Searches for dark matter annihilation signatures in the Segue 1 satellite galaxy with the MAGIC-I telescope

Aleksić, J.; Álvarez, Ezequiel; Antonelli, L. A.; Antoranz, P.; Asensio, M.; Backes, Michael; Barrio, J. A.; Bastieri, D.; González, J. Becerra; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Böck, R.; Boller, A.; Bonnoli, G.; Tridon, D. Borla; Braun, I.; Bretz, T.; Cañellas, A.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Cossio, L.; Covino, S.; Dazzi, F.; Angelis, A. De; Pozo, E. De Cea del; Lotto, B. De; Mendez, C. Delgado; Ortega, A. Diago; Doert, M.; Domínguez, A.; Prester, D. Dominis; Dorner, D.; Doro, M.; Elsäesser, D.; Ferenc, D.; Fonseca, M. V.; Font, L.; Fruck, C.; López, R. J. García; Garczarczyk, M.; Garrido, Daniel; Giavitto, G.; Godinović, N.; Hadasch, D.; Häfner, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, Dario; Huber, Bernhard A.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Krause, J.; Barbera, A. La; Lelas, D.; Leonardo, E.; Lindfors, E.; Lombardi, S.; López, M.; Lorenz, E.; Makariev, M.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Munar-Androver, P.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paiano, S.; Paneque, D.; Paoletti, R.; Pardo, Sharon; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauß, F.; Pérez-Torres, M. A.; Peršić, M.; Peruzzo, L.; Pilia, M.; Pochon, J.; Prada, Francisco; Moroni, P. G. Prada; Prandini, E.; Puljak, I.; Reichardt, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Rügamer, S.; Saggion, A.; Saito, Koji; Saito, T.; Salvati, M.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, Steven N.; Sillanpää, A.; Sitarek, J.; Sobczyńska, D.; Spanier, F.; Spiro, S.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Surić, T.; Takalo, L. O.; Takami, H.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thom, M.; Tibolla, O.; Torres, D. F.; Treves, A.; Vankov, H.; Vogler, P.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.; Fornasa, Mattia; Essig, Rouven; Sehgal, Neelima; Strigari, Louis E.

doi:10.1088/1475-7516/2011/06/035

Cited by 99 publications

(94 citation statements)

References 108 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Because of the high energy and thus photon-limited regime in which ACTs operate, the dSphs are analyzed via an on-off strategy described above. Figures 16 and 17 present the limits on σ ann v from MAGIC (Aleksic et al, 2011) and VERITAS (Rico, 2011) observations of Segue 1. Figures 16 and 17 clearly show that ACTs are more sensitive to the higher dark matter mass regime than the Fermi-LAT analysis, though because of smaller exposures the limits are weaker by a couple of orders of magnitude as compared to the Fermi-LAT limits.…”

Section: Dwarf Spheroidalsmentioning

confidence: 99%

“…The indicated limits are Figure 16 Limits on the annihilation cross section as a function of WIMP mass, assuming 100% annihilation to bb and ττ . From the MAGIC collaboration (Aleksic et al, 2011). Figure 17 Limits on the annihilation cross section as a function of WIMP mass, assuming 100% annihilation to bb and ττ , and W + W − .…”

Section: Dwarf Spheroidalsmentioning

confidence: 99%

See 1 more Smart Citation

Galactic searches for dark matter

2013

View full text Add to dashboard Cite

For nearly a century, more mass has been measured in galaxies than is contained in the luminous stars and gas. Through continual advances in observations and theory, it has become clear that the dark matter in galaxies is not comprised of known astronomical objects or baryonic matter, and that identification of it is certain to reveal a profound connection between astrophysics, cosmology, and fundamental physics. The best explanation for dark matter is that it is in the form of a yet undiscovered particle of nature, with experiments now gaining sensitivity to the most well-motivated particle dark matter candidates. In this article, I review measurements of dark matter in the Milky Way and its satellite galaxies and the status of Galactic searches for particle dark matter using a combination of terrestrial and space-based astroparticle detectors, and large scale astronomical surveys. I review the limits on the dark matter annihilation and scattering cross sections that can be extracted from both astroparticle experiments and astronomical observations, and explore the theoretical implications of these limits. I discuss methods to measure the properties of particle dark matter using future experiments, and conclude by highlighting the exciting potential for dark matter searches during the next decade, and beyond.

