and Cosmology

Recommendations

Info

1. Introduction <strong>and</strong> Overview 28 Fig. 1.28. The two Keck telescopes on Mauna Kea. With Keck I the era of large telescopes was heralded in 1993 Fig. 1.29. The left panel shows a map of the location of the VLT on Cerro Paranal. It can be reached via Antofagasta, about a two-hour flight north of Santiago de Chile. Then another three-hour trip by car through a desert (see Fig. 1.30) brings one to the site. Paranal is shown on the right during the construction phase; in the foreground we can see the construction camp. The top of the mountain was flattened to get a leveled space (of diameter ∼ 300 m) large enough to accommodate the telescopes <strong>and</strong> the facilities used for optical interferometry (VLTI) able galaxies of redshift z 3, which are normally so dim that they cannot be examined with smaller telescopes. The largest ground-based telescope project to date was the construction of the Very Large Telescope (VLT) of the European Southern Observatory (ESO), consist-
Page 2:
Peter Schneider Extragalactic Astro
Page 8:
Prof. Dr. Peter Schneider Argelande
Page 12:
Preface VI ter aspects are discusse
Page 16:
List of Contents VIII 2.5.1 The Gra
Page 20:
List of Contents X 5. Active Galact
Page 24:
List of Contents XII 8. Cosmology I
Page 28:
List of Contents XIV D. Recommended
Page 32: 1. Introduction and Overview 2 Fig.
Page 36: 1. Introduction and Overview 4 othe
Page 40: 1. Introduction and Overview 6 obje
Page 44: 1. Introduction and Overview 8 Fig.
Page 48: 1. Introduction and Overview 10 Fig
Page 60: 1. Introduction and Overview 16 of
Page 64: 1. Introduction and Overview 18 app
Page 80: 1. Introduction and Overview 26 spe
Page 86: 1.3 The Tools of Extragalactic Astr
Page 100: 2. The Milky Way as a Galaxy 36 Fig
Page 104: 2. The Milky Way as a Galaxy 38 ric
Page 108: 2. The Milky Way as a Galaxy 40 tri
Page 112: 2. The Milky Way as a Galaxy 42 Fig
Page 116: 2. The Milky Way as a Galaxy 44 gra
Page 120: 2. The Milky Way as a Galaxy 46 A s
Page 124: 2. The Milky Way as a Galaxy 48 a l
Page 128: 2. The Milky Way as a Galaxy 50 iro
Page 132: 2. The Milky Way as a Galaxy 52 is
Page 136:
2. The Milky Way as a Galaxy 54 is
Page 140:
2. The Milky Way as a Galaxy 56 The
Page 144:
2. The Milky Way as a Galaxy 58 whe
Page 148:
2. The Milky Way as a Galaxy 60 If
Page 152:
2. The Milky Way as a Galaxy 62 Con
Page 156:
2. The Milky Way as a Galaxy 64 Fig
Page 160:
2. The Milky Way as a Galaxy 66 The
Page 164:
2. The Milky Way as a Galaxy 68 fac
Page 168:
2. The Milky Way as a Galaxy 70 the
Page 172:
2. The Milky Way as a Galaxy 72 nif
Page 176:
2. The Milky Way as a Galaxy 74 pro
Page 180:
Page 184:
2. The Milky Way as a Galaxy 78 bee
Page 188:
Page 192:
Page 196:
2. The Milky Way as a Galaxy 84 any
Page 202:
3. The World of Galaxies 87 The ins
Page 206:
3.1 Classification these names are
Page 210:
3.2 Elliptical Galaxies 91 Fig. 3.5
Page 214:
3.2 Elliptical Galaxies 93 Fig. 3.7
Page 218:
3.2 Elliptical Galaxies anisotropic
Page 222:
3.2 Elliptical Galaxies Fig. 3.12.
Page 226:
3.3 Spiral Galaxies 99 Fig. 3.14. T
Page 230:
3.3 Spiral Galaxies 101 Fig. 3.15.
Page 234:
3.3 Spiral Galaxies luminous galaxi
Page 238:
3.4 Scaling Relations 105 Fig. 3.20
Page 242:
3.4 Scaling Relations gas, which ca
Page 246:
3.5 Black Holes in the Centers of G
Page 250:
3.5 Black Holes in the Centers of G
Page 254:
3.6 Extragalactic Distance Determin
Page 258:
3.6 Extragalactic Distance Determin
Page 262:
3.7 Luminosity Function of Galaxies
Page 266:
3.7 Luminosity Function of Galaxies
Page 270:
3.8 Galaxies as Gravitational Lense
Page 274:
Page 278:
Page 282:
Page 286:
Page 290:
3.9 Population Synthesis 131 Fig. 3
Page 294:
3.9 Population Synthesis The integr
Page 298:
3.9 Population Synthesis photometri
Page 302:
3.9 Population Synthesis 137 Fig. 3
Page 306:
3.10 Chemical Evolution of Galaxies
