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Cluster Magnetic Fields Greg Taylor (NRAO)

Cluster Magnetic Fields Greg Taylor (NRAO). The Riddle of Cooling Flows in Galaxies and Clusters of Galaxies. See also: Carilli & Taylor ARA&A 2002, p.319. Feretti et al. 1998 WSRT at 90cm. B ~ 0.4 m G. B ~ 0.3 m G. Raphaeli 2001. B ~ 5 m G. Vikhlinin et al 2001 A3667

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Cluster Magnetic Fields Greg Taylor (NRAO)

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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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