THE GALACTIC MAGNETIC FIELD

By R. Jansson, G. Farrar. 2012

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With this Letter, we complete our model of the Galactic magnetic field (GMF), by using the WMAP7 22 GHz total synchrotron intensity map and our earlier results to obtain a 13-parameter model of the Galactic random field, and to determine the strength of the striated random field. In combination with our 22-parameter description of the regular GMF, we obtain a very good fit to more than 40,000 extragalactic Faraday rotation measures and the WMAP7 22 GHz polarized and total intensity synchrotron emission maps. The data call for a striated component to the random field whose orientation is aligned with the regular field, having zero mean and rms strength ≈20% larger than the regular field. A noteworthy feature of the new model is that the regular field has a significant out-of-plane component, which had not been considered earlier. The new GMF model gives a much better description of the totality of data than previous models in the literature.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/1f747028615e474dca6b7c9f08dc103b67f07784

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Citations in the corpus

SIMULATIONS OF DISK GALAXIES WITH COSMIC RAY DRIVEN GALACTIC WINDS (2013, background): “…scales (∼100 pc), the strength of the random component of the galactic magnetic field is several times higher than the average field strength (e.g. Jansson & Farrar 2012) because galaxy formation processes (e.g. supernovae and hydrodynamical turbulence) in the disk (Breitschwerdt et al. 1991)…”
Planck 2015 results: XIX. Constraints on primordial magnetic fields (2015, unknown): “Although the precise geometry of these magnetic fields remains uncertain (see, e.g., Ruiz-Granados et al. 2010; Jansson & Farrar 2012), the Galactic Faraday depth could be a foreground for the primordial Faraday depth, at least on large scales.”
Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust (2014, background): “…Gaensler & Johnston 1995; Haverkorn et al. 2008), the GMF also possesses an ordered random (e.g., Beck 2009; Jaffe et al. 2010), or striated random (Jansson & Farrar 2012a), component, whose orientation remains nearly constant over large scales, but whose strength and sign vary on small scales.”
The Karl G. Jansky Very Large Array Sky Survey (VLASS). Science Case and Survey Design (2019, background): “…the improvement of electrondensity and magnetic field models for the Milky Way (e.g., Cordes & Lazio 2002; Yao et al. 2017; Van Eck et al. 2011; Jansson & Farrar 2012) by finding more pulsars in the Galactic Plane and Bulge, the discovery of compact binary systems (powerful laboratories for…”
Simulations of magnetic fields in isolated disc galaxies (2012, result): “We note that the structure of the simulated magnetic field is in good agreement with observational data of spiral galaxies (Beck 2007; Jansson & Farrar 2012b).”
An Indication of Anisotropy in Arrival Directions of Ultra-high-energy Cosmic Rays through Comparison to the Flux Pattern of Extragalactic Gamma-Ray Sources (2018, methodology): “We checked the plausibility of the best-fit search radius obtained above 39 EeV by simulating sky maps passed through the Galactic magnetic field from Jansson & Farrar (2012), including a random component with a coherence length of 60 pc as in Erdmann et al. (2016).”
Galactic synchrotron emission with cosmic ray propagation models (2013, methodology): “Pshirkov et al. (2011) selected two benchmark models, fitting different B-fields to the observed RMs. Jansson & Farrar (2012b), instead, derived their best-fitting model including also a striated component.”
CRPropa 3—a public astrophysical simulation framework for propagating extraterrestrial ultra-high energy particles (2016, methodology): “The galactic magnetic field models proposed by Jansson & Farrar [10, 15] and Pshirkov et al.”
The Nine Lives of Cosmic Rays in Galaxies (2015, methodology): “A new model by Jansson & Farrar (2012a) based on WMAP radio surveys and 40000 extragalactic rotation measures was compared with synchrotron data in Jansson & Farrar (2012b), and with WMAP polarization data in Farrar (2014).”