Observational SETI Programs (Through the Decades)

Below is a master list for observable SETI programs through September 2017. This was largely inspired by the work of Jill Tarter in her 2001 review. A brief description of the values for each entry:

  • Time
  • Observers
  • Site
  • Instrument size (assumed to be the diameter of a telescope)
  • Search Frequency (in Megahertz, for radio searches)
  • Search Wavelength (in nanometers, for optical searches)
  • Frequency Resolution (in hertz, for radio searches)
  • Other Resolution (for non-radio searches, can be temporal, angular, spectral resolution, etc)
  • Objects observed (a description of what was observed)
  • Flux limits (in watts per square meter)
  • Total hours (hours observed)
  • References (Citation information)
  • Link (Link to the published paper)
  • Comments (Usually a summary of the program)

A link to download the Google sheets version is here.

The units in the written cells take precedence over those in the row headers. The cells may have addition comments as well.

Search by decade:

1960s 1970s 1980s 1990s 2000s 2010s
Date 1960
Observer(s) DRAKE “OZMA”
Site NRAO
Instrument Size (m) 26
Search Frequency (MHz) 1420 – 1420.4
Search Wavelength (nm)
Frequency Resolution (Hz) 100
Other Resolution
Objects (Hz) 2 STARS
Flux Limit (W m-2) 1 x 10-22
Total Hours 200
Reference DRAKE, F.D., Sky & Telescope, 39, p. 140 (1960).
Link
Comments Single channel receiver.
Date 1964 – 1965
Observer(s) KARDASHEV & SHOLOMITSKII
Site CRIMEA DEEP SPACE STATION
Instrument Size (m) 16 (8 ANTENNAS)
Search Frequency (MHz) 923
Search Wavelength (nm)
Frequency Resolution (Hz) 10 x 106
Other Resolution
Objects (Hz) 2 QUASARS
Flux Limit (W m-2) 2 x 10-20
Total Hours 80
Reference KARDASHEV, N.S., Soviet A.J., 217 (1964). SHOLOMITSKII, G.B., IAU Information Bulletin on Variable Stars (February 27, 1965). New York Times editorial, p. 36 (April 13, 1965).

GINDILIS, L.M., DUBINSKIJ, B.A. and RUDNITSKIJ, G.M., “SETI Investigations in the USSR,” paper #IAA-88-544, presented at IAF Congress, Bangalore, India (1988).
Link
Comments Reported detection of CTA102 as possible Type III civilization.
Date 1966
Observer(s) KELLERMAN
Site CSIRO
Instrument Size (m) 64
Search Frequency (MHz) MANY BETWEEN 350 & 5000
Search Wavelength (nm)
Frequency Resolution (Hz) FULL BANDWIDTH FOR EACH FEED
Other Resolution
Objects (Hz) 1 GALAXY (1934-63)
Flux Limit (W m-2) 1 X 10-18
Total Hours
Reference KELLERMAN, K.I., Australian Journal of Physics, 19, p. 195 (1966).
Link
Comments No “notch” of ETI origin was detected in galaxy 1934-63.
Date 1968 – 1982
Observer(s) TROITSKII
Site GORKY
Instrument Size (m) DIPOLE
Search Frequency (MHz)
Search Wavelength (nm) 30 x 107, 16 x 107, 8 x 107, 3 x 107
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2)
Total Hours CONTINUING
Reference Interview in Leningradskaya Pravda (Nov. 2, 1982).
Link
Comments Search over all sky visible by single dipole.
Date 1968 – 1969
Observer(s) TROITSKII, STARODUBTSEV, GERSHTEJIN & RAKHLIN
Site ZIMENKIE, USSR
Instrument Size (m) 5
Search Frequency (MHz) 926 – 928, 1421 – 1423
Search Wavelength (nm)
Frequency Resolution (Hz) 13
Other Resolution
Objects (Hz) 11 STARS + M31
Flux Limit (W m-2) 2 x 10-21
Total Hours 12
Reference TROITSKII, V.S., STARODUBTSEV, A.M., GERSHTEIN, L.I., and RAKHLIN, V.L., Soviet AJ, 15, p. 508 (1971).
Link
Comments 20 filters of width 100 KHz divided into 25 channels with F = 13 Hz spaced 4 KHz apart and stepped in frequency.
Date 1969 – 1983
Observer(s) TROITSKII, BONDAR, & STARODUBTSEV
Site GORKII, CRIMEA, MURMANSK AND PRIMORSKIJ REGIONS
Instrument Size (m) DIPOLES
Search Frequency (MHz) 1863, 927, 600
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) ALL SKY SEARCH FOR SPORADIC PULSES
Flux Limit (W m-2) 10-22 W/m2/Hz
Total Hours 1200 PER YEAR (ON AVERAGE)
Reference TROITSKII, V.S., BONDAR, L.N., and STRODUBTSEV, A.M., Soviet Phys.-Usp., 17, p. 607 (1975).
Link
Comments Network of isotropic detectors: cross correlation from 2 or 4 sites over 8000 km.
Date 1970 – 1972
Observer(s) SLYSH
Site NANÇAY
Instrument Size (m) 40 x 240
Search Frequency (MHz) 1667, 1665
Search Wavelength (nm)
Frequency Resolution (Hz) 4000
Other Resolution
Objects (Hz) 10 NEAREST STARS
Flux Limit (W m-2)
Total Hours
Reference
Link
Comments Looked for signals at OH frequency between observations of OH Masers.
Date 1970 – 1972
Observer(s) SLYSH, PASHCHENKO, RUDNITSKII, & LEKHT
Site NANÇAY
Instrument Size (m) 40 x 240
Search Frequency (MHz) 1667, 1665
Search Wavelength (nm)
Frequency Resolution (Hz) 4000
Other Resolution
Objects (Hz) 5 OH MASERS
Flux Limit (W m-2)
Total Hours 2
Reference Pashchenko, et al., “Measurement of One-Dimensional Function of Distribution for Signals from Galactic Sources,” Astronomicheskii Tsirkulyar, No. 626, pp. 1-3 (1971).
Pashchenko, et al., “Investigation of the Density of Probability for Interstellar Hydroxyl Radio Lines,” Uchebynkh Zavedenii-Radio Fizika, 16, pp. 1344-1349 (1973).
Lekht, et al., “Investigations of Statistical Properties of OH Maser Sources,” Pis’ma V Astronomicheskii Zhurnal, 1, pp. 29-32 (1975).
Link
Comments Searched for deviation from Gaussian Emission statistics in 5 OH Maser sources that might indicate transmissions from another civilization.
Date 1971 – 1972
Observer(s) VERSCHUUR “OZPA”
Site NRAO
Instrument Size (m) 91, 43
Search Frequency (MHz) 1419.8 – 1421, 1410 – 1430
Search Wavelength (nm)
Frequency Resolution (Hz) 490, 6900
Other Resolution
Objects (Hz) 9 STARS
Flux Limit (W m-2) 5 x 10-24, 2 x 10-23
Total Hours 13
Reference VERSCHUUR, G.L., Icarus, 19, p. 329 (1973).
Link
Comments 384 channel correlator online.
Date 1972
Observer(s) KARDASHEV, POPOV, SOGLASNOV ET AL.
Site CRIMEA, RT-22
Instrument Size (m) 22
Search Frequency (MHz) 8570
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) GALACTIC CENTER
Flux Limit (W m-2)
Total Hours
Reference GINDILIS, L.M., DUBINSKIJ, B.A. and RUDNITSKIJ, G.M., “SETI Investigations in the USSR,” paper #IAA-88-544, presented at IAF Congress, Bangalore, India (1988).
Link
Comments Looked for statistical anomolies in continuum emission from galactic center.
Date 1972 – 1974
Observer(s) KARDASHEV, GINDILIS, POPOV, SOGLASNOV, SPANGENBERG, STEINBERG ET AL.
Site CAUCASUS, PAMIR, KAMCHATKA, MARS 7 SPACECRAFT
Instrument Size (m) 38, 60
Search Frequency (MHz) 371, 408, 458, 535
Search Wavelength (nm)
Frequency Resolution (Hz) 5 x 106
Other Resolution
Objects (Hz) OMNI-DIRECTIONAL
Flux Limit (W m-2) 2 x 10-16, – 7 x 10-15
Total Hours 150
Reference GINDILIS, L.M., DUBINSKIJ, B.A. and RUDNITSKIJ, G.M., “SETI Investigations in the USSR,” paper #IAA-88-544, presented at IAF Congress, Bangalore, India (1988).
Link
Comments “Eavesdropping” search for pulses. Synchronous dispersion reception.
Date 1972 – 1976
Observer(s) BRIDLE & FELDMAN “QUI APPELLE?”
Site ARO
Instrument Size (m) 46
Search Frequency (MHz) 22230.08 – 22240.08
Search Wavelength (nm)
Frequency Resolution (Hz) 3 x 104
Other Resolution
Objects (Hz) 70 STARS
Flux Limit (W m-2) 10-22
Total Hours 140
Reference
Link
Comments 70 solar-type stars within 45 light years have been observed to date.
Date 1972 – 1976
Observer(s) PALMER & ZUCKERMAN “OZMA II”
Site NRAO
Instrument Size (m) 91
Search Frequency (MHz) 1413 – 1425, 1420.1 – 1420.7
Search Wavelength (nm)
Frequency Resolution (Hz) 6.4 x 104, 4000
Other Resolution
Objects (Hz) 674 STARS
Flux Limit (W m-2) 10-23
Total Hours 500
Reference PALMER, P. and ZUCKERMAN, B., The NRAO Observer, 13, No.6, p. 26 (1972). SHEAFFER, R., Spaceflight, 19, No.9, p. 307 (1977).
Link
Comments 384 channel correlator online.
Date 1973 – 1974
Observer(s) SHVARTSMAN ET AL. “MANIA”
Site SPECIAL ASTROPHYSICAL OBSERVATORY
Instrument Size (m) 0.6
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution D = 10 -6 Å
Objects (Hz) 21 PECULIAR OBJECTS
Flux Limit (W m-2)
Total Hours
Reference SHVARTSMAN, V.F., Communications of the Special Astrophysical Obser., 19, p. 39 (1977).
Link
Comments Optical search for short pulses of length 3 x 10-7 to 300 seconds, & narrow laser lines. Prototype for later system on 6m telescope.
