Dark matter constraints from a joint analysis of dwarf Spheroidal galaxy observations with VERITAS

Archambault, S.; Archer, A.; Benbow, W.; Bird, R.; Bourbeau, Etienne; Brantseg, Thomas; Buchovecky, M.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cerruti, M.; Christiansen, J. L.; Connolly, Michael; Cui, Wei; Daniel, M. K.; Feng, Q.; Finley, J. P.; Fleischhack, Henrike; Fortson, L.; Furniss, A.; Geringer-Sameth, Alex; Griffin, S.; Grube, J.; Hütten, Moritz; Håkansson, N.; Hanna, D.; Hervet, O.; Holder, J.; Hughes, G.; Hummensky, B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kelley-Hoskins, N.; Kertzman, M.; Kieda, D.; Koushiappas, Savvas M.; Krause, M.; Krennrich, F.; Lang, M. J.; Lin, T. T. Y.; McArthur, S.; Moriarty, P.; Mukherjee, R.; Nieto, D.; O’Brien, Stephan; Ong, R. A.; Otte, A. N.; Park, N.; Pohl, M.; Popkow, A.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Richards, G.; Roache, E.; Rulten, C. B.; Sadeh, I.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Smith, A. W.; Staszak, D.; Telezhinsky, I.; Trépanier, Samuel; Tucci, J. V.; Tyler, J.; Wakely, S. P.; Weinstein, A. J.R.; Wilcox, P.; Williams, D. A.; Zitzer, B.

doi:10.1103/physrevd.95.082001

Cited by 109 publications

(123 citation statements)

References 46 publications

(60 reference statements)

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“…With the high-dark-matter-density regions observed in astrophysical objects and the high-energy reach of astrophysical experiments, DM masses much greater than 1 TeV can be identified through their annihilation or decay products. Several experiments are currently searching for these particles [15][16][17][18][19][20][21][22][23][24] and several more are planned [25][26][27]. Nothing have been found yet but the parameter space for discovery is shrinking with time.…”

Section: Contentsmentioning

confidence: 99%

Searching for dark matter in the Galactic halo with a wide field of view TeV gamma-ray observatory in the Southern Hemisphere

Viana

Schoorlemmer

Albert

et al. 2019

J. Cosmol. Astropart. Phys.

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Despite mounting evidence that astrophysical dark matter exists in the Universe, its fundamental nature remains unknown. In this paper, we present the prospects to detect and identify dark matter particles through the observation of very-high-energy ( TeV) gamma-rays coming from the annihilation or decay of these particles in the Galactic halo. The observation of the the Galactic Center and a large fraction of the halo by a future wide field-of-view gamma-ray observatory located in the southern hemisphere would reach unprecedented sensitivity to dark matter particles in the mass range of ∼500 GeV to ∼2 PeV. Combined with other gamma-ray observatories (present and future) a thermal relic annihilation cross-section could be probed for all particle masses from ∼80 TeV down to the GeV range in most annihilation channels.

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Section: Contentsmentioning

confidence: 99%

Searching for dark matter in the Galactic halo with a wide field of view TeV gamma-ray observatory in the Southern Hemisphere

Viana

Schoorlemmer

Albert

et al. 2019

J. Cosmol. Astropart. Phys.

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“…These gamma-ray DM searches are complemented at larger WIMP masses by ground-based imaging atmospheric Cherenkov telescopes (IACTs) such as MAGIC, VERITAS and H.E.S.S. [26][27][28].An important fraction of objects in the Fermi-LAT catalogs are unidentified sources (unIDs), i.e., objects with no clear single association or counterpart, to either a known object identified at other wavelengths, or to a known source type emitting only in gamma rays (such as certain pulsars). 1 There is the exciting possibility that some of these unIDs may actually be DM subhalos.…”

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confidence: 99%

Unidentified gamma-ray sources as targets for indirect dark matter detection with theFermi-Large Area Telescope

