Abramowski A, Acero F, Aharonian F, Akhperjanian A G, Anton G, Balenderan S, Balzer A, Barnacka A, Becherini Y, Becker Tjus J, Bernlöhr K, Birsin E, Biteau J, Bochow A, Boisson C, Bolmont J, Bordas P, Brucker J, Brun F, Brun P, Bulik T, Carrigan S, Casanova S, Cerruti M, Chadwick P M, Chaves R C G, Cheesebrough A, Colafrancesco S, Cologna G, Conrad J, Couturier C, Dalton M, Daniel M K, Davids I D, Degrange B, Deil C, deWilt P, Dickinson H J, Djannati-Ataï A, Domainko W, Drury L O'C, Dubus G, Dutson K, Dyks J, Dyrda M, Egberts K, Eger P, Espigat P, Fallon L, Farnier C, Fegan S, Feinstein F, Fernandes M V, Fernandez D, Fiasson A, Fontaine G, Förster A, Füßling M, Gajdus M, Gallant Y A, Garrigoux T, Gast H, Giebels B, Glicenstein J F, Glück B, Göring D, Grondin M-H, Häffner S, Hague J D, Hahn J, Hampf D, Harris J, Heinz S, Heinzelmann G, Henri G, Hermann G, Hillert A, Hinton J A, Hofmann W, Hofverberg P, Holler M, Horns D, Jacholkowska A, Jahn C, Jamrozy M, Jung I, Kastendieck M A, Katarzyński K, Katz U, Kaufmann S, Khélifi B, Klepser S, Klochkov D, Kluźniak W, Kneiske T, Komin Nu, Kosack K, Kossakowski R, Krayzel F, Krüger P P, Laffon H, Lamanna G, Lefaucheur J, Lemoine-Goumard M, Lenain J-P, Lennarz D, Lohse T, Lopatin A, Lu C-C, Marandon V, Marcowith A, Masbou J, Maurin G, Maxted N, Mayer M, McComb T J L, Medina M C, Méhault J, Menzler U, Moderski R, Mohamed M, Moulin E, Naumann C L, Naumann-Godo M, de Naurois M, Nedbal D, Nekrassov D, Nguyen N, Niemiec J, Nolan S J, Ohm S, de Oña Wilhelmi E, Opitz B, Ostrowski M, Oya I, Panter M, Parsons R D, Paz Arribas M, Pekeur N W, Pelletier G, Perez J, Petrucci P-O, Peyaud B, Pita S, Pühlhofer G, Punch M, Quirrenbach A, Raue M, Reimer A, Reimer O, Renaud M, de Los Reyes R, Rieger F, Ripken J, Rob L, Rosier-Lees S, Rowell G, Rudak B, Rulten C B, Sahakian V, Sanchez D A, Santangelo A, Schlickeiser R, Schulz A, Schwanke U, Schwarzburg S, Schwemmer S, Sheidaei F, Skilton J L, Sol H, Spengler G, Stawarz L, Steenkamp R, Stegmann C, Stinzing F, Stycz K, Sushch I, Szostek A, Tavernet J-P, Terrier R, Tluczykont M, Trichard C, Valerius K, van Eldik C, Vasileiadis G, Venter C, Viana A, Vincent P, Völk H J, Volpe F, Vorobiov S, Vorster M, Wagner S J, Ward M, White R, Wierzcholska A, Wouters D, Zacharias M, Zajczyk A, Zdziarski A A, Zech A, Zechlin H-S
Universität Hamburg, Institut für Experimentalphysik, Luruper Chaussee 149, D 22761 Hamburg, Germany.
Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3, CC 72, Place Eugène Bataillon, F-34095 Montpellier Cedex 5, France.
Phys Rev Lett. 2013 Jan 25;110(4):041301. doi: 10.1103/PhysRevLett.110.041301. Epub 2013 Jan 22.
Gamma-ray line signatures can be expected in the very-high-energy (E(γ)>100 GeV) domain due to self-annihilation or decay of dark matter (DM) particles in space. Such a signal would be readily distinguishable from astrophysical γ-ray sources that in most cases produce continuous spectra that span over several orders of magnitude in energy. Using data collected with the H.E.S.S. γ-ray instrument, upper limits on linelike emission are obtained in the energy range between ∼ 500 GeV and ∼ 25 TeV for the central part of the Milky Way halo and for extragalactic observations, complementing recent limits obtained with the Fermi-LAT instrument at lower energies. No statistically significant signal could be found. For monochromatic γ-ray line emission, flux limits of (2 × 10(-7) -2 × 10(-5)) m(-2) s(-1) sr(-1) and (1 × 10(-8) -2 × 10(-6)) m(-2) s(-1)sr(-1) are obtained for the central part of the Milky Way halo and extragalactic observations, respectively. For a DM particle mass of 1 TeV, limits on the velocity-averaged DM annihilation cross section ⟨σv⟩(χχ → γγ) reach ∼ 10(-27) cm(3)s(-1), based on the Einasto parametrization of the Galactic DM halo density profile.
由于太空中暗物质（DM）粒子的自湮灭或衰变，预计在甚高能（E(γ)>100 GeV）领域会出现伽马射线谱线特征。这样的信号将很容易与天体物理伽马射线源区分开来，在大多数情况下，天体物理伽马射线源产生的连续谱能量范围跨越几个数量级。利用高能立体视野望远镜（H.E.S.S.）伽马射线仪器收集的数据，在银河系晕中心部分和河外观测中，在约500 GeV至约25 TeV的能量范围内获得了线状发射的上限，补充了费米大面积望远镜（Fermi-LAT）仪器在较低能量下最近获得的上限。未发现具有统计显著性的信号。对于单色伽马射线谱线发射，分别在银河系晕中心部分和河外观测中获得了通量极限（2×10^(-7)-2×10^(-5)）m^(-2) s^(-1) sr^(-1) 和（1×10^(-8)-2×10^(-6)）m^(-2) s^(-1) sr^(-1)。对于质量为1 TeV的暗物质粒子，基于银河系暗物质晕密度分布的艾纳斯托（Einasto）参数化，速度平均暗物质湮灭截面⟨σv⟩(χχ → γγ) 的极限达到约10^(-27) cm^(3)s^(-1)。
