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Article Contents

ABSTRACT

1.INTRODUCTION
1.1.Review Scope and Type
1.2.Polarimetry

2.SELECTED CELESTIAL ZONES IN OUR GALAXY
2.1.Methodology and Techniques
2.1.1.Optical dust absorption
2.1.2.Infrared Dust Emission
2.1.3.Radio Zeeman Effect
2.1.4.Radio Faraday Rotation
2.2.Interstellar objects ( ~ 1 to 50 pc)
2.2.1.Excess line width Wexcess relationship with Object size R
2.2.2.Globules and Magnetic Fields
2.2.3.Narrow Magnetized Features
2.2.4.Magnetic field versus Gas density, on medium linear scales (B ~ n0.5)
2.2.5.Magnetic field shapes in Dusty Elongated Molecular Clouds
2.3.Interstellar Superbubbles and shells with B ~ n1 (~ 50 to 500 pc)
2.4.Magnetic fields and Supernovae (B ~ n1)
2.5.The Center of the Milky Way Galaxy's disk (~ 8 kpc away)

3.THE MILKY WAY AS A WHOLE
3.1.Magnetic fields and Interstellar Superbubbles
3.2.Magnetic fields and Spiral Arms (~ 15 kpc)
3.3.Distribution of Breg, with galactic radius
3.3.1.Direction of Breg
3.3.2.Location of zero Breg
3.3.3.Strength of Breg
3.4.Distribution of Bran, and strength
3.5.Larger scale view - ASS or BSS
3.5.1.ASS for the Milky Way
3.5.2.Pitfalls of the BSS model
3.6.Seeds of galactic magnetism
3.6.1.Primordial cosmological magnetic seeds in galaxies
3.6.2.Battery origin for magnetic seeds in galaxies
3.6.3.Recent local origins for the magnetic seeds in galaxies
3.7.Galactic Magnetic field Interpretations - dynamos or not ?
3.7.1.Basic notions
3.7.2.Future trends in Galactic Dynamos

4.NEARBY SPIRAL GALAXIES
4.1.Methodology - different methods to obtain the magnetic field strength
4.1.1.Faraday Method
4.1.2.Equipartition Method
4.1.3.Cosmic-ray Method
4.1.4.Comparisons
4.2.Galactic magnetic field B and star formation SF
4.2.1.Observed weak relationship of B with SF
4.2.2.Expected weak relationship of B with SF
4.2.3.Magnetic fields versus Gas density, on large linear scales (B ~ n0.2)
4.2.4.Gas density versus Star Formation
4.2.5.Magnetic fields in violent star-forming (starburst) galaxies
4.3.Magnetic field shape in Andromeda (M31) and other galaxies
4.4.Magnetic field B in galactic disks and neutral hydrogen HI
4.4.1.B shapes and HI masses
4.4.2.B shapes and HI shapes - companions or bars
4.5.Magnetic fields in Halos of spiral galaxies

5.ELLIPTICAL GALAXIES, DISTANT GALAXIES, CLUSTERS AND VOIDS, QUASARS AND COSMIC SCALES
5.1.Individual Galaxies and quasars (~ 200 kpc)
5.2.Clusters of galaxies as the largest magnets ( ~ 5 to 50 Mpc)
5.2.1.Several sources per individual cluster of galaxies
5.2.2.One source per individual cluster of galaxies
5.2.3.Seeds for magnetic fields in clusters of galaxies
5.3.Large Scale Voids in space (~ 100 to 200 Mpc)
5.4.Cosmological scales
5.4.1.Foreground Cosmological Screen (~ 20 Gigaparsecs)
5.4.2.Background Cosmological Surface ( ~ 8000 Gpc)

6.SUMMARY AND FUTURE TRENDS

REFERENCES