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Fundamentals of Radio Astronomy: Observational Methods [Hardback]

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(Union College, Schenectady, New York, USA), (University of Massachusetts Amherst, Massachusetts, USA), (National Autonomous University of Mexico, Morelia)
  • Formāts: Hardback, 352 pages, height x width: 254x178 mm, weight: 771 g, 4 Tables, black and white; 7 Illustrations, color; 144 Illustrations, black and white
  • Sērija : Series in Astronomy and Astrophysics
  • Izdošanas datums: 03-Dec-2015
  • Izdevniecība: CRC Press Inc
  • ISBN-10: 1420076760
  • ISBN-13: 9781420076769
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Fundamentals of Radio Astronomy: Observational MethodsPalielināt
  • Formāts: Hardback, 352 pages, height x width: 254x178 mm, weight: 771 g, 4 Tables, black and white; 7 Illustrations, color; 144 Illustrations, black and white
  • Sērija : Series in Astronomy and Astrophysics
  • Izdošanas datums: 03-Dec-2015
  • Izdevniecība: CRC Press Inc
  • ISBN-10: 1420076760
  • ISBN-13: 9781420076769
Citas grāmatas par šo tēmu:
Permanent link: https://www.kriso.lv/db/9781420076769.html
Keywords:
As evidenced by five Nobel Prizes in physics, radio astronomy in its 80-year history has contributed greatly to our understanding of the universe. Yet for too long, there has been no suitable textbook on radio astronomy for undergraduate students.

Fundamentals of Radio Astronomy: Observational Methods is the first undergraduate-level textbook exclusively devoted to radio astronomy telescopes and observation methods. This book, the first of two volumes, explains the instrumentation and techniques needed to make successful observations in radio astronomy. With examples interspersed throughout and problems at the end of each chapter, it prepares students to contribute to a radio astronomy research team.

Requiring no prior knowledge of astronomy, the text begins with a review of pertinent astronomy basics. It then discusses radiation physics, the collection and detection of astronomical radio signals using radio telescopes, the functioning of various components of radio telescopes, and the processes involved in making successful radio observations. The book also provides a conceptual understanding of the fundamental principles of aperture synthesis and a more advanced undergraduate-level discussion of real-world interferometry observations.

Web ResourceA set of laboratory exercises is available for download on the books CRC Press web page. These labs use the Small Radio Telescope (SRT) and the Very Small Radio Telescope (VSRT) developed for educational use by MITs Haystack Observatory. The web page also includes a Java package that demonstrates the principles of Fourier transforms, which are needed for the analysis of interferometric data.

Recenzijas

"This is an excellent introduction for students wanting to get into the exciting world of radio astronomy. It starts at the basics and builds up nicely to provide readers with the understanding they will need for both single dish observing and radio interferometry. The separation of the more mathematically challenging aspects means that it can be used at a variety of levels, including for advanced undergraduate or postgraduate students. Given the wealth of radio research facilities, such as the JVLA, ALMA, and the upcoming SKA, this is also a very timely textbook. I will start using it immediately in my training programs." Melvin Hoare, Professor of Astrophysics, University of Leeds

"Since the detection of HI at 21 cm wavelength and the discovery of CO in dark clouds, radio astronomy has been a central tool in studies of the interstellar medium and star forming clouds. This has been even more true with the advent of cm and mm interferometers, and the more recent availability of the EVLA and ALMA has transformed the study of circumstellar disks and of outflows. This two-volume set of introductory textbooks provide the essential foundation for students who plan to use radio observations in the study of molecular clouds, HII regions, and star formation. While one volume focuses on the instrumentation, telescopes, and observing methods of radio astronomy, the other deals with the astrophysical processes that give rise to radio emission. All three authors have taught radio astronomy courses, and the books are organized with questions and problems after each chapter. The books are also equipped with extensive appendices with supporting material that focus on background and technical information."

