Utilizing cosmic-ray positron and electron observations to probe the averaged properties of Milky Way pulsars

Cholis, Ilias; Krommydas, Iason

doi:10.5281/zenodo.5659004

Cited by 1 publication

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“…In a separate paper (Krommydas & Cholis 2023), we explore the possible impact these lower-energy features have on dark matter limits. We make publicly available our burst simulations in Cholis & Krommydas (2022a), while our background simulations are available through Cholis & Krommydas (2021, 2022b.…”

Section: Results and Conclusionmentioning

confidence: 99%

Possible Counterpart Signal of the Fermi Bubbles at the Cosmic-Ray Positrons

Cholis

Krommydas

2023

ApJ

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The inner Galaxy has hosted cosmic-ray burst events, including those responsible for the gamma-ray Fermi bubbles and the eROSITA bubbles in X-rays. In this work, we study the Alpha Magnetic Spectrometer positron fraction and find three features around 12, 21, and 48 GeV, of which the lowest energy has a 1.4–4.9σ significance, depending on astrophysical background assumptions. Using background simulations that explain the cosmic-ray positron fraction, positron flux, and electron plus positron flux by primary and secondary cosmic rays and cosmic rays from local pulsars, we test these spectral features as originating from electron/positron burst events from the inner Galaxy. We find the 12 GeV feature to be explained by an event of age τ ≃ 3–10 Myr, in agreement with the proposed age of the Fermi bubbles. Furthermore, the energy in cosmic-ray electrons and positrons propagating along the Galactic disk and not within the Fermi bubbles volume is estimated to be 1051.5–1057.5 erg, or O(10−4) − O(1) the cosmic-ray energy causing the Fermi bubbles. We advocate that these positron fraction features are the counterpart signals of the Fermi bubbles, or of substructures within them, or of the eROSITA bubbles.

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