1. Weak Signal Detection of Virgo A www.dmradas.co.uk Exploring some Limitations in Amateur Radio Astronomy Dr David Morgan Exploring some Limitations in Amateur Radio Astronomy 17/5/2014

2. Weak Signal Detection of Virgo AContents www.dmradas.co.uk 3m Dish L Band Horn 408MHz Quagis Antennas & Receiver properties Radio source strength & spectra Limitations with small antennas

3. Weak Signal Detection of Virgo A Telescope Characteristics www.dmradas.co.uk Antenna properties

4. Weak Signal Detection of Virgo A Antenna Fundamentals Two fundamental properties of an antenna of concern to amateur radio astronomers Gain Beamwidth These are related – the higher the gain the smaller the beamwidth We want both high gain and narrow beamwidth Gain = sensitivity Beamwidth = spatial selectivity www.dmradas.co.uk 8 0 HPBW Need Large antenna aperture A 3m dia. dish polar diagram

5. Weak Signal Detection of Virgo A Antenna Equations Antenna Gain G =      ) A  Aperture efficiency A= Antenna aperture m 2  wavelength www.dmradas.co.uk Antenna Beamwidth For a reflector antenna, the area is simply the projected area. For a circular reflector of diameter D, the area is A =  D 2 /4 and the gain is G =  (  D / ) 2 HPBW =    / D  a factor that depends on the shape of the reflector and the method of illumination For a typical antenna G = 27,000/ (  ) 2 Antenna diameter drives performance

6. Weak Signal Detection of Virgo A At UHF things get big Rare to find an amateur with a 9m antenna www.dmradas.co.uk John Smith (1924 -1998) with 9m dish

7. Weak Signal Detection of Virgo A Yagis vs Dishes Would not tend to use a small dish at UHF Yagi arrays probably cheaper and easier to build But – effective aperture must be similar to dish area So arrays will be a few metres square Complicated to construct and phase together www.dmradas.co.uk DL7APV Array (used for EME) Part of my 408MHz Quagi Array

8. Weak Signal Detection of Virgo AConsequences Can have high sensitivity and good spatial resolution at 11GHz with1m antenna ~40dB gain and few degrees HPBW Reasonable gain and resolution with 2.4m dish at C band ~ 35dB gain and <5 degrees HPBW Workable sensitivity and resolution with 3m dish at 1.4GHz eg 30dB gain and >5 degrees HPBW But low gain and poor spatial resolution with 3m dish at 408MHz eg 19dB gain and 18 degrees HPBW Impractical at VHF (space & cost) www.dmradas.co.uk

9. Weak Signal Detection of Virgo A Result of Antenna limitations L band is probably most practical, useful and affordable option for amateurs (L Band (IEEE) = 1-2GHz)

10. Weak Signal Detection of Virgo A Noise and Gain Stability www.dmradas.co.uk Receiver Requirements Band coverage Available bandwidths Detector functions Sensitivity Noise & gain stability Discuss the last two items

11. Weak Signal Detection of Virgo A LNAs and Receivers Receiver must have high gain and low noise System Noise figure (N F ) determined by first amplifier Low Noise Amplifiers (LNA) now capable of 0.2dB at 1.4GHz Conventional Coms receiver or SDR sensitivities are adequate when used with LNA ( gains of 20 – 40dB) Noise & gain stability are crucial: Maintain common parameters from hour to hour and day to day – to enable radio maps etc to be made. www.dmradas.co.uk ICOM IC-R7000 Receiver FunCube Dongle SDR Realtek RTL2832U DVB-TV dongle

12. Weak Signal Detection of Virgo A SDR Dongle Receivers The common SDR Dongles have gaps in frequency coverage FCDPro RTL FCDPro+ 1MHz10MHz100MHz1GHz2GHz Frequency 60 1.1 1.27 1.7 240 4201.9 26 1.11.25 2.2 Device Frequency Coverage for FCD & RTL Dongle Devices 408MHz 1.4GHz Coverage Gaps