Date 1973 – 1986
Observer(s) DIXON, EHMAN, RAUB & KRAUS
Site OSURO
Instrument Size (m) 53
Search Frequency (MHz) 1420.15 – 1420.65
Search Wavelength (nm)
Frequency Resolution (Hz) -328443
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2) 1.5 x 10-21
Total Hours 100000
Reference DIXON, R.S. and COLE, D.M., Icarus, 30, p. 267 (1977). KRAUS, J.D., “We Wait and Wonder,” Cosmic Search, 1, No. 3, p. 32 (1979).
Link
Comments Receiver is tuned to hydrogen rest frequency relative to Galactic Center (as a function of direction).
Date 1973 – 1998
Observer(s) Brown, ; Klein, ; Dixon, R.; Ehman, ; Raub, ; Kraus, ; Childers, Cole, D. M.; et. al
Site OSURO
Instrument Size (m) 53
Search Frequency (MHz) 1421.75 – 1424.25
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6, 100, 10
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2) 1.5 x 10-21
Total Hours 5
Reference (1.) “The Ohio Sky Surveys,” Big Ear Radio Observatory, (2005). (2.) Dixon, R. S.; Cole, D. M.; et. al “A modest all-sky search for narrowband radio radiation near the 21-cm hydrogen line” American Association for the Advancement of Science, Symposium on the Search for Extraterrestrial Intelligence, Boston, Mass., Feb. 18-24, 1976. Icarus, vol. 30, Feb. 1977, p. 267-273, 02/1977.
Link ***http://www.setileague.org/articles/bigear.htm#to***
***http://adsabs.harvard.edu/abs/1977Icar…30..267***
Comments Using SERENDIP processor. Have searched declinations +8 to -36. By 1989 it had searched declinations +62 to -22 and was continuing to -36. The receiver was tuned in to hydrogen’s rest frequency relative to the Galactic Center (as a function of direction). Program ended when OSU sold observatory site to golf course developer. It was the longest running sky-survey with improving capabilities over time. This survey of the entire sky between the telescope declination limits of +63 ° and -36 ° is continuous in direction, making no assumptions as to where an extraterrestrial transmitter might be located in space. Out to a distance of 1000 light years, there are an average of three F-, G-, and K-type stars in the beam of the telescope at all times. The telescope is a meridian transit instrument, with half-power beamwidths at 21 cm of 8 arcmin in right ascension and 40 arcmin in declination. The system temperature is approximately 100° K, and an integration time of 10 sec was used. No confirmed narrowband extraterrestrial signals have been found.
Date 1974
Observer(s) WISHNIA
Site “COPERNICUS SATELLITE”
Instrument Size (m) 1
Search Frequency (MHz) 3 x 109
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 3 STARS
Flux Limit (W m-2)
Total Hours
Reference MORRISON, P., letter to directors of Radio Observatories dated 08/29/75 which appears in NASA SP-419, p. 204 (1975).
Link
Comments Search for UV laser lines.
Date 1975 – 1979
Observer(s) ISRAEL & DE RUITER
Site WRST
Instrument Size (m) 1500 MAX BASELINE
Search Frequency (MHz) 1415
Search Wavelength (nm)
Frequency Resolution (Hz) 4 x 106
Other Resolution
Objects (Hz) 50 STAR FIELDS
Flux Limit (W m-2) 2 x 10-23
Total Hours 400
Reference
Link
Comments Searches of “cleaned” maps prepared for the WRST background survey. Looked for positional coincidence between residual signals & AGK2 stars.
Date 1975 – 1976
Observer(s) SAGAN & DRAKE
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 1420, 1667, 2377 – 2383
Search Wavelength (nm)
Frequency Resolution (Hz) 1000
Other Resolution
Objects (Hz) FOUR GALAXIES
Flux Limit (W m-2) 3 x 10-25
Total Hours 100
Reference SAGAN, C. and DRAKE, F., Scientific American, 232, p. 80 (1974).
Link
Comments Search for type II civilizations in local group galaxies.
Date 1976
Observer(s) CLARK, BLACK, CUZZI & TARTER
Site NRAO
Instrument Size (m) 43
Search Frequency (MHz) 8522 – 8523
Search Wavelength (nm)
Frequency Resolution (Hz) 5
Other Resolution
Objects (Hz) 4 STARS
Flux Limit (W m-2) 2 x 10-24
Total Hours 7
Reference
Link
Comments VLBI high speed tape recorder combined with software direct Fourier transformation to produce extreme frequency resolution (non-real time).
Date 1976 – 1985
Observer(s) BOWYER ET AL. (U.C. BERKELEY) “SERENDIP”
Site HCRO
Instrument Size (m) 26
Search Frequency (MHz) 917 – 937, 1410 – 1430, 1602 – 1605, 1853 – 1873, 5000
Search Wavelength (nm)
Frequency Resolution (Hz) 1000
Other Resolution
Objects (Hz) ALL SKY SURVEY
Flux Limit (W m-2) 1.15 x 10-22
Total Hours
Reference BOWYER, S, ZEITLAND, G.M., TARTER, J., LAMPTON, M., and WELCH, W.J., “The Berkeley Parasitic SETI Program,” Icarus, 53 pp.147-155 (1983).
Link
Comments Automated survey parasitic to radio astronomical observations.
Date 1977
Observer(s) STULL & DRAKE
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 1664 – 1668
Search Wavelength (nm)
Frequency Resolution (Hz) 0.5
Other Resolution
Objects (Hz) 6 STARS
Flux Limit (W m-2) 10-26
Total Hours 10
Reference TARTER, J., CUZZI, J., BLACK, D., CLARK, T., STULL, M., and DRAKE, F., “SETI: High Sensitivity Search at NASA with High Speed Tape Recorders,” paper #79-A-43 presented at 30th IAF Congress in Munich, Germany (1979).
Link
Comments High speed tape combined with optical processor to produce extreme frequency resolution (non-real time).
Date 1977
Observer(s) TARTER, BLACK, CUZZI & CLARK
Site NRAO
Instrument Size (m) 91
Search Frequency (MHz) 1665 – 1667
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 200 STARS
Flux Limit (W m-2) 10-24
Total Hours 100
Reference TARTER, J., BLACK, D., CUZZI, J., and CLARK, T., Icarus, 42, p. 136 (1980).
Link
Comments VLBI high speed recorder combined with software direct Fourier transformation to produce extreme frequency resolution (non-real time).
Date 1977 – ON
Observer(s) WIELEBINSKI & SEIRADAKIS
Site MPIFR
Instrument Size (m) 100
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 20000000
Other Resolution
Objects (Hz) 3 STARS
Flux Limit (W m-2) 4 x 10-23
Total Hours 2
Reference
Link
Comments Candidate stars inserted into ongoing program which searches for pulsed signals with periods of 0.3 to 1.5 sec.
Date 1978
Observer(s) COHEN, MALKAN & DICKEY
Site NAIC, HRO, CSIRO
Instrument Size (m) 305, 36, 64
Search Frequency (MHz) 1665, 1667, 22235.08, 1612.231
Search Wavelength (nm)
Frequency Resolution (Hz) 9500, 65000, 4500
Other Resolution
Objects (Hz) 25 GLOBULAR CLUSTERS
Flux Limit (W m-2) 1.8 x 10-25, 1.1 x 10-22 , 1.5 x 10-24
Total Hours 40, 20, 20
Reference COHEN, N., and MALKAN, M., and DICKEY, J., Icarus, 41, p. 198 (1980).
Link
Comments Passive search for Type II & III civilizations using astronomical data originally observed to detect H 2 O & OH masers in globular clusters.
Date 1978
Observer(s) HOROWITZ
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 0.015
Other Resolution
Objects (Hz) 185 STARS
Flux Limit (W m-2) 8 x 10-28
Total Hours 80
Reference HOROWITZ, P., Science, 201, p. 733 (1978).
HOROWITZ, P. and FORSTER, J., “Project Sentinel: Ultra-Narrowband SETI at Harvard/Smithsonian,” The Search for Extraterrestrial Life: Recent Developments, M.D. Papagiannis (ed.), D. Reidel Publishing Co., Dordrecht, pp. 291- 303 (1985).
Link
Comments Assumes that signal frequency was corrected at the source to arrive at rest in Heliocentric or barycentric laboratory frame.
Date 1978
Observer(s) KNOWLES & SULLIVAN
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 130 – 500 (SPOT)
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 2 STARS
Flux Limit (W m-2) 2 x 10-24
Total Hours 5
Reference SULLIVAN, W.T. III, BROWN, S., and WETHERHILL, C., Science, 199, p. 377 (1978).
Link
Comments Attempted “eavesdropping” using MKI VLBI tapes as in Black, et al., 1977.
Date 1978
Observer(s) MAKOVETSKIJ, GINDILIS, ET AL.
Site ZELENCHUKSKAYA, RATAN-600
Instrument Size (m) 7.4 x 450 (ONE SECTOR)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) BARNARD’S STAR
Flux Limit (W m-2)
Total Hours 6 DAYS
Reference Gindilis, L.M., “Radio Astronomy and Search for Extraterrestrial Civilizations–Development of Investigations in the USSR,” Trudy Gaish, 58, pp. 87-118 (1986).
Link
Comments In accordance with “Magic Time” prediction by Makovetskij for Barnard’s Star and Nova Cygni 1975, signals were searched for in September, 1978.
Date 1978 – 1980
Observer(s) MICHAEL J. HARRIS
Site INTERPLANETARY NETWORK DATA
Instrument Size (m) PIONEER VENUS & VENERA 11 & 12 SPACECRAFT
Search Frequency (MHz)
Search Wavelength (nm) 20 keV – 1 MeV
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 54 GAMMA RAY BURST EVENTS
Flux Limit (W m-2)
Total Hours
Reference HARRIS, M.J., “A Search for Linear Alighments of Gamma Ray Burst Sources,” JBIS 43, p. 551 (1990).
Link
Comments Attempt to find 3 GRB events in a straight line, each having same velocity (from e ± e – annihilation line) that could indicate trajectory of an interstellar spacecraft.
