Modeling Large-Scale Magnetic Fields in the Milky Way - ESA

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Cartoon example:coherent+ isotropic random+ inhomogeneous+ anisotropic• With a reasonable estimate for ne,RMs give Bcoh.• Added simple homogeneous,isotropic GRF produces most of thetotal I but not its morphology.• Amplification of random field inarms (inhomogeneous), but stillisotropic, can fit total I but not PI.• Random field stretched along arm giving“ordered random “ component in additionto the isotropic random component.=> With three observables,constrain three field components:Bcoh, Biso, and BordT. Jaffe @ ESAC, 30 May 2013
First results:• 8 parameters fit: φ0, a0 - a4(arms+ring), BRMS, ford.• Orientation of spiral matches NE2001ne model.• Reversal in Scutum-Crux arm and“molecular ring”.• Coherent, isotropic random, orderedfield energy densities in ratios of 1:5:3(roughly 2, 4, and 3 μG along armridges, but this is model dependent).• Weak Sag-Carina arm? Mentioned inBenjamin et al. (2005) using GLIMPSEcounts. Two dominant arms?Reversals?Jaffe et al. (2010)Main limitation: assumes simple power-law CRE spectrum from 0.1 to 1000 GeV. ButCRE spectrum is degenerate with ford. To break the degeneracy, need an additionalfrequency.Interestingly, 2.3 GHz total I is not compatible with this model!T. Jaffe @ ESAC, 30 May 2013
Page 1 and 2: Modeling Galactic Magnetic Fieldswi
Page 3 and 4: CMB foregrounds: Planck view(ESA, H
Page 5 and 6: External galaxies: other examplesNG
Page 7 and 8: Small-scale field: TurbulenceEMLS I
Page 9 and 10: GeometryCoherent• Coherent contri
Page 11 and 12: A very brief review of recent workT
Page 13 and 14: Field reversals?• Reversals => dy
Page 15 and 16: Local structure?• Sky visibly dom
Page 17 and 18: Modeling: hammurabi• Hammurabi Co
Page 19 and 20: Cartoon example:T. Jaffe @ ESAC, 30
Page 21 and 22: Cartoon example:coherent+ isotropic
Page 23: Cartoon example:coherent+ isotropic
Page 27 and 28: CRE results:0.408 GHz(total I)2.3 G
Page 29 and 30: Spiral arm ridges: separable?Spiral
Page 31 and 32: Arm modulation?• Model of shock c
Page 33 and 34: Small scales: turbulence and depola
Page 35 and 36: Radio spurs, microwave haze, and Fe
Page 37 and 38: Prospects:• C-Band All Sky Survey
Page 39 and 40: SKA!SKA will allow Faraday RM measu

Modeling Large-Scale Magnetic Fields in the Milky Way - ESA

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