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Article Dans Une Revue Astronomy and Astrophysics - A&A Année : 2023

Cosmic-ray electron transport in the galaxy M 51

Résumé

Indirect observations of the cosmic-ray electron (CRE) distribution via synchrotron emission is crucial for deepening the understanding of the CRE transport in the interstellar medium, and in investigating the role of galactic outflows. In this paper, we quantify the contribution of diffusion and advection dominated transport of cosmic-ray electrons in the galaxy M51 considering relevant energy loss processes. We use recent measurement from M51 that allow for the derivation of the diffusion coefficient, the star formation rate, and the magnetic field strength. With this input, we solve the 3D transport equation numerically including the spatial dependence as provided by the measurements, using the open-source transport framework CRPropa (v3.1). We include three-dimensional transport (diffusion and advection), and the relevant loss processes. We find that the data can be described well with the parameters from recent measurements. For the best fit, it is required that the wind velocity, following from the observed star formation rate, must be decreased by a factor of 5. We find that a model in which the inner galaxy is dominated by advective escape and the outer galaxy by diffusive one fits the data well. Three-dimensional modeling of cosmic-ray transport in the face-on galaxy M51 allows for conclusions about the strength of the outflow of such galaxies by quantifying the need for a wind in the description of the cosmic-ray signatures. This opens up the possibility of investigating galactic winds in face-on galaxies in general.

Dates et versions

hal-03718259 , version 1 (08-07-2022)

Identifiants

Citer

Julien Dörner, Patrick Reichherzer, Julia Becker Tjus, Volker Heesen. Cosmic-ray electron transport in the galaxy M 51. Astronomy and Astrophysics - A&A, 2023, 669, pp.A111. ⟨10.1051/0004-6361/202244331⟩. ⟨hal-03718259⟩
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