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E-raamat: Panchromatic View of Galaxies

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(Laboratoire d'Astrophysique de Marseille, France)
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  • Ilmumisaeg: 13-Jan-2012
  • Kirjastus: Blackwell Verlag GmbH
  • Keel: eng
  • ISBN-13: 9783527640263
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Panchromatic View of GalaxiesSuurem pilt
  • Formaat: EPUB+DRM
  • Ilmumisaeg: 13-Jan-2012
  • Kirjastus: Blackwell Verlag GmbH
  • Keel: eng
  • ISBN-13: 9783527640263
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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.

Arvustused

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)

 

Preface XIII
1 Introduction 1(14)
1.1 Galaxies
1(3)
1.2 A Multifrequency Approach
4(6)
1.3 The Purpose of this Book
10(5)
Part One Emitting Sources and Radiative Processes in Galaxies 15(44)
2 X-ray
17(8)
2.1 Continuum
17(8)
2.1.1 Discrete Sources
18(2)
2.1.2 X-ray Emission in Active Galaxies
20(1)
2.1.3 Hot Gas
21(4)
3 UV-Optical-NIR
25(16)
3.1 Continuum: Stellar Emission
26(2)
3.2 Emission Lines
28(7)
3.2.1 Hydrogen Lines
32(2)
3.2.2 Metals
34(1)
3.3 Absorption Lines
35(4)
3.3.1 Hydrogen Lines
37(1)
3.3.2 Other Elements
38(1)
3.4 Molecular Lines
39(2)
3.4.1 H2 Near-Infrared Emission Lines
39(1)
3.4.2 H2 UV Absorption Lines
39(2)
4 The Infrared
41(10)
4.1 Continuum: Dust Emission
42(2)
4.2 Emission Lines
44(7)
4.2.1 PAHs
44(1)
4.2.2 Cooling Lines in PDR
45(2)
4.2.3 H2 Lines
47(2)
4.2.4 Dust Absorption of Lyα Scattered Photons
49(2)
5 Millimeter and Centimeter Radio
51(8)
5.1 Continuum
51(3)
5.1.1 Free-Free Emission
52(1)
5.1.2 Synchrotron Emission
53(1)
5.1.3 Dust Emission
53(1)
5.2 Emission Lines
54(3)
5.2.1 Molecular Lines
54(1)
5.2.2 HI
55(2)
5.3 Absorption Lines
57(4)
5.3.1 HI
57(2)
Part Two Derived Quantities 59(134)
6 Properties of the Hot X-ray Emitting Gas
61(2)
6.1 X-ray Luminosity
61(1)
6.2 Gas Temperature
61(2)
7 Dust Properties
63(8)
7.1 The Far-IR Luminosity
63(2)
7.2 Dust Mass and Temperature
65(6)
8 Radio Properties
71(6)
8.1 Determining the Contribution of the Different Radio Components
71(3)
8.1.1 Synchrotron vs. Free-Free Radio Emission in the Centimeter Domain
71(1)
8.1.2 The Emission of the Cold Dust Component at λ < 1.5mm
72(2)
8.2 The Radio Luminosity
74(3)
9 The Spectral Energy Distribution
77(14)
9.1 The Emission in the UV to Near-Infrared Spectral Domain
79(5)
9.1.1 UV, Optical, and Near-IR Colors
81(2)
9.1.2 Fitting SEDs with Population Synthesis Models
83(1)
9.2 The Dust Emission in the Infrared Domain
84(6)
9.2.1 Mid- and Far-Infrared Colors
86(4)
9.3 The Thermal and Nonthermal Radio Emission
90(1)
10 Spectral Features
91(16)
10.1 Galaxy Characterization through Emission and Absorption Lines
91(10)
10.1.1 Classification of the Nuclear Activity
92(1)
10.1.2 Classification of Post-Starburst and Post-Star-Forming Galaxies
92(3)
10.1.3 Line Diagnostics
95(6)
10.2 Gas Metallicity from Emission Lines
101(2)
10.3 Stellar Age and Metallicity from Absorption Lines
103(4)
11 Gas Properties
107(18)
11.1 Gas Density, Mass, and Temperature
107(18)
11.1.1 The Atomic HI Mass
108(7)
11.1.2 The Molecular H2 Mass
115(10)
12 Dust Extinction
125(18)
12.1 Galactic Extinction
126(6)
12.1.1 Extinction Curve
127(5)
12.2 Internal Attenuation
132(11)
12.2.1 Attenuation of the Emission Lines
133(1)
12.2.2 Attenuation of the Stellar Continuum
134(9)
13 Star Formation Tracers
143(18)
13.1 The Initial Mass Function
143(1)
13.2 The Star Formation Rate
144(2)
13.3 The Birthrate Parameter and the Specific Star Formation Rate
146(1)
13.4 The Star Formation Efficiency and the Gas Consumption Time Scale