Date 1978 – 1996
Observer(s) SHVARTSMAN ET AL. “MANIA”
Site SPECIAL ASTROPHYSICAL OBSERVATORY
Instrument Size (m) 6
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution D = 10 -6 Å
Objects (Hz) 93 OBJECTS
Flux Limit (W m-2) 3 x 10-4
Total Hours 250
Reference SCHVARTSMAN, V.F., “SETI in Optical Range with the 6M Telescope (MANIA),” in Bioastronomy: The Next Steps, G. Marx (ed.), Kluwer Academic Publishers, pp. 389-390 (1988), BESHIN ET. AL., “Methods and Results of an Optical Search for Extraterrestrial Civilizations,” Astrophysics and Space Science 252: 51-57 (1997).
Link
Comments Have searched 30 Radio Objects with Continuous Optical Spectra to date, looking for optical pulses form potential Kardashev type II or III civilizations.
Date 1979
Observer(s) COLE & EKERS
Site CSIRO
Instrument Size (m) 64
Search Frequency (MHz) 4995 – 5005, 4999 – 5001
Search Wavelength (nm)
Frequency Resolution (Hz) 107, 106
Other Resolution
Objects (Hz) NEARBY F, G & K STARS
Flux Limit (W m-2) 4 x 10-18
Total Hours 50
Reference COLE, T.N. and EKERS, R.D., Proc-ASA, 3, p. 328 (1979).
Link
Comments Simultaneous pulsed events in both 2 MHz & 10 MHz filters are sought detectors having time resolution of 4 µ seconds.
Date 1979
Observer(s) FREITAS & VALDES
Site LEUSCHNER OBSERVATORY, UCB
Instrument Size (m) 0.76
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) STABLE “HALO ORBITS” ABOUT L4 & L5 LIBRATION POINTS IN EARTH-MOON SYSTEM
Flux Limit (W m-2) m_v ≤14 (magnitude)
Total Hours 30
Reference FREITAS, R.A. and VALDES, F., Icarus, 42, p. 442 (1980).
Link
Comments Attempt to discover evidence of discrete objects (such as interstellar probes) in stable orbits about L4, L5 by study of 90 photographic plates.
Date 1979 – 1980
Observer(s) Tarter, Jill C.; Black, D.; Cuzzi, J; Clark, T.
Site NRAO
Instrument Size (m) 91
Search Frequency (MHz) 1665 – 1667
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 200 stars
Flux Limit (W m-2) 1.1 x 10-23
Total Hours 100
Reference Tarter, J., Black, D., Cuzzi, J., Clark, T., “A high-sensitivity search for extraterrestrial intelligence at lambda 18 CM”, Icarus, 42, p. 136 (1980).
Link
Comments VLBI high speed recorder combined with software direct Fourier transformation to produce extreme frequency resolution (non-real time). This was the first search at the frequency of the OH lines.
Date 1979 – 1981
Observer(s) TARTER, CLARK, DUQUET & LESYNA
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 1418.4 – 1422.4, 1664 – 1668
Search Wavelength (nm)
Frequency Resolution (Hz) 5, 600
Other Resolution
Objects (Hz) 200 STARS
Flux Limit (W m-2) 1 x 10-25
Total Hours 100
Reference TARTER, J.C., CLARK, T.A., DUQUET, R., and LESYNA, L., Acta Astronautica, 10, p. 277 (1983).
Link
Comments Rapid 1-bit sampler & high speed tape recorder run in parallel with 1008 channel correlator. Software direct Fourier transformation as in Black, et al., 1977.
Date 1979 – 1982
Observer(s) JPL, UCB “SERENDIP”
Site DSS 14
Instrument Size (m) 64
Search Frequency (MHz) S & X BAND (B=10 MHz)
Search Wavelength (nm)
Frequency Resolution (Hz) 1000
Other Resolution
Objects (Hz) APPARENT POSITIONS OF NASA SPACECRAFT
Flux Limit (W m-2) 8 x 10-24
Total Hours 400
Reference BOWYER, S, ZEITLAND, G.M., TARTER, J., LAMPTON, M., and WELCH, W.J., “The Berkeley Parasitic SETI Program,” Icarus, 53 pp.147-155 (1983).
Link
Comments Automated survey parasitic to spacecraft tracking operations using 512 channel auto-correlator & 100 channel correlator micro-processor control.
Date 1980
Observer(s) WITTEBORN
Site NASA – U OF A, MT. LEMON
Instrument Size (m) 1.5
Search Frequency (MHz)
Search Wavelength (nm) 8500 – 13500
Frequency Resolution (Hz)
Other Resolution 1 µ
Objects (Hz) 20 STARS
Flux Limit (W m-2) N MAGNITUDE EXCESS < 1.7
Total Hours 50
Reference
Link
Comments Search for IR excess due to Dyson spheres around solar type stars. Target stars were chosen because too faint for spectral type.
Date 1980 – 1981
Observer(s) SUCHKIN, TOKAREV ET AL.
Site NIRFI, GORKII, GAISH, MOSCOW
Instrument Size (m)
Search Frequency (MHz) 9.3
Search Wavelength (nm)
Frequency Resolution (Hz) 1500
Other Resolution
Objects (Hz) L4 & L5 LIBRATION POINTS OF EARTH-MOON SYSTEM
Flux Limit (W m-2)
Total Hours 20
Reference Presented at SETI-81 International Symposium held in Tallinn, Estonia (1981).
Link
Comments Radar reflections sought from artifacts in parking orbits.
Date 1981
Observer(s) LORD & O’DEA
Site U. MASS
Instrument Size (m) 14
Search Frequency (MHz) 115000
Search Wavelength (nm)
Frequency Resolution (Hz) 20000, 125000, 4 x 108
Other Resolution
Objects (Hz) NORTH GALACTIC ROTATION AXIS b = 5˚ -> 90˚
Flux Limit (W m-2) 10-21
Total Hours 50
Reference
Link
Comments Search for signals J=1-0 CO line from a transmitter somewhere along the Galactic rotation axis.
Date 1981
Observer(s) SHOSTAK & TARTER “SIGNAL”
Site WRST
Instrument Size (m) 3000 MAX BASELINE
Search Frequency (MHz) 1420.24 – 1420.56
Search Wavelength (nm)
Frequency Resolution (Hz) 1200
Other Resolution
Objects (Hz) GALACTIC CENTER
Flux Limit (W m-2) 10-24
Total Hours 4
Reference SHOSTAK, S. and TARTER, J., “SIGNAL (Search for Intelligence in the Galactic Nucleus with the Array of the Lowlands),” paper #IAA-82-262 presented at IAF Congress, Paris, France (1982).
Link
Comments Use of interferometer to search for pulsed signals from Galactic Center in range of periods from 40 seconds to 2 hours.
Date 1981
Observer(s) TALENT
Site KPNO
Instrument Size (m) 2.1
Search Frequency (MHz)
Search Wavelength (nm) 357.5 – 535
Frequency Resolution (Hz)
Other Resolution 10 Å
Objects (Hz) 3 STARS
Flux Limit (W m-2)
Total Hours 0.2
Reference 1982 preprint “21 cm Radio Emissions with Geometric Fine Structure” by Gray, Dixon, Ehman and Talent. Cited by Freitas in JBIS 38, p. 106 (1985).
Link
Comments Search for enhanced stellar lines of praseodymium, neodymium, zirconium as evidence for dumping of nuclear wastes into stellar atmospheres.
Date 1981
Observer(s) TARTER & ISRAEL
Site WRST
Instrument Size (m) 3000 MAX BASELINE
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 4 x 106, 10 x 106
Other Resolution
Objects (Hz) 85 STAR FIELDS
Flux Limit (W m-2) 6 x 10-22 – 6 x 10-24
Total Hours 600
Reference TARTER, J. and ISRAEL. F.P., Acta Astronautica, 9, p. 415 (1982).
Link
Comments Parasitic search similar to Israel & DeRuiter using “uncleaned” maps stored at Groningen & Leiden, & AGK3 catalog.
Date 1981 – 1981
Observer(s) Shostak, S., Tarter, J.
Site WRST
Instrument Size (m) 3000 MAX BASELINE
Search Frequency (MHz) 1420.24 – 1420.56
Search Wavelength (nm)
Frequency Resolution (Hz) 1200
Other Resolution
Objects (Hz) GALACTIC CENTER
Flux Limit (W m-2) 10-24
Total Hours 4
Reference Shostak, S., Tarter, J., “SIGNAL (Search for Intelligence in the Galactic Nucleus with the Array of the Lowlands),” paper #IAA-82-262 presented at IAF Congress, Paris, France (1982).
Link
Comments Use of interferometer to search for pulsed signals from Galactic Center in range of periods from 40 seconds to 2 hours.
Date 1981 – 1982
Observer(s) VALDES & FREITAS “SETA”
Site KPNO
Instrument Size (m) 0.61
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) EARTH-MOON THROUGH L5, SUN-EARTH L1, L2
Flux Limit (W m-2) 10 ≤ m v ≤ 19 (magnitude)
Total Hours 70
Reference VALDES, F. and FREITAS, R.A. Jr., Icarus 53, p. 453 (1983).
Link
Comments Attempt to see discrete artifacts (≥ few m in size) in stable orbits near Lagrange points. Studies 137 III aF photographic plates.
Date 1981 – 1982
Observer(s) Lord, S.; O’Dea,
Site U. Mass
Instrument Size (m) 14
Search Frequency (MHz) 115000
Search Wavelength (nm)
Frequency Resolution (Hz) 20000, 125000, 4 x 108
Other Resolution
Objects (Hz) NORTH GALACTIC ROTATION AXIS b = 5° -> 90°
Flux Limit (W m-2) 10-21
Total Hours 50
Reference Tarter, J., “SETI Observations World Wide,” The search for extraterrestrial life: Recent developments; Proceedings of the Symposium, Boston, MA, June 18-21, 1984 (A86-38126 17-88). Dordrecht, D. Reidel Publishing Co., 1985, p. 271-290 (1985).
Link http://adsabs.harvard.edu/full/1985IAUS..112..271
Comments Search for signals J=1-0 CO line from a transmitter somewhere along the Galactic rotation axis
Date 1981 – 1988
Observer(s) BIRAUD & TARTER
Site NANÇAY
Instrument Size (m) 40 x 240
Search Frequency (MHz) 1420.08 – 1420.72, 1665 – 1667
Search Wavelength (nm)
Frequency Resolution (Hz) 48.8
Other Resolution
Objects (Hz) 343 STARS
Flux Limit (W m-2) 1 x 10-24
Total Hours ~600
Reference TARTER, J.C., “Statistics of ‘Excess’ Observatory Noise at the Nançay Telescope and Elsewhere,” paper #IAA-85-473, presented at 36th IAF Congress in Stockholm, Sweden (1985). Biraud, F., Acta Astronautica, 10, p. 759 (1985).
