Abdalla H, Spencer S, Aharonian F, Ait Benkhali F, Anguner EO, Arcaro C, Armand C, Armstrong T, Ashkar H, Backes M, Baghmanyan V, Barbosa-Martins V, Barnacka A, Barnard M, Becherini Y, Berge D, Bernloehr K, Bi B, Bottcher M, Boisson C, Bolmont J, De Bony De Lavergne M, Breuhaus M, Brose R, Brun F, Bulik T, Bylund T, Cangemi F, Caroff S, Casanova S, Chambery P, Catalano J, Chand T, Chen A, Cotter G, Curylo M, Dalgleish H, Mbarubucyeye JD, Davids ID, Davies J, Devin J, Djannati-Atai A, Dmytriiev A, Donath A, Doroshenko V, Dreyer L, Du Plessis L, Duffy C, Egberts K, Einecke S, Emery G, Ernenwein JP, Feijen K, Fegan S, Fiasson A, De Clairfontaine GF, Fontaine G, Funk S, Fuessling M, Gabici S, Gallant YA, Ghafourizade S, Giavitto G, Giunti L, Glawion D, Glicenstein JF, Grondin MH, Hattingh S, Haupt M, Hermann G, Hinton JA, Hofmann W, Hoischen C, Holch TL, Holler M, Hörbe M, Horns D, Huang Z, Huber D, Jamrozy M, Jankowsky D, Jankowsky F, Joshi V, Jung-Richardt I, Kasai E, Katarzyński K, Katz U, Khangulyan D, Khelifi B, Klepser S, Kluzniak W, Komin N, Konno R, Kosack K, Kostunin D, Kreter M, Kukec Mezek G, Kundu A, Lamanna G, Le Stum S, Lemiere A, Lemoine-Goumard M, Lenain JP, Leuschner F, Levy C, Luashvili A, Lohse T, Lypova I, Mackey J, Majumdar J, Malyshev D, Malyshev D, Marandon V, Marchegiani P, Marcowith A, Mares A, Martí-Devesa G, Marx R, Maurin G, Meintjes PJ, Meyer M, Mitchell A, Moderski R, Mohrmann L, Montanari A, Moore C, Morris P, Moulin E, Muller J, Murach T, Nakashima K, Nayerhoda A, De Naurois M, Ndiyavala H, Niemiec J, Noel A, Oberholzer L, O'Brien P, Ohm S, Olivera-Nieto L, De Ona Wilhelmi E, Ostrowski M, Panter M, Panny S, Parsons RD, Peron G, Pita S, Poireau V, Prokhorov DA, Prokoph H, Puhlhoefer G, Punch M, Quirrenbach A, Reichherzer P, Reimer A, Reimer O, Remy Q, Renaud M, Rieger F, Romoli C, Rowell G, Rudak B, Rueda Ricarte H, Ruiz-Velasco E, Sahakian V, Sailer S, Salzmann H, Sanchez DA, Santangelo A, Sasaki M, Schäfer J, Schüssler F, Schutte HM, Schwanke U, Senniappan M, Seyffert AS, Shapopi JNS, Shiningayamwe K, Simoni R, Sinha A, Spackman H, Sol H, Specovius A, Spencer ST, Spir-Jacob M, Stawarz L, Sun L, Steenkamp R, Stegmann C, Steinmassl S, Steppa C, Takahashi T, Tanaka T, Tavernier T, Taylor AM, Terrier R, Thorpe-Morgan C, Thiersen JHE, Tluczykont M, Tomankova L, Tsirou M, Tsuji M, Tuffs R, Uchiyama Y, Van Der Walt DJ, van Eldik C, Van Rensburg C, Van Soelen B, Vasileiadis G, Veh J, Venter C, Vincent P, Viana A, Vink J, Voelk HJ, Wagner SJ, Werner F, White R, Wierzcholska A, Wong YW, Yassin H, Yusafzai A, Zacharias M, Zanin R, Zargaryan D, Zdziarski AA, Zech A, Zhu SJ, Zmija A, Zorn J, Zouari S, Żywucka N (2021)
Publication Type: Journal article, Original article
Publication year: 2021
Book Volume: 918
Article Number: 17
Journal Issue: 1
Cosmological N-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter (DM) subhalos. These subhalos could shine in gamma-rays and eventually be detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-Large Area Telescope Objects (UFOs) to identify them as possible tera-electron-volt-scale DM subhalo candidates. We search for very-high-energy (E greater than or similar to 100 GeV) gamma-ray emissions using H.E.S.S. observations toward four selected UFOs. Since no significant very-high-energy gamma-ray emission is detected in any data set of the four observed UFOs or in the combined UFO data set, strong constraints are derived on the product of the velocity-weighted annihilation cross section sigma v by the J factor for the DM models. The 95% confidence level observed upper limits derived from combined H.E.S.S. observations reach sigma vJ values of 3.7 x 10(-5) and 8.1 x 10(-6) GeV(2 )cm(-2 )s(-1) in the W (+) W (-) and tau (+) tau (-) channels, respectively, for a 1 TeV DM mass. Focusing on thermal weakly interacting massive particles, the H.E.S.S. constraints restrict the J factors to lie in the range 6.1 x 10(19)-2.0 x 10(21) GeV(2 )cm(-5) and the masses to lie between 0.2 and 6 TeV in the W (+) W (-) channel. For the tau (+) tau (-) channel, the J factors lie in the range 7.0 x 10(19)-7.1 x 10(20) GeV(2 )cm(-5) and the masses lie between 0.2 and 0.5 TeV. Assuming model-dependent predictions from cosmological N-body simulations on the J-factor distribution for Milky Way-sized galaxies, the DM models with masses >0.3 TeV for the UFO emissions can be ruled out at high confidence level.
APA:
Abdalla, H., Spencer, S., Aharonian, F., Ait Benkhali, F., Anguner, E.O., Arcaro, C.,... Żywucka, N. (2021). Search for Dark Matter Annihilation Signals from Unidentified Fermi-LAT Objects with HESS. Astrophysical Journal, 918(1). https://doi.org/10.3847/1538-4357/abff59
MLA:
Abdalla, H., et al. "Search for Dark Matter Annihilation Signals from Unidentified Fermi-LAT Objects with HESS." Astrophysical Journal 918.1 (2021).
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