001_ $$0J.Holder.1$$aHolder, J.$$b21
000576705 7001_ $$0T.B.Humensky.1$$aHumensky, T. B.$$b22
000576705 7001_ $$aJin, W.$$b23
000576705 7001_ $$0P.Kaaret.1$$aKaaret, P.$$b24
000576705 7001_ $$0M.Kertzman.6$$aKertzman, M.$$b25
000576705 7001_ $$0P:(DE-H253)PIP1084929$$aKherlakian, M.$$b26$$udesy
000576705 7001_ $$0D.B.Kieda.1$$aKieda, D.$$b27
000576705 7001_ $$0P:(DE-H253)PIP1093214$$aKleiner, T. K.$$b28$$udesy
000576705 7001_ $$aKorzoun, N.$$b29
000576705 7001_ $$0F.Krennrich.1$$aKrennrich, F.$$b30
000576705 7001_ $$aLang, M. J.$$b31
000576705 7001_ $$0M.Lundy.1$$aLundy, M.$$b32
000576705 7001_ $$0P:(DE-H253)PIP1011664$$aMaier, G.$$b33
000576705 7001_ $$0C.E.McGrath.1$$aMcGrath, C. E.$$b34
000576705 7001_ $$0P.Moriarty.5$$aMoriarty, P.$$b35
000576705 7001_ $$0S.OBrien.4$$aO'Brien, S.$$b36
000576705 7001_ $$aOng, R. A.$$b37
000576705 7001_ $$0P:(DE-H253)PIP1083020$$aPfrang, K.$$b38$$udesy
000576705 7001_ $$0P:(DE-H253)PIP1010085$$aPohl, Martin$$b39$$udesy
000576705 7001_ $$0John.Quinn.1$$aQuinn, J.$$b40
000576705 7001_ $$0K.J.Ragan.1$$aRagan, K.$$b41
000576705 7001_ $$0P.T.Reynolds.1$$aReynolds, P. T.$$b42
000576705 7001_ $$0E.Roache.11$$aRoache, E.$$b43
000576705 7001_ $$0J.L.Ryan.1$$aRyan, J. L.$$b44
000576705 7001_ $$0P:(DE-H253)PIP1006066$$aSadeh, I.$$b45
000576705 7001_ $$0Lab.Saha.1$$aSaha, L.$$b46
000576705 7001_ $$0M.Santander.19$$aSantander, M.$$b47
000576705 7001_ $$0G.H.Sembroski.3$$aSembroski, G. H.$$b48
000576705 7001_ $$aShang, R.$$b49
000576705 7001_ $$0Megan.Splettstoesser.1$$aSplettstoesser, M.$$b50
000576705 7001_ $$0J.V.Tucci.1$$aTucci, J. V.$$b51
000576705 7001_ $$0V.V.Vassiliev.2$$aVassiliev, V. V.$$b52
000576705 7001_ $$0D.A.Williams.1$$aWilliams, D. A.$$b53
000576705 7001_ $$0P:(DE-HGF)0$$aVERITAS Collaboration$$b54$$eCollaboration Author
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000576705 9131_ $$0G:(DE-HGF)POF4-613$$1G:(DE-HGF)POF4-610$$2G:(DE-HGF)POF4-600$$3G:(DE-HGF)POF4$$4G:(DE-HGF)POF$$aDE-HGF$$bForschungsbereich Materie$$lMatter and the Universe$$vMatter and Radiation from the Universe$$x0
000576705 9141_ $$y2023
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