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112 6. Faraday rotation in two extreme environments IMAGE: 07_PSPC_CONVL_AS_1.3_OGEOM.FITS CNTRS: 07_1.3_I_4.FITS 0 0.0002 0.0004 0.0006 0.0008 37 49 00 50 kpc DECLINATION (J2000) 37 48 00 37 47 00 37 46 00 37 45 00 07 58 40 07 58 30 RIGHT ASCENSION (J2000) 07 58 20 Figure 6.1: Overlay of the X-ray emission (ROSAT PSPC) around 0755+37 on radio contours at 1.385 GHz at 4.0 arcsec resolution. Table 6.3: Frequencies, bandwidths and angular resolutions used in the RM and Burn law k images. Details of the 0755+37 dataset are given in the Appendix. source ν ∆ν beam [MHz] [MHz] [arcsec] 0755+37 1385.1 12.5 1.3-4.0 1464.9 4860.1 100 M 87 4635.1 50 0.4 4735.0 4835.1 4935.0 8085.1 8335.1 8535.1 8785.1 by G.B. Taylor. The RM maps were calculated only at pixels with polarization angle uncertainties ≤10 ◦ at all frequencies. The RM maps have not been corrected for the Galactic contribution. For 0755+37, this is estimated to be negligible (-1±2 rad m −2 ; Simard-Normandin et al. 1981). For M 87, the value is less well-determined, but the source is at very high Galactic latitude, and the associated RM must be very small compared with the measured values (see below). Values of σ RM integrated over the maps are not corrected for the fitting errorσ RMfit , I produced Burn law k images at the same resolutions and using the same frequencies as the RM maps. Weighted least-squares fits were made to the fractional polarization maps ln p(λ) as a 112
6.2. Two-dimensional analysis: rotation measure and depolarization 113 Figure 6.2: Composite radio image of M87 showing the complex structure on multiple spatial scales and at several frequencies. In the present work, the RM from the central cone-like structure, shown in more detail in the top-left panel, has been analysed. Image courtesy of NRAO/AUI. ROSAT XMM−Newton Chandra Figure 6.3: X-ray images of the centre of the Virgo cluster showing different scales: ROSAT (left) XMM-Newton (middle) Chandra (right). The increasing resolution has shown a complex structure in the hot gas. Courtesy of W. Forman. function ofλ 4 (Eq. 3.5), using a modified version of AIPS RM task. Only data with p>4σ p at each frequency were included in the fits. 6.2.1 0755+37: images Two RM images have been produced, at resolutions of 1.3 and 4.0 arcsec. Both of the fits are very good, showing no evidence for deviations fromλ 2 rotation, although the total range of rotation is quite small. The RM maps are both shown in Fig. 6.4. 113
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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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2.3. Radio source - environment int
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2.3. Radio source - environment int
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Chapter 3 Magnetic fields in the ho
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3.1. Introduction 23 Figure 3.1: Ex
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3.1. Introduction 25 to the relativ
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3.2. Faraday Rotation 27 The RM can
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3.2. Faraday Rotation 29 Figure 3.4
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3.3. Depolarization 31 3.3 Depolari
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3.5. The magnetic field profile 33
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3.6. Tangled magnetic field 35 rad
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3.7. The magnetic field power spect
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Chapter 4 Structure of the magneto-
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4.1. The radio source 3C 449: gener
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4.3. The Faraday rotation in 3C 449
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4.3. The Faraday rotation in 3C 449
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4.4. Depolarization 51 Figure 4.4:
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4.4. Depolarization 53 1.25 arcsec
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4.5. Two dimensional analysis 55 sm
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4.5. Two dimensional analysis 57 Fi
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4.6. Three-dimensional analysis 59
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Page 83 and 84: 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
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Page 125 and 126: Chapter 6 Faraday rotation in two e
Page 127: 6.2. Two-dimensional analysis: rota
Page 131 and 132: 6.2. Two-dimensional analysis: rota
Page 133 and 134: 6.2. Two-dimensional analysis: rota
Page 135 and 136: 6.3. Two-dimensional analysis: stru
Page 137 and 138: 6.4. Preliminary conclusions 121 Ta
Page 139 and 140: 6.4. Preliminary conclusions 123
Page 141 and 142: Summary and conclusions The goal of
Page 143 and 144: 6.5. Summary 127 responsible for th
Page 145 and 146: 6.6. General conclusions 129 radio
Page 147 and 148: 6.7. Future prospects 131 and is th
Page 149: Appendix 133
Page 152 and 153: 136 Data reduction and imaging of l
Page 160 and 161: 144 BIBLIOGRAPHY Bîrzan, L., Raffe
Page 162 and 163: 146 BIBLIOGRAPHY Ensslin, T.A. & Go
Page 164 and 165: 148 BIBLIOGRAPHY Jeltema, T.E. & Pr
Page 166 and 167: 150 BIBLIOGRAPHY Owen, F.N., 1989,
Page 168 and 169: 152 BIBLIOGRAPHY 152
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