Methods of Registration of Weak Radio Signals

详细信息    查看全文

• 刊名：Lecture Notes in Computer Science
• 出版年：2017
• 出版时间：2017
• 年：2017
• 卷：10220
• 期：1
• 页码：47-63
• 参考文献：1.Malofeev, V.M.: Measurements of the pulse energy of weak pulsars at frequencies of 61 and 102 MHz. Astron. Lett. 19, 138–142 (1993)
  2.Malofeev, V.M., Malov, O.I.: Detection of Geminga as a radiopulsar. Nature 389, 697–699 (1997)CrossRef
  3.Chashei, I.V., et al.: Global structure of the turbulent solar wind during 24 solar activity maxima from IPS observations with the multibeam radio telescope BSA LPI at 111 MHz. Solar Phys. 290, 2577–2587 (2015)CrossRef
  4.Tyul’bashev, S.A.: A study of radio sources using interplanetary scintillations at 111 MHz. Core-dominated sources. Astron. Rep. 53, 19–29 (2009)CrossRef
  5.Turnbull, M.C., Tarter, J.C.: Target selection for SETI: 1. A catalog of nearby habitable stellar systems. Astrophys. J. Suppl. Ser. 145, 181–198 (2003)
  6.Turnbull, M.C., Tarter, J.C.: Target selection for SETI. II. Tycho-2 Dwarfs, old open clusters, and the nearest 100 stars. Astrophys. J. Suppl. Ser. 149, 423–436 (2003)CrossRef
  7.Siemion, A.P.V., et al.: A 1.1 to 1.9 GHz SETI survey of the Kepler field: I. A search for narrow-band emission from select targets. Astrophys. J. 767, 94–107 (2013)CrossRef
  8.Steele, B.: It’s the 25th anniversary of Earth’s first (and only) attempt to phone ET, Cornell News, 12 November 1999
  9.Ehman, J.B.: The Big Ear Wow!-Signal: What We Know and Don’t Know About It After 20 Years, Big Ear Radio Observatory (1997). www.​bigear.​org/​wow20th.​htm
  10.Shostak, S.: SETI detects possible signal at 11 GHz frequency from sun-like star (2016). phys.​org/​news/​2016-08-seti-ghz-frequency-sun-like-star.​html
  11.Klimenko, S.V., Nikitin, I.N., Malofeev, V.M.: StarWatch: radio astronomical monitoring in virtual environment. In: Proceedings of CyberWorlds 2015, Gotland, Sweden, pp. 361–364. IEEE (2015)
  12.Nikitin, I.N.: Statistical analysis of narrow-band signals at setilive.org (2015). arXiv:​org/​abs/​1502.​04887
  13.Klimenko, S.V., et al.: On signals with Doppler drift, fast Fourier transform and search for extraterrestrial intelligence. In: Proceedings of SCVRT 2013, Protvino, Russia, 26–28 November 2013
  14.Klimenko, S.V., Nikitin, I.N.: On statistical data accumulation, Radon transform and search for extraterrestrial intelligence. In: Proceedings of CPT 2014, Cyprus, Larnaca, 11–18 May 2014
  15.Konich, K., et al.: Radio astronomical monitoring in virtual environment. Procedia Comput. Sci. 66, 592–601 (2015)CrossRef
  16.Osgood, D., Ekers, R.D.: SETI 2020: A Roadmap for the Search for Extraterrestrial Intelligence. SETI Press, Mountain View (2002)
  17.Siemion, A.P.V., et al.: Searching for extraterrestrial intelligence with the square kilometre array. In: Proceedings of Science, AASKA14, p. 116 (2015). arxiv.​org/​abs/​1412.​4867
  18.Kardashev, N.S., et al.: Review of scientific topics for the Millimetron space observatory. Physics-Uspekhi 57, 1199–1229 (2014)CrossRef
  19.Welch, J., et al.: The Allen Telescope Array: the first widefield, panchromatic, snapshot radio camera for radio astronomy and SETI. Proc. IEEE 97(8), 1438–1447 (2009). arxiv.​org/​abs/​0904.​0762
  20.Harp, G.R.: Using multiple beams to distinguish radio frequency interference from SETI signals. Radio Sci. 40, RS5S10 (2005). arxiv.​org/​abs/​1309.​3826
  21.Harp, G.R., Wright, M.C.H.: Simulations of Primary Beam Sidelobe Confusion with the ATA Primary Beam, MEMO 74, SETI Institute, March 2007
  22.Cullers, D.K., Deans, S.R. (eds.) SETI Algorithms, Chap. 4, The DADD (Doubling Accumulation Drift Detection) algorithm, SETI Institute (1989). ftp://​ftp.​seti.​org/​gharp/​SetiAlgorithms-CullersDeans.​pdf
  23.Chandra, S.: Finite Transform Library (FTL), Version 1.50 (2013). finitetransform.​sourceforge.​net
  24.Staelin, D.H.: Fast folding algorithm for detection of periodic pulse trains. Proc. IEEE 57, 724 (1969)CrossRef
  25.Harp, G.R., et al.: A new class of SETI beacons that contain information. In: Communication with Extraterrestrial Intelligence. State University of New York Press (2011). arxiv.​org/​abs/​1211.​6470
  26.Tutorials, S.: Signal Processing and SETI setiquest.​org/​about/​tutorials , The Doppler Effect setilive.​org/​about , How would we know that the signal is from ET? www.​seti.​org/​faq , SETI Institute 2011–2015
  27.Hinkenjann, A., et al.: Large, ultra high resolution displays - LUHRDs. IEEE Virtual Reality (IEEE VR), March 2015. Tutorial. sites.​google.​com/​site/​luhrdtutorial
  28.Duda, R.O., Hart, P.E.: Use of the hough transformation to detect lines and curves in pictures. Comm. ACM 15, 11–15 (1972)CrossRef MATH
  29.Marsaglia, G.: The Marsaglia Random Number CDROM Including the Diehard Battery of Tests of Randomness. Florida State University (1995). stat.​fsu.​edu/​pub/​diehard
  30.Brown, R.G., Eddelbuettel, D., Bauer, D.: Dieharder: A Random Number Test Suite Version 3.31.1 (2004). www.​phy.​duke.​edu/​~rgb/​General/​dieharder.​php
  31.Klimenko, S.V., et al.: StarWatch 2.0: RFI filter for SETI signals. In: Proceedings of CyberWorlds 2016, Chongqing, China (accepted)
  32.Rampadarath, H., et al.: The first very long baseline interferometric SETI experiment. Astron. J. 144, 38 (2012)CrossRef
  33.ALMA Links with Other Observatories to Create Earth-size Telescope, ALMA Observatory (2015). www.​almaobservatory.​org
  