Page 310:
4. Cosmology I: Homogeneous Isotrop
Page 314:
4.1 Introduction and Fundamental Ob
Page 318:
4.2 An Expanding Universe the Hubbl
Page 322:
4.2 An Expanding Universe in which
Page 326:
4.2 An Expanding Universe physical
Page 330:
4.2 An Expanding Universe time. Hen
Page 334:
4.3 Consequences of the Friedmann E
Page 338:
Page 342:
Page 346:
Page 350:
4.4 Thermal History of the Universe
Page 354:
Page 358:
Page 362:
Page 366:
4.5 Achievements and Problems of th
Page 370:
Page 374:
Page 378:
5. Active Galactic Nuclei 175 The l
Page 382:
5.1 Introduction 5.1 Introduction 5
Page 386:
5.1 Introduction 179 Fig. 5.5. Radi
Page 390:
5.1 Introduction The synchrotron sp
Page 394:
5.2 AGN Zoology have in common stro
Page 398:
5.3 The Central Engine: A Black Hol
Page 402:
Page 406:
Page 410:
Page 414:
Page 418:
5.4 Components of an AGN 5.4 Compon
Page 422:
5.4 Components of an AGN transition
Page 426:
5.4 Components of an AGN Fig. 5.22.
Page 430:
5.4 Components of an AGN by magneti
Page 434:
5.4 Components of an AGN sible to o
Page 438:
5.4 Components of an AGN ity of an
Page 444:
5. Active Galactic Nuclei 208 radia
Page 448:
5. Active Galactic Nuclei 210 Fig.
Page 452:
5. Active Galactic Nuclei 212 5.5.4
Page 456:
5. Active Galactic Nuclei 214 elect
Page 460:
5. Active Galactic Nuclei 216 QSOs
Page 464:
5. Active Galactic Nuclei 218 tion.
Page 470:
5.6 AGNs and Cosmology 221 ize hydr
Page 474:
6. Clusters and Groups of Galaxies
Page 478:
6.1 The Local Group 225 Table 6.1.
Page 484:
Page 488:
Page 492:
Page 496:
Page 500:
Page 504:
Page 508:
Page 512:
Page 516:
Page 520:
Page 524:
Page 528:
Page 532:
Page 536:
Page 540:
Page 544:
Page 548:
Page 552:
Page 556:
Page 560:
Page 564:
Page 568:
Page 572:
Page 576:
Page 582:
7. Cosmology II: Inhomogeneities in
Page 586:
7.2 Gravitational Instability gravi
Page 590:
7.2 Gravitational Instability i.e.,
Page 594:
7.3 Description of Density Fluctuat
Page 598:
7.4 Evolution of Density Fluctuatio
Page 602:
7.4 Evolution of Density Fluctuatio
Page 606:
7.5 Non-Linear Structure Evolution
Page 610:
Page 614:
Page 618:
Page 622:
Page 626:
Page 630:
Page 634:
Page 638:
Page 642:
7.7 Origin of the Density Fluctuati
Page 648:
8. Cosmology III: The Cosmological
Page 652:
Page 656:
Page 660:
Page 664:
Page 668:
Page 672:
Page 676:
Page 680:
Page 684:
Page 688:
Page 692:
Page 696:
Page 700:
Page 704:
Page 708:
Page 712:
Page 716:
Page 720:
Page 724:
Page 728:
Page 732:
352 8. Cosmology III: The Cosmologi
Page 736:
Page 740:
9. The Universe at High Redshift 35
Page 744:
Page 748:
Page 752:
Page 756:
Page 760:
Page 764:
Page 768:
Page 772:
Page 776:
Page 780:
Page 784:
Page 788:
Page 792:
Page 796:
Page 800:
Page 804:
Page 808:
Page 812:
Page 816:
Page 820:
Page 824:
Page 828:
Page 832:
Page 836:
Page 842:
10. Outlook 407 In the final chapte
Page 846:
10. Outlook telescope will start a
Page 850:
10. Outlook New windows to the Univ
Page 854:
10. Outlook understand why the dens
Page 858:
Appendix
Page 864:
A. The Electromagnetic Radiation Fi
Page 868:
Page 872:
Page 878:
B. Properties of Stars 425 In this
Page 882:
B.3 Structure and Evolution of Star
Page 886:
B.3 Structure and Evolution of Star
Page 894:
D. Recommended Literature 433 In th
Page 898:
D.3 Review Articles, Current Litera
Page 904:
E. Acronyms Used 438 GRB Gamma-Ray
Page 910:
F. Figure Credits 441 Chapter 1 1.1
Page 914:
F. Figure Credits 1.25 Source: R. W
Page 918:
F. Figure Credits Nik Szymanek. bot
Page 922:
F. Figure Credits 5.5 Credit: Laing
Page 926:
F. Figure Credits 6.26 Source: http
Page 930:
F. Figure Credits 8.24 Credit: Hu &
Page 934:
Subject Index 453 A AB magnitudes 4
Page 938:
Subject Index 455 Doppler effect 38
Page 942:
Subject Index 457 -dampedLyα syste
Page 946:
Subject Index 459 virial theorem 13
show all

and Cosmology

Create successful ePaper yourself

Delete template?

Save as template?