Link
Comments Eight level, 1024 channel auto-correlator, with stepped first LO to extend frequency coverage at 48 Hz resolution.
Date 1982
Observer(s) HOROWITZ, TEAGUE, LINSCOTT, CHEN & BACKUS, “SUITCASE SETI”
Site NAIC
Instrument Size (m) 305
Search Frequency (MHz) 2840.8, 1420.4
Search Wavelength (nm)
Frequency Resolution (Hz) 0.03
Other Resolution
Objects (Hz) 250 STARS & 150 STARS
Flux Limit (W m-2) 4 x 10-26 – 6 x 10-28
Total Hours 75
Reference HOROWITZ, P. and FORSTER, J., “Project Sentinel: Ultra-Narrowband SETI at Harvard/Smithsonian,” The Search for Extraterrestrial Life: Recent Developments, M.D. Papagiannis (ed.), D. Reidel Publishing Co., Dordrecht, pp. 291- 303 (1985).
Link
Comments Dual 64K channel real time microprocessor based spectrum analyzer with video archiving & swept LO frequency to test “magic frequencies.”
Date 1982
Observer(s) VALLEE & SIMARD-NORMANDIN
Site ARO
Instrument Size (m) 46
Search Frequency (MHz) 10522
Search Wavelength (nm)
Frequency Resolution (Hz) 185 x 106
Other Resolution
Objects (Hz) GALACTIC CENTER MERIDIAN
Flux Limit (W m-2) 10-19
Total Hours 72
Reference VALLEE, J.P., “Search for Strongly Polarized Radio Emission from E.T.I. and an Optimistic Approach to the Great Silence (Fermi’s Paradox),” The Search for Extraterrestrial Life: Recent Developments, M.D. Papagiannis (ed.), D. Reidel Publishing Co., Dordrecht, pp. 321-325 (1985).
Link
Comments Search for strongly polarized signals by mapping field 1/4′ x 25′ along l = 0°.
Date 1983
Observer(s) DAMASHEK
Site NRAO
Instrument Size (m) 92
Search Frequency (MHz) 382 – 398
Search Wavelength (nm)
Frequency Resolution (Hz) 2 x 106
Other Resolution
Objects (Hz) SKY SURVEY (PULSARS)
Flux Limit (W m-2) 2 x 10-22
Total Hours 700
Reference
Link
Comments Sixteen MHz sampled at 60 Hz; 8 contiguous frequency channels. Search for single dispersed pulses and telemetry (bit stream) signals.
Date 1983
Observer(s) VALDES & FREITAS
Site HCRO
Instrument Size (m) 26
Search Frequency (MHz) 1514 – 1518
Search Wavelength (nm)
Frequency Resolution (Hz) 4.9, 76000
Other Resolution
Objects (Hz) 80 STARS & 12 NEARBY STARS
Flux Limit (W m-2) 3 x 10-24
Total Hours 100
Reference VALDES, F. and FREITAS, R.A. Jr., Icarus 65, pp. 152-157 (1986).
Link
Comments Search for radioactive tritium line from Nuclear fusion by another technology.
Date 1983 – 1983
Observer(s) GULKIS
Site DSS 43
Instrument Size (m) 64
Search Frequency (MHz) 8000, 2375 – 2385
Search Wavelength (nm)
Frequency Resolution (Hz) 40000
Other Resolution
Objects (Hz) PARTIAL SOUTHERN SKY
Flux Limit (W m-2) 2 x 10-22
Total Hours 800 – ON
Reference KUIPER, T. and GULKIS, S., The Planetary Report, 3, p. 17 (1983).
Link
Comments Sky survey of constant declination strips (3 from -28.9 to -34.3 by April 1983) whenever antenna stowed.
Date 1983 – 1984
Observer(s) CULLERS
Site AMSETI
Instrument Size (m) 2
Search Frequency (MHz) ~1420, ≤ 1000
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz)
Flux Limit (W m-2)
Total Hours CONTINUING
Reference
Link
Comments Low noise GaAs FETS and micros with satellite TV dishes, by Silicon Valley Hams, with NASA Ames consultation.
Date 1983 – 1985
Observer(s) HOROWITZ “SENTINEL”
Site OAK RIDGE (HARVARD UNIVERSITY)
Instrument Size (m) 26
Search Frequency (MHz) 1420.40575, 1667.3590
Search Wavelength (nm)
Frequency Resolution (Hz) 0.03
Other Resolution
Objects (Hz) SKY SURVEY
Flux Limit (W m-2) 5 x 10-25
Total Hours CONTINUING
Reference HOROWITZ, P. and FORSTER, J., “Project Sentinel: Ultra-Narrowband SETI at Harvard/Smithsonian,” The Search for Extraterrestrial Life: Recent Developments, M.D. Papagiannis (ed.), D. Reidel Publishing Co., Dordrecht, pp. 291- 303 (1985).
Link
Comments “Suitcase SETI” as the backend of automated sky survey at 2 magic frequencies over a 3 year observing period.
Date 1983 – 1988
Observer(s) GRAY
Site SMALL SETI OBSERVATORY
Instrument Size (m) 4
Search Frequency (MHz) 1419.5 – 1421.5
Search Wavelength (nm)
Frequency Resolution (Hz) 1 – 40
Other Resolution
Objects (Hz) SKY SURVEY & -27¤
Flux Limit (W m-2) 10-22
Total Hours CONTINUING
Reference GRAY, R.H., published in The Search for Extraterrestrial Intelligence: Proceedings of NRAO Workshop at NRAO, Green Bank, West Virginia, May 1985, K. Kellermann and G. Seielstad (eds.), NRAO/AUI Publishers, p. 205 (1986).
Link
Comments Dedicated meridian transit search system constructed by amateurs, operated during evenings.
Date 1983 – 1988
Observer(s) STEPHENS
Site INTERSTELLAR ELECTRO-MAGNETICS INSTITUTE AT HAY RIVER, NWT
Instrument Size (m) TWO 18m x 18m (28m EQUIVALENT)
Search Frequency (MHz) 1415 – 1425
Search Wavelength (nm)
Frequency Resolution (Hz) 30000
Other Resolution
Objects (Hz) NORTHERN SKY SURVEY
Flux Limit (W m-2) T sys ~75K
Total Hours CONTINUING
Reference
Link
Comments Two sixty four foot square surplus tropo-scatter dishes combined for use as dedicated amateur SETI observatory. Coverage is 30° -> 45° declination. Discontinued due to lack of funding.
Date 1984
Observer(s) SLYSH
Site SATELLITE
Instrument Size (m) RADIOMETER
Search Frequency (MHz) 37000
Search Wavelength (nm)
Frequency Resolution (Hz) 4 x 108
Other Resolution
Objects (Hz) ALL SKY 3° K BB
Flux Limit (W m-2) T/T ≤ .01
Total Hours 6000
Reference SLYSH, V.I., “A Search in the Infrared to Microwave for Astroengineering Activity,” The Search for Extraterrestrial Life: Recent Developments, M.D. Papagiannis (ed.), D. Reidel Publishing Co., Dordrecht, p.p. 315-319 (1985).
Link
Comments Lack of fluctuations 3 ≥ K background radiation on angular scales of 10 -2 Strd. rules out optically thick Dyson spheres radiating more than 1 L o within 100 pc.
Date 1985 – 1992
Observer(s) BOWYER, WERTHEIMER & LAMPTON “SERENDIP II”
Site NRAO
Instrument Size (m) 92
Search Frequency (MHz) 400 – 3500
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) SKY AREAS OBSERVED BY ASTRONOMERS
Flux Limit (W m-2) 4 x 10-24
Total Hours CONTINUING
Reference BOWYER, S., WERTHEIMER, D. and LINDSAY, V., “The Berkeley Piggyback SETI Program: Serendip II” in Bioastronomy: The Next Steps, G. Marx (ed.), Kluwer Academic Publishers, Dordrecht (1988).
Link
Comments Automated search that piggybacks on radioastronomical observations. Scans available 3.5 MHz of available IF 65 KHz at a time, recording events above threshold for off line processing.
Date 1985 – 1995
Observer(s) HOROWITZ “META SETI”
Site OAKRIDGE (HARVARD UNIVERSITY)
Instrument Size (m) 26
Search Frequency (MHz) 1420.4, 1665.4, 1667.3, 2840.8
Search Wavelength (nm)
Frequency Resolution (Hz) 0.05
Other Resolution
Objects (Hz) SKY SURVEY
Flux Limit (W m-2) 1.3 x 10-24
Total Hours CONTINUING
Reference HOROWITZ, P., published in The Search for Extraterrestrial Intelligence: Proceedings of NRAO Workshop at NRAO, Green Bank, West Virginia, May 1985, K. Kellermann and G. Seielstad (eds.), NRAO/AUI Publishers, p. 99 (1986).
Link
Comments Signal Processing Hardware from “SENTINEL” was replicated 128 times to produce 8.4 x 106 channels. Six sequential observations of each patch of sky are made to cover 2 orthogonal circular polarizations & 3 rest frames (Sun/Earth, Galactic Center, 3 K Background).
Date 1986
Observer(s) ARKHIPOV
Site
Instrument Size (m)
Search Frequency (MHz) 408
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) HD 21899, HD 100623, HD 187691 & HD 187923
Flux Limit (W m-2)
Total Hours
Reference Arkhipov, A.V., Academy of Sciences Ukranian SSR Institute of Radiophysics and Electronics, preprint No. 303 (1986).
Link
Comments Search through 408 MHz Molonglo Survey Catalog of Radio Sources found 4 solar-type stars within 130″ of radio source position. Suggested as leakage emission from orbital industrial processing facility ~1000 AU from star.
Date 1986
Observer(s) MIRABEL
Site NRAO
Instrument Size (m) 43
Search Frequency (MHz) 4829.620 – 4829.776
Search Wavelength (nm)
Frequency Resolution (Hz) 76
Other Resolution
Objects (Hz) GALACTIC CENTER & 33 NEARBY STARS
Flux Limit (W m-2) 6 x 10-25 to 10-24
Total Hours 144
Reference
Link
Comments Search at H 2 CO frequency. Included star HD170493 located in front of dark “anti-maser” cloud.