show abstract

Section: Dwarf Spheroidalsmentioning

confidence: 99%

Section: Dwarf Spheroidalsmentioning

confidence: 99%

Galactic searches for dark matter

2013

View full text Add to dashboard Cite

show abstract

“…Although the extensive searches to date yield null results, tremendous progress has been made in recent years in the underground direct searches [1][2][3][4][5][6][7][8][9][10][11][12], in the indirect astrophysical searches [13][14][15][16][17][18][19][20], and at colliders [22][23][24][25][26][27].…”

Section: Introductionmentioning

confidence: 99%

Light neutralino dark matter: direct/indirect detection and collider searches

Han

Liu

2014

J. High Energ. Phys.

View full text Add to dashboard Cite

We study the neutralino being the Lightest Supersymmetric Particle (LSP) as a cold Dark Matter (DM) candidate with a mass less than 40 GeV in the framework of the Next-to-Minimal-Supersymmetric-Standard-Model (NMSSM). We find that with the current collider constraints from LEP, the Tevatron and the LHC, there are three types of light DM solutions consistent with the direct/indirect searches as well as the relic abundance considerations: (i) A 1 , H 1 -funnels, (ii) stau coannihilation and (iii) sbottom coannihilation. Type-(i) may take place in any theory with a light scalar (or pseudo-scalar) near the LSP pair threshold; while Type-(ii) and (iii) could occur in the framework of Minimal-Supersymmetric-Standard-Model (MSSM) as well. We present a comprehensive study on the properties of these solutions and point out their immediate relevance to the experiments of the underground direct detection such as superCDMS and LUX/LZ, and the astro-physical indirect search such as Fermi-LAT. We also find that the decays of the SM-like Higgs boson may be modified appreciably and the new decay channels to the light SUSY particles may be sizable. The new light CP-even and CP-odd Higgs bosons will decay to a pair of LSPs as well as other observable final states, leading to interesting new Higgs phenomenology at colliders. For the light sfermion searches, the signals would be very challenging to observe at the LHC given the current bounds. However, a high energy and high luminosity lepton collider, such as the ILC, would be able to fully cover these scenarios by searching for events with large missing energy plus charged tracks or displaced vertices.

show abstract

“…The Fermi-LAT [32,55,56], H.E.S.S. [57], VERITAS [33,58], and MAGIC [59,60] collaborations have all looked at dwarf spheroidal galaxies for low-background signals of dark matter annihilation. In Figure 2.…”

Section: Discussionmentioning

confidence: 99%

Sensitivity of HAWC to high-mass dark matter annihilations

Abeysekara¹,

Alfaro²,

Álvarez³

et al. 2014

Phys. Rev. D

View full text Add to dashboard Cite

The High Altitude Water Cherenkov (HAWC) observatory is a wide field-of-view detector sensitive to gamma rays of 100 GeV to a few hundred TeV. Located in central Mexico at 19• North latitude and 4100 m above sea level, HAWC will observe gamma rays and cosmic rays with an array of water Cherenkov detectors. The full HAWC array is scheduled to be operational in Spring 2015. In this paper, we study the HAWC sensitivity to the gamma-ray signatures of high-mass (multiTeV) dark matter annihilation. The HAWC observatory will be sensitive to diverse searches for dark matter annihilation, including annihilation from extended dark matter sources, the diffuse 2 gamma-ray emission from dark matter annihilation, and gamma-ray emission from non-luminous dark matter subhalos. Here we consider the HAWC sensitivity to a subset of these sources, including dwarf galaxies, the M31 galaxy, the Virgo cluster, and the Galactic center. We simulate the HAWC response to gamma rays from these sources in several well-motivated dark matter annihilation channels. If no gamma-ray excess is observed, we show the limits HAWC can place on the dark matter cross-section from these sources. In particular, in the case of dark matter annihilation into gauge bosons, HAWC will be able to detect a narrow range of dark matter masses to cross-sections below thermal. HAWC should also be sensitive to non-thermal cross-sections for masses up to nearly 1000 TeV. The constraints placed by HAWC on the dark matter cross-section from known sources should be competitive with current limits in the mass range where HAWC has similar sensitivity. HAWC can additionally explore higher dark matter masses than are currently constrained.

show abstract

Searches for dark matter annihilation signatures in the Segue 1 satellite galaxy with the MAGIC-I telescope

Cited by 99 publications

References 108 publications

Galactic searches for dark matter

Galactic searches for dark matter

Light neutralino dark matter: direct/indirect detection and collider searches

Sensitivity of HAWC to high-mass dark matter annihilations

Contact Info

Product

Resources

About