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5.6 AGNs <strong>and</strong> <strong>Cosmology</strong> 221 ize hydrogen (Fig. 5.41). If such a system is located at z limit in the spectrum of a QSO, the spectrum at λ
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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 118 should
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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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5. Active Galactic Nuclei 178 the r
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5. Active Galactic Nuclei 180 of re
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5. Active Galactic Nuclei 182 emiss
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5. Active Galactic Nuclei 184 surve
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5. Active Galactic Nuclei 186 chang
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188 5. Active Galactic Nuclei diffe
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Page 442: 5.5 Family Relations of AGNs ing t
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Page 458: 5.6 AGNs and Cosmology a given freq
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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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