Date 1986 – 1989
Observer(s) DIXON & BOLINGER
Site OSURO
Instrument Size (m) 53
Search Frequency (MHz) 1400 – 1700
Search Wavelength (nm)
Frequency Resolution (Hz) 100, 10, 2000
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2) 1.5 x 10-22
Total Hours 20000
Reference
Link
Comments
Date 1986 – ON
Observer(s) COLOMB, MARTIN & LEMARCHAND
Site IAR
Instrument Size (m) 30
Search Frequency (MHz) 1415.4057, 1425.4057, 1667
Search Wavelength (nm)
Frequency Resolution (Hz) 2500
Other Resolution
Objects (Hz) 78 SOLAR-TYPE STARS
Flux Limit (W m-2) 5 x 10-23
Total Hours 320
Reference Colomb, F.R., Martin, M.C. and LEMARCHAND, G.A., “SETI Observational Program in Argentina,” Acta Astronautica, 26, 3/4, pp. 211-212 (1992).
Link
Comments 34 of 78 Southern Hemisphere solar-type stars have been examined at 21cm to date. All stars will be searched at 21 cm & 18 cm within 1 yr.
Date 1987
Observer(s) GRAY
Site OAK RIDGE (HARVARD UNIVERSITY)
Instrument Size (m) 26
Search Frequency (MHz) 1220.41 – 1620.41
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution 0.05″
Objects (Hz) SKY POSITION CORRESPONDING TO OSURO’s 1977 “WOW” SIGNAL
Flux Limit (W m-2) 1.5 x 10-24
Total Hours 16
Reference GRAY, R.H., “A Search of the ‘WOW’ Locale for Intermittent Radio Signals,” Icarus 112, pp. 485-489 (1994).
Link
Comments Used “META SETI” system (see Ref.27) to track position on sky that produced the “WOW” signal at OSURO in 1977.
Date 1987
Observer(s) TARTER, KARDASHEV & SLYSH
Site VLA
Instrument Size (m) 26 (9 ANTENNAS)
Search Frequency (MHz) 1612.231
Search Wavelength (nm)
Frequency Resolution (Hz) 6105
Other Resolution
Objects (Hz) G357.3-1.3
Flux Limit (W m-2)
Total Hours 1
Reference
Link
Comments Remote observation (by VLA staff) of IRAS source near galactic center to determine if source could be nearby Dyson sphere. Source confirmed as OH/IR star.
Date 1988
Observer(s) BANIA & ROOD
Site NRAO
Instrument Size (m) 43
Search Frequency (MHz) 8665
Search Wavelength (nm)
Frequency Resolution (Hz) 305
Other Resolution
Objects (Hz) 24 “VEGA-LIKE” STARS WITH 60 MICRON EXCESSES (IRAS)
Flux Limit (W m-2) 1 Jy
Total Hours 50
Reference BANIA, T.M and ROOD, R.T., “Search for Interstellar Beacons at the 3He+ Hyperfine Transition Frequency,” Third Decennial US-USSR Conference on SETI, Santa Cruz, August 1991. ASP Conf. Series 47, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 357-365 (1993).
Link
Comments Searching for narrow band, obviously artificial, signal at the frequency of 3He+ spin-flip, being radiated by advanced civilizations that have colonized their planetary systems.
Date 1989 – ON
Observer(s) CHILDERS & DIXON
Site OSURO
Instrument Size (m) 53
Search Frequency (MHz) 1400 – 1700
Search Wavelength (nm)
Frequency Resolution (Hz) 100, 10, 2000
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2) 1.5 x 10-22
Total Hours 60000
Reference
Link
Comments Have searched declinations +62 to –22 so far. Continuing to -36.
Date 1990
Observer(s) BLAIR ET AL.
Site CSIRO
Instrument Size (m) 64
Search Frequency (MHz) 4461.98 – 4462.03
Search Wavelength (nm)
Frequency Resolution (Hz) 100
Other Resolution
Objects (Hz) 100 SOLAR-TYPE STARS VISIBLE ONLY FROM SOUTHERN HEMISPHERE
Flux Limit (W m-2) 2 Jy
Total Hours 60
Reference BLAIR, D.G., NORRIS, R., WELLINGTON, K.J., WILLIAMS, A. and WRIGHT, A., “A Test for the Interstellar Contact Channel Hypothesis in SETI,” Bioastronomy: The Search for Extraterrestrial Life, J. Heidmann and M. Klein (eds.), Springer-Verlag, Berlin, LNP 390, pp. 271-279 (1991).
Link
Comments Magic frequency search at pi times hydrogen line frequency. 1280 channels were arranged to sample three reference frames: solar barycenter, stellar barycenter and geocenter.
Date 1990
Observer(s) GRAY
Site OAK RIDGE (HARVARD UNIVERSITY)
Instrument Size (m) 26
Search Frequency (MHz) 1420.2 – 1420.6
Search Wavelength (nm)
Frequency Resolution (Hz) 0.05
Other Resolution
Objects (Hz) M31 AND M33
Flux Limit (W m-2)
Total Hours 50
Reference
Link
Comments Long integrations (5 hours per HPBW) on 10 11 stars at once, looking for low duty cycle signals.
Date 1990 – 1995
Observer(s) GRAY
Site SMALL SETI OBSERVATORY
Instrument Size (m) 4
Search Frequency (MHz) 1419.5 – 1420.5
Search Wavelength (nm)
Frequency Resolution (Hz) 1 – 100
Other Resolution
Objects (Hz)
Flux Limit (W m-2) 10-21
Total Hours ONGOING ~6 HOURS/NIGHT
Reference GRAY, R.H., “Small SETI Radio Telescope Mark II: 8,192 Channels,” SETI Quest Vol. 2 No. 4 (November 1995).
Link
Comments Dedicated meridian transit search system constructed by amateurs, automated operation at night.
Date 1990 – ON
Observer(s) BETZ
Site MT. WILSON
Instrument Size (m) 1.65 M ELEMENT OF TOWNES IR INTERFEROMETER
Search Frequency (MHz)
Search Wavelength (nm) 10000
Frequency Resolution (Hz) 3.5 x 106
Other Resolution
Objects (Hz) 100 NEARBY SOLAR-TYPE STARS
Flux Limit (W m-2) 1 MW TRANSMITTER OUT TO 20pc
Total Hours CONTINUING
Reference BETZ. A.L., “A Search for Infrared Laser Signals,” Third Decennial US-USSR Conference on SETI, ASP Conference Series Vol. 47, S. Shostak (ed.), pp. 373-379 (1993).
Link
Comments Search for IR beacons at CO 2 laser frequency using narrowband acousto-optical spectrometer.
Date 1990 – 2010
Observer(s) LEMARCHAND “META II”
Site INSTITUTE FOR ARGENTINE RADIOASTRONOMY (IAR)
Instrument Size (m) 30 (ONE OF TWO)
Search Frequency (MHz) 1420.4, 1667, 3300
Search Wavelength (nm)
Frequency Resolution (Hz) 0.05
Other Resolution
Objects (Hz) SKY SURVEY OF SOUTHERN SKIES AND 90 TARGET STARS, AND OH MASERS
Flux Limit (W m-2) 10-23 – 7 x 10-25
Total Hours ONGOING
Reference COLOMB, F.R., HURRELL, E.E., LEMARCHAND, G.A., AND olade, j.c., “Results of Two Years of SETI Observations with META II”, Progress in the Search for Extraterrestrial Life, ASP Conference Series Vol. 74, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 345-352 (1995).
Link
Comments Search for signals that have been Doppler compensated to rest frame of SS barycenter, Galactic Center or CMB. A duplicate of META system build by Argentinian engineers under the guidance of Prof. Horowitz at Harvard and financed by the Planetary Society. Simultaneous observations with META over declination range -10° to -30°. Major upgrades in 1996 to permit long integration times, and switching between antennas. Search through OH masers looking for amplified signals.
Date 1992 – 1993
Observer(s) NASA “HRMS” SKY SURVEY
Site GOLDSTONE, CA
Instrument Size (m) 26, 34
Search Frequency (MHz) 1700, 8300 – 8700
Search Wavelength (nm)
Frequency Resolution (Hz) 19
Other Resolution
Objects (Hz) 72 SKY FRAMES AT X-BAND AND 130 SKY FRAMES REPEATEDLY MAPPING 3 GALACTIC PLANE REGIONS AT L-BAND IN SEQUENTIAL CIRCULAR POLARIZATION
Flux Limit (W m-2) 9.8 x 10-23
Total Hours 1386
Reference LEVIN, S., OLSEN, E.T., BACKUS, C., and GULKIS, S., “The NASA HRMS Sky Survey X-B and Observations: A Progress Report,” Progress in the Search for Extraterrestrial Life, ASP Conference Series Vol. 74, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 470-477 (1995).
Link
Comments No detection of non-human technology.
Date 1992 – 1993
Observer(s) NASA “HRMS” TARGETED SEARCH
Site ARECIBO, PR
Instrument Size (m) 305
Search Frequency (MHz) 1300 – 2400
Search Wavelength (nm)
Frequency Resolution (Hz) 46759
Other Resolution
Objects (Hz) 25 STARS
Flux Limit (W m-2) 5 x 10-24
Total Hours 200
Reference TARTER, J. , “HRMS: Where We’ve Been, and Where We’re Going,” Progress in the Search for Extraterrestrial Life, ASP Conference Series Vol. 74, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 456-469 (1995).
Link
Comments No detection of non-human technology.
Date 1992 – 1993
Observer(s) Oliver, ; Levin, S.; Olsen, E.T.; Backus, C.; Gulkis, S.; HRMS Sky Survey,
Site GOLDSTONE, CA
Instrument Size (m) 34
Search Frequency (MHz) 8300 – 8600
Search Wavelength (nm)
Frequency Resolution (Hz) 40 x 106
Other Resolution
Objects (Hz) X-band survey
Flux Limit (W m-2) 5 x 10-22
Total Hours
Reference Levin, S., Olsen, E.T., Backus, C., Gulkis, S., “The NASA HRMS Sky Survey X-Band Observations: A Progress Report,” Progress in the Search for Extraterrestrial Life ASP Conference Series, Vol. 74, p. 471, G. Seth Shostak (ed.) (1995).
