Search for Dark Matter Annihilations towards the Inner Galactic Halo from 10 Years of Observations with H.E.S.S.

Abdallah, H.; Abramowski, A.; Aharonian, F.; Benkhali, F. Ait; Akhperjanian, A. G.; 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, Yudong; Davids, I. D.; Degrange, B.; Deil, C.; 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, A.; 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.; Löhse, T.; Lorentz, M.; Lui, Roger; Lypova, I.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; Meintjes, P. J.; Menzler, U.; Meyer, M.; Mitchell, Alison; Moderski, R.; Mohamed, M.; Morå, K.; Moulin, Emmanuel; Murach, T.; Naurois, M. de; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, Hirokazu; Ohm, S.; Öttl, S.; Ostrowski, M.; Oya, I.; Padovani, M.; Panter, M.; Parsons, R. D.; Arribas, M. Paz; Pekeur, N. W.; Pelletier, G.; 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.; Seyffert, A. S.; Shafi, N.; Simoni, R.; Sol, H.; Spanier, F.; Spengler, G.; Spieß, F.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Tavernet, J.‐P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; 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.117.111301

Cited by 327 publications

(498 citation statements)

References 25 publications

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“…Below hundreds of TeV in DM mass, these annihilation limits are not as strong as those from the HESS collaboration study of the GC [70]. However, our limits are much less -13 -JCAP02(2018)049 Figure 9.…”

Section: Dark Matter Annihilation Limitsmentioning

confidence: 66%

“…Limits for an Einasto (orange) profile are shown as in figures 7-10. Segue 1 dwarf galaxy limits from MAGIC [68], GC limits from HESS [70], HAWC limits from dwarf galaxies, and the model for IceCube neutrinos from decaying DM [7] are also shown as in for the hadronic and bosonic DM channels. For leptonic and neutrino dark matter channels, many neutrinos are produced, so the IceCube limits are stronger than those in our analysis.…”

Section: Dark Matter Decay Limitsmentioning

confidence: 99%

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A search for dark matter in the Galactic halo with HAWC

Abeysekara

Albert

Alfaro

et al. 2018

J. Cosmol. Astropart. Phys.

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Abstract. The High Altitude Water Cherenkov (HAWC) gamma-ray observatory is a wide field-of-view observatory sensitive to 500 GeV -100 TeV gamma rays and cosmic rays. With its observations over 2/3 of the sky every day, the HAWC observatory is sensitive to a wide variety of astrophysical sources, including possible gamma rays from dark matter. Dark matter annihilation and decay in the Milky Way Galaxy should produce gamma-ray signals across many degrees on the sky. The HAWC instantaneous field-of-view of 2 sr enables observations of extended regions on the sky, such as those from dark matter in the Galactic halo. Here we show limits on the dark matter annihilation cross-section and decay lifetime from HAWC observations of the Galactic halo with 15 months of data. These are some of the most robust limits on TeV and PeV dark matter, largely insensitive to the dark matter morphology. These limits begin to constrain models in which PeV IceCube neutrinos are explained by dark matter which primarily decays into hadrons.

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Section: Dark Matter Annihilation Limitsmentioning

confidence: 66%

Section: Dark Matter Decay Limitsmentioning

confidence: 99%

A search for dark matter in the Galactic halo with HAWC

Abeysekara

Albert

Alfaro

et al. 2018

J. Cosmol. Astropart. Phys.

Self Cite

View full text Add to dashboard Cite

show abstract

“…This second argument however does not hold for recent HESS limits [84] from 254 hours of observation of the GC. Nonetheless, to recast them for secluded DM models we could not use the same prescription we used for ANTARES limits, because of reason i) above.…”

Section: Indirect Detection Constraintsmentioning

confidence: 94%

Asymmetric dark matter: residual annihilations and self-interactions

et al. 2018

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Dark matter (DM) coupled to light mediators has been invoked to resolve the putative discrepancies between collisionless cold DM and galactic structure observations. However, γ-ray searches and the CMB strongly constrain such scenarios. To ease the tension, we consider asymmetric DM. We show that, contrary to the common lore, detectable annihilations occur even for large asymmetries, and derive bounds from the CMB, γ-ray, neutrino and antiproton searches. We then identify the viable space for self-interacting DM. Direct detection does not exclude this scenario, but provides a way to test it.

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“…In addition, we considered the limits given by the HESS Collaboration [57]. As they do not use the same set of parameter values for the DM halo profiles as ours, we renormalised their limits following the J-Factors calculated for our different halo profiles NFW, Einasto and Burkert to be consistent with the rest of our study.…”

Section: Jhep11(2017)132mentioning

confidence: 99%

“…This allows us to characterise the morphology of their sources and to observe regions where the dark matter particle density is expected to be large and to produce a sizeable flux. The Fermi-LAT space-borne telescope covers the GeV energy range whereas the ground based Cherenkov telescopes HESS [57], MAGIC [58], VERITAS [59] and HAWC [60] are sensitive to the TeV range. Since the density of dark matter particle is peaked in the center of the galaxy, the galactic center is one of the best targets to look for a dark matter signal.…”

Section: Jhep11(2017)132mentioning

confidence: 99%

Robustness of dark matter constraints and interplay with collider searches for New Physics

Arbey

Robbins

Mahmoudi

et al. 2017

J. High Energ. Phys.

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Abstract:We study the implications of dark matter searches, together with collider constraints, on the phenomenological MSSM with neutralino dark matter and focus on the consequences of the related uncertainties in some detail. We consider, inter alia, the latest results from AMS-02, Fermi-LAT and XENON1T. In particular, we examine the impact of the choice of the dark matter halo profile, as well as the propagation model for cosmic rays, for dark matter indirect detection and show that the constraints on the MSSM differ by one to two orders of magnitude depending on the astrophysical hypotheses. On the other hand, our limited knowledge of the local relic density in the vicinity of the Earth and the velocity of Earth in the dark matter halo leads to a factor 3 in the exclusion limits obtained by direct detection experiments. We identified the astrophysical models leading to the most conservative and the most stringent constraints and for each case studied the complementarities with the latest LHC measurements and limits from Higgs, SUSY and monojet searches. We show that combining all data from dark matter searches and colliders, a large fraction of our supersymmetric sample could be probed. Whereas the direct detection constraints are rather robust under the astrophysical assumptions, the uncertainties related to indirect detection can have an important impact on the number of the excluded points.

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Search for Dark Matter Annihilations towards the Inner Galactic Halo from 10 Years of Observations with H.E.S.S.

Cited by 327 publications

References 25 publications

A search for dark matter in the Galactic halo with HAWC

A search for dark matter in the Galactic halo with HAWC

Asymmetric dark matter: residual annihilations and self-interactions

Robustness of dark matter constraints and interplay with collider searches for New Physics

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