Search for Very High-energy Gamma Rays from the Northern Fermi Bubble Region with HAWC

Abeysekara, A. U.; Albert, A.; Alfaro, R.; Álvarez, C.; Álvarez, José David Ruiz; Arceo, R.; Arteaga‐Velázquez, J. C.; Solares, H. A. Ayala; Barber, Ahron S.; Bautista-Elivar, N.; Becerril, A.; Belmont‐Moreno, E.; BenZvi, S.; Berley, D.; Braun, J.; Brisbois, C.; Caballero-Mora, K. S.; Capistrán, T.; Carramiñana, A.; Casanova, S.; Castillo, M.; Cotti, U.; Cotzomi, J.; León, S. Coutińo de; León, C. De; Fuente, Eduardo de la; Hernández, R. Díaz; Dingus, B. L.; DuVernois, Michael; Díaz–Vélez, Juan Carlos; Ellsworth, R. W.; Engel, Kristi; Fick, B.; Fiorino, D. W.; Fleischhack, Henrike; Fraija, N.; García-González, J. A.; Garfias, F.; Gerhardt, M.; Muñoz, A. González; González, M. M.; Goodman, J. A.; Hampel-Arias, Z.; Harding, J. Patrick; Hernández, S.; Hernández-Almada, A.; Hinton, J. A.; Hona, B.; Hui, C. M.; Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, Vikas; Kaufmann, S.; Kieda, D.; Lara, A.; Lauer, R.; Lee, W. H.; Lennarz, D.; Vargas, H. León; Linnemann, J.; Longinotti, A. L.; Raya, Gabriel; Luna-García, R.; López-Coto, R.; Malone, K.; Marinelli, S. S.; Martı́nez, O.; Martínez-Castellanos, I.; Martínez-Castro, J.; Martínez-Huerta, H.; Matthews, John; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.; Nellen, L.; Newbold, M.; Nisa, Mehr; Noriega-Papaqui, R.; Pelayo, R.; Pretz, J.; Pérez-Pérez, E. G.; Ren, Z.; Rho, Chang Dong; Rivière, C.; Rosa-González, D.; Rosenberg, M.; Ruiz-Velasco, E.; Salazar, H.; Greus, F. Salesa; Sandoval, A.; Schneider, M.; Schoorlemmer, H.; Sinnis, G.; Smith, A. J.; Springer, R. W.; Surajbali, P.; Taboada, I.; Tibolla, O.; Tollefson, K.; Torres, I.; Ukwatta, T. N.; Vianello, G.; Weisgarber, T.; Westerhoff, S.; Wisher, I. G.; Wood, J.; Yapici, T.; Yodh, G.; Zepeda, A.; Zhou, H.

doi:10.3847/1538-4357/aa751a

Cited by 45 publications

(68 citation statements)

References 21 publications

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“…A search for gamma-ray signals from the Northern Fermi Bubble region has been presented in ref. [50]. The same analysis procedure, data, analysis bins, and search region are used here.…”

Section: Methodsmentioning

confidence: 99%

“…The data are binned according to f Hit,the fraction of functioning photomultipliers triggered in an air shower event. Table 1 in [50] defines the values for each analysis bin. For details about the detector see ref.…”

Section: Methodsmentioning

confidence: 99%

“…[50], is to estimate the background. There are three main factors that need to be considered for this: to distinguish the air showers produced by hadronic cosmic rays from those produced by gamma rays; to find the isotropic flux of hadronic cosmic rays through the direct integration (DI) method [52]; and to remove the effects of the large-scale cosmic-ray anisotropy [53].…”

Section: Methodsmentioning

confidence: 99%

“…• The systematic errors are well-characterized, including an understanding of the background exclusion mask and well-behaved background significance distribution [50] The DM limits do not strongly depend on the chosen region-of-interest, but the characterized systematics and lack of astrophysical gamma rays in the Northern Fermi Bubble region-ofinterest makes the analysis robust. Additionally, this is an excellent example of how DM limits are based on flux limits, so a calculated flux limit can be used to limit DM annihilation and decay.…”

Section: Using Hawc To Constrain Dmmentioning

confidence: 99%

“…This leverages the previous analysis done in ref. [50] which has characterized the HAWC analysis of this region of the sky. The previous analysis of the Northern Fermi Bubble can be conveniently adapted for HAWC searches for galactocentric DM because:…”

Section: Using Hawc To Constrain Dmmentioning

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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“…A search for gamma-ray signals from the Northern Fermi Bubble region has been presented in ref. [50]. The same analysis procedure, data, analysis bins, and search region are used here.…”

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Methodsmentioning

confidence: 99%

Section: Using Hawc To Constrain Dmmentioning

confidence: 99%

Section: Using Hawc To Constrain Dmmentioning

confidence: 99%

See 3 more Smart Citations

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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Cosmic ray feedback in galaxies and galaxy clusters

Ruszkowski,

Pfrommer

2023

Astron Astrophys Rev

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Understanding the physical mechanisms that control galaxy formation is a fundamental challenge in contemporary astrophysics. Recent advances in the field of astrophysical feedback strongly suggest that cosmic rays (CRs) may be crucially important for our understanding of cosmological galaxy formation and evolution. The appealing features of CRs are their relatively long cooling times and relatively strong dynamical coupling to the gas. In galaxies, CRs can be close to equipartition with the thermal, magnetic, and turbulent energy density in the interstellar medium, and can be dynamically very important in driving large-scale galactic winds. Similarly, CRs may provide a significant contribution to the pressure in the circumgalactic medium. In galaxy clusters, CRs may play a key role in addressing the classic cooling flow problem by facilitating efficient heating of the intracluster medium and preventing excessive star formation. Overall, the underlying physics of CR interactions with plasmas exhibit broad parallels across the entire range of scales characteristic of the interstellar, circumgalactic, and intracluster media. Here we present a review of the state-of-the-art of this field and provide a pedagogical introduction to cosmic ray plasma physics, including the physics of wave–particle interactions, acceleration processes, CR spatial and spectral transport, and important cooling processes. The field is ripe for discovery and will remain the subject of intense theoretical, computational, and observational research over the next decade with profound implications for the interpretation of the observations of stellar and supermassive black hole feedback spanning the entire width of the electromagnetic spectrum and multi-messenger data.

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