Search for Photon-Linelike Signatures from Dark Matter Annihilations with H.E.S.S.

Abramowski, A.; Acero, Fabio; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Tjus, J. Becker; 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. J.; Feinstein, F.; Fernandes, M. V.; Fernández, 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, Joachim; Hampf, D.; Harris, J.; Heinz, Sebastian; Heinzelmann, G.; Henri, G.; Hermann, G.; Hillert, Andreas; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jachołkowska, 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.; Löhse, 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, Emmanuel; Naumann, C. L.; Naumann-Godó, M.; Naurois, M. de; Nedbal, D.; Nekrassov, D.; Nguyen, N.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Wilhelmi, E. de Oña; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Arribas, M. Paz; Pekeur, N. W.; Pelletier, G.; Pérez, J.; Petrucci, P.-O.; Peyaud, B.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Reimer, A.; Renaud, M.; Reyes, R. de los; Rieger, F.; Ripken, J.; Rob, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sánchez, David; Santangelo, A.; Schlickeiser, R.; Schulz, Alexander; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sheidaei, F.; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tavernet, J.‐P.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Vorster, M.; Wagner, S. J.; Ward, M. J.; White, R.; Wierzcholska, A.; Wouters, D.; Zacharias, M.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.

doi:10.1103/physrevlett.110.041301

Cited by 228 publications

(391 citation statements)

References 25 publications

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“…6 The details of our factorization theorem, which is identical to the wino result, can be found in [7,8]. Because of the more involved operator structure, we will also decompose 6 Strictly speaking, O2 in eq. (3.1) contains a fifth collinear structure, which we could call O e c = BD BD.…”

Section: Jhep03(2016)213mentioning

confidence: 90%

“…The possibility of such experiments to set stringent limits on the wino scenario was explored in [2,5]. By combining a numerical calculation of the Sommerfeld enhancement with a tree-level annihilation of WIMPs to γγ + 1 2 γZ, they found that the HESS experiment ruled out the wino by a factor of 15 under the assumption of an NFW dark matter halo profile [6]. In particular though, [5] extended their annihilation calculation to one-loop and found a reduction in rate by ∼ 4× at the thermal relic mass of 3 TeV.…”

Section: Jhep03(2016)213mentioning

confidence: 99%

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Semi-inclusive wino and higgsino annihilation to LL′

Baumgart¹,

Vaidya²

2016

J. High Energ. Phys.

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We systematically compute the annihilation rate for winos and higgsinos into the final state relevant for indirect detection experiments, γ + X. The radiative corrections to this process receive enhancement from the large Bloch-Nordsieck-Violating Sudakov logarithm, log(2M χ /M W ). We resum the double logs and include single logs to fixed order using a formalism that combines nonrelativistic and soft-collinear effective field theories. For the wino case, we update an earlier exclusion adapting results of the HESS experiment. At the thermal relic mass of 3 TeV, LL corrections result in a ∼30% reduction in rate relative to LL. Nonetheless, single logs do not save the wino, and it is still excluded by an order of magnitude. Experimental cuts produce an endpoint region which, our results show, significantly effects the higgsino rate at its thermal-relic mass near 1 TeV and is deserving of further study.

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Section: Jhep03(2016)213mentioning

confidence: 90%

Section: Jhep03(2016)213mentioning

confidence: 99%

Semi-inclusive wino and higgsino annihilation to LL′

Baumgart¹,

Vaidya²

2016

J. High Energ. Phys.

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“…[63]. The Fermi -LAT upper limits on σ ann v extend from ∼10 −29 cm 3 s −1 at m χ = 10 GeV to ∼10 −27 cm 3 s −1 at m χ = 300 GeV, while the H.E.S.S.…”

Section: Annihilationmentioning

confidence: 99%

“…This is why this feature has been so appealing, and many searches for a hint of it have been conducted so far, in galaxy clusters [60], Milky Way dSph satellites [61], and in the GC and Halo [62,63]. In addition, it is worth mentioning that there is a recently claimed hint of a line-like signal at ∼130 GeV in the Fermi -LAT data of the GC region [40,64]: if the observed signal originates from direct DM annihilation into two photons, the WIMP particle should have a mass of m χ = 129±2.4 +7 −13 GeV and an annihilation rate (assuming the Einasto profile) of σ ann v γγ = (1.27± 0.32 +0.…”

Section: Gamma-ray Linesmentioning

confidence: 99%

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Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

Aleksić

2016

Springer Theses

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Abstract. We present the results of stereoscopic observations of the satellite galaxy Segue 1 with the MAGIC Telescopes, carried out between 2011 and 2013. With almost 160 hours of good-quality data, this is the deepest observational campaign on any dwarf galaxy performed so far in the very high energy range of the electromagnetic spectrum. We search this large data sample for signals of dark matter particles in the mass range between 100 GeV and 20 TeV. For this we use the full likelihood analysis method, which provides optimal sensitivity to characteristic gamma-ray spectral features, like those expected from dark matter annihilation or decay. In particular, we focus our search on gamma-rays produced from different final state Standard Model particles, annihilation with internal bremsstrahlung, monochromatic lines and box-shaped signals. Our results represent the most stringent constraints to the annihilation cross-section or decay lifetime obtained from observations of satellite galaxies, for masses above few hundred GeV. In particular, our strongest limit (95% confidence level) corresponds to a ∼500 GeV dark matter particle annihilating into τ + τ − , and is of order σ ann v ≃ 1.2×10 −24 cm 3 s −1 -a factor ∼40 above the σ ann v thermal value.

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2014

Beyond the Standard Model of Elementary Particle Physics

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Search for Photon-Linelike Signatures from Dark Matter Annihilations with H.E.S.S.

Cited by 228 publications

References 25 publications

Semi-inclusive wino and higgsino annihilation to LL′

Semi-inclusive wino and higgsino annihilation to LL′

Optimized Dark Matter Searches in Deep Observations of Segue 1 with MAGIC

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