Handbook on Radio Astronomy -Third Edition
Introduction to the third edition by the Chairman of ITU-R Working Party 7D (Radio Astronomy)
PREFACE
TABLE OF CONTENTS
PREAMBLE- Radio Astronomy and Society
0.1 Introduction to astronomy
0.2 The role of radio astronomy
0.3 Economic and societal value
0.3.1 Introduction
0.3.2 Economic and societal value of radio astronomy research
0.3.2.1 Telecommunication technology
0.3.2.2 Interferometric technology
0.3.2.3 Computing technology
0.3.2.4 Medical technology
0.3.2.5 Time and frequency standards
0.3.2.6 Earth observation
0.3.2.7 Geodesy
0.3.2.8 Mining technology
0.3.2.9 Radar astronomy
0.4 Solar Radio Monitoring
0.4.1 Introduction
0.4.2 Overview of solar radio monitoring
0.4.3 Impact and societal value
0.4.3.1 Environmental applications studies / monitoring
0.4.3.2 Technical/Infrastructural uses
Solar-driven effects on satellites
Ionospheric effects
Geomagnetic effects on ground systems
0.5 Trends in radio astronomy
0.6 Conclusions
CHAPTER 1 - Introduction
1.1 The Radiocommunication Sector and World Radiocommunication Conferences
1.2 The Radio Regulations and frequency allocations
1.3 Radio astronomy as a radiocommunication service
1.4 Frequency allocation problems for radio astronomy
REFERENCES
CHAPTER 2 - Characteristics of the Radio Astronomy Service
2.1 The RAS
2.2 Origin and nature of cosmic radio emissions
2.3 Continuum radiation
2.3.1 Time variability of continuum radiation
2.3.2 Measurement of continuum radiation
2.4 Spectral-line radiation
2.4.1 Types of spectral lines
2.4.2 Measurement of spectral lines
2.5 Modern Practice
2.6 Conclusion
REFERENCES
CHAPTER 3 - Preferred frequency bands for radio astronomy observations
3.1 General considerations
3.1.1 Ground-based radio astronomy observations
3.1.2 Space-based radio astronomy observations
3.2 Preferred continuum bands
3.2.1 Observations at low frequencies
3.2.2 High frequency bands for continuum observations
3.3 Bands for spectral-line observations
CHAPTER 4 - Vulnerability of radio astronomy observations to interference
4.1 Introduction
4.2 Basic considerations in the calculation of interference levels
4.2.1 Detrimental-level criterion for interference
4.2.2 Antenna response pattern
4.2.3 Averaging time (integration time)
4.2.4 Percentage of time lost to interference
4.3 Sensitivity of radio astronomy systems and threshold values of detrimental interference
4.3.1 Theoretical considerations
4.3.2 Estimates of sensitivity and detrimental interference levels
4.4 Response of interferometers and arrays to radio interference
4.5 Pulsars
4.6 Achieved sensitivities
4.7 Discussion of interference
4.7.1 Interference levels
4.7.2 Interference from astronomical sources
4.7.3 Special considerations for transmitters on geostationary satellites
4.7.4 Filtering
4.7.5 Interference levels capable of damaging or saturating a radioastronomy receiver
4.8 Monte Carlo analysis
ANNEX 1 TO CHAPTER 4 - Side-lobe model from Recommendation ITU-R S.1428
REFERENCES
CHAPTER 5 - Sharing the radio astronomy bands with other services
5.1 General remarks
5.1.1 Protection criteria for the RAS
5.2 Separation distances required for sharing with a single transmitter (see Recommendation ITU-R RA.1031)
5.3 Sharing within LoS
5.4 Sharing with services with terrestrial transmitters
5.5 Sharing with mobile services
5.6 Sharing in radio astronomy bands below 40 GHz
5.6.1 The band 1 330-1 427 MHz
5.6.2 The band 4 800-5 000 MHz
5.6.3 The bands 22.01-22.21 and 22.21-22.5 GHz
5.7 Sharing in radio astronomy bands above 40 GHz
5.7.1 Sharing between 60 and 275 GHz
5.7.2 Sharing above 275 GHz
5.8 Sharing with deep-space research
5.9 Time sharing
5.9.1 Time and frequency sharing coordination
REFERENCES
CHAPTER 6 - Interference to Radio Astronomy from transmitters in other bands
6.1 Introduction
6.1.1 Definitions from the RR
6.1.2 Additional definitions
6.1.3 Mechanisms of interference from transmitters in other bands
6.2 Limits for unwanted emissions from active services
6.2.1 Limits within the spurious emissions domain
6.2.2 Limits within the OoB emissions domain
6.2.3 Limits on unwanted emissions of active services to protect radio astronomy bands
6.3 Performance of radio astronomy receivers
6.3.1 Filtering of band-edge interference
6.3.2 Non-linear effects and intermodulation
6.3.3 Linearity
6.3.4 Filtering and digitization
6.4 Interference from transmitters of services in other bands
6.4.1 Services which could cause interference to radio astronomy through adjacent-band and harmonic mechanisms
6.4.2 The transition to digital television and its impact on the unprotected use by the radio astronomy service of bands used for terrestrial television broadcasting
6.4.2.1 Australia
6.4.2.2 Brazil
6.4.2.3 Japan
6.4.2.4 United States of America
6.4.3 Interference from satellite transmissions
6.4.3.1 Geostationary satellites
6.4.3.2 Non-geostationary satellites
6.4.3.2.1 Example of unwanted emissions from the fixed-satellite service
6.4.3.3 Potential cases of harmonic interference from satellites
6.4.3.3.1 Second harmonic radiation in the 23.6-24.0 GHz band from broadcasting satellites
6.4.3.3.2 Second-harmonic radiation near 22.2 GHz from the FSS
6.4.3.3.3 Second-harmonic radiation in the 4 990-5 000 MHz band from the radiodetermination satellite and mobile satellite band