The Star Formation Newsletter No 323, November 2019

Preface, xi
Acknowledgments, xv
Chapter 1 Introductory Material 1(30)
1.1 Brief History Of Radio Astronomy
2(2)
1.2 Some Fundamentals Of Radio Waves
4(6)
1.2.1 Electromagnetic Radiation
4(3)
1.2.2 Spectroscopy
7(3)
1.3 Finding Our Way In The Sky
10(11)
1.3.1 Sky Coordinate System: Right Ascension and Declination
10(3)
1.3.2 Observer-Centered Definitions
13(4)
1.3.3 Apparent Sizes
17(4)
1.4 Basic Structure Of A Traditional Radio Telescope
21(4)
1.4.1 Parabolic Reflector
21(1)
1.4.2 Mount
22(2)
1.4.3 Feeds, Receivers, and Computer
24(1)
1.5 Radio Maps
25(3)
Questions And Problems
28(3)
Chapter 2 Introduction to Radiation Physics 31(44)
2.1 Measures Of The Amount Of Radiation
31(9)
2.1.1 Total Energy Emitted
31(1)
2.1.2 Luminosity
32(1)
2.1.3 Flux
32(1)
2.1.4 Flux Density
33(2)
2.1.5 Intensity
35(5)
2.1.6 Relation between Intensity and the Electric Field and Magnetic Field Waves
40(1)
2.2 Blackbody Radiation
40(12)
2.3 Rayleigh—Jeans Approximation
52(2)
2.4 Brightness Temperature
54(2)
2.5 Coherent Radiation
56(4)
2.6 Interference Of Light
60(2)
2.7 Polarization Of Radiation
62(9)
2.7.1 Stokes Parameters
67(4)
Questions And Problems
71(4)
Chapter 3 Radio Telescopes 75(52)
3.1 Radio Telescope Reflectors, Antennas, And Feeds
76(18)
3.1.1 Primary Reflectors
76(4)
3.1.2 Beam Pattern
80(5)
3.1.3 Feeds and Primary Reflector Illumination
85(4)
3.1.4 Surface Errors
89(3)
3.1.5 Beam Pattern Revisited
92(2)
3.2 Heterodyne Receivers
94(8)
3.2.1 Transmission Lines
95(1)
3.2.2 Front-End Receiver Components
96(4)
3.2.3 Back-End Receiver Components
100(2)
3.2.4 High-Frequency Heterodyne Receivers
102(1)
3.3 Noise, Noise Temperature, And Antenna Temperature
102(7)
3.4 Bolometer Detectors
109(1)
3.5 Spectrometers
110(6)
3.5.1 Filter Bank Spectrometer
110(2)
3.5.2 Digital Spectrometers
112(4)
3.6 Very Low-Frequency Radio Astronomy
116(8)
3.6.1 Low-Frequency Window
116(1)
3.6.2 Antennas
116(5)
3.6.3 Receivers
121(2)
3.6.4 Radio Frequency Interference
123(1)
Questions And Problems
124(3)
Chapter 4 Single-Dish Radio Telescope Observations 127(54)
4.1 Basic Measurements With A Single-Dish Telescope
128(8)
4.1.1 Switched Observations
128(2)
4.1.2 Determination of System Temperature
130(1)
4.1.3 Measurement of Antenna Temperature
131(1)
4.1.4 Uncertainty in the Measured Antenna Temperature
131(5)
4.2 Antenna Beam
136(9)
4.2.1 Beam Power Pattern and Antenna Solid Angle
137(1)
4.2.2 Main Beam and Angular Resolution
138(3)
4.2.3 Main Beam Efficiency
141(3)
4.2.4 Detected Power from Extended Sources
144(1)
4.3 Observing Resolved Versus Unresolved Sources
145(7)
4.3.1 Unresolved Sources
145(1)
4.3.2 Resolved Sources
146(3)
4.3.3 Uniform Source That Fills the Sky
149(1)
4.3.4 Brightness Temperature versus Antenna Temperature, Beam Dilution, and Beam Filling Factor
150(2)
4.4 SPECTRAL-LINE OBSERVATIONS
152(3)
4.4.1 Spectral Parameters
152(2)
4.4.2 Frequency Switching
154(1)
4.5 Obtaining Radio Images
155(10)
4.5.1 Convolution with Beam Pattern
157(6)
4.5.2 Deconvolution
163(2)
4.6 Calibration Of A Radio Telescope
165(5)
4.6.1 Pointing Corrections
165(1)
4.6.2 Calibration of the Gain, Effective Area, and Gain Curve
166(2)
4.6.3 Measuring the Beam Pattern and Main Beam Efficiency
168(1)
4.6.4 Calculating Antenna Solid Angle and Main Beam Efficiency
169(1)
4.7 Telescope Sensitivity Considerations In Planning An Observation
170(3)
4.8 Polarization Calibration
173(3)
Questions And Problems
176(5)
Chapter 5 Aperture Synthesis Basics: Two-Element Interferometers 181(40)
5.1 Why Aperture Synthesis?
183(1)
