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Unraveling the Mystery of Magnetic Fields in Galaxy Clusters

This study investigates the enigmatic cooling flows in galaxies and clusters, focusing on the role of magnetic fields. Through various observations, including data from Chandra and VLA, we aim to characterize magnetic field distributions and their correlations with electron density, X-ray luminosity, and radio luminosity. Our future plans include advanced modeling, exploring high-redshift sources, and examining rotation measure distributions across multiple sightlines within clusters. Understanding these interactions is crucial for interpreting the dynamics of galaxy clusters and their evolution.

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Unraveling the Mystery of Magnetic Fields in Galaxy Clusters

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  1. Cluster Magnetic FieldsGreg Taylor(NRAO) The Riddle of Cooling Flows in Galaxies and Clusters of Galaxies See also: Carilli & Taylor ARA&A 2002, p.319

  2. Feretti et al. 1998 WSRT at 90cm B ~ 0.4 mG

  3. B ~ 0.3 mG Raphaeli 2001

  4. B ~ 5 mG Vikhlinin et al 2001 A3667 Chandra 0.5 – 4keV

  5. B ~ 10 mG Carilli & Taylor 2002 (ARA&A)

  6. Venturi & Taylor (1999) z = 0.67 VLBA Observations

  7. Centaurus cluster Chandra + VLA

  8. Fabian et al. 2003 Chandra + VLA

  9. Clarke et al. KEY red = embedded blue = background black = control

  10. Taylor, Inoue & Tabara (1992) z = 1.18 Crawford & Fabian (1996) found obscured power-law X-ray component with ROSAT  probably not in a high-z cluster

  11. n = 4 Murgia et al. in prep potential ~ k-a |Bk|2 ~ Cn2k-n where n = a - 2 n = 3 n n = 2

  12. Standard treatment overestimates the true field strength

  13. Faraday rotation (embedded) 2 – 20 distribution of cell sizes, n = 2

  14. Future Plans • Explore modeling results • Characterize magnetic field distributions • Look for correlations in B, ne, Lx, Lr • New observations with EVLA • Study high redshift, high RM sources • Examine multiple sightlines in clusters • Study RM distributions of faint sources

  15. Perley & Carilli (1996) Cygnus A B-Vectors VLA @ 8.5 GHz 10 kpc

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