Alma Mater Studiorum Universit`a degli Studi di Bologna ... - Inaf

More documents

Recommendations

Info

82 5. Ordered magnetic fields around radio galaxies Table 5.3: Frequencies, bandwidths and angular resolutions used in the RM and Burn law k images discussed in Sects. 5.3 and 5.4, respectively. source ν ∆ν beam [MHz] [MHz] [arcsec] 0206+35 1385.1 25 1.2 1464.9 25 4885.1 50 3C 353 1385.0 12.5 1.3 1665.0 12.5 4866.3 12.5 8439.9 12.5 3C 270 1365.0 25 1.65 1412.0 12.5 4860.1 100 1365.0 25 5.0 1412.0 12.5 1646.0 25 4860.1 100 M 84 1413.0 25 1.65 4885.1 50 1385.1 50 4.5 1413.0 25 1464.9 50 4885.1 50 shown by Laing & Bridle (1987), but is derived from four-frequency data and has a higher signalto-noise ratio. In the fainter regions of 0206+35 (for which only three frequencies are available and the signal-to-noise ratio is relatively low), the RM task occasionally failed to determine the nπ ambiguities in position angle correctly. In order to remove these anomalies, I first produced a lower-resolution, but high signal-to-noise RM image by convolving the 1.2 arcsec RM map to a beamwidth of 5 arcsec FWHM. From this map I derived the polarization-angle rotations at each of the three frequencies and subtracted them from the observed 1.2 arcsec polarization angle maps at the same frequency to derive the residuals at high resolution. Then, I fit the residuals without allowing any nπ ambiguities and added the resulting RM’s to the values determined at low resolution. This procedure allowed us to obtain an RM map of 0206+35 free of significant deviations fromλ 2 rotation and fully consistent with the 1.2-arcsec measurements. I have verified that the polarization angles accurately follow the relation∆Ψ∝λ 2 over the full range of position angle essentially everywhere except for small areas around the opticallythick cores: representative plots ofΨagainstλ 2 for 0206+35 are shown in Fig. 5.4. The lack of deviations fromλ 2 rotation in all of the radio galaxies is fully consistent with the assumption that the Faraday rotating medium is mostly external to the sources. The RM maps are shown in Fig. 5.2. The typical rms error on the fit is≈2 rad m −2 . No 82
5.3. Rotation measure images 83 correction for the Galactic contribution has been applied. All of the RM maps show two-dimensional patterns, RM bands, across the lobes with characteristic widths ranging from 3 to 12 kpc. Multiple bands parallel to each other are observed in the western lobe of 0206+35, the eastern lobe of 3C 353 and the southern lobe of M 84. In all cases, the iso-RM contours are straight and perpendicular to the major axes of the lobes to a very good approximation: the very straight and well-defined bands in the eastern lobes of both 0206+35 (Fig. 5.2a) and 3C 353 (Fig. 5.2d) are particularly striking. The entire area of M 84 appears to be covered by a banded structure, while in the central parts of 0206+35 and 3C 270 and the western lobe of 3C 353, regions of isotropic and random RM fluctuations are also present. I also derived profiles of〈RM〉 along the radio axis of each source, averaging over boxes a few beamwidths long (parallel to the axes), but extended perpendicular to them to cover the entire width of the source. The boxes are all large enough to contain many independent points. The profiles are shown in Fig. 5.5. For each radio galaxy, I also plot an estimate of the Galactic contribution to the RM derived from a weighted mean of the integrated RM’s for non-cluster radio sources within a surrounding area of 10 deg 2 (Simard-Normandin et al. 1981). In all cases, both positive and negative fluctuations with respect to the Galactic value are present. In 0206+35 (Fig. 5.2a), the largest-amplitude bands are in the outer parts of the lobes, with a possible low-level band just to the NW of the core. The most prominent band (with the most negative RM values) is in the eastern (receding) lobe, about 15 kpc from the core (Fig. 5.5a). Its amplitude with respect to the Galactic value is about 40 rad m −2 . This band must be associated with a strong ordered magnetic field component along the line of sight. If corrected for the Galactic contribution, the two adjacent bands in the eastern lobe would have RM with opposite signs and the field component along the line of sight must therefore reverse. M 84 (Fig. 5.2b) displays an ordered RM pattern across the whole source, with two wide bands of opposite sign having the highest absolute RM values. There is also an abrupt change of sign across the radio core (see also Laing & Bridle 1987). The negative band in the northern lobe (associated with the approaching jet) has a larger amplitude with respect to the Galactic value than the corresponding (positive) feature in the southern lobe (Fig. 5.5c). 3C 270 (Fig. 5.2c) shows two large bands: one on the front end of the eastern lobe, the other in the middle of the western lobe. The bands have opposite signs and contain the extreme positive and negative values of the observed RM. The peak positive value is within the eastern band at the extreme end of the lobe (Fig. 5.5e). The RM structure of 3C 353 (Fig. 5.2d) is highly asymmetric. The eastern lobe shows a strong pattern, made up of four bands, with very straight iso-RM contours which are almost 83
Page 1:
Alma Mater Studiorum Università de
Page 5:
To Hypatia from Alexandria in Egypt
Page 9 and 10:
Contents Abstract i 1 Physics of ra
Page 11 and 12:
4.6.3 The outer scale of the magnet
Page 13 and 14:
Abstract The existence of diffuse m
Page 15 and 16:
2. Two-dimensional Monte Carlo simu
Page 17 and 18:
Chapter 1 Physics of radio galaxies
Page 19 and 20:
1.2. Non-thermal emission mechanism
Page 21 and 22:
1.2. Non-thermal emission mechanism
Page 23 and 24:
1.3. Radio galaxies 7 FR II sources
Page 25 and 26:
1.3. Radio galaxies 9 (a) (b) Figur
Page 27 and 28:
1.3. Radio galaxies 11 pressure, th
Page 29 and 30:
Chapter 2 The X-ray environment of
Page 31 and 32:
2.2. The thermal component 15 Figur
Page 33 and 34:
2.3. Radio source - environment int
Page 35 and 36:
2.3. Radio source - environment int
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 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: 5.3. Rotation measure images 81 IMA
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
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 154 and 155:
Page 156 and 157:
Page 158 and 159:
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
show all

Alma Mater Studiorum Universit`a degli Studi di Bologna ... - Inaf

Create successful ePaper yourself

Delete template?

Save as template?