6.4.3.3.4 Third-harmonic radiation in the 1 400-1 427 MHz band from the meteorological-satellite service
6.5 Unwanted emissions from wideband modulation
6.5.1 Usage of broadband modulation
6.5.2 Pulse shaping to reduce unwanted emissions
6.5.3 Example of interference from broadband modulation.
6.5.4 Example: Radio interference from the IRIDIUM (HIBLEO-2) MSS system
6.5.4.1 RAS operations in the band 1610.6-1613.8 MHz
6.5.4.2 IRIDIUM constellation description
6.5.4.3 Nature and characteristics of the IRIDIUM interference.
6.5.4.4 Measurements and verification
6.5.4.5 Measurements at Leeheim MS on 8-9.6.2010
6.6 Conclusions
REFERENCES
CHAPTER 7 - Special techniques, applications and observing locations
7.1 Introduction
7.2 VLBI, including Space VLBI
7.2.1 Space VLBI
7.2.1.1 Space VLBI projects
7.2.1.2 Distinctive features of Space VLBI and their recent evolution
7.2.1.3 Frequency requirements for operation of space VLBI
7.2.2 Geodetic applications using VLBI
7.3 Radio astronomy from the L2 Sun-Earth Lagrangian point
7.4 Radio astronomy from the shielded zone of the Moon
7.4.1 The shielded zone of the Moon
7.4.2 Spectral ranges preferred for observations from the Moon
7.4.3 Regulation of use of the shielded zone of the Moon
7.5 Terrestrial sites with low atmospheric absorption
7.5.1 Antarctica
7.5.2 Cerro Chajnantor, Chile
7.5.3 Mauna Kea, Hawaii
7.5.4 Mt. Graham, Arizona
7.6 Pulsar observations and application as time standards
7.6.1 Pulsars as standard clocks
7.6.2 Pulsars as reference coordinate objects
7.7 Solar monitoring
REFERENCES
CHAPTER 8 - Interference mitigation
8.1 Introduction - Objectives
8.2 Signatures of RFI sources and their impact
8.3 RFI Mitigation Methodologies - layers of mitigation
8.4 Pro-active methods - changing the RFI environment
8.5 Pre-detection & post-detection
8.6 Pre-correlation
8.6.1 Antenna-based digital processing
8.6.2 Adaptive (temporal) noise cancellation
8.6.3 Spatial filtering and null steering
8.7 At correlation
8.8 Post-correlation - before or during imaging
8.9 Implementation at telescopes - strategy
8.10 Conclusions
CHAPTER 9 - Radio quiet zones
9.1 Introduction
9.1.1 Definition and general requirements of a radio quiet zone
9.1.2 Role of regulation
9.2 Considerations in developing an RQZ
9.2.1 Geographic
9.2.2 Frequency
9.2.3 Impact of RFI on RAS observations
9.3 Electromagnetic environment
9.3.1 Intentional radiators
9.3.2 Unintentional radiators
9.3.3 Propagation of interfering signals
9.4 Methods to achieve an RQZ
9.4.1 Receive-side methods
9.4.2 Transmit-side methods – Managing an RQZ
9.4.2.1 Legislative and regulatory control
9.4.2.2 Alternative technologies and network design
9.5 Implications in establishing an RQZ
9.5.1 Maintenance of RQZs
9.5.2 Long–term considerations
CHAPTER 10 - Searches for extraterrestrial intelligence (Seti) using observations at radio frequencies
10.1 Introduction
10.2 Detectability of SETI signals
10.3 Signal intensity
10.4 Receiving system sensitivity
10.4.1 Minimum detectable signal power
10.5 Antenna pointing direction
10.6 Signal identification and interference rejection
10.7 Candidate bands to be searched
REFERENCES
CHAPTER 11 - Ground-based radar astronomy
11.1 Introduction
11.2 Sensitivity issues
11.3 Operational modes and bandwidth requirements
11.4 Radar astronomy installations