Link ***http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?1995ASPC…74..471L&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf***
Comments The SSPS, or Sky Survey Prototype System is a distinct subdivision of the NASA HRMS survey. The prototype system is working well. It is being used to gain experience which will be applied in the running of the Opertation system, SSOS. The search looks for Singlets and Doublets. The strongest of these targets are kept and reobserved within two hours of initial detection. During the lookbacks, several sky frames are observed at once to increase accuracy. Thus far no anomalies which might indicate ETI signals have been found.
Date 1992 – 1997
Observer(s) BOWYER, WERTHIMER & DONNELLY “SERENDIP III”
Site ARECIBO
Instrument Size (m) 305
Search Frequency (MHz) 424 – 436
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) SURVEY OF 30% OF SKY
Flux Limit (W m-2) 5 x 10-25
Total Hours CONTINUING
Reference DONNELLY, C., BOWYER, S., WERTHIMER, D. and MALINA, R.F., “Forty Trillion Signals from SERENDIP: The Berkeley SETI Program,” Progress in the Search for Extraterrestrial Life, ASP Conference Series Vol. 74, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 284-290 (1995).
Link
Comments 4 million channels are under observation. Commensal search occurring at twice sidereal rate in backwards direction while radio astronomers track targets using the feeds and receivers on carriagehouse 1.
Date 1993
Observer(s) JUGAKU, NOGUCHI & NISHIMURA
Site INFRARED TELESCOPE OF INSTITUTE OF SPACE AND ASTRONAUTICAL SCIENCE, JAPAN AND INFRARED TELESCOPE AT XINGLONG STATION OF THE BEIJING ASTRONOMICAL OBSERVATORY
Instrument Size (m) 1.3, 1.26
Search Frequency (MHz)
Search Wavelength (nm) 2200, 12000
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 180 SOLAR-TYPE STARS
Flux Limit (W m-2)
Total Hours
Reference JUGAKU, J., NOGUCHI, K., NISHIMURA, S., “A Search for Dyson Spheres Around Late-Type Stars in the Solar Neighborhood,” Progress in the Search for Extraterrestrial Life, ASP Conference Series Vol. 74, S. Shostak (ed.), Astronomical Society of the Pacific, San Francisco, pp. 381-385 (1995).
Link
Comments Searched for 12 µ excess radiation from IRAS catalog stars by using K-[12] color index in attempt to find Dyson Spheres.
Date 1993
Observer(s) STEFFES & DeBOER
Site NRAO/TUCSON
Instrument Size (m) 12
Search Frequency (MHz) 203000
Search Wavelength (nm)
Frequency Resolution (Hz) 32
Other Resolution
Objects (Hz) 40 STARS + 3 LOCATIONS NEAR GALACTIC CENTER
Flux Limit (W m-2) 2.3 x 10-19
Total Hours 25
Reference Steffes, P.G. and DeBOER, D.R., “A SETI Search of Nearby Solar-Type Stars at the 203 GHz Positronium Hyperfine Resonance,” Icarus 107, pp. 215-218 (1994).
Link
Comments No artificial signals detected near positronium line.
Date 1993 – 1995
Observer(s) LEMARCHAND ET AL. “META II TARGET SEARCH”
Site INSTITUTO ARGENTINO DE RADIOASTRONOMIA (IAR)
Instrument Size (m) 30
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 0.05
Other Resolution
Objects (Hz) TARGETED SEARCH < 8 – 10°
Flux Limit (W m-2) 10-24
Total Hours 290
Reference LEMARCHAND, G.A., “SETI From the Southern Hemisphere,” SETI Quest, Vol. 2, No. 2, pp. 13-18 (1996).
Link
Comments All * < 5 pc and solar type * -> 50 ly yr. 80 stars total.
Date 1994
Observer(s) MAUERSBERGER, WILSON, ROOD, BANIA, HEIN & LINHART
Site IRAM/PICO VELETA
Instrument Size (m) 30
Search Frequency (MHz) 203000
Search Wavelength (nm)
Frequency Resolution (Hz) 106, 9700
Other Resolution
Objects (Hz) 16 STARS + GALACTIC CENTER
Flux Limit (W m-2) 0.2 – 20 x 1015
Total Hours ~5
Reference MAUERSBERGER, R., WILSON, T.L., ROOD, R.T., BANIA, T.M., HEIN, H. and LINKART, A., “SETI at the Spin – Flip Line Frequency of Positronium,” Astron. Astrophys. 306, pp. 141-144 (1996).
Link
Comments Search at Positronium line towards nearby stars and stars with IR excess that might be Dyson spheres.
Date 1995
Observer(s) GRAY
Site NRAO/VLA
Instrument Size (m) 27-ELEMENT ARRAY of 26M ANTENNAS
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 6104, 381
Other Resolution
Objects (Hz) OSU “WOW” LOCALE
Flux Limit (W m-2) 10 & 100 mJy/beam/channel
Total Hours 4
Reference
Link
Comments Search of the OSU “WOW” locale with 4 arcsec synthesized beam.
Date 1995
Observer(s) NORRIS (PHOENIX COOPERATIVE SCIENCE)
Site ATNF/PARKES and MOPRA
Instrument Size (m) 64, 22
Search Frequency (MHz) 1200 – 3000
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) GALACTIC CENTER
Flux Limit (W m-2) 1.3 x 10-25
Total Hours 24
Reference
Link
Comments Galactic Center searched for beacon.
Date 1995
Observer(s) SETI INSTITUTE PROJECT PHOENIX
Site ATNF/PARKES and MOPRA
Instrument Size (m) 64, 22
Search Frequency (MHz) 1200 – 3000
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 206 STARS, 1200 – 1750 MHz 105 STARS, 1750 – 3000 MHz
Flux Limit (W m-2) 1.32 x 10-25 FOR HALF of 1750 – 3000 MHz OBSERVATIONS. 1.82 x 10-25 FOR ALL OTHER OBSERVATIONS
Total Hours 2600
Reference BACKUS, P., “The Phoenix Search Results at Parkes,” Acta Astronautica 42, No. 10-12, pp. 651-654 (1998).
Dreher, J., “The Phoenix Signal Detection System,” Acta Astronautica 42, No. 10-12, pp. 635-640 (1998).
Link
Comments Immediate two-site, pseudo-interferometric follow-up observations of candidate signals. Targets were solar-type stars visible only from southern hemisphere. No detection of non-human technology.
Date 1995
Observer(s) SHOSTAK, EKERS, and VAILE (PHOENIX COOPERATIVE SCIENCE)
Site ATNF/PARKES
Instrument Size (m) 64
Search Frequency (MHz) 1200 – 1750
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 3 FIELDS IN THE SMC
Flux Limit (W m-2) 1.9 x10-25
Total Hours 24
Reference Shostak, S., Ekers, R., and Vaile, R., “A Search for Artificial Signals from the Small Magellanic Cloud”, A.J. 112, pp 164-166 (1996).
Link
Comments Search of > 10 7 stars contained within the three fields of the SMC. Limit on detectable transmitters of 1.5×10 18 W EIRP.
Date 1995
Observer(s) SULLIVAN, WELLINGTON, SHOSTAK, BACKUS, AND CORDES (PHOENIX COOPERATIVE SCIENCE)
Site ATNF/PARKES
Instrument Size (m) 64
Search Frequency (MHz) 1415 – 1425
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) GALACTIC CENTER AND 5° HIGH STRIP +/-15°LONGITUDE ALONG GALACTIC PLANE
Flux Limit (W m-2) 1.5 – 10 x 10-25
Total Hours 48
Reference Sullivan, III, W.T., Wellington, K.J., Shostak, G.S., Backus, P.R., and Cordes, J.M., “A Galactic Center Search for Extraterrestrial Intelligent Signals.” Poster paper #P4-17 presented at 5th International Conference on Bioastronomy, IAU Colloquium No. 161, Capri, Italy (July 1-5, 1996).
Link
Comments Multiple 30-second observations of strip along Galactic Plane and the Galactic Center, looking for repetitive signals.
Date 1995
Observer(s) TE LINTEL HEKKERT AND TARTER (PHOENIX COOPERATIVE SCIENCE)
Site ATNF/PARKES and MOPRA
Instrument Size (m) 64, 22
Search Frequency (MHz) 1200 – 3000
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 4 POTENTIAL DYSON SPHERES
Flux Limit (W m-2) 1.9 x 10-25
Total Hours 48
Reference
Link
Comments Candidate Dyson Sphere selection criteria: IRAS PSC sources with temperatures from 300-500K, that were not identified in OH/IR or CO(1-0) surveys, and had galactic latitudes > 5°.
Date 1995
Observer(s) ZADNIK ET AL. (PHOENIX COOPERATIVE SCIENCE)
Site ATNF/PARKES
Instrument Size (m) 64
Search Frequency (MHz) 4462, 4532, 8295, 8393, 8666
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 49 STARS CLOSER THAN 11.5 pc
Flux Limit (W m-2) 3.5 AND 5.0 Jy
Total Hours 48
Reference Zadnik, M.G., Winterflood, J., Williams, A.J., Wellington, K.J., Vaile, R. Tarter, J., Norris, R., Heiligman, G., Blair, D.G., and Backus, P., “Interstellar Communication Channel Search of Solar-Type Targets Closer than 11 pc.” Poster paper #P4-21 presented at 5th International Conference on Bioastronomy, IAU Colloquium No. 161, Capri, Italy (July 1-5, 1996).
Link
Comments Magic Frequency search at π*HI, e*OH, 2π*HI, e*(OH + H), 3 H e
Date 1995 – 1998
Observer(s) BROWN, KLEIN & DIXON
Site OSURO
Instrument Size (m) 53
Search Frequency (MHz) 1421.75 – 1424.25
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) ALL SKY SEARCH
Flux Limit (W m-2) UNKNOWN AS YET
Total Hours 5000
Reference
Link
Comments Using SERENDIP processor. Have searched declinations +8 to -36. Program ended when OSU sold observatory site to golf course developer.
Date 1995 – 1998
Observer(s) KINGSLEY
Site COLUMBUS OPTICAL SETI OBSERVATORY, OHIO
Instrument Size (m) 0.25
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) NEARBY SOLAR-TYPE STARS
Flux Limit (W m-2) TRANSMITTERS WITH PEAK INSTANTANEOUS POWER > 10 18 W
Total Hours
Reference KINGSLEY, S. “Prototype Optical SETI Observatory” in Proceedings of the Search for Extraterrestrial Intelligence (SETI), in the Optical Spectrum II, Jan 31 – Feb 1, 1996, Proc. SPIE 2704:102. < http://www.coseti.org>
Link
Comments Broadband optical search for short pulses (~1 nanosecond) that instantaneously outshine the host star.
