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68 4. The magneto-ionic medium around 3C 449 (a) (b) (c) (d) (e) Figure 4.12: (a): Comparison of the observed pseudo-structure function of the 5.5-arcsec RM image as described in the text (points) with the predictions of the BPL model (curves, derived using a Hankel transform). The predicted curves are forΛ max =205 (blue dotted), 65 (continuous magenta) and 20 kpc (green dashed). (b) and (c): structure functions of the observed (points) and synthetic 5.5-arcsec RM images produced with theΛ max =205,20 kpc andΛ max =65 kpc, respectively. (d) and (e) as (a) and (c) respectively, but at 1.25-arcsec resolution. The error bars are the rms from 35 structure functions at a givenΛ max , in (a) and (d) are representative error bars from the model withΛ max =65 kpc. 68
4.7. Summary and comparison with other sources 69 1. The absence of deviations fromλ 2 rotation over a wide range of polarization position angle implies that a pure foreground Faraday screen with no mixing of radio-emitting and thermal electrons is a good approximation for 3C 449 (Sec. 4.3). 2. The best estimate for the Galactic contribution to the RM of 3C 449 is a constant value of −160.7 rad m −2 (Sec. 4.3.2). 3. The dependence of the degree of polarization on wavelength is well fitted by a Burn law. This is also consistent with pure foreground rotation, with the residual depolarization observed at the higher resolution being due to unresolved RM fluctuations across the beam (Sec. 4.4). There is no evidence for a detailed correlation of radio-source structure with either RM or depolarization. 4. There is no obvious anisotropy in the RM distribution, consistent with the assumption that the magnetic field is an isotropic, Gaussian random variable. 5. The RM structure functions for six different regions of the source are consistent with the hypothesis that only the amplitude of the RM power spectrum varies across the source. 6. A broken power-law spectrum of the form given in Eq. 4.4 with q l = 2.07, q h =2.98, f b =0.031 arcsec −1 and f max = 1.67 arcsec −1 (corresponding to a spatial scaleΛ min =0.2 kpc) is consistent with the observed structure functions and depolarizations for all six regions. No single power law provides a good fit to all of the structure functions. 7. The high-frequency cut-off in the power spectrum is required to model the depolarization data. 8. The profiles ofσ RM strongly suggest that most of the fluctuating component of RM is associated with the intra-group gas, whose core radius is comparable with the characteristic scale of the profile (Sec. 4.3.1). The symmetry of the profile is consistent with the idea that the radio source axis is close to the plane of the sky. 9. I therefore simulated the RM distributions expected for an isotropic, random magnetic field in the hot plasma surrounding 3C 449, assuming the density model derived by Croston et al. (2008). 10. These three-dimensional simulations show that the dependence of magnetic field on density is best modeled by a broken power-law function with B(r)∝n e (r) close to the nucleus and B(r)≈ constant at larger distances. 11. With this density model, the best estimate of the central magnetic field strength is B 0 = 3.5±1.2µG. 69
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Alma Mater Studiorum Università de
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To Hypatia from Alexandria in Egypt
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Contents Abstract i 1 Physics of ra
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4.6.3 The outer scale of the magnet
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Abstract The existence of diffuse m
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2. Two-dimensional Monte Carlo simu
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Chapter 1 Physics of radio galaxies
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1.2. Non-thermal emission mechanism
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1.2. Non-thermal emission mechanism
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1.3. Radio galaxies 7 FR II sources
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1.3. Radio galaxies 9 (a) (b) Figur
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1.3. Radio galaxies 11 pressure, th
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Chapter 2 The X-ray environment of
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2.2. The thermal component 15 Figur
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Page 37 and 38: Chapter 3 Magnetic fields in the ho
Page 39 and 40: 3.1. Introduction 23 Figure 3.1: Ex
Page 41 and 42: 3.1. Introduction 25 to the relativ
Page 43 and 44: 3.2. Faraday Rotation 27 The RM can
Page 45 and 46: 3.2. Faraday Rotation 29 Figure 3.4
Page 47 and 48: 3.3. Depolarization 31 3.3 Depolari
Page 49 and 50: 3.5. The magnetic field profile 33
Page 51 and 52: 3.6. Tangled magnetic field 35 rad
Page 53 and 54: 3.7. The magnetic field power spect
Page 59 and 60: Chapter 4 Structure of the magneto-
Page 61 and 62: 4.1. The radio source 3C 449: gener
Page 63 and 64: 4.3. The Faraday rotation in 3C 449
Page 65 and 66: 4.3. The Faraday rotation in 3C 449
Page 67 and 68: 4.4. Depolarization 51 Figure 4.4:
Page 69 and 70: 4.4. Depolarization 53 1.25 arcsec
Page 71 and 72: 4.5. Two dimensional analysis 55 sm
Page 73 and 74: 4.5. Two dimensional analysis 57 Fi
Page 75 and 76: 4.6. Three-dimensional analysis 59
Page 83: 4.7. Summary and comparison with ot
Page 87 and 88: 4.7. Summary and comparison with ot
Page 89 and 90: Chapter 5 Ordered magnetic fields a
Page 91 and 92: 5.1. The Sample 75 35 49 00 ROSAT P
Page 93 and 94: 5.1. The Sample 77 5.1.1 0206+35 02
Page 95 and 96: 5.2. Analysis of RM and depolarizat
Page 97 and 98: 5.3. Rotation measure images 81 IMA
Page 99 and 100: 5.3. Rotation measure images 83 cor
Page 101 and 102: 5.4. Depolarization 85 Therefore, a
Page 103 and 104: 5.5. Rotation measure structure fun
Page 105 and 106: 5.6. Rotation-measure bands from co
Page 111 and 112: 5.7. Rotation-measure bands from a
Page 113 and 114: 5.7. Rotation-measure bands from a
Page 115 and 116: 5.8. Discussion 99 5.8 Discussion 5
Page 117 and 118: 5.8. Discussion 101 line−of−sig
Page 119 and 120: 5.8. Discussion 103 flat slopes. I
Page 121 and 122: 5.9. Conclusions and outstanding qu
Page 123 and 124: 5.9. Conclusions and outstanding qu
Page 125 and 126: Chapter 6 Faraday rotation in two e
Page 127 and 128: 6.2. Two-dimensional analysis: rota
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6.3. Two-dimensional analysis: stru
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6.4. Preliminary conclusions 121 Ta
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6.4. Preliminary conclusions 123
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Summary and conclusions The goal of
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6.5. Summary 127 responsible for th
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6.6. General conclusions 129 radio
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6.7. Future prospects 131 and is th
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Appendix 133
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136 Data reduction and imaging of l
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144 BIBLIOGRAPHY Bîrzan, L., Raffe
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146 BIBLIOGRAPHY Ensslin, T.A. & Go
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148 BIBLIOGRAPHY Jeltema, T.E. & Pr
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150 BIBLIOGRAPHY Owen, F.N., 1989,
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152 BIBLIOGRAPHY 152
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