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9. The Universe at High Redshift 372 Fig. 9.17. Ultra-luminous Compact X-ray Sources (ULXs) in starburst galaxies. Upper left: the discrete X-ray sources in the Antenna galaxies; the size of the image is 4 ′ × 4 ′ .Lowerleft: optical (image) and (inlaid) Chandra image of the starburst galaxy NGC 253. Four of the ULXs are located within one kiloparsec from the center of the galaxy. The X-ray image is 2. ′ 2 × 2. ′ 2. Upper right: 5 ′ × 5 ′ Chandra image of the starburst galaxy M82; the diffuse radiation (red) is emitted by gas at T ∼ 10 6 K which is heated by the starburst and flows out from the central region of the galaxy. It is supposed that M82 had a collision with its companion M81 (see Fig. 6.7) within the last 10 8 yr, by which the starburst has been triggered. Lower right: the luminosity function of the ULXs in some starburst galaxies Characteristics of EROs. Examining galaxies with a low K-band flux, one finds either galaxies with low stellar mass at low redshifts, or galaxies at high redshift with high optical (due to redshift) luminosity. But since the luminosity function of galaxies is relatively flat for L L ∗ , one expects the latter to dominate the surveys, due to the larger volume at higher z. In fact, K-band surveys detect galaxies with a broad redshift distribution.
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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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9. The Universe at High Redshift 39
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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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