• 作者单位：Stanislav Klimenko (15)
  Andrey Klimenko (16)
  Kira Konich (17)
  Igor Nikitin (18)
  Lialia Nikitina (18)
  Valery Malofeev (19)
  Sergey Tyul’bashev (19)
  
  15. Institute of Computing for Physics and Technology, Moscow Institute for Physics and Technology (State University), Protvino, Russia
  16. Cyprus Space Exploration Organisation, Nicosia, Cyprus
  17. Bauhaus University, Weimar, Germany
  18. Fraunhofer Institute for Algorithms and Scientific Computing, Sankt Augustin, Germany
  19. Pushchino Radio Astronomy Observatory, Lebedev Physical Institute, Pushchino, Russia
  
• 丛书名：Transactions on Computational Science XXIX
• ISBN：978-3-662-54563-8
• 卷排序：10220

文摘

In this paper we will consider a problem of registration of radio signals from distant sources, natural (pulsars) or artificial (SETI signals). These signals possess a number of common properties, i.e. they are weak, almost indistinguishable from the background noise, are strongly localized on celestial sphere, have spectral characteristics smeared by dispersion on interstellar medium and Doppler drift, suffer from near-Earth electromagnetic interference. In this paper we will overview existing methods for registration of such signals and discuss some alternatives. We implement selected methods as data filters connected to data processing workflow, with 3D Virtual Environment as a frontend, integrate the methods into a system for radio astronomical monitoring StarWatch and apply them for detection of pulsar signals from BSA telescope at Pushchino Radio Astronomy Observatory and narrow band signals in SETI database (setilive.org).