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Searches for gamma-ray lines and `pure WIMP' spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S

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arxiv 1810.00995 v1 pith:3TAHURKF submitted 2018-10-01 astro-ph.HE hep-exhep-ph

Searches for gamma-ray lines and `pure WIMP' spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S

H.E.S.S. Collaboration: H. Abdalla , F. Aharonian , F. Ait Benkhali , E.O. Ang\"uner , M. Arakawa , C. Arcaro , C. Armand , M. Arrieta
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M. Backes M. Barnard Y. Becherini J. Becker Tjus D. Berge S. Bernhard K. Bernl\"ohr R. Blackwell M. B\"ottcher C. Boisson J. Bolmont S. Bonnefoy P. Bordas J. Bregeon F. Brun P. Brun M. Bryan M. B\"uchele T. Bulik T. Bylund M. Capasso S. Caroff A. Carosi S. Casanova M. Cerruti N. Chakraborty S. Chandra R.C.G. Chaves A. Chen S. Colafrancesco B. Condon I.D. Davids C. Deil J. Devin P. deWilt L. Dirson A. Djannati-Ata\"i A. Dmytriiev A. Donath V. Doroshenko L.O'C. Drury J. Dyks K. Egberts G. Emery J.-P. Ernenwein S. Eschbach S. Fegan A. Fiasson G. Fontaine S. Funk M. F\"u{\ss}ling S. Gabici Y.A. Gallant F. Gat\'e G. Giavitto D. Glawion J.F. Glicenstein D. Gottschall M.-H. Grondin J. Hahn M. Haupt G. Heinzelmann G. Henri G. Hermann J.A. Hinton W. Hofmann C. Hoischen T. L. Holch M. Holler D. Horns D. Huber H. Iwasaki A. Jacholkowska M. Jamrozy D. Jankowsky F. Jankowsky L. Jouvin I. Jung-Richardt M.A. Kastendieck K. Katarzy\'nski M. Katsuragawa U. Katz D. Kerszberg D. Khangulyan B. Kh\'elifi J. King S. Klepser W. Klu\'zniak Nu. Komin K. Kosack S. Krakau M. Kraus P.P. Kr\"uger G. Lamanna J. Lau J. Lefaucheur A. Lemi\`ere M. Lemoine-Goumard J.-P. Lenain E. Leser T. Lohse M. Lorentz R. L\'opez-Coto I. Lypova D. Malyshev V. Marandon A. Marcowith C. Mariaud G. Mart\'i-Devesa R. Marx G. Maurin P.J. Meintjes A.M.W. Mitchell R. Moderski M. Mohamed L. Mohrmann E. Moulin T. Murach S. Nakashima M. de Naurois H. Ndiyavala F. Niederwanger J. Niemiec L. Oakes P. O'Brien H. Odaka S. Ohm M. Ostrowski I. Oya M. Padovani M. Panter R.D. Parsons C. Perennes P.-O. Petrucci B. Peyaud Q. Piel S. Pita V. Poireau A. Priyana Noel D.A. Prokhorov H. Prokoph G. P\"uhlhofer M. Punch A. Quirrenbach S. Raab R. Rauth A. Reimer O. Reimer M. Renaud F. Rieger L. Rinchiuso C. Romoli G. Rowell B. Rudak E. Ruiz-Velasco V. Sahakian S. Saito D.A. Sanchez A. Santangelo M. Sasaki R. Schlickeiser F. Sch\"ussler A. Schulz U. Schwanke S. Schwemmer M. Seglar-Arroyo M. Senniappan A.S. Seyffert N. Shafi I. Shilon K. Shiningayamwe R. Simoni A. Sinha H. Sol F. Spanier A. Specovius M. Spir-Jacob {\L}. Stawarz R. Steenkamp C. Stegmann C. Steppa T. Takahashi J.-P. Tavernet T. Tavernier A.M. Taylor R. Terrier L. Tibaldo D. Tiziani M. Tluczykont C. Trichard M. Tsirou N. Tsuji R. Tuffs Y. Uchiyama D.J. van der Walt C. van Eldik C. van Rensburg B. van Soelen G. Vasileiadis J. Veh C. Venter A. Viana P. Vincent J. Vink F. Voisin H.J. V\"olk T. Vuillaume Z. Wadiasingh S.J. Wagner R.M. Wagner R. White A. Wierzcholska R. Yang D. Zaborov M. Zacharias R. Zanin A.A. Zdziarski A. Zech F. Zefi A. Ziegler J. Zorn N. \.Zywucka (the H.E.S.S. Collaboration) M. Cirelli P. Panci F. Sala J. Silk M. Taoso
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classification astro-ph.HE hep-exhep-ph
keywords annihilationannihilationscasedarkdwarfgalaxiesgamma-raylimits
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved
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Dwarf spheroidal galaxies are among the most promising targets for detecting signals of Dark Matter (DM) annihilations. The H.E.S.S. experiment has observed five of these systems for a total of about 130 hours. The data are re-analyzed here, and, in the absence of any detected signals, are interpreted in terms of limits on the DM annihilation cross section. Two scenarios are considered: i) DM annihilation into mono-energetic gamma-rays and ii) DM in the form of pure WIMP multiplets that, annihilating into all electroweak bosons, produce a distinctive gamma-ray spectral shape with a high-energy peak at the DM mass and a lower-energy continuum. For case i), upper limits at 95\% confidence level of about $\langle \sigma v \rangle \lesssim 3 \times 10^{-25}$ cm$^3$ s$^{-1}$ are obtained in the mass range of 400 GeV to 1 TeV. For case ii), the full spectral shape of the models is used and several excluded regions are identified, but the thermal masses of the candidates are not robustly ruled out.

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