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9.7 Gamma-Ray Bursts 403 Fig. 9.41. Gamma-ray light curves of various gamma-ray bursts; the different time-scales on the x-axis should be particularly noted. All these light curves appear to be very dissimilar Neutron stars are concentrated towards the disk of the Galaxy, hence the distribution of GRBs should feature a clear anisotropy – except for the case that the typical distance of the sources is very small ( 100 pc), much smaller than the scale-height of the disk. In the latter case, the distribution might possibly be isotropic, but the flux distribution would necessarily have to follow the law N(> F) ∝ F −3/2 , as expected for a homogeneous distribution of sources, which was discussed in Sect. 4.1.2. Because this is clearly not the case, a dif-
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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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5. Active Galactic Nuclei 194 For a
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5. Active Galactic Nuclei 196 5.4.2
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5. Active Galactic Nuclei 198 wheth
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5. Active Galactic Nuclei 202 There
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5. Active Galactic Nuclei 204 Binar
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5.5 Family Relations of AGNs ing t
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5.5 Family Relations of AGNs 209 Fi
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5.5 Family Relations of AGNs relati
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5.5 Family Relations of AGNs 213 Fi
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5.6 AGNs and Cosmology a given freq
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5.6 AGNs and Cosmology Φ(L, z) dL
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5.6 AGNs and Cosmology at very high
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5. Active Galactic Nuclei 222 QSO w
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6. Clusters and Groups of Galaxies
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6. Clusters and Groups of Galaxies
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6.2 Galaxies in Clusters and Groups
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6.3 X-Ray Radiation from Clusters o
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6.4 Scaling Relations for Clusters
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6.4 Scaling Relations for Clusters
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6.5 Clusters of Galaxies as Gravita
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6.6 Evolutionary Effects M/L ≈ 80
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6.6 Evolutionary Effects 271 Fig. 6
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6.6 Evolutionary Effects Fig. 6.45.
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6.6 Evolutionary Effects satellites
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7. Cosmology II: Inhomogeneities in
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280 7. Cosmology II: Inhomogeneitie
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8. Cosmology III: The Cosmological
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8.1 Redshift Surveys of Galaxies a
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8.1 Redshift Surveys of Galaxies SD
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8.1 Redshift Surveys of Galaxies 31
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Physical space Linear regime Redshi
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8.1 Redshift Surveys of Galaxies ie
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8.2 Cosmological Parameters from Cl
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8.2 Cosmological Parameters from Cl
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8.3 High-Redshift Supernovae and th
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8.3 High-Redshift Supernovae and th
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8.4 Cosmic Shear ity one can separa
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8.5 Origin of the Lyman-α Forest F
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8.5 Origin of the Lyman-α Forest p
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8.5 Origin of the Lyman-α Forest 3
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8.6 Angular Fluctuations of the Cos
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8.7 Cosmological Parameters smaller
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8.7 Cosmological Parameters Fig. 8.
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8.7 Cosmological Parameters measure
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9. The Universe at High Redshift 35
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9.1 Galaxies at High Redshift one e
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9.1 Galaxies at High Redshift Fig.
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9.1 Galaxies at High Redshift neutr
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9.1 Galaxies at High Redshift break
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9.1 Galaxies at High Redshift to sc
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9.1 Galaxies at High Redshift the H
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9.2 New Types of Galaxies 369 Fig.
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9.2 New Types of Galaxies dust. A m
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9.2 New Types of Galaxies 373 Fig.
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9.2 New Types of Galaxies Fig. 9.21
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Page 842: 10. Outlook 407 In the final chapte
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Page 858: Appendix
Page 864: A. The Electromagnetic Radiation Fi
Page 878: B. Properties of Stars 425 In this
Page 882: 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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