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2. ARGOS Double - Heterodyne - FFT - Radio - Spectrometer RAPP ETH Zürich Minikolloquium June 11th 2002 Michael Arnold / Christian Monstein Astronomical Receiver Gathers Outer Space (Tyler Brulée)

3. Directory Specifications (required / measured) Instrument comparison Open day application 15.06.2002 Usage sites Focal plane unit Double heterodyne receiver Frequency diagram Backend hardware Backend software Backend realtime aspects Backend dataflow First results Team members Development time, costs Summary ARGOS related URL`s

4. Specifications ParameterRequiredMeasured Frequency range1415 ± 25 MHz 1415 ± 125 MHz Bandwidth> 50 MHz250 MHz Polarization1 linearvertical Spectra/sec>= 10010...15 Integration (TD, FD)‚must‘‚in progress‘ Channels or bins> 32up to 50`000 tested Offseterror vs temp.nil< 0.03 dB/K Offseterror vs ac-powernil< 10 µdB/Vac Gainerror vs temp.nil< 0.03 dB/K Gainerror vs ac-powernil< 10 µdB/Vac Frequency errornil< 160 ppm / < 5ppm Timing error< 50 msec/dayTBD Power consumption nil191W (RX only) Sensitivity< 5 sfu800/300 Jansky rms System temp.< 2 dB (175K)530/250 Kelvin Dynamic broadbandnil> 40 dB Dynamic FFT> 24 dB~ 50 dB Liftime> 5 yearTBD

5. Instrument comparison ParameterARGOSPHOENIX-2CALLISTO ReceivertypeFFTFrequency agileFrequency agile Frequency range1290-1570 MHz100-4000 MHz47-862 MHz Obs.-bandwidth250 MHz3900 MHz815 MHz Resolution (FD)  250 MHz {i}1, 3, 10 MHz110 KHz (65 KHz) Resolution (TD)> 66 msec500 µs...1sec {i}2 msec...10 sec {i} Polarizationlinear (vertical)L, R, I, Vlinear Sampletime/pixel2 nsec0.5 msec2 msec (TBD) Channels1...  {ii}1...20001...12500 System temp.250/530 K {iii}TBD {iii}TBD {iii} RMS noise300/800 JanskyTBD {iii}TBD {iii} Dynamic range~ 50 dB> 40 dB> 40 dB {i} depending on number of channels {ii} not yet checked; tested until 50'000 {iii} with/without calibration unit

6. Open day application 15.06.2002 Receiver 1415 MHz±125 MHz Impedance matching 75/50  DC-decoupling Possible sources: Solar radio noise between 11,70 GHz and 12,75 GHz Satellite signals (downlinks) Methanol CH 3 OH @ 12,178 GHz ± doppler shift Cherenkow radiation from moon due to impact of TeV cosmic particles IF=1578 MHz SAT-receiver + power supply LNC

7. Usage sites 5m antenna Zürich 1 GHz-2.6 GHz (system tests only) 5m antenna Bleien 300 MHz - 3 GHz + 80 cm-SAT 10 GHz - 12 GHz 7m antenna Bleien 100 MHz - 4 GHz Option: Gorner Grat with 3m Cassegrain 210 - 820 GHz

8. Focal plane unit PIN- switch #1 PIN- switch #2 Preamplifier, 1-4 GHz NF 0.9dB, G +35 dB -3 dB Noise Source +35 dB ENR Input from antenna feed Ta/Cali +28V To/Texc +15V/0,3A Output to receiver Termination 50  @ To=300K  J1.0 J2.0J1.1=PD3 J2.2=PD2 J1.2=PD4 J2.1=PD1 +5V/-12V

