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HawkRAO
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About HawkRAO
Vela Pulsar Observations
Detection of Two Vela Pulsar 'Glitches'
B0833-45 Daily Observations
Latest Observation Results
Invalid Results Gallery
Observation System Information
PDMP Results Gallery
Vela Pulsar
Sample Data Files
Technical Notes
Links
Cosmic Maser Projects Overview
Sensitivity Calculations
Extra-Galactic Hydrogen Line Observations
Hydrogen Line Emissions
System Design
Data Analysis
Results
Initial Activities
Developing Custom Applications
Detecting the Magellanic Clouds
Comparison Between 8-bit and 1-bit Data Results
Improvements in 'Dark Frame' Subtraction and Results Graph Corrections
Improving S/N by Integrating Daily Runs
Mitigating Against the Effects of RFI
Matching Plots with the LAB Survey Results
Negative Results with NGC300
Negative Results with the Magellanic Stream
Improving Agreement with LAB Survey Results (LMC)
Improving Agreement with LAB Survey Results (SMC)
Overall Conclusion
External Galaxies
The Magellanic Clouds - Our Near Galactic Neighbours
The Magellanic Stream
The Andromeda Galaxy (M31/NGC224 )
The Triangulum Galaxy (M33/NGC598 )
NGC300 - a Spiral Galaxy Far, Far Away...
Links
Dispersed Radio Transients (DRATs)
Archival Data
Starting Point
Fast Search Algorithm
Search Software
Low-DM Dispersed Transients Found
Crab Pulsar Giant Pulses ?
Complete Archive Processing
High Dispersion Transients
Summary - Dispersed Transients
Miscellaneous Sub-Projects
Sawbird LNA Bandpass Plots
Re-tuning Duplexers for Bandpass Filter Mode
Programming FE-5680A RFS
10 MHz Distribution Amplifier
MAX2870 Sig Gen Frequency Accuracy
Modifying Signal Generator to External Reference - Part I
Modifying Signal generator to External Reference - Part II
Software Control of MAX2870 LCD Signal Generator
Measurement of Ku-Band LO Frequencies: H/W-Based
Measurement of Ku-Band LO Frequencies: S/W-Based
Test Gear
Components for RA
Sawbird LNAs
Bandpass Filters On Hand
Ku-Band LNBFs
HawkRAO Antennas
Circularly-Polarised Yagis
3 m TVRO Dish Antenna
Neutron Star Group
Amateur Pulsar Hunters
Challenges for Amateur Pulsar Detection
The 'EME' Factor
Strength of the Pulsar Signal
Nature of the Signal
Effects of Scintillation
Effects of Dispersion
Doppler Effects
Polarisation Effects
Method of Detection
Effect of Parameters
Which Observation Frequency ?
Some Worked Examples for Small Antennas at 400 MHz
Required Minimum Antenna Gain for Detection of the 100 Strongest Pulsars
Frequency Accuracy
General Description of Equipment
Verification of Results
The Scientific Method
Ultimate Responsibility for Verification of Results
Further Details About the Importance of the Scientific Method
Location of Observatory - RFI and Ground Noise
Some Information About 'Folding'
Conclusion
Technical Topics - Pulsar
About Pulsars
Epoch Folding Basics
Relative Flux Density of Pulsars
Accounting for Vela's Glitch Behaviour
Dispersion Delay for 2 MHz Bandwidth at 400 MHz and 1400 MHz
Software
Articles - Pulsar
Links - Pulsar
Contact
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Results
Results obtained by incremental improvements to the observation system
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