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More About This Title A Panchromatic View of Galaxies
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As a result, observers will be able to interpret galaxies and their structure.
English
English
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 Lyα Scattered Photons 49
5 Millimeter and Centimeter Radio 51
5.1 Continuum 51
5.1.1 Free–Free 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. Free–Free Radio Emission in the Centimeter Domain 71
8.1.2 The Emission of the Cold Dust Component at λ _ 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
13.9.4 Radio Recombination Lines 157
13.10 Population Synthesis Models 158
13.10.1 Dating a Star Formation Event 158
14 Light Profiles and Structural Parameters 161
14.1 The Surface Brightness Profile 161
14.1.1 Extended Radial Profiles 161
14.1.2 The Central Surface Brightness Profile of Early-Type Galaxies 162
14.1.3 The Vertical Light Profile of Late-Type Galaxies 166
14.2 Structural Parameters 166
14.2.1 Total Magnitudes, Effective Radii and Surface Brightnesses 166
14.2.2 Bulge to Disk Ratio 167
14.3 Morphological Parameters 168
14.3.1 Concentration Index 168
14.3.2 Asymmetry 168
14.3.3 Clumpiness 169
14.3.4 The Gini Coefficient G and the Second-Order Moment of the Brightest 20% of the Galaxy’s Flux M20 169
15 Stellar and Dynamical Masses 171
15.1 Stellar Mass Determination Using Population Synthesis Models 171
15.2 Dynamical Mass 175
15.2.1 Rotation Curves and the Dark Matter Distribution 177
15.2.2 The Total Mass of Elliptical Galaxies from Kinematical Measurements 184
15.2.3 The Total Mass of Elliptical Galaxies from X-ray Measurements 185
15.2.4 The Mass of the Supermassive Black Hole 187
Part Three Constraining Galaxy Evolution 193
16 Statistical Tools 195
16.1 Galaxy Number Counts 195
16.1.1 Observed Number Counts 197
16.2 Luminosity Function 200
16.2.1 Parametrization of the Luminosity Function 203
16.2.2 Luminosity Distributions and Bivariate Luminosity Functions 204
16.2.3 The Observed Luminosity Functions 205
16.3 Luminosity Density 209
16.3.1 The Cosmic Star Formation History and Build Up of the Stellar Mass 211
17 Scaling Relations 215
17.1 Spectrophotometric Relations 216
17.1.1 The Color–Magnitude and Color–Color Relations 216
17.1.2 The Mass–Metallicity Relation 218
17.1.3 The Mass–Gas Relation 220
17.1.4 The Mass–Star Formation Rate Relation 222
17.2 Structural Relations 223
17.2.1 The Surface Brightness–Absolute Magnitude Relation 223
17.2.2 The Kormendy Relation 224
17.3 Kinematical Relations 224
17.3.1 The Tully–Fisher Relation 225
17.3.2 The Faber–Jackson Relation and the Fundamental Plane 228
17.3.3 The k-Space 230
17.4 Supermassive Black Hole Scaling Relations 231
18 Matter Cycle in Galaxies 235
18.1 The Star Formation Process 236
18.1.1 The Schmidt Law 236
18.2 Feedback 239
18.2.1 The Feedback of AGNs 239
18.2.2 The Feedback of Massive Stars 242
19 The Role of the Environment onGalaxy Evolution 245
19.1 Tracers of Different Environments 245
19.1.1 Detection of High-Density Regions 246
19.1.2 Other Quantitative Tracers of High-Density Environments 249
19.2 Measuring the Induced Perturbations 250
19.2.1 Other Tracers of Induced Perturbations 253
Appendix A Photometric Redshifts and K-Corrections 255
A.1 The Photometric Redshifts 255
A.1.1 UV-Optical-Near-Infrared Photo-z 255
A.1.2 Far Infrared-Radio Continuum Photo-z 258
A.2 The K-Correction 258
Appendix B Broad Band Photometry 263
B.1 Photometric Systems 263
Appendix C Physical and Astronomical Constants and Unit Conversions 267
References 269
Index 319
English
“This book is well-sourced and draws widely on the literature, giving access to a wide range of examples of use of the methods the author advocates – and making the book an especially useful resource for those starting in the field.” (Astronomy & Geophysics, 1 August 2012)