13. Weak Signal Detection of Virgo A Noise /Gain Stability FunCube Dongle Pro + : Stability is better than 0.05dB over 3 hours www.dmradas.co.uk Cheap stable SDR receivers widely available No important receiver limitations

14. Weak Signal Detection of Virgo A Objects to Observe www.dmradas.co.uk Astronomical Radio Sources What sources are in the Northern Hemisphere ? How strong are they ? – are they detectable by Amateurs ? What spectrum do they have ? Are they discrete or spatially distributed ? Key parameters Source Flux Spectrum Angular Size

15. Weak Signal Detection of Virgo A Source Signal Strengths Look at typical source signal strength www.dmradas.co.uk Power Flux Density (W m -2 Hz -1) 10 -15 Broadcast signals 100  V/m 10 -17 1  V/m 10 -19 10 -21 10 -23 10 -25 1Jy=10 -26 W m -2 Hz -1 Assuming 6kHz bandwidth 10 10 3 10 5 10 7 10 9 10 11 Power Flux Density Jy (10 -26 W m -2 Hz -1) Communication receiver Sun storms Supernova remnants Radio galaxies Jupiter Pulsars

16. Weak Signal Detection of Virgo A Radio Sources – signal strengths In more detail www.dmradas.co.uk 1 10 10 2 10 3 10 4 10 5 10 6 10 7 10 8 10 9 Power Density Jy (10 -26 W m -2 Hz -1 ) Solar storms & plages Quiet sun Solar bursts Sun Taurus A Virgo A Pulsars Jupiter Cassiopeia A Cygnus A Orion Neb. These are ‘continuous’ sources – not dealing with radio transients

17. Weak Signal Detection of Virgo A Source Spectrum drives receiver frequency Each source has its own predominant radiation mechanism This determines the emission spectrum The source spectrum drives the telescope configuration eg Frequency of operation, Gain & Antenna size SUN : Thermal Source SNR : Synchrotron Source Galactic Hydrogen : Line Source quiet sun storms bursts 1cm 3cm 10cm 1m 3m 10m Wavelength 10 4 10 10 6 10 10 10 10 10 Power flux density (10 -26 W m -2 Hz -1 ) Hercules Virgo Cygnus Cassiopeia 1cm 10cm 1m 10m Wavelength 1 10 2 10 3 10 4 Power flux density (10 -26 W m -1 Hz -1 ) P x ( =wavelength, x=spectral index) 1420MHz 1421MHz H Line Spectrum

18. Weak Signal Detection of Virgo A Radiation Mechanisms Source Spectra : Three mechanisms – Three spectra www.dmradas.co.uk 1cm 10cm 1m 10m Wavelength 1 10 10 2 10 3 Radiated Power P x y z P=  kT/ 2 K = Boltzmann's const T= temperature    Semi-transparentopaque Thermal Spectrum Ion moving electron electromagnetic emission Synchrotron radiation (non thermal) Ionised gas (thermal) 1cm 10cm 1m 10m Wavelength 1 10 10 2 10 3 Relative power flux Synchrotron Spectrum magnetic field charged particle v r circular polarization linear polarization 1cm 10cm 1m 10m Wavelength 1 10 10 2 Relative power flux Hydrogen 21cm OH 18cm Methanol 4cm Line spectrum electron reverses spin & radiates a photon proton electron

19. Weak Signal Detection of Virgo A What can amateurs measure? – some examples Use microwave receiver for thermal sources Few interesting objects to detect Small objects < 0.5 0 diameter - eg SUN & Moon Measurements will be HPBW limited (~2 0 ) www.dmradas.co.uk 11GHz image of SUN ~2 0 Using L band for H line Measuring Doppler shifts & mapping galaxy Reasonable spatial resolution achievable Galactic H line Use L Band for Synchrotron emission Galactic emission can be mapped Reasonable spatial resolution achievable SNRs are discrete sources – smeared out by large HPBW This makes SNRs difficult to detect Galactic Synchrotron Try using UHF for Synchrotron emissions Higher signal but worse antenna gain – no improvement HPBW rather poor – limited spatial resolution Extra galactic interferometry