Coronado-Blázquez

Domínguez

Aguirre-Santaella

et al. 2019

J. Cosmol. Astropart. Phys.

115

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One of the predictions of the ΛCDM cosmological framework is the hierarchical formation of structure, giving rise to dark matter (DM) halos and subhalos. When the latter are massive enough they retain gas (i.e., baryons) and become visible. This is the case of the dwarf satellite galaxies in the Milky Way (MW). Below a certain mass, halos may not accumulate significant amounts of baryons and remain completely dark. However, if DM particles are Weakly Interacting Massive Particles (WIMPs), we expect them to annihilate in subhalos, producing gamma rays which can be detected with the Fermi satellite. Using the three most recent point-source Fermi Large Area Telescope (LAT) catalogs (3FGL, 2FHL and 3FHL), we search for DM subhalo candidates among the unidentified sources, i.e., sources with no firm association to a known astrophysical object. We apply several selection criteria based on the expected properties of the DM-induced emission from subhalos, which allow us to significantly reduce the list of potential candidates. Then, by characterizing the minimum detection flux of the instrument and comparing our sample to predictions from the Via Lactea II (VL-II) N-body cosmological simulation, we place conservative and robust constraints on the σv − m DM parameter space. For annihilation via the τ + τ − channel, we put an upper limit of 4 × 10 −26 (5 × 10 −25 ) cm 3 s −1 for a mass of 10 (100) GeV. A critical improvement over previous treatments is the repopulation we made to include low-mass subhalos below the VL-II mass resolution. With more advanced subhalo candidate filtering the sensitivity reach of our method can potentially improve these constraints by a factor 3 (2) for τ + τ − (bb) channel.are an example of the most massive members of this population [11]. Yet, these dSphs are exceptional objects, in that they are massive enough to retain baryons (i.e., gas) and form stars. Conversely, the vast majority of the Galactic DM subhalos are not expected to host baryons and therefore remain completely dark [12]. Given their much larger number density, many of these small subhalos will be much closer to the Earth than the bigger ones, making them potentially interesting for dark matter searches.Should the Weakly Interacting Massive Particle (WIMP) DM model be correct (see, e.g., [13, 14] for a review), these objects may be detectable in the gamma-ray data. WIMPs can achieve the correct relic DM abundance (the so-called "WIMP miracle") through selfannihilation in the early Universe. Self-annihilation of WIMPs gives rise to a Standard Model (SM) particle-antiparticle pair which, among other possible subsequent by-products, typically yields gamma-ray photons. The ongoing self-annihilation of WIMPs in subhalos could be bright enough to be detectable.Since its launch in 2008, the Large Area Telescope on board the NASA Fermi Gammaray Space Telescope (Fermi-LAT) has been surveying the sky searching for gamma-ray sources [15]. The Fermi-LAT is a pair conversion telescope designed to observe the energy band from 20 MeV to gre...

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“…Figure 5: Limit on the thermally-averaged dark matter annihilation cross section σ A υ obtained for the combined analysis as a function of the WIMP mass m χ assuming the NFW halo profile for the τ + τ − (left) and bb (right) annihilation channel. Also shown are limits from IceCube [2], ANTARES [1], VERITAS [12], Fermi-MAGIC [13], as well as HESS [14]. It should be noted that this combined analysis treated under-fluctuations differently than what is presented in the ANTARES paper.…”

Section: Resultsmentioning

confidence: 99%

Combined Search for Neutrinos from Dark Matter Annihilation in the Galactic Center using IceCube and ANTARES

Sánchez¹,

Iovine²,

Tönnis³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The ANTARES and IceCube neutrino telescopes have both searched for neutrinos from dark matter annihilation in the Galactic Centre, putting limits on the thermally-averaged dark matter self-annihilation cross section σ A υ . For WIMP masses above 100 GeV, the most stringent limits were obtained by the ANTARES neutrino telescope, while for lower masses, limits achieved by IceCube are more competitive. The limits obtained by the two detectors are of comparable order of magnitude for WIMP masses going from 50 to 1000 GeV, making this mass range particularly interesting for a combined analysis. In this contribution, we present the limits of the first combined search for dark matter self-annihilation in the centre of the Milky Way using ANTARES and IceCube. The model parameters and the likelihood method were unified, thereby providing a benchmark for future dark matter searches conducted by each collaboration. By combining data of both detectors, we obtained improved limits with respect to the original limits published by the two collaborations.

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Dark matter constraints from a joint analysis of dwarf Spheroidal galaxy observations with VERITAS

Cited by 109 publications

References 46 publications

Searching for dark matter in the Galactic halo with a wide field of view TeV gamma-ray observatory in the Southern Hemisphere

Searching for dark matter in the Galactic halo with a wide field of view TeV gamma-ray observatory in the Southern Hemisphere

Unidentified gamma-ray sources as targets for indirect dark matter detection with theFermi-Large Area Telescope

Combined Search for Neutrinos from Dark Matter Annihilation in the Galactic Center using IceCube and ANTARES

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