Search for a Dark Matter Annihilation Signal from the Galactic Center Halo with H.E.S.S.

Abramowski, A.; Acero, Fabio; Aharonian, F.; Akhperjanian, A. G.; Anton, G.; Barnacka, A.; Almeida, U. Barres de; Bazer‐Bachi, A. R.; Becherini, Y.; Becker, J.; Behera, B.; Bernlöhr, K.; Bochow, A.; Boisson, C.; Bolmont, J.; Bordas, P.; Borrel, V.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Büsching, I.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Charbonnier, A.; Chaves, R. C. G.; Cheesebrough, A.; Chounet, L.‐M.; Clapson, A. C.; Coignet, G.; Conrad, J.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; Dickinson, H. J.; Djannati‐Ataï, A.; Domainko, W.; Drury, L. O’c.; Dubois, F.; Dubus, G.; Dyks, J.; Dyrda, M.; Egberts, K.; Eger, P.; Espigat, P.; Fallon, L.; Farnier, C.; Fegan, S. J.; Feinstein, F.; Fernandes, M. V.; Fiaßon, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gallant, Y. A.; Gast, H.; Gérard, L.; Gerbig, D.; Giebels, B.; Glicenstein, J. F.; Glück, B.; Goret, P.; Göring, D.; Hague, J. D.; Hampf, D.; Hauser, M.; Heinz, Sebastian; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hoffmann, A.; Hofmann, W.; Hofverberg, P.; Horns, D.; Jachołkowska, A.; Jager, O. C. de; Jahn, C.; Jamrozy, M.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Keogh, D.; Kerschhaggl, M.; Khangulyan, D.; Khélifi, B.; Klochkov, D.; Kluźniak, W.; Kneiske, T.; Komin, Nu.; Kosack, K.; Kossakowski, R.; Laffon, H.; Lamanna, G.; Lennarz, D.; Löhse, T.; Lopatin, A.; Lu, C. C.; Marandon, V.; Marcowith, A.; Masbou, J.; Maurin, D.; Maxted, N.; McComb, T. J. L.; Medina, M. C.; Méhault, J.; Moderski, R.; Moulin, Emmanuel; Naumann, C. L.; Naumann-Godó, M.; Naurois, M. de; Nedbal, D.; Nekrassov, D.; Nguyen, N.; Nicholas, B.; Niemiec, J.; Nolan, S. J.; Ohm, S.; Olive, J.‐F.; Wilhelmi, E. de Oña; Opitz, B.; Ostrowski, M.; Panter, M.; Arribas, M. Paz; Pedaletti, G.; Pelletier, G.; Petrucci, P.-O.; Pita, S.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raue, M.; Rayner, S. M.; Reimer, A.; Reimer, O.; Renaud, M.; Reyes, R. de los; Rieger, F.; Ripken, J.; Rob, L.; Rosier‐Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Ryde, F.; Sahakian, V.; Santangelo, A.; Schlickeiser, R.; Schöck, F. M.; Schönwald, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Shalchi, A.; Sikora, Marek; Skilton, J. L.; Sol, H.; Spengler, G.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Sushch, I.; Szostek, A.; Tavernet, J.‐P.; Terrier, R.; Tibolla, O.; Tluczykont, M.; Valerius, K.; Eldik, C. van; Vasileiadis, G.; Venter, C.; Vialle, J. P.; Viana, A.; Vincent, P.; Vivier, M.; Völk, H. J.; Volpe, F.; Vorobiov, S.; Vorster, M.; Wagner, S. J.; Ward, M. J.; Wierzcholska, A.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H. S.

doi:10.1103/physrevlett.106.161301

Cited by 249 publications

(316 citation statements)

References 32 publications

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“…collaboration has set the most constraining limits on the annihilation interaction rate for masses >1 TeV, reaching ∼ 7 × 10 25 cm 2 · s 1 at 1 TeV for the bb channel (70).…”

Section: Observational Resultsmentioning

confidence: 99%

Indirect detection of dark matter with γ rays

Funk

2014

Proc. Natl. Acad. Sci. U.S.A.

