H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

Abdalla, H.; Abramowski, A.; Aharonian, F.; Benkhali, F. Ait; Akhperjanian, A. G.; Andersson, Tom; Angüner, E. O.; Arrieta, M.; Aubert, Pierre; Backes, Michael; Balzer, A.; Barnard, M.; Becherini, Y.; Tjus, Julia Becker; Berge, D.; Bernhard, S.; Bernlöhr, K.; Birsin, E.; Blackwell, R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Bulik, T.; Capasso, M.; Carr, J.; Casanova, S.; Chakraborty, Nachiketa; Chalmé-Calvet, R.; Chaves, R. C. G.; Chen, A.; Chevalier, J.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Condon, B.; Conrad, J.; Couturier, C.; Cui, Yuxin; Davids, I. D.; Degrange, B.; Deil, C.; Devin, J.; deWilt, P.; Djannati‐Ataï, A.; Domainko, W.; Donath, Axel; Drury, L. O'c.; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Ernenwein, J.-P.; Eschbach, S.; Farnier, C.; Fegan, S. J.; Fernandes, M. V.; Fiaßon, A.; Fontaine, G.; Förster, A.; Funk, Sebastian; Füßling, M.; Gabici, S.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giavitto, G.; Giebels, B.; Glicenstein, J. F.; Gottschall, D.; Goyal, Ashok; Grondin, M.-H.; Grudzińska, M.; Hadasch, D.; Hahn, Joachim; Hawkes, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, Andreas; Hinton, Jim; Hofmann, W.; Hoischen, C.; Holler, M.; Horns, D.; Ivascenko, A.; Jachołkowska, A.; Jamrozy, M.; Janiak, M.; Jankowsky, D.; Jankowsky, F.; Jingo, M.; Jogler, T.; Jouvin, L.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kerszberg, Daniel; Khélifi, B.; Kieffer, Michel; King, Johannes; Klepser, S.; Klochkov, D.; Kluźniak, W.; Kolitzus, D.; Komin, Nu.; Kosack, K.; Krakau, S.; Kraus, Martin; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lau, J.; Lees, J. P.; Lefaucheur, J.; Lefranc, V.; Lemière, A.; Lemoine‐Goumard, M.; Lenain, J.‐P.; Leser, E.; Liu, R.; Löhse, T.; Lorentz, M.; Lypova, I.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; Meintjes, P. J.; Meyer, M.; Mitchell, Alison; Moderski, R.; Mohamed, M.; Morå, K.; Moulin, Emmanuel; Murach, T.; Naurois, M. de; Niederwanger, F.; Niemiec, J.; Oakes, L.; O’Brien, P. T.; Odaka, Hirokazu; Ohm, S.; Ostrowski, M.; Öttl, S.; Oya, I.; Padovani, M.; Panter, M.; Parsons, R. D.; Arribas, M. Paz; Pekeur, N. W.; Pelletier, G.; Perennes, C.; Petrucci, P.-O.; Peyaud, B.; Pita, S.; Poon, H.; Prokhorov, Dmitry; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Reimer, A.; Reimer, O.; Renaud, M.; Reyes, R. de los; Rieger, F.; Romoli, C.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Šálek, D.; Sánchez, David; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schüßler, F.; Schulz, Alexander; Schwanke, U.; Schwemmer, S.; Settimo, M.; Seyffert, A. S.; Shafi, N.; Shilon, I.; Simoni, R.; Sol, H.; Spanier, F.; Spengler, G.; Spies, F.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Tavernet, J.‐P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tluczykont, M.; Trichard, C.; Tuffs, R.; Walt, Johan van der; Eldik, C. van; Soelen, B. van; Vasileiadis, G.; Veh, J.; Venter, C.; Viana, A.; Vincent, P.; Vink, Jacco; Voisin, F.; Völk, H. J.; Vuillaume, Thomas; Wadiasingh, Zorawar; Wagner, S. J.; Wagner, P.; Wagner, R. M.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Yang, R.; Zabalza, V.; Zaborov, D.; Zacharias, M.; Zdziarski, A. A.; Zech, A.; Zefi, F.; Ziegler, Andreas; Żywucka, N.

doi:10.1103/physrevlett.117.151302

Cited by 49 publications

(67 citation statements)

References 20 publications

(25 reference statements)

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“…As noted above, by contrast, the diphoton branching fraction for KK gravitons lie in the range of ∼ 4 − 8%, depending upon how the various SM fields are localized. The existing limits on this mode arise from both the Fermi-LAT [5] and HESS [6,7] Galactic Center (GC) data sets, with the actual constraints being strongly dependent upon whether a cored or cusped DM profile is assumed to be applicable at the GC. Future measurements by CTA [8] are expected to significantly improve the existing constraints over a reasonable DM mass range.…”

Section: Jhep10(2017)094mentioning

confidence: 99%

“…These s-channel terms will clearly dominate in the regions near graviton KK resonances through triple graviton coupling processes such as G 3 → 2G 1 . 7 These types of decays (in the absence of graviton BLKTs) were considered in ref. [48] and the analysis presented there can be straightforwardly generalized to cover this more complex situation.…”