20. Weak Signal Detection of Virgo A 11 GHz Radiometer image School Radiometer project – show some principles of Radio Astronomy Satellites SUN was behind building here Unknown signal sources Can see radio emission from chimneys South20 0 East of SouthWestNorth West Azimuth Elevation 0 to 45 0 0 45 0 www.dmradas.co.uk

21. Weak Signal Detection of Virgo A Galactic H line Declination (degrees) 22 21 20 19 18 17 Right Ascension (hrs) Galactic Centre Cygnus Arm -10 0 10 20 30 40 50 60 Hydrogen Line Velocity Distribution As amateurs we can measure the intensity, spatial distribution and velocities of Hydrogen in the galactic plane. Galactic Longitude Velocity Frequency Hydrogen Velocity v Galactic Longitude Plane Galactic Longitude

22. Weak Signal Detection of Virgo A 0 20 40 60 80 100 120 140 160 180 Azimuth Bearing (degrees) Elevation (degrees) 0 65 60 55 50 45 40 35 30 25 20 15 10 5 1420.4MHz Image of Milky Way 13.08 GMT 28/11/2013 NorthSouth East HPBW Galactic Centre Cygnus arm Ground Noise

23. Weak Signal Detection of Virgo A What is difficult for amateurs? Difficult to detect discrete sources at UHF / VHF We are limited by using small antennas Only moderate gain Relatively wide beamwidths Discrete sources << beamwidth Leads to source intensity loss & spatial smearing How significant is the effect for discrete sources ?

24. Weak Signal Detection of Virgo A Wide beams & point sources Evaluating loss of signal and point source smearing Antenna temperature relationship with source flux density T A = ‘Antenna Temperature’, S = Source flux A e = Effective Area, k = 1.38x10 -23 J K -1  A = Antenna beam solid angle, P n = polar response MB T B = source brightness Temp,  S = source solid angle (1 0 K=1.38 x 10 −23 W Hz −1 ) http://www.cv.nrao.edu/course/astr534/AntennaTheory.html

25. Weak Signal Detection of Virgo A Two examples For a hot source like the SUN, TB~10 4 K Angular diameter = 0.5 0 With a 5 0 HPBW antenna beam Source will only add 100K to the antenna temperature. www.dmradas.co.uk Using an antenna main beam HPBW = 8 0 Angular diameter = 5 arc min, T B = 3792 0 K Background galactic plane Temp = 86 0 K 8 0 beam Cass A Galactic plane Example: Cass A Example: SUN

26. Weak Signal Detection of Virgo A Cass A example For Cass A set in the galactic plane background Contribution from Cass A Temp = 0.411 0 K Background GP temp = 86 0 K So Cass A is hardly detectable against 86 0 K background with a ‘Total Power’ system Detection of ‘point’ sources requires very narrow beams www.dmradas.co.uk 5 arc min Cass A

27. Weak Signal Detection of Virgo A Discrete Source is lost in background Must have a larger antenna with a narrower beam to detect SNRs or extra galactic objects when using a Total Power System Requires Antenna HPBW of < 1 0 at UHF (Synchrotron Sources) Better than 20m diameter required. www.dmradas.co.uk Without access to a large antenna the only practical way for amateurs to observe point sources is with Interferometry