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The details of what constitutes the majority of the mass that makes up dark matter in the Universe remains one of the prime puzzles of cosmology and particle physics today-80 y after the first observational indications. Today, it is widely accepted that dark matter exists and that it is very likely composed of elementary particles, which are weakly interacting and massive [weakly interacting massive particles (WIMPs)]. As important as dark matter is in our understanding of cosmology, the detection of these particles has thus far been elusive. Their primary properties such as mass and interaction cross sections are still unknown. Indirect detection searches for the products of WIMP annihilation or decay. This is generally done through observations of γ-ray photons or cosmic rays. Instruments such as the Fermi large-area telescope, high-energy stereoscopic system, major atmospheric gamma-ray imaging Cherenkov, and very energetic radiation imaging telescope array, combined with the future Cherenkov telescope array, will provide important complementarity to other search techniques. Given the expected sensitivities of all search techniques, we are at a stage where the WIMP scenario is facing stringent tests, and it can be expected that WIMPs will be either be detected or the scenario will be so severely constrained that it will have to be rethought. In this sense, we are on the threshold of discovery. In this article, I will give a general overview of the current status and future expectations for indirect searches of dark matter (WIMP) particles.T here is a broad consensus that dark matter (DM) is made up of elementary particles. The most promising candidates are weakly interacting massive particles (WIMPs), particularly if they also form the lightest supersymmetric particle. The general assumption is that the thermal freeze-out in the early Universe leaves a relic density of dark matter particles in the current Universe (after the freeze-out, the particles become too diluted to annihilate in appreciable numbers and thermal energies were too low to produce them; the comoving density is therefore roughly constant since then). The annihilation of these particles into standard model particles controls the abundance in the Universe; thus, there is a tight connection between the annihilation cross section and cosmologically relevant quantities. For particles annihilating (in the simplest case, i.e., annihilating through S waves) (1), the relic density only depends on the annihilation cross section σ ann weighted by the average velocity of the particle (2) Ω χ h 2 = 0:11 3 × 10 −26 cm 3 · s −1 hσ ann vi :As the value for the relic dark matter density from cosmic microwave background (CMB) observations is Ω χ h 2 = 0:113 ± 0:004 (3), it follows that the expected velocity-weighted annihilation cross section is in the range of 3 × 10 −26 cm 3 · s −1 . This represents a striking connection that for typical gauge couplings to ordinary standard model particles and a dark matter mass at the weak interaction scale, WIMPs have the...

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“…collaboration has set the most constraining limits on the annihilation interaction rate for masses >1 TeV, reaching ∼ 7 × 10 25 cm 2 · s 1 at 1 TeV for the bb channel (70).…”

Section: Observational Resultsmentioning

confidence: 99%

Indirect detection of dark matter with γ rays

Funk

2014

Proc. Natl. Acad. Sci. U.S.A.

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“…(assuming generic qq final state, [47]); and iii) ∼48 hours of the Segue 1 observations with VERITAS [24]. Note, however, that the VERITAS results have been questioned in reference [28], where it is discussed why the VERITAS limits could be over-constraining by a factor two or more.…”

Section: Secondary Photons From Final State Standard Model Particlesmentioning

confidence: 99%

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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“…HESS measurements of signals coming from the Galactic Centre set limits of σv ≈ 10 −25 − 10 −24 cm 3 /s for DM masses up to TeV scales [44].…”

Section: Jhep11(2014)016mentioning

confidence: 99%

Dark matter with two inert doublets plus one Higgs doublet

Keus

King

Moretti

et al. 2014

J. High Energ. Phys.

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Following the discovery of a Higgs boson, there has been renewed interest in the general 2-Higgs-Doublet Model (2HDM). A model with One Inert Doublet plus One Higgs Doublet (I(1+1)HDM), where one of the scalar doublets is "inert" (since it has no vacuum expectation value and does not couple to fermions) has an advantage over the 2HDM since it provides a good Dark Matter (DM) candidate, namely the lightest inert scalar. Motivated by the existence of three fermion families, here we consider a model with two scalar doublets plus one Higgs doublet (I(2+1)HDM), where the two scalar doublets are inert. The I(2+1)HDM has a richer phenomenology than either the I(1+1)HDM or the 2HDM. We discuss the new regions of DM relic density in the I(2+1)HDM with simplified couplings and address the possibility of constraining the model using recent results from the Large Hadron Collider (LHC) and DM direct detection experiments.

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Search for a Dark Matter Annihilation Signal from the Galactic Center Halo with H.E.S.S.

Cited by 249 publications

References 32 publications

Indirect detection of dark matter with γ rays

Indirect detection of dark matter with γ rays

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

Dark matter with two inert doublets plus one Higgs doublet

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