Measurement of the high-energy gamma-ray emission from the Moon with the Fermi Large Area Telescope

Ackermann, M.; Ajello, M.; Albert, A.; Atwood, W. B.; Baldini, Luca; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bonino, R.; Bottacini, E.; Bregeon, J.; Bruel, Pascal; Buehler, R.; Caliandro, G. A.; Cameron, R. A.; Caragiulo, M.; Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Chekhtman, A.; Chiang, J.; Chiaro, G.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Costanza, F.; Cuoco, A.; Cutini, S.; D’Ammando, F.; Angelis, A. De; Palma, F. de; Desiante, R.; Digel, S. W.; Venere, L. Di; Drell, P. S.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Franckowiak, A.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Harding, A. K.; Hewitt, J. W.; Horan, D.; Hou, X.; Iafrate, G.; Jóhannesson, G.; Kamae, T.; Kuss, M.; Larsson, Stefan; Latronico, L.; Li, J.; Li, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill, J. D.; Maldera, S.; Manfreda, Alberto; Mayer, M.; Mazziotta, M. N.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monzani, M. E.; Morselli, A.; Murgia, S.; Nuss, E.; Omodei, N.; Orlando, E.; Ormes, J. F.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Pivato, G.; Rainò, S.; Rando, R.; Razzano, M.; Reimer, A.; Reimer, O.; Reposeur, T.; Sgrò, C.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli, P.; Takahashi, H.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Troja, E.; Vianello, G.; Winer, B. L.; Wood, K. S.; Yassine, M.; Cerutti, F.; Ferrari, A.; Sala, P.

doi:10.1103/physrevd.93.082001

Cited by 28 publications

(26 citation statements)

References 32 publications

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“…8, within their statistical errors. 14 The high-energy emission of the Moon peaked at about 200 MeV, with a similar intensity than the Sun [54]. However, at higher energies, it has an energy spectrum that is steeper than that of the Sun.…”

Section: Effect Of the Gamma-ray Emission From The Sunmentioning

confidence: 98%

Angular power spectrum of the diffuse gamma-ray emission as measured by the Fermi Large Area Telescope and constraints on its dark matter interpretation

et al. 2016

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The isotropic gamma-ray background arises from the contribution of unresolved sources, including members of confirmed source classes and proposed gamma-ray emitters such as the radiation induced by dark matter annihilation and decay. Clues about the properties of the contributing sources are imprinted in the anisotropy characteristics of the gamma-ray background. We use 81 months of Pass 7 Reprocessed data from the Fermi Large Area Telescope to perform a measurement of the anisotropy angular power spectrum of the gamma-ray background. We analyze energies between 0.5 and 500 GeV, extending the range considered in the previous measurement based on 22 months of data. We also compute, for the first time, the cross-correlation angular power spectrum between different energy bins. We find that the derived angular spectra are compatible with being Poissonian, i.e. constant in multipole. Moreover, the energy dependence of the anisotropy suggests that the signal is due to two populations of sources, contributing, respectively, below and above ∼2 GeV. Finally, using data from state-of-the-art numerical simulations to model the dark matter distribution, we constrain the contribution from dark matter annihilation and decay in Galactic and extragalactic structures to the measured anisotropy. These constraints are competitive with those that can be derived from the average intensity of the isotropic gamma-ray background.

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Section: Effect Of the Gamma-ray Emission From The Sunmentioning

confidence: 98%

Angular power spectrum of the diffuse gamma-ray emission as measured by the Fermi Large Area Telescope and constraints on its dark matter interpretation

et al. 2016

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“…The Sun and Moon emission are modulated by the solar magnetic field, which deflects cosmic rays more (and therefore reduces γ-ray emission) when the Sun is at maximum activity. For that reason, the model used in 3FGL (based on the first 18 months of data when the Sun was near minimum) was not adequate for 8 yr. We used the improved model of the lunar emission (Ackermann et al 2016a) and a data-based model of the solar disk and inverse-Compton scattering on the solar light (S. Raino 2019, private communication).…”

Section: Solar and Lunar Templatementioning

confidence: 99%

Fermi Large Area Telescope Fourth Source Catalog

Abdollahi

Acero

Ackermann

et al. 2020

ApJS

Self Cite

1,203

842

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We present the fourth Fermi Large Area Telescope catalog (4FGL) of γ-ray sources. Based on the first eight years of science data from the Fermi Gamma-ray Space Telescope mission in the energy range from 50MeV to 1TeV, it is the deepest yet in this energy range. Relative to the 3FGL catalog, the 4FGL catalog has twice as much exposure as well as a number of analysis improvements, including an updated model for the Galactic diffuse γ-ray emission, and two sets of light curves (one-year and two-month intervals). The 4FGL catalog includes 5064 sources above 4σ significance, for which we provide localization and spectral properties. Seventy-five sources are modeled explicitly as spatially extended, and overall, 358 sources are considered as identified based on angular extent, periodicity, or correlated variability observed at other wavelengths. For 1336 sources, we have not found plausible counterparts at other wavelengths. More than 3130 of the identified or associated sources are active galaxies of the blazar class, and 239 are pulsars.

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“…Requiring that the actual capture rate is smaller by the factor 1/200 than this geometric maximum gives constraints on the DM parameters. Likewise, the γ-ray flux from the Moon is measured by the Fermi-LAT satellite to be ∼ 10 −4 MeV/cm 2 s [18], which corresponds to the total power of ∼ 3 × 10 −7 TW. Again, requiring that the limb of DM annihilations around Moon does not over-shine this measured value gives additional constraints on DM parameters.…”

Section: Introductionmentioning

confidence: 99%

Constraints on dark matter from the Moon

Garani

Tinyakov

2020

Physics Letters B

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New and complimentary constraints are placed on the spin-independent interactions of dark matter with baryonic matter. Similar to the Earth and other planets, the Moon does not have any major internal heat source. We derive constraints by comparing the rate of energy deposit by dark matter annihilations in the Moon to 12 mW/m 2 as measured by the Apollo mission. For light dark matter of mass O(10) GeV, we also examine the possibility of dark matter annihilations in the Moon limb. In this case, we place constraints by comparing the photon flux from such annihilations to that of the Fermi-LAT measurement of 10 −4 MeV/cm 2 s. This analysis excludes spin independent cross section 10 −37 cm 2 for dark matter mass between 30 and 50 GeV.

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Measurement of the high-energy gamma-ray emission from the Moon with the Fermi Large Area Telescope

Cited by 28 publications

References 32 publications

Angular power spectrum of the diffuse gamma-ray emission as measured by the Fermi Large Area Telescope and constraints on its dark matter interpretation

Angular power spectrum of the diffuse gamma-ray emission as measured by the Fermi Large Area Telescope and constraints on its dark matter interpretation

Fermi Large Area Telescope Fourth Source Catalog

Constraints on dark matter from the Moon

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