9. Double heterodyne receiver XX +26dB+15dB+41dB local oscillator-1 10,000GHz +13dBm local oscillator-2 8,710GHz +13dBm Power- divider Reference clock 10MHz +6dBm ± 3dBm Power- divider Logarithmic detector 25mV/dB analog-digital- converter 8bit 500Ms/sec PC -1.7dB 100µA Video Lowpassfilter DC-250MHz 1. mixer2. mixer LSB-bandpassfilter 8,585GHz ± 125MHz -3dB Radio - Telescope 1290 - 1540 MHz isolator equalizer- amplifier 1. IF- amplifier 2. IF- amplifier IF2=IF1-Flo IF1=Fsy-Frf Frf=Fsy-IF2-Flo IF2=Fsy-Flo-Frf Coaxial cable ~60m -9dB...-35dB

10. Frequency diagram F1h=8,710GHz F1z=8,585GHz F1l=8,460GHz Fh=1,540 GHz Fl=1,290 GHz Power Frequency 1. mixer stage F2h = 250 MHz F2l = 0.0 GHz = dc 2. Localoscillator LO2 = 8,710 GHz Power Frequency 2. mixer stage Selection with lowpassfilter F1 = LO1 ± Frf = 8,585 GHz ± 125 MHz F2 = F1 - LO2 = 125 MHz ± 125 MHz Upper sideband USB will not be used Selection of lower sideband LSB by bandpassfilter Frf =1,415 GHz 1. Localoscillator LO1 = 10,000 GHz

11. PC Hardware: Pentium III 800 MHz (Win98) 384 MByte RAM ~40 GByte HD Acqiris Digitizer 500 Msamples/sec 2 Msamples on-board memory 8bit Resolution 50  input impedance LabView Driver Backend hardware

12. Backend software

13. 50`000 lines/spectrum (  =5KHz) Spectral integration down to 500 lines/spectrum Sampletime 2ns (500MHz) 100  s per data array (one line of spectrum) Fastest Win98 timeslice 1ms  needs fast integration Bottle neck disc I/O and integration process in time Backend realtime aspects

14. Fileserver pisces.ethz.ch hercules.ethz.ch Webserver ARGOS Receiver /ftp/pub/hedc/fs/data1/rag/observations/argos /argos/ plutos.ethz.ch Argos Controller D:/data/*.raw Overview ftp via php ftp.php Backend dataflow

15. First results Simulation of RADAR-pulses (top) and a small bandwidth, drifting signal to check cross-modulation sensitivity of the preamplifier in the focal plane unit. Here, rf-power is to high thus ‚ghosts‘ apear parallel to signal. TestbandFrequencyrangemax Power ERMES-pager168-172 MHz< -23 dBm Telepager400-430 MHz< - 36 dBm Citizenband900-1350 MHz< - 24 dBm RADAR1300-1350 MHz< -64 dBm NATEL D/GSM1710-1855 MHz< -23 dBm max. power is 5µW (16mV @ 50  )

16. Sun-transit seen with ARGOS & PHOENIX-2 FFT-spectrometer BW=spacing=500KHz Frequency agile spectrometer BW=10MHz, spacing=30MHz No background subtraction applied... ARGOS PHOENIX-2

17. Team members Defending NF-budget & requirementsArnold Benz Mechanical design & manufacturing Frieder Aebersold Software design, integration & testMichael Arnold PostprocessingPeter Messmer Manufacturing of focal plane unitAndreas James Manufacturing ARGOS-receiverRoland Moser Manufacturing FOPA-controllerRoland Moser Conceptual & hardware designChristian Monstein

18. Development time, costs Hardware design+manufacturing1.4 year with 10% = 280h Software design1.3 year with 10% = 260h System integration0.2 year with 20% = 80h System tests0.5 year with 25% = 250h Total 870h Material costsSFr. 67`000

19. Summary A cheap instrument compared to PHOENIX-2, AOS Portable (more or less) Flexibel in terms of bandwidth resp. number of channels Observation of molecule lines possible Experience with LabView in real time environment Curious about scientific results Observation of solar radio noise in Ku-band on June 15th

20. ARGOS related URL`s Status ARGOShttp://pisces.ethz.ch/argos/index.php More Infoshttp://www.astro.phys.ethz.ch/rapp/ ETH Astronomical Institute Christian Monstein Scheuchzerstrasse 7 CH-8092 Zürich monstein@astro.phys.ethz.ch