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1.3 The Tools of Extragalactic Astronomy 33 Fig. 1.33. The left image shows the Compton Gamma Ray Observatory (CGRO) mounted on the Space Shuttle manipulator arm. This NASA satellite carried out observations between 1991 and 2000. It was finally shut down after a gyroscope failed, and it burned up in the Earth’s atmosphere in a controlled re-entry. ESA’s Integral observatory, in operation since 2002, is shown on the right discovered many AGNs at very high energies above 20 MeV, which hints at extreme processes taking place in these objects. The successor of the CGRO, the Integral satellite, was put into orbit as an ESA mission by a Russian Proton rocket at the end of 2002. At a weight of two tons, it is the heaviest ESA satellite that has been launched thus far. It is primarily observing at energies of 15 keV to 10 MeV in the gamma range, but has additional instruments for observation in the optical and X-ray regimes.
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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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2. The Milky Way as a Galaxy 58 whe
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2. The Milky Way as a Galaxy 60 If
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2. The Milky Way as a Galaxy 62 Con
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2. The Milky Way as a Galaxy 64 Fig
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2. The Milky Way as a Galaxy 66 The
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2. The Milky Way as a Galaxy 68 fac
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2. The Milky Way as a Galaxy 70 the
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2. The Milky Way as a Galaxy 72 nif
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2. The Milky Way as a Galaxy 74 pro
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2. The Milky Way as a Galaxy 78 bee
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2. The Milky Way as a Galaxy 84 any
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3. The World of Galaxies 87 The ins
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3.1 Classification these names are
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3.2 Elliptical Galaxies 91 Fig. 3.5
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3.2 Elliptical Galaxies 93 Fig. 3.7
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3.2 Elliptical Galaxies anisotropic
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3.2 Elliptical Galaxies Fig. 3.12.
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3.3 Spiral Galaxies 99 Fig. 3.14. T
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3.3 Spiral Galaxies 101 Fig. 3.15.
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3.3 Spiral Galaxies luminous galaxi
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3.4 Scaling Relations 105 Fig. 3.20
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3.4 Scaling Relations gas, which ca
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3.5 Black Holes in the Centers of G
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3.5 Black Holes in the Centers of G
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3.6 Extragalactic Distance Determin
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3.6 Extragalactic Distance Determin
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3.7 Luminosity Function of Galaxies
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3.7 Luminosity Function of Galaxies
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3.8 Galaxies as Gravitational Lense
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3.9 Population Synthesis 131 Fig. 3
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3.9 Population Synthesis The integr
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3.9 Population Synthesis photometri
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3.9 Population Synthesis 137 Fig. 3
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3.10 Chemical Evolution of Galaxies
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4. Cosmology I: Homogeneous Isotrop
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4.1 Introduction and Fundamental Ob
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4.2 An Expanding Universe the Hubbl
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4.2 An Expanding Universe in which
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4.2 An Expanding Universe physical
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4.2 An Expanding Universe time. Hen
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4.3 Consequences of the Friedmann E
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4.4 Thermal History of the Universe
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4.5 Achievements and Problems of th
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5. Active Galactic Nuclei 175 The l
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5.1 Introduction 5.1 Introduction 5
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5.1 Introduction 179 Fig. 5.5. Radi
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5.1 Introduction The synchrotron sp
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5.2 AGN Zoology have in common stro
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5.3 The Central Engine: A Black Hol
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5.4 Components of an AGN 5.4 Compon
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5.4 Components of an AGN transition
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5.4 Components of an AGN Fig. 5.22.
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5.4 Components of an AGN by magneti
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5.4 Components of an AGN sible to o
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5.4 Components of an AGN ity of an
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5. Active Galactic Nuclei 208 radia
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5. Active Galactic Nuclei 210 Fig.
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5. Active Galactic Nuclei 212 5.5.4
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5. Active Galactic Nuclei 214 elect
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5. Active Galactic Nuclei 216 QSOs
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5. Active Galactic Nuclei 218 tion.
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5.6 AGNs and Cosmology 221 ize hydr
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6. Clusters and Groups of Galaxies
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6.1 The Local Group 225 Table 6.1.
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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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