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9.6 Galaxy Formation <strong>and</strong> Evolution 399 Fig. 9.40. In the top panels, one of the most massive halos at z = 6.2 from the Millennium simulation (see Fig. 7.12) is shown, whereas in the bottom panels, the corresponding distribution in this spatial region at z = 0 is shown. Thus, this early massive halo is now located in the center of a very massive galaxy cluster. In the panels on the left, the mass distribution is displayed, with the corresponding distribution of galaxies as determined from a semi-analytic model, which is shown in the right-h<strong>and</strong> panels. Galaxies at z = 6.2 are all blue since their stellar population must be young, whereas at z = 0, most galaxies contain an old stellar population, here indicated by the red color. Each of the panels shows the projected distribution in a cube with a comoving side length of 10h −1 Mpc
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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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Page 842: 10. Outlook 407 In the final chapte
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Page 858: Appendix
Page 864: 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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