CHF100.00
Download est disponible immédiatement
Describing how to investigate all kinds of galaxies through a multifrequency analysis, this text is divided into three different sections. The first describes the data currently available at different frequencies, from X-rays to UV, optical, infrared and radio millimetric and centimetric, while explaining their physical meaning. In the second section, the author explains how these data can be used to determine physical parameters and quantities, such as mass and temperature. The final section is devoted to describing how the derived quantities can be used in a multifrequency analysis to study such physical processes as the star formation cycle and constrain models of galaxy evolution. As a result, observers will be able to interpret galaxies and their structure.
Auteur
Alessandro Boselli is Head of the group Physics of Galaxies at the Laboratoire d'Astrophysique de Marseille, France. He got his academic degree in physics at the Universita di Milano (Italy) and his PhD in astrophysics at the Observatoire de Paris-Meudon (France) under the supervision of J. Lequeux. He then worked at the Max-Planck Institute for Nuclear Physics in Heidelberg (Germany). His research activity is focused on the study of the formation and evolution of galaxies.
Texte du rabat
A Panchromatic View of Galaxies illustrates how galaxies can be studied through multifrequency analysis. Divided into three different sections, the author first describes the data currently available at different frequencies, from X-rays to UV, optical, infrared and radio, and discusses the different emission processes and the nature of the emitting sources. In the second section, he explains how these data can be used to determine the most important physical, structural and kinematical parameters and quantities necessary for a coherent study of galaxies. The final section describes how these derived quantities can be used in a multifrequency analysis to study the matter cycle that gave birth to galaxies and, at the same time, pose strong observational constraints on models of galaxy formation. This book is thus a useful and practical guide for the interpretation and the use of all kind of multifrequency data in the study of galaxy evolution.
From the Contents:
Part I: Emitting Sources and Radiative Processes in Galaxies
Millimeter and Centimeter Radio
Part II: Derived Quantities
Stellar and Dynamical Masses
Part III: Constraining Galaxy Evolution
Contenu
Preface XIII
1 Introduction 1
1.1 Galaxies 1
1.2 A Multifrequency Approach 4
1.3 The Purpose of this Book 10
Part One Emitting Sources and Radiative Processes in Galaxies 15
2 X-ray 17
2.1 Continuum 17
2.1.1 Discrete Sources 18
2.1.2 X-ray Emission in Active Galaxies 20
2.1.3 Hot Gas 21
3 UV-Optical-NIR 25
3.1 Continuum: Stellar Emission 26
3.2 Emission Lines 28
3.2.1 Hydrogen Lines 32
3.2.2 Metals 34
3.3 Absorption Lines 35
3.3.1 Hydrogen Lines 37
3.3.2 Other Elements 38
3.4 Molecular Lines 39
3.4.1 H2 Near-Infrared Emission Lines 39
3.4.2 H2 UV Absorption Lines 39
4 The Infrared 41
4.1 Continuum: Dust Emission 42
4.2 Emission Lines 44
4.2.1 PAHs 44
4.2.2 Cooling Lines in PDR 45
4.2.3 H2 Lines 47
4.2.4 Dust Absorption of Ly Scattered Photons 49
5 Millimeter and Centimeter Radio 51
5.1 Continuum 51
5.1.1 FreeFree Emission 52
5.1.2 Synchrotron Emission 53
5.1.3 Dust Emission 53
5.2 Emission Lines 54
5.2.1 Molecular Lines 54
5.2.2 HI 55
5.3 Absorption Lines 57
5.3.1 HI 57
Part Two Derived Quantities 59
6 Properties of the Hot X-ray Emitting Gas 61
6.1 X-ray Luminosity 61
6.2 Gas Temperature 61
7 Dust Properties 63
7.1 The Far-IR Luminosity 63
7.2 Dust Mass and Temperature 65
8 Radio Properties 71
8.1 Determining the Contribution of the Different Radio Components 71
8.1.1 Synchrotron vs. FreeFree Radio Emission in the Centimeter Domain 71
8.1.2 The Emission of the Cold Dust Component at _ 1.5mm 72
8.2 The Radio Luminosity 74
9 The Spectral Energy Distribution 77
9.1 The Emission in the UV to Near-Infrared Spectral Domain 79
9.1.1 UV, Optical, and Near-IR Colors 81
9.1.2 Fitting SEDs with Population Synthesis Models 83
9.2 The Dust Emission in the Infrared Domain 84
9.2.1 Mid- and Far-Infrared Colors 86
9.3 The Thermal and Nonthermal Radio Emission 90
10 Spectral Features 91
10.1 Galaxy Characterization through Emission and Absorption Lines 91
10.1.1 Classification of the Nuclear Activity 92
10.1.2 Classification of Post-Starburst and Post-Star-Forming Galaxies 92
10.1.3 Line Diagnostics 95
10.2 Gas Metallicity from Emission Lines 101
10.3 Stellar Age and Metallicity from Absorption Lines 103
11 Gas Properties 107
11.1 Gas Density, Mass, and Temperature 107
11.1.1 The Atomic HI Mass 108
11.1.2 The Molecular H2 Mass 115
12 Dust Extinction 125
12.1 Galactic Extinction 126
12.1.1 Extinction Curve 127
12.2 Internal Attenuation 132
12.2.1 Attenuation of the Emission Lines 133
12.2.2 Attenuation of the Stellar Continuum 134
13 Star Formation Tracers 143
13.1 The Initial Mass Function 143
13.2 The Star Formation Rate 144
13.3 The Birthrate Parameter and the Specific Star Formation Rate 146
13.4 The Star Formation Efficiency and the Gas Consumption Time Scale 147
13.5 Hydrogen Emission Lines 147
13.6 UV Stellar Continuum 151
13.7 Infrared 152
13.7.1 Integrated Infrared Luminosity 152
13.7.2 Monochromatic Infrared Luminosities 153
13.8 Radio Continuum 153
13.9 Other Indicators 155
13.9.1 The X-ray Luminosity 155
13.9.2 Forbidden Lines 156
13.9.3 [CII] 157 ...