5.2 Two-Element Interferometer
184(2)
5.3 Observations Of A Single-Point Source
186(5)
5.3.1 Response of the Additive Interferometer
188(2)
5.3.2 Response of the Multiplicative Interferometer
190(1)
5.3.3 Effect of Noise
190(1)
5.4 Fringe Function
191(4)
5.5 Visibility Function
195(5)
5.5.1 Analysis of Visibilities for a Single-Point Source
198(2)
5.6 Observations Of A Pair Of Unresolved Sources
200(6)
5.7 Observations Of A Single Extended Source
206(3)
5.8 Coherence And The Effects Of Finite Bandwidth And Integration Time
209(5)
5.8.1 Bandwidth Smearing
209(3)
5.8.2 Time Smearing
212(2)
5.9 Basic Principles Of Interferometry
214(2)
Questions And Problems
216(5)
Chapter 6 Aperture Synthesis: Advanced Discussion 221(60)
6.1 Cross-Correlation Of Received Signals
222(2)
6.2 Complex-Valued Cross-Correlation
224(3)
6.3 Complex Correlation Of A Point Source At A Single Frequency
227(1)
6.4 Extended Sources And The Fourier Transform
228(1)
6.5 Fourier Transforms For Some Common Source Shapes
229(2)
6.5.1 Visibility Function of a Point Source
230(1)
6.5.2 Visibility Function of Two Point Sources
230(1)
6.5.3 Visibility Function of a Gaussian Profile
231(1)
6.6 Three Dimensions, The Earth's Rotation, And The Complex Fringe Function
231(6)
6.7 Nonzero Bandwidth And Finite Integration Time
237(4)
6.8 Source Structure And The Visibility Function
241(8)
6.8.1 Sky Coordinates and the Visibility Function
241(3)
6.8.2 uv-Plane
244(2)
6.8.3 Visibility Functions of Simple Structures
246(3)
6.9 The Earth's Rotation And UV Tracks
249(3)
6.10 Interferometers As Spatial Filters
252(6)
6.11 Sensitivity And Detection Limits
258(5)
6.11.1 Noise in a Visibility
259(1)
6.11.2 Image Sensitivity
260(2)
6.11.3 Brightness Sensitivity
262(1)
6.12 Calibration
263(2)
6.13 Image Formation
265(11)
6.13.1 Image Dimensions and Gridding Parameters
266(1)
6.13.2 Dirty Map and Dirty Beam
267(3)
6.13.3 uv Weighting Schemes
270(1)
6.13.4 CLEANing the Map: Deconvolving the Dirty Beam
271(2)
6.13.5 Self-Calibration and Closure Phase and Amplitude
273(3)
6.14 Very Long Baseline Interferometry
276(2)
6.14.1 VLBI Resolution and Sensitivity
277(1)
6.14.2 Hardware Considerations for VLBI
277(1)
6.14.3 Fringe Searching or Fringe Fitting
278(1)
Questions And Problems
278(3)
Appendix I: Constants And Conversions, 281(2)
Appendix II: Derivation Of Beam Pattern, 283(8)
Appendix III: Cross-Correlations, 291(4)
Appendix IV: Complex-Exponential Form Of Wave Functions, 295(6)
Appendix V: Primer On Fourier Transforms, With Focus On Use In Aperture Synthesis, 301(12)
Appendix VI: Convolution Theorem, 313(2)
Appendix VII: Interferometer Simulation Activities, 315(8)
Index, 323
Jonathan M. Marr is a senior lecturer of physics and astronomy at Union College. His research involves high-resolution, radio-wavelength observations of radio galaxies and the Galactic center. He earned a PhD in astronomy from the University of California, Berkeley.

Ronald L. Snell is a professor of astronomy at the University of Massachusetts, Amherst. His research interests include the physical and chemical properties of molecular clouds, star formation, and molecular outflows; he also has extensive experience observing at radio wavelengths. He earned a PhD in astronomy from the University of Texas at Austin.

Stanley E. Kurtz is a professor of radio astronomy and astrophysics at the National Autonomous University of Mexico. His research interests include massive star formation, the interstellar medium, and radio astronomy instrumentation and techniques. He earned a PhD in physics from the University of Wisconsin at Madison.