Section: Jhep10(2017)094mentioning

confidence: 99%

“…6 We will make this assumption for all DM spin assignments in all benchmark cases independently of where the DM is localized. 7 Recall that the graviton KK spectrum satisfies the ordering mG 2 < 2mG 1 < mG 3 .…”

Section: Jhep10(2017)094mentioning

confidence: 99%

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Gravity-mediated dark matter annihilation in the Randall-Sundrum model

Rueter

Rizzo

Hewett

2017

J. High Energ. Phys.

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Observational evidence for dark matter stems from its gravitational interactions, and as of yet there has been no evidence for dark matter interacting via other means. We examine models where dark matter interactions are purely gravitational in a RandallSundrum background. In particular, the Kaluza-Klein tower of gravitons which result from the warped fifth dimension can provide viable annihilation channels into Standard Model final states, and we find that we can achieve values of the annihilation cross section, σv , which are consistent with the observed relic abundance in the case of spin-1 dark matter. We examine constraints on these models employing both the current photon line and continuum indirect dark matter searches, and assess the prospects of hunting for the signals of such models in future direct and indirect detection experiments.

show abstract

Section: Jhep10(2017)094mentioning

confidence: 99%

Section: Jhep10(2017)094mentioning

confidence: 99%

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Gravity-mediated dark matter annihilation in the Randall-Sundrum model

Rueter

Rizzo

Hewett

2017

J. High Energ. Phys.

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“…This survey will allow us to probe a larger source region of DM annihilations and alleviate the impact of the uncertainty of the DM distribution in the inner kiloparsec of the Milky Way on the sensitivity to DM annihilations. A limited data set (∼15 h) of this survey using 2014 observations with the fifth telescope only was used to constrain the presence of a 130 GeV DM line in the vicinity of the GC [45]. Observations including the fifth telescope will allow us to probe DM lines down to 100 GeV.…”

mentioning

confidence: 99%

Search for γ -Ray Line Signals from Dark Matter Annihilations in the Inner Galactic Halo from 10 Years of Observations with H.E.S.S.

Abdallah¹,

Abramowski²,

Aharonian³

et al. 2018

Phys. Rev. Lett.

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139

140

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Spectral lines are among the most powerful signatures for dark matter (DM) annihilation searches in very-high-energy γ rays. The central region of the Milky Way halo is one of the most promising targets given its large amount of DM and proximity to Earth. We report on a search for a monoenergetic spectral line from self-annihilations of DM particles in the energy range from 300 GeV to 70 TeV using a twodimensional maximum likelihood method taking advantage of both the spectral and spatial features of the signal versus background. The analysis makes use of Galactic center observations accumulated over ten years (2004)(2005)(2006)(2007)(2008)(2009)(2010)(2011)(2012)(2013)(2014) with the H.E.S.S. array of ground-based Cherenkov telescopes. No significant γ-ray excess above the background is found. We derive upper limits on the annihilation cross section hσvi for monoenergetic DM lines at the level of 4 × 10 −28 cm 3 s −1 at 1 TeV, assuming an Einasto DM profile for the Milky Way halo. For a DM mass of 1 TeV, they improve over the previous ones by a factor of 6. The present constraints are the strongest obtained so far for DM particles in the mass range 300 GeV-70 TeV. Groundbased γ-ray observations have reached sufficient sensitivity to explore relevant velocity-averaged cross sections for DM annihilation into two γ-ray photons at the level expected from the thermal relic density for TeV DM particles.

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“…The current upper bounds from the Fermi-LAT [7] and H.E.S.S. [8,34] data are shown. All points on the contour satisfy the observed relic density.…”

Section: Direct Detectionmentioning

confidence: 99%

Dark matter in the Randall-Sundrum model with non-universal coupling

Goyal

Islam

Kumar

2019

J. High Energ. Phys.

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We consider simplified dark matter models (DM) interacting gravitationally with the standard model (SM) particles in a Randall-Sundrum (RS) framework. In this framework, the DM particles interact through the exchange of spin-2 Kaluza-Klein (KK) gravitons in the s-channel with the SM particles. The parameter space of the RS model with universal couplings to SM particles is known to be strongly constrained from the LHC data. We are thus led to consider models with non-universal couplings. The first model we consider in this study is a top-philic graviton model in which only the right-handed top quarks are taken to interact strongly with the gravitons. In the second, the lepto-philic model, we assume that only the right-handed charged leptons interact strongly with the gravitons. We extend the study to include not only the scalar, vector and spin-1/2 fermions but also spin-3/2 fermionic dark matter. We find that there is a large parameter space in these benchmark models where it is possible to achieve the observed relic density consistent with the direct and indirect searches and yet not to be constrained from the LHC data.

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H.E.S.S. Limits on Linelike Dark Matter Signatures in the 100 GeV to 2 TeV Energy Range Close to the Galactic Center

Cited by 49 publications

References 20 publications

Gravity-mediated dark matter annihilation in the Randall-Sundrum model

Gravity-mediated dark matter annihilation in the Randall-Sundrum model

Search for γ -Ray Line Signals from Dark Matter Annihilations in the Inner Galactic Halo from 10 Years of Observations with H.E.S.S.

Dark matter in the Randall-Sundrum model with non-universal coupling

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