28. Weak Signal Detection of Virgo A This table summarises the issues when restricted to small antennas www.dmradas.co.uk FrequencyPerformancePossible SourcesRemarks KU Band 11GHz High gain, narrow beams (<2 0 ) Few of interest ‘High performance’ system but little of interest to detect C Band 4 GHz Medium gain, reasonable beam As above No ‘available’ sources L Band 1.4 -1.6GHz Satisfactory gain, rather wide beam (5 0 -8 0 ) Galactic H Line Low spatial resolution but OK for Galactic Hydrogen work UHF 408MHz Low gain, poor beamwidth Many synchrotron SNRs, galaxies etc Many sources, but poor sensitivity and resolution VHF 150MHzNeed very large antenna Many SNRs and Pulsars Not really practical for amateurs (thermal only) H Line is best target for amateurs

29. Weak Signal Detection of Virgo A Hydrogen Line measurements So as amateurs with modest antennas we can do a good job of measuring H Line emission - as Galactic features fill the beam (T A = T B ) with only a little spatial smearing Hydrogen Emission distribution 8 0 HPBW

30. Weak Signal Detection of Virgo A Big Aspirations ? Where does this leave UK amateur radio astronomers? Each of us is working with small antennas >10m dia antenna too expensive for an individual Clubs or groups unlikely to have funds, commitment & discipline to collaborate on large scale project However – it has been done ! Dwingeloo telescope in Holland Stockert telescope in Germany Now in service for Amateur Radio Astronomers & EME What are the chances of a similar UK project ? What a challenge that would be …….. www.dmradas.co.uk Dwingeloo Stockert

31. Weak Signal Detection of Virgo A Possible amateur radio astronomy at Goonhilly (Cornwall) Two large dishes at Goonhilly will soon be used for professional Radio Astronomy – amateurs may be able to play a part ?? Goonhilly 1 (L band) Goonhilly 3 (C band)

32. Weak Signal Detection of Virgo A Getting Involved at Goonhilly Thank You www.dmradas.co.uk Would you like to consider participating in Amateur Radio Astronomy at Goonhilly ? Put your contact details in the book

33. Weak Signal Detection of Virgo A

34. Cass A example For Cass A set in the galactic plane background Discrete source lost in the background with an 8 0 beam Cass A Temp = 0.411 0 K Background GP temp = 86 0 K So Cass A is hardly detectable against 86 0 K background with a ‘Total Power’ system Detection of ‘point’ sources requires very narrow beams www.dmradas.co.uk Cass A Temp = 3792 x 0.0153 / 0.00000166 T CassA    S 5 arc min Cass A Look at a simple spreadsheet model of the situation

35. Weak Signal Detection of Virgo A Simple spread sheet model Use Excel to model point source in a wide beam www.dmradas.co.uk Create a beam profile Generate a ‘slightly noisy’ background level 8080 8080 Background Galactic Noise Add in Cass A ‘ point source’ 8080 8080 Cass A = 44x Background 5 arc min Sum the background noise power Sum the noise power + ‘point’ source Calculate % change with point source

36. Weak Signal Detection of Virgo A Discrete extra galactic objects - interferometry Observing extragalactic synchrotron objects at UHF with small antennas results in poor spatial resolution (HPBW ~18 0 - 3m A E ) Example: M87 / Virgo A galaxy Only ~ 100Jy at 408MHz Fortunately it is out of GP – less obscured Still difficult to determine as a point source with Total Power receiver www.dmradas.co.uk Synchrotron emission from Milky Way GP Virgo A expected 03:12hrs Total Power Interferometer Convolution

37. Weak Signal Detection of Virgo A H Line – Sky View So as amateurs we can do a good job of measuring H Line emission as Galactic features fill the beam (T A = T B ) & only a little smearing I produced H Line maps in celestial coordinates (2006) Wanted to know what Galaxy looked line in Az and El How we would see it – if we had Radio Eyes 0 20 40 60 80 100 120 140 160 180 Azimuth Bearing (degrees) Elevation (degrees) 0 65 60 55 50 45 40 35 30 25 20 15 10 5 1420.4MHz Image of Milky Way 13.08 GMT 28/11/2013 NorthSouth East