and Cosmology

Recommendations

Info

1. Introduction <strong>and</strong> Overview 20 Fig. 1.18. “Jansky’s Merry-Go-Round”. By turning the structure in an azimuthal direction, a rough estimate of the position of radio sources could be obtained Fig. 1.19. With a diameter of 305 m, the Arecibo telescope in Puerto Rico is the largest single-dish telescope in the world; it may also be known from the James Bond movie “Goldeneye”. The disadvantage of its construction is its lack of steerability. Tracking of sources is only possible within narrow limits by moving the secondary mirror Green Bank Telescope (see Fig. 1.20) after the old one collapsed in 1988. With Effelsberg, for example, starformation regions can be investigated. Using molecular line spectroscopy, one can measure their densities <strong>and</strong> temperatures. Magnetic fields also play a role in star formation, though many details still need to be clarified. By measuring the polarized radio flux, Effelsberg has mapped the magnetic fields of numerous spiral galaxies. In addition, due to its huge collecting area Effelsberg plays an important role in interferometry at very long baselines (see below). Because of the long wavelength, the angular resolution of even large radio telescopes is fairly low, compared to optical telescopes. For this reason, radio
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 70: 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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?