147(1)
13.5 Hydrogen Emission Lines
147(4)
13.6 UV Stellar Continuum
151(1)
13.7 Infrared
152(1)
13.7.1 Integrated Infrared Luminosity
152(1)
13.7.2 Monochromatic Infrared Luminosities
153(1)
13.8 Radio Continuum
153(2)
13.9 Other Indicators
155(3)
13.9.1 The X-ray Luminosity
155(1)
13.9.2 Forbidden Lines
156(1)
13.9.3 [ CII]
157(1)
13.9.4 Radio Recombination Lines
157(1)
13.10 Population Synthesis Models
158(3)
13.10.1 Dating a Star Formation Event
158(3)
14 Light Profiles and Structural Parameters
161(10)
14.1 The Surface Brightness Profile
161(5)
14.1.1 Extended Radial Profiles
161(1)
14.1.2 The Central Surface Brightness Profile of Early-Type Galaxies
162(4)
14.1.3 The Vertical Light Profile of Late-Type Galaxies
166(1)
14.2 Structural Parameters
166(2)
14.2.1 Total Magnitudes, Effective Radii and Surface Brightnesses
166(1)
14.2.2 Bulge to Disk Ratio
167(1)
14.3 Morphological Parameters
168(3)
14.3.1 Concentration Index
168(1)
14.3.2 Asymmetry
168(1)
14.3.3 Clumpiness
169(1)
14.3.4 The Gini Coefficient G and the Second-Order Moment of the Brightest 20% of the Galaxy's Flux M20
169(2)
15 Stellar and Dynamical Masses
171(22)
15.1 Stellar Mass Determination Using Population Synthesis Models
171(4)
15.2 Dynamical Mass
175(20)
15.2.1 Rotation Curves and the Dark Matter Distribution
177(7)
15.2.2 The Total Mass of Elliptical Galaxies from Kinematical Measurements
184(1)
15.2.3 The Total Mass of Elliptical Galaxies from X-ray Measurements
185(2)
15.2.4 The Mass of the Supermassive Black Hole
187(6)
Part Three Constraining Galaxy Evolution 193(62)
16 Statistical Tools
195(20)
16.1 Galaxy Number Counts
195(5)
16.1.1 Observed Number Counts
197(3)
16.2 Luminosity Function
200(9)
16.2.1 Parametrization of the Luminosity Function
203(1)
16.2.2 Luminosity Distributions and Bivariate Luminosity Functions
204(1)
16.2.3 The Observed Luminosity Functions
205(4)
16.3 Luminosity Density
209(6)
16.3.1 The Cosmic Star Formation History and Build Up of the Stellar Mass
211(4)
17 Scaling Relations
215(20)
17.1 Spectrophotometric Relations
216(7)
17.1.1 The Color-Magnitude and Color-Color Relations
216(2)
17.1.2 The Mass-Metallicity Relation
218(2)
17.1.3 The Mass-Gas Relation
220(2)
17.1.4 The Mass-Star Formation Rate Relation
222(1)
17.2 Structural Relations
223(1)
17.2.1 The Surface Brightness-Absolute Magnitude Relation
223(1)
17.2.2 The Kormendy Relation
224(1)
17.3 Kinematical Relations
224(7)
17.3.1 The Tully-Fisher Relation
225(3)
17.3.2 The Faber-Jackson Relation and the Fundamental Plane
228(2)
17.3.3 The k-Space
230(1)
17.4 Supermassive Black Hole Scaling Relations
231(4)
18 Matter Cycle in Galaxies
235(10)
18.1 The Star Formation Process
236(3)
18.1.1 The Schmidt Law
236(3)
18.2 Feedback
239(6)
18.2.1 The Feedback of AGNs
239(3)
18.2.2 The Feedback of Massive Stars
242(3)
19 The Role of the Environment on Galaxy Evolution
245(10)
19.1 Tracers of Different Environments
245(5)
19.1.1 Detection of High-Density Regions
246(3)
19.1.2 Other Quantitative Tracers of High-Density Environments
249(1)
19.2 Measuring the Induced Perturbations
250(5)
19.2.1 Other Tracers of Induced Perturbations
253(2)
Appendix A Photometric Redshifts and K-Corrections 255(8)
A.1 The Photometric Redshifts
255(3)
A.1.1 UV-Optical-Near-Infrared Photo-z
255(3)
A.1.2 Far Infrared-Radio Continuum Photo-z
258(1)
A.2 The K-Correction
258(5)
Appendix B Broad Band Photometry 263(4)
B.1 Photometric Systems
263(4)
Appendix C Physical and Astronomical Constants and Unit Conversions 267(2)
References 269(50)
Index 319
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.
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