RT Journal Article
T1 A search for dark matter in Triangulum II with the MAGIC telescopes
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fidalgo, David Friedrich Carreto
A1 Fonseca González, María Victoria
A1 Hoang, Kim Dinh
A1 López Moya, Marcos
A1 Peñil Del Campo, Pablo
A1 Saha, Lab
AB We present the first results from very-high-energy observations of the dwarf spheroidal satellite candidate Triangulum II with the MAGIC telescopes from 62.4 h of good-quality data taken between August 2016 and August 2017. We find no gamma-ray excess in the direction of Triangulum II, and upper limits on both the differential and integral gamma-ray flux are presented. Currently, the kinematics of Triangulum II are affected by large uncertainties leading to a bias in the determination of the properties of its dark matter halo. Using a scaling relation between the annihilation J-factor and heliocentric distance of well-known dwarf spheroidal galaxies, we estimate an annihilation J-factor for Triangulum II for WIMP dark matter of log[J(ann)(0.5 degrees)/GeV2 cm(-5)] = 19.35 +/- 0.37. We also derive a dark matter density profile for the object relying on results from resolved simulations of Milky Way sized dark matter halos. We obtain 95% confidence-level limits on the thermally averaged annihilation cross section for WIMP annihilation into various Standard Model channels. The most stringent limits are obtained in the tau(-)tau(+) final state, where a cross section for annihilation down to <sigma(ann)nu > = 3.05 x 10(-24) cm(3) s(-1) is excluded. (C) 2020 Elsevier B.V. All rights reserved.
PB Elsevier B.V.
SN 2212-6864
YR 2020
FD 2020-05
LK https://hdl.handle.net/20.500.14352/6334
UL https://hdl.handle.net/20.500.14352/6334
LA eng
NO © 2020 Elsevier B.V. All rights reserved. Artículo escrito por 161 autores. We would also like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, Germany, the Italian INFN and INAF, Italy, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017-87055-C22-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS, Japan and MEXT, Japan, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia ``Severo Ochoa'' SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia ``María de Maeztu'' MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka, Croatia Project 13.12.1.3.02, by the DFG, Germany Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre, Polland grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq, Brazil and FAPERJ, Brazil.
NO Ministerio de Economía y Competitividad (MINECO)/FEDER
NO Centro de Excelencia "Severo Ochoa"
NO Unidad de Excelencia "María de Maeztu''
NO German BMBF, Germany Federal Ministry of Education & Research (BMBF)
NO German MPG, Germany
NO Italian INAF, Italy
NO Italian INFN, Italy
NO Swiss National Fund SNF
NO Swiss National Science Foundation (SNSF)
NO Indian Department of Atomic Energy
NO Japanese JSPS, Japan
NO MEXT, Japan Ministry of Education, Culture, Sports, Science and Technology
NO Bulgarian Ministry of Education and Science, National RI Roadmap Project
NO Academy of Finland
NO Croatian Science Foundation (HrZZ)
NO University of Rijeka, Croatia
NO DFG, Germany Collaborative Research Centers German Research Foundation (DFG)
NO Polish National Research Centre, Polland
NO Brazilian MCTIC, Brazil
NO Brazilian CNPq, Brazil
NO Brazilian FAPERJ, Brazil
DS Docta Complutense
RD 10 abr 2025