Status hardware, software and what next? Harry Keizer 1, Simon Bijlsma 1, Daniela de Paulis 1,3,Marc Wolf 1,2.

Transcription

1 Status hardware, software and what next? Harry Keizer 1, Simon Bijlsma 1, Daniela de Paulis 1,3,Marc Wolf 1,2 1 Stichting CAMRAS, 2 University of Central Lancashire, 3 University of Plymouth 5 June 2017

2 Agenda CAMRAS Foundation achievements and next steps DT characteristics Generic DT parameters signal processing Observable transients with DT Observation Strategy DT improvement suggestions

3 CAMRAS Foundation Dwingeloo Telescope Industrial Monument

4 CAMRAS Foundation I Dwingeloo Telescope Industrial Monument

5 CAMRAS Foundation I CAMRAS volunteers

6 CAMRAS Foundation I CAMRAS volunteers

7 CAMRAS Foundation I CAMRAS outreach

8 CAMRAS Foundation I CAMRAS outreach

9 achievements and next steps (SaH) software into DT pipeline Initial SaH discussion with Berkeley SETI group (Eric Korpela, Jeff Cobb (Berkeley)) Discussion on KLT (Nicolò Antonietti (Torino)) SaH build on VM by Matthieu Jeantot (CAMRAS) Porting SaH build on CAMRAS infrastructure Created new FPGA firmware for SDR/SETI purpose Converting of DT backend format (1 channel) into DR2 format (16 channel) Testing pipeline using fake tool and GNU-radio generated test files

10 achievements and next steps (SaH) software into DT pipeline Initial SaH discussion with Berkeley SETI group (Eric Korpela, Jeff Cobb (Berkeley)) Discussion on KLT (Nicolò Antonietti (Torino)) SaH build on VM by Matthieu Jeantot (CAMRAS) Porting SaH build on CAMRAS infrastructure Created new FPGA firmware for SDR/SETI purpose Converting of DT backend format (1 channel) into DR2 format (16 channel) Testing pipeline using fake tool and GNU-radio generated test files Next steps End to end testing of pipeline Define test strategy Define processing strategy (Work Unit distribution) (Korpela et al. 2001) Implement observation and processing strategy

11 achievements and next steps (SaH) software into DT pipeline Initial SaH discussion with Berkeley SETI group (Eric Korpela, Jeff Cobb (Berkeley)) Discussion on KLT (Nicolò Antonietti (Torino)) SaH build on VM by Matthieu Jeantot (CAMRAS) Porting SaH build on CAMRAS infrastructure Created new FPGA firmware for SDR/SETI purpose Converting of DT backend format (1 channel) into DR2 format (16 channel) Testing pipeline using fake tool and GNU-radio generated test files Next steps End to end testing of pipeline Define test strategy Define processing strategy (Work Unit distribution) (Korpela et al. 2001) Implement observation and processing strategy Future Add astropulse (Siemion et al. 2010) Develop KLT add on (requires high computational power)

12 DT characteristics DT pipeline

13 DT characteristics DT pipeline Backend modes Pulsar mode: 256 spectral bins, 2136 spectra/second Line mode: 2048 spectral bins, 267 spectra/second Raw mode: unprocessed 70MS/s 10bit, 700Mb/s output SDR mode, 5MHz: 5MHz of bandwidth centered around 21.4 MHz, 16bit IQ, GnuRadio compatible

14 DT characteristics DT pipeline Backend modes Pulsar mode: 256 spectral bins, 2136 spectra/second Line mode: 2048 spectral bins, 267 spectra/second Raw mode: unprocessed 70MS/s 10bit, 700Mb/s output SDR mode, 5MHz: 5MHz of bandwidth centered around 21.4 MHz, 16bit IQ, GnuRadio compatible Signal processing

15 DT characteristics DT pipeline Backend modes Pulsar mode: 256 spectral bins, 2136 spectra/second Line mode: 2048 spectral bins, 267 spectra/second Raw mode: unprocessed 70MS/s 10bit, 700Mb/s output SDR mode, 5MHz: 5MHz of bandwidth centered around 21.4 MHz, 16bit IQ, GnuRadio compatible Signal processing Splitter Software

16 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy

17 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy Gain variation 21 versus 154 points

18 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy Gain variation 21 versus 154 points Spacial resolution GHz

19 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy Gain variation 21 versus 154 points Spacial resolution GHz Frequency resolution (10 khz) (CAS A absorption line)

20 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy Gain variation 21 versus 154 points Spacial resolution GHz Frequency resolution (10 khz) (CAS A absorption line) Time resolution (2 ms) [Credit CAMRAS]

21 Generic DT parameters System Equivalent Flux Density (SEFD) 540 mjy Gain variation 21 versus 154 points Spacial resolution GHz Frequency resolution (10 khz) (CAS A absorption line) Time resolution (2 ms) [Credit CAMRAS] Radio Frequency Interference (RFI) [Credit CAMRAS]

22 signal processing broadband transit signal

23 signal processing broadband transit signal narrowband transit signal

24 signal processing broadband transit signal narrowband transit signal narrowband pulsed signal

25 signal processing broadband transit signal narrowband transit signal narrowband pulsed signal chirped signal

26 signal processing broadband transit signal narrowband transit signal narrowband pulsed signal chirped signal chirped pulsed signal

27 Observable transients with DT Pulsar B , DM delay 11 ms, temporal resolution 1ms Strong repeating FRBs can be observed Follow-up observations radio sources, e.g. FRBs EMP small Black Holes as discussed by Siemion et al. (2010) SETI signals

28 Observation Strategy Transient Tracking Follow-up observations SETI objects

29 DT improvement suggestions Frontend Second Antenna for polarization and sensitivity improvement Fibre connections to backend to reduce noise Define frequency windows in relation to RFI for DT Stabilization of gain variation Add reference noise source for calibration Backend and signal processing Increase bandwidth 2.5MHz Backend mode Automated calibration Software add-ons like Astropulse and KLT Open hardware, e.g. CASPER or CAMRAS FPGA firmware

30 Conclusion Nearing the completion of the manual pipeline Peer review of pipeline required to check sanity of pipeline group to define Citizen Scientist structure Define observation strategy for in cooperation with institutions (BOINC, Astropulse, KLT) CAMRAS will work on next generation Frontend and Backend Help appreciated to speed up the implementation process of SaH

31 Thank you! team from the Netherlands

32 Baars, J. W. M. et al. (1977). The absolute spectrum of CAS A - an accurate flux density scale and a set of secondary calibrators. In: aap 61, pp Korpela, Eric et al. (2001). SETI@home-massively distributed computing for SETI. In: Computing in Science and Engineering 3.1, pp Maccone, C. (2007). Innovative SETI by the KLT. In: Bursts, Pulses and Flickering: Wide-Field Monitoring of the Dynamic Radio Sky, p. 34. Siemion, A. et al. (2010). New SETI sky surveys for radio pulses. In: Acta Astronautica 67, pp