Date 1995 – 1999
Observer(s) HOROWITZ ET AL. (BETA)
Site OAK RIDGE OBSERVATORY
Instrument Size (m) 26
Search Frequency (MHz) 1400 – 1720
Search Wavelength (nm)
Frequency Resolution (Hz) 0.5
Other Resolution
Objects (Hz) SKY SURVEY FROM -30° to + 60° DECLINATION
Flux Limit (W m-2) 2.2 x 10-22
Total Hours SUSPENDED IN SPRING 1999
Reference LEIGH, d. AND HOROWITZ, p. “Strategies, Implementation And Results Of BETA” in Bioastronomy ‘99 – A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 459 (2000).
Link
Comments Waterhole search, using dual-beams and omni antenna to discriminate against RFI. Project BETA (Billion channel ExtraTerrestrial Assay) is follow-on to META. Project interrupted when wind blew antenna off its mount. Repairs are under way.
Date 1995 – 2010
Observer(s) SETI LEAGUE PROJECT ARGUS
Site MULTIPLE SITES WORLD-WIDE (CURRENTLY ~100)
Instrument Size (m) ~3 – 10 (SATELLITE TV DISHES)
Search Frequency (MHz) 1420 – 1720
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) ALL SKY
Flux Limit (W m-2) 10-21
Total Hours ONGOING
Reference SETI League Project Argus. <http://www.setileague.org>
Link
Comments Plan to organize up to 5000 radio amateurs to provide continuous sky coverage for strong, transient signals using systems that can be bought and built by individuals. SETI League currently has 1257 members running 105 sites in 19 countries.
Date 1996
Observer(s) BIRAUD AND AIRIEAU
Site NANÇAY OBSERVATORY
Instrument Size (m) 40 x 240
Search Frequency (MHz) 1419.7 – 1420.3, 1657.8 – 1662.2
Search Wavelength (nm)
Frequency Resolution (Hz) 50
Other Resolution
Objects (Hz) 4 STARS WITH GIANT PLANETS (51 Peg, 47 UMa, 70 Vir, Gl 229)
Flux Limit (W m-2) 10-24
Total Hours 40
Reference
Link
Comments Search of newly discovered extrasolar planetary systems using observing protocol from Biraud and Tarter 1981-1988 SETI program at Nançay.
Date 1996
Observer(s) LOCKETT, BLAIR & ZADNIK
Site PERTH OPTICAL OBSERVATORY
Instrument Size (m) 1
Search Frequency (MHz)
Search Wavelength (nm) 572
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 24 NEARBY STARS
Flux Limit (W m-2)
Total Hours
Reference
Link
Comments Search for microsecond laser pulses.
Date 1996 – 1998
Observer(s) SETI INSTITUTE PROJECT PHOENIX
Site NRAO AND WOODBURY, GA
Instrument Size (m) 43, 30
Search Frequency (MHz) 1200 – 3000 DUAL POL
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 195 STARS
Flux Limit (W m-2) 1.3 x 10-25
Total Hours 4200
Reference CULLERS, D.K., “Project Phoenix And Beyond” in Bioastronomy ‘99 – A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 451 (2000).
Link
Comments Longer observations provided same ensitivity as achieved Australia.
Date 1996 – 1998
Observer(s) TILGNER, HEINRICHSEN, KRUGER, PACHER, WALKER, WOLSTENCROFT
Site ISO (INFRARED SPACE OBSERVATORY) SATELLITE, ISOPHOT PHOTOPOLARIMETER
Instrument Size (m) 0.6
Search Frequency (MHz)
Search Wavelength (nm) 3000 – 100000
Frequency Resolution (Hz)
Other Resolution 0.2 MICRONS (3 MICRON FILTER BAND) 51 MICRONS (90 MICRON FILTER BAND)
Objects (Hz) 6 SOLAR-TYPE STARS AND 1 INFRARED-EXCESS TARGET STAR
Flux Limit (W m-2) 30 – 90 x 10-29 (S/N = 10)
Total Hours 1.3 HOURS (GUARANTEED SCHEDULE)
Reference Tilgner, C.N. and Heinrichsen, I., “A Program to Search for Dyson Spheres With the Infrared Space Observatory,” paper #IAA-95-IAA.9.1.11, IAF Congress, Oslo, Norway (October 1995).
Link
Comments Search for astro-engineering products like Dyson Spheres and rings by separation of their infrared spectra from that of the host star.
Date 1996 – 1998
Observer(s) Cullers, D.K.; SETI Institute Project Phoenix,
Site NRAO; Woodbury
Instrument Size (m) 43, 30
Search Frequency (MHz) 1200 – 3000 dual pol
Search Wavelength (nm)
Frequency Resolution (Hz) 0.7
Other Resolution
Objects (Hz) 195 stars
Flux Limit (W m-2) 1.3 x 10-25
Total Hours 4200
Reference Cullers, D.K., “Project Phoenix And Beyond,” Bioastronomy “˜99 “” A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 451 (2000).
Link http://adsabs.harvard.edu/full/2000ASPC..213..451
Comments Continuation for NASA HRMS targeted search of nearby stars, using real-time data
Date 1996 – ON
Observer(s) WERTHIMER ET AL. (SERENDIP IV)
Site ARECIBO
Instrument Size (m) 305
Search Frequency (MHz) 1370 – 1470
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) SURVEY OF 30% OF SKY VISIBLE FROM ARECIBO
Flux Limit (W m-2) 5 x10-24
Total Hours ONGOING
Reference Werthimer, D., Bowyer, S., Ng, D., Donnelly, C., Cobb, J., Lampton, M., and Airieau, S., “The Berkeley SETI Program: SERENDIP IV Instrumentation.” Poster paper #P4-20 presented at 5th International Conference on Bioastronomy, IAU Colloquium No. 161, Capri, Italy (July 1-5, 1996).
Link
Comments Commensal search occurring at twice sidereal rate in backwards direction while radio astronomers track targets using Gregorian system.
Date 1997 (A), 1999 (B)
Observer(s) BAMBI (BOB AND MIKE’S BIG INVESTMENT), SARA (SOCIETY OF AMATEUR RADIO ASTRONOMERS) MEMBERS
Site A IN CALIFORNIA, B IN COLORADO
Instrument Size (m) 2.6 (A); 3 (B)
Search Frequency (MHz) 3700 – 4200
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) NORTHERN SKY SURVEY
Flux Limit (W m-2) NO FORMAL OBSERVING PROGRAM HAS YET BEGUN
Total Hours ONGOING
Reference Lash,R. and Fremont, M. “Up and running at 4 GHz: the SETI-capable Radio Telescope” in Radio Astronomy, the journal of the Society of Amateur Radio Astronomers, June/July 1994, pp1-6.
Link
Comments Amateur radio enthusiasts using TVRO components and software FFTs to try coordinated search.
Date 1997 – 2009
Observer(s) Cobb, Jeff; Lebofsky, M.; Werthimer, D.; Bowyer, S.; Lampton, M.; SERENDIP IV,
Site NAIC, Arecibo
Instrument Size (m) 305
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz) 20
Other Resolution
Objects (Hz) Sky Survey
Flux Limit (W m-2)
Total Hours
Reference Cobb, Jeff, Lebofsky, M., Werthimer, D., Bowyer, S., Lampton, M., “SERENDIP IV: Data Acquisition, Reduction, and Analysis,” Bioastronomy 99: A New Era in the Search for Life (2000).
Link http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?2000ASPC..213..485C&data_type=PDF_HIGH&whole_paper=YES&type=PRINTER&filetype=.pdf
Comments Pigyback search from upgraded Gregorian feed platform at Arecibo Observatory, similar to previous versions of SERENDIP. It ran with around the clock observation. 40 spectrum analysis/post-processing boards worked at the same time. The calculated power spectra was normalized with an 8000 channel boxcar. Every five seconds, the telescope’s pointing coordinates were taken. The spectra was calculated and the normal slew rates were passed on. Any RFI was removed. Algorithms detected signal patterns, persistence, pulsing, and high-power events. SERENDIP IV looked for persistence in frequency over time. Candidates were reobserved.
Date 1997 (A), 2000 (B), 2004 (C)
Observer(s) Jugaku and Nishimura
Site Archival from IRAS
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm) 2200 – 12000
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) (A) 50 stars
(B) 135 stars
(C) 19 stars
Flux Limit (W m-2)
Total Hours
Reference (A) Jugaku and Nishimura 1997 at the IAU Colloquium 161
(B) Jugaku and Nishimura 2000 in Bioastronomy 1999
(C) Jugaku and Nishimura 2004 in Bioastronomy 2002
Link (A) http://adsabs.harvard.edu/abs/1997abos.conf..707
(B) http://adsabs.harvard.edu/full/2000ASPC..213..581
(C) http://adsabs.harvard.edu/abs/2004IAUS..213..437
Comments Search for 12 µ excess radiation from IRAS catalog stars by using K-[12] color index in attempt to find Dyson Spheres.
Date 1998 – 2002
Observer(s) MARCY, REINES, BUTLER, VOGT
Site LICK, KECK
Instrument Size (m) 10
Search Frequency (MHz)
Search Wavelength (nm) 400 – 500
Frequency Resolution (Hz)
Other Resolution λ/Δλ = 50000
Objects (Hz) 600 FGK STARS WITHIN 100 pc
Flux Limit (W m-2) 1 x 10-13
Total Hours 500
Reference Butler, R.P., Marcy, G. W., Williams, E., McCarthy, C., Dosanjh, P., Vogt, S. S “Attaining Doppler Precision of 3 meters/sec,” PASP v.108, p.500
Link
Comments Search through archival data for narrowband continuous optical laser emission lines.
Date 1998 – 2004
Observer(s) SETI INSTITUTE PROJECT PHOENIX
Site ARECIBO OBSERVATORY AND LOVELL TELESCOPE AT JODRELL BANK
Instrument Size (m) 305, 76
Search Frequency (MHz) 1200 TO 3000 DUAL POL
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 1000 NEARBY STARS (500 OBSERVED TO DATE)
Flux Limit (W m-2) 1 x 10-26
Total Hours 1300 HOURS TO DATE
Reference SHOSTAK, S. and TARTER, J. “Project Phoenix Enters Adulthood,” paper #IAA-99-IAA.9.1.01, IAF Congress, Amsterdam, The Netherlands (October 1999).
Link
Comments Continuation of NASA HRMS targeted search of 1000 nearby stars, using real-time data reduction and a pair of widely separated observatories to help discriminate against RFI.
Date 1998 – 2005
Observer(s) HOROWITZ ET AL. (HARVARD OPTICAL SETI)
Site OAK RIDGE OBSERVATORY
Instrument Size (m) 1.5
Search Frequency (MHz)
Search Wavelength (nm) 350 – 700
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 13000 SOLAR-TYPE STARS OF WHICH 4000 OBSERVED TO DATE
Flux Limit (W m-2) 4 x 10-9 PEAK IN < 5 ns PULSE, OR 4 x 10-20 AVERAGE PER 500 SECOND OBSERVATION
Total Hours ONGOING
Reference HOWARD, A., ET AL., “Optical SETI at Harvard-Smithsonian” in Bioastronomy ‘99 – A New Era in Bioastronomy,Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 545 (2000)
Link
Comments Search for nanosecond laser pulses, with hybrid avalanche photodiodes in coincidence. Piggybacks on nightly searches for extrasolar planets. Soon to be operated in coincidence with cloned detector on 0.9 m telescope at Princeton.
Date 1998 – 2010
Observer(s) WERTHIMER
Site LEUSCHNER OBSERVATORY
Instrument Size (m) 0.8
Search Frequency (MHz)
Search Wavelength (nm) 300 – 650
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 800 SOLAR-TYPE STARS
Flux Limit (W m-2) 1.5 x 10-9 PEAK DURING 1ns PULSE, OR 1.5 x 10-20 AVERAGE PER 100 SECOND OBSERVATION
Total Hours 200 (ONGOING)
Reference LAMPTON, M., “Optical SETI: The Next Search Frontier” in Bioastronomy ‘99 – A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 565 (2000)
Link
Comments First optical search to use two high time resolution photomultiplier tubes in coincidence to look for nanosecond pulses.
Date 1998 – ON
Observer(s) SETI AUSTRALIA SOUTHERN SERENDIP
Site PARKES
Instrument Size (m) 64
Search Frequency (MHz) 1411.59 – 1429.23
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) SOUTHERN SKY SURVEY
Flux Limit (W m-2) 4 x 10-24
Total Hours ONGOING
Reference STOOTMAN, F. ET AL., “The Southern SERENDIP Project” in Bioastronomy ‘99 – A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 491 (2000).
Link
Comments Comensal search that uses 2 out of 13 beams of Parkes focal plane anrray to discriminate against RFI.
Date 1999 – ON
Observer(s) WERTHIMER AND ANDERSON (SETI@HOME)
Site ARECIBO
Instrument Size (m) 305
Search Frequency (MHz) 1419.16 – 1421.66
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) DATA TAKEN FROM SERENDIP IV – SKY VISIBLE FROM ARECIBO
Flux Limit (W m-2) 5 x 10-25
Total Hours ONGOING
Reference ANDERSON, D. “Internet Computing for SETI” in Bioastronomy ‘99 – A New Era in Bioastronomy, Proceedings of a Conference held on the Kohala Coast, Hawaii, 2-6 Aug. 1999, ASP Conference Series 213, p. 511 (2000).
Link
Comments Hugely successful experiment in distributed computing. Permits more sophisticated processing of a fraction of SERENDIP IV data by harnessing idle CPU cycles of 3 million personal and corporate computers.
Date 2000 – 2005
Observer(s) Howard, Andrew; Horowitz, P.; Coldwell, C.; Klein, S.; Sung, A.; Wolff, J.; Caruso, J.; Latham, D.; Papaliolios C., ; Stefanik, R.; Zajac, J.; Harvard OSETI Targeted Search,
Site Oak Ridge Observatory
Instrument Size (m) 1.5
Search Frequency (MHz)
Search Wavelength (nm) 350 – 720
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) ~11,000 F, G, and K dwarfs.
Flux Limit (W m-2) 100 photons/m2
Total Hours 2378
Reference Howard, A.W.; Horowitz, P.; Wilkinson, D.T.; Coldwell, C.M.; Groth, E.J.; Jarosik, N.; Latham, D.W.; Stefanik, R.P.; Willman, A.J. Jr.; Wolff, J.; Zajac, J.M., “Search for Nanosecond Optical Pulses from Nearby Solar-Type Stars,” The Astrophysical Journal, Vol. 613, Issue 2, pg. 1270-1284 (2004).
Link ***http://iopscience.iop.org/0004-637X/613/2/1270/pdf/60101.web.pdf***
Comments A beamsplitter follwed by a pair of fast hybrid avalanche detectors is triggered in coincidence to record the time and intensity profile of large pulses. In 2001 this search partnered with Princeton to create the Harvard-Princeton OSETI collaborated search for some time. However, Harvard Targeted OSETI continued to observe throughout and afterwards.
Date 2000 – 2010
Observer(s) MONTEBUGNOLI (SETItalia)
Site MEDICINA
Instrument Size (m) 32
Search Frequency (MHz) 1415 – 1425, 4255 – 4265
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz) NORTHERN SKY
Flux Limit (W m-2)
Total Hours ONGOING
Reference MONTEBUGNOLI, S. <http://www-radiotelescopio.bo.cnr.it/setiweb/home.htm>
Link
Comments Commensal sky survey using Medicina telescope and SERENDIP signal processing boards.
Date 2000 – ON
Observer(s) BHATHAL AND DARCY
Site CAMPBELLTOWN ROTARY OBSERVATORY, OZ OSETI
Instrument Size (m) 0.4, 0.3
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 200 SOLAR-TYPE STARS AND 25 GLOBULAR CLUSTERS
Flux Limit (W m-2) 6 x 10-9 PEAK DURING 1ns PULSE
Total Hours ONGOING
Reference Bhatal, R. <http://www.coseti.org/ragbir00.htm>
Link
Comments Dedicated telescope built for SETI. Uses high time resolution photodiodes in coincidence to search for laser pulses, and coincidence between two telescopes separated by 20 m to bring down false alarm rate. Soon to be teamed with microwave search of same objects.
Date 2001
Observer(s) Werthimer, Dan; SEVENDIP,
Site Leuschener Observatory
Instrument Size (m) 0.76
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 2500 nearby stars + globular clusters and nearby galaxies
Flux Limit (W m-2)
Total Hours
Reference Werthimer, Dan, Anderson, David, Bowyer, Stuart, Cobb, Jeff, Demorest, Paul, “Searching for ET with Help from Three Million Volunteers: The SETI@home, Serendip, Sevendip and Spock SETI Programs,” IAF abstracts, 34th COSPAR Scientific Assembly, The Second World Space Congress, held 10-19 October, 2002 in Houston, TX, USA. (2002).
Link ***2002iaf..confE.365W***
Comments A search for nanosecond optical laser pulses using 3 PMTs in coincidence to reudce false positive rates. Running since 2001.
Date 2001 – ON
Observer(s) DRAKE ET AL., LICK OPTICAL SETI
Site LICK OBSERVATORY, UC SANTA CRUZ
Instrument Size (m) 1 (NICKEL REFLECTOR)
Search Frequency (MHz)
Search Wavelength (nm) 550
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 5039 SOLAR-TYPE STARS PLANNED
Flux Limit (W m-2) 1 x 10-9 PEAK DURING 1 ns PULSE, OR 1 x 10-20 AVERAGE PER 100 SECOND OBSERVATION
Total Hours SUSPENDED IN SPRING 1999
Reference DRAKE, ET AL., Lick Optical SETI <http://seti.ucolick.org/optical>
Link
Comments Uses three photodiodes in coincidence to eliminate background events.
Date 2002
Observer(s) Amy E. Reines and Geoffrey W. Marcy
Site Keck-I/HIRES
Instrument Size (m) 10
Search Frequency (MHz)
Search Wavelength (nm) 400 – 500
Frequency Resolution (Hz)
Other Resolution λ/Δλ = 70000
Objects (Hz) 577 F, G, K, and M stars
Flux Limit (W m-2) 3.4 x 10-17
Total Hours Not specified, used 4 years of data with ~20 spectra per star
Reference Reines A. and Marcy G. 2002 PASP 114 416
Link http://iopscience.iop.org/article/10.1086/342496/meta
Comments Search for emission lines having widths too narrow to be natural from the host star, as well as for lines broadened by astrophysical mechanisms
Date 2002 – 2004
Observer(s) Blair, David G.; Zadnik, Marjan G.
Site Perth-Lowell Telescope
Instrument Size (m) 0.61
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz) 1
Other Resolution
Objects (Hz) 60 solar-type stars
Flux Limit (W m-2) ~1 mJy
Total Hours
Reference Blair, David G., Zadnik, Marjan G., “A Search for Optical Beacons: Implications of Null Results,” Astrobiology, Volume 2, Issue 3, pp. 305-312 (2002).
Link
Comments Search for optical beacons in the vicinity of 60 solar-type stars with null results.
Date 2002
Observer(s) Werthimer, Dan; Anderson, David; Bowyer, Stuart; Cobb, Jeff; Demorest, Paul; SPOCK,
Site Leuschener Observatory
Instrument Size (m) 0.76
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz)
Flux Limit (W m-2)
Total Hours
Reference Werthimer, Dan, Anderson, David, Bowyer, Stuart, Cobb, Jeff, Demorest, Paul, “Searching for ET with Help from Three Million Volunteers: The SETI@Home, Serendip, Sevendip and Spock SETI Programs,” IAF abstracts, 34th COSPAR Scientific Assembly, The Second World Space Congress, held 10-19 October, 2002 in Houston, TX, USA., p.IAA-9-1-09IAF abstracts, 34th COSPAR Scientific Assembly, The Second World Space Congress, held 10-19 October, 2002 in Houston, TX, USA., p.IAA-9-1-09, meeting abstract (2002).
Link ***2002iaf..confE.365W***
Comments Using optical spectra accquired at Keck as part of a planet search run by Marcy, Et al., SPOCK searches for narrow-band continuous signals.
Date 2004
Observer(s) Conroy, Charlie; Werthimer, