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5.4 Components of an AGN sible to obtain detailed images of QSO host galaxies (see Fig. 5.26) and thus to include them in the class of galactic nuclei. In these investigations, it was also found that the host galaxies of QSOs are often heavily disturbed, e.g., by tidal interaction with other galaxies or even by merging processes. These disturbances of the gravitational potential are considered essential for the gas to overcome the angular momentum barrier and to flow towards the center of the galaxy. At the same time, such disturbances seem to increase the star-formation rate enormously, because starburst galaxies are also often characterized by disturbances and interactions. A close connection seems to exist between AGN activity and starbursts. Optical and NIR images of QSOs (see Fig. 5.26) cannot unambiguously answer the question of whether QSO hosts are spirals or ellipticals. Today it seems established that the hosts of low-redshift QSOs are predominantly massive and bulge-dominated galaxies. This finding is in good agreement with the fact that the black hole mass in “normal” galaxies scales with the mass of the spheroidal component of the galaxies. It was recently found that higher-redshift QSOs are also hosted by massive elliptical galaxies. Furthermore, the host galaxies of radio-loud QSOs seem to be systematically more luminous than that of radio-quiet QSOs. 203 Fig. 5.26. HST images of QSOs. In all cases the host galaxy can clearly be identified, with the QSO itself being visible as a (central) point source in these images. Top left: PG 0052+251 is located in the center of an apparently normal spiral galaxy. Lower left: PHL 909 seems to be located in the center of a normal elliptical galaxy. Top center: the QSO IRAS 04505−2958 is obviously part of a collision of two galaxies and may be provided with “fuel” by material ripped from the galaxies by tidal forces. Surrounding the QSO core, a region of active star formation is visible. PG 1012+008 (lower center) is also part of a pair of merging galaxies. Top right: the host galaxy of QSO 0316−346 seems to be about to capture a tidal tail. Lower right: the QSO IRAS 13218+0552 seems to be located in a galaxy which just went through a merger process
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Peter Schneider Extragalactic Astro
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Prof. Dr. Peter Schneider Argelande
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Preface VI ter aspects are discusse
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List of Contents VIII 2.5.1 The Gra
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List of Contents X 5. Active Galact
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List of Contents XII 8. Cosmology I
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List of Contents XIV D. Recommended
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1. Introduction and Overview 2 Fig.
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1. Introduction and Overview 4 othe
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1. Introduction and Overview 6 obje
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1. Introduction and Overview 8 Fig.
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1. Introduction and Overview 10 Fig
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1. Introduction and Overview 16 of
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1. Introduction and Overview 18 app
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1. Introduction and Overview 26 spe
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2. The Milky Way as a Galaxy 35 The
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2.2 Determination of Distances With
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2.3 The Structure of the Galaxy Fig
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2.3 The Structure of the Galaxy a c
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2.3 The Structure of the Galaxy Fig
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2.3 The Structure of the Galaxy B-s
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2.3 The Structure of the Galaxy Fro
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2.3 The Structure of the Galaxy tha
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2.4 Kinematics of the Galaxy 57 2.4
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2.4 Kinematics of the Galaxy which
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2.4 Kinematics of the Galaxy where
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2.4 Kinematics of the Galaxy center
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2.5 The Galactic Microlensing Effec
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2.6 The Galactic Center have been e
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2.6 The Galactic Center 79 Fig. 2.3
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2.6 The Galactic Center Fig. 2.36.
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2.6 The Galactic Center 83 Fig. 2.3
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2.6 The Galactic Center hence, this
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3. The World of Galaxies 88 million
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3. The World of Galaxies 90 100M
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3. The World of Galaxies 92 Table 3
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3. The World of Galaxies 94 arrives
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96 3. The World of Galaxies This in
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3. The World of Galaxies 98 Boxines
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3. The World of Galaxies 100 Wherea
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3. The World of Galaxies 102 the po
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3. The World of Galaxies 104 The ki
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3. The World of Galaxies 106 Fig. 3
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3. The World of Galaxies 108 where
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3. The World of Galaxies 110 angula
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3. The World of Galaxies 116 LMC sh
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3. The World of Galaxies 124 The de
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3. The World of Galaxies 130 An eve
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3. The World of Galaxies 132 3.9 Po
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3. The World of Galaxies 136 3.9.4
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3. The World of Galaxies 140 by no
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4. Cosmology I: Homogeneous Isotrop
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5. Active Galactic Nuclei 176 Fig.
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6. Clusters and Groups of Galaxies
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7. Cosmology II: Inhomogeneities in
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7.2 Gravitational Instability gravi
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7.2 Gravitational Instability i.e.,
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7.3 Description of Density Fluctuat
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7.4 Evolution of Density Fluctuatio
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7.4 Evolution of Density Fluctuatio
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7.5 Non-Linear Structure Evolution
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7.7 Origin of the Density Fluctuati
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8. Cosmology III: The Cosmological
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352 8. Cosmology III: The Cosmologi
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9. The Universe at High Redshift 35
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10. Outlook 407 In the final chapte
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10. Outlook telescope will start a
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10. Outlook New windows to the Univ
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10. Outlook understand why the dens
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Appendix
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A. The Electromagnetic Radiation Fi
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B. Properties of Stars 425 In this
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B.3 Structure and Evolution of Star
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B.3 Structure and Evolution of Star
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D. Recommended Literature 433 In th
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D.3 Review Articles, Current Litera
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E. Acronyms Used 438 GRB Gamma-Ray
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F. Figure Credits 441 Chapter 1 1.1
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F. Figure Credits 1.25 Source: R. W
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F. Figure Credits Nik Szymanek. bot
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F. Figure Credits 5.5 Credit: Laing
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F. Figure Credits 6.26 Source: http
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F. Figure Credits 8.24 Credit: Hu &
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Subject Index 453 A AB magnitudes 4
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Subject Index 455 Doppler effect 38
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Subject Index 457 -dampedLyα syste
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Subject Index 459 virial theorem 13
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