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270 6 MACRO– AND MICRO–JETS DRIVEN BY BLACK HOLES Figure 124: M 87 in the Virgo cluster is historically the first jet detected in optical emission (Curtis 1918). With HST the structure of this jet is nicely visible, the jet ends beyond the extension of the core region of the optical galaxy (top). This jet has been imaged in radio, optical and X–ray emission (bottom). M 87 is however not a typical DRAGN.
6.1 DRAG(o)Ns – FR I and FR II 271 Figure 125: Structure of the archetypical DRAGN Cygnus A. scribed as the ”core” coincides with the galactic nucleus. Most of the radio emission does not come directly from the well-collimated ”jets”, but from the broader ”lobes” that are found around the jet paths. The plasma in the lobes is believed to have been supplied by the jets over millions of years. In the more powerful DRAGNs, there are usually small, bright radio ”hot spots” near the boundaries of each lobe. These hot spots thought to be where strong shocks form near the ends of the supersonic jet outflows in the powerful DRAGNs. The environs of a galaxy are not a perfect vacuum. The jets must travel first through the atmosphere of the galactic nucleus, then through the interstellar medium of the host galaxy, then (if they get that far without being slowed down by interaction) through the successively lower densities and pressures of the outer halo of the galaxy, the intra-cluster medium (ICM) of any surrounding group or cluster of galaxies, and finally into the low-density inter-galactic medium. The jets do not flow freely away from the AGN, but must push their way through these external media. Fanaroff–Riley Classification: A landmark in the study of extragalactic radio sources was the demonstration by Fanaroff and Riley (1974) of the existence of a relatively sharp morphological transition at a radio luminosity P178 MHz 2.5 ×
Page 1 and 2: CONTENTS 265 Contents 6 Macro- and
Page 3 and 4: 6 Macro- and Micro-Jets Driven by B
Page 5: 6.1 DRAG(o)Ns - FR I and FR II 269
Page 9 and 10: 6.1 DRAG(o)Ns - FR I and FR II 273
Page 11 and 12: 6.2 Jets as Super(magneto)sonic Col
Page 13 and 14: 6.2 Jets as Super(magneto)sonic Col
Page 15 and 16: 6.3 Fundamental Parameters for Jets
Page 17 and 18: 6.3 Fundamental Parameters for Jets
Page 19 and 20: 6.4 A 3-Phase Model for Kiloparsec-
Page 25 and 26: 6.5 Relativistic Jet Propagation 28
Page 27 and 28: 6.6 Structure and Emission of Micro
Page 37 and 38: 6.7 Formation of Micro-Jets 301 6.7
Page 39 and 40: 6.7 Formation of Micro-Jets 303 Fig
Page 41 and 42: 6.7 Formation of Micro-Jets 305 Thi
Page 43 and 44: 6.7 Formation of Micro-Jets 307 VLB
Page 45 and 46: 6.7 Formation of Micro-Jets 309 as
Page 53 and 54: 6.7 Formation of Micro-Jets 317 the
Page 55 and 56: 7.1 The Dark Age 319 Figure 152: Da
Page 57 and 58:
7.3 The First Quasars 321 Figure 15
Page 59 and 60:
7.3 The First Quasars 323 Bromm & L
Page 61:
REFERENCES 325 [17] Leahy, P. 1993,
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