CONSTRAINTS ON THE GALACTIC HALO DARK MATTER FROM<i>FERMI</i>-LAT DIFFUSE MEASUREMENTS

Ackermann, M.; Ajello, M.; Atwood, W. B.; Baldini, Luca; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Brandt, T. J.; Bregeon, J.; Brigida, M.; Bruel, Pascal; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cuoco, A.; Cutini, S.; D’Ammando, F.; Angelis, A. De; Palma, F. de; Dermer, C. D.; Silva, E. Do Couto E; Drell, P. S.; Drlica-Wagner, A.; Falletti, L.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Germani, S.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Guiriec, S.; Gustafsson, M.; Hadasch, D.; Hayashida, M.; Horan, D.; Hughes, R. E.; Jackson, M. S.; Jogler, T.; Jóhannesson, G.; Johnson, A. S.; Kamae, T.; Knödlseder, J.; Kuss, M.; Landé, J.; Latronico, L.; Lionetto, Andrea; Garde, M. Llena; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Méhault, J.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monte, C.; Monzani, M. E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godó, M.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Orienti, M.; Orlando, E.; Ormes, J. F.; Paneque, D.; Panetta, J.; Pesce-Rollins, M.; Pierbattista, M.; Piron, F.; Pivato, G.; Poon, H.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Romoli, C.; Sbarra, C.; Scargle, Jeffrey D.; Sgrò, C.; Siskind, E. J.; Spandre, G.; Spinelli, P.; Stawarz, Ł.; Strong, A. W.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, Takaaki; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Tosti, G.; Troja, E.; Usher, T.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Wallace, E.; Wood, K. S.; Wood, M.; Yang, Z.; Zaharijaš, Gabrijela; Zimmer, S.

doi:10.1088/0004-637x/761/2/91

Cited by 218 publications

(239 citation statements)

References 71 publications

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“…[58] could lead to the τ χ lower limits of the order of ∼(10 24 -10 26 ) s for m χ between 1 and 20 TeV. Figure 14 shows the results of this work, assuming the 2-body decay of scalar DM [56]), and VERITAS (dotted lines, [24]). For the leptonic channels, µ + µ − and τ + τ − , also shown are the regions that allow fit to the PAMELA, Fermi -LAT and H.E.S.S.…”

Section: Secondary Photons From Final State Standard Model Particlesmentioning

confidence: 82%

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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Section: Secondary Photons From Final State Standard Model Particlesmentioning

confidence: 82%

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

Aleksić

2016

Springer Theses

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“…In addition, because of the proximity the γ ray distribution can be expected to be resolved, and therefore the exact choice of the expected radial profile of the dark matter distribution has a rather large effect when deriving the limits (in choosing the optimal extraction region). Data from the Fermi LAT have been used to search for an annihilation signal from the galactic dark matter halo (63) and also from the central part of the Galaxy (64). In both cases, rather conservative limits that assume only the Galactic diffuse emission and dark matter annihilation to contribute to the observed signals provide limits that are comparable to those reached by the stacking of dwarf spheroidals.…”

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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“…The lifetime of Weak-scale DM is constrained from observations with the Fermi Large Area Telescope (Fermi LAT) to τ 10 26 sec [28][29][30][31][32], many orders of magnitude larger than the age of the Universe. For DM below O(100 MeV), the usual gamma ray constraints from the Fermi LAT do not apply, although the instruments on several other satellites (listed in table 1 below) are sensitive to photons with energies well below a GeV.…”

Section: Jhep11(2013)193mentioning

confidence: 99%

Constraining light dark matter with diffuse X-ray and gamma-ray observations

Essig

Kuflik

McDermott

et al. 2013

J. High Energ. Phys.

311

431

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We present constraints on decaying and annihilating dark matter (DM) in the 4 keV to 10 GeV mass range, using published results from the satellites HEAO-1, INTEGRAL, COMPTEL, EGRET, and the Fermi Gamma-ray Space Telescope. We derive analytic expressions for the gamma-ray spectra from various DM decay modes, and find lifetime constraints in the range 10 24 − 10 28 sec, depending on the DM mass and decay mode. We map these constraints onto the parameter space for a variety of models, including a hidden photino that is part of a kinetically mixed hidden sector, a gravitino with Rparity violating decays, a sterile neutrino, DM with a dipole moment, and a dark pion. The indirect constraints on sterile-neutrino and hidden-photino DM are found to be more powerful than other experimental or astrophysical probes in some parts of parameter space. While our focus is on decaying DM, we also present constraints on DM annihilation to electron-positron pairs. We find that if the annihilation is p-wave suppressed, the galactic diffuse constraints are, depending on the DM mass and velocity at recombination, more powerful than the constraints from the Cosmic Microwave Background.

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CONSTRAINTS ON THE GALACTIC HALO DARK MATTER FROMFERMI-LAT DIFFUSE MEASUREMENTS

Cited by 218 publications

References 71 publications

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

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

Indirect detection of dark matter with γ rays

Constraining light dark matter with diffuse X-ray and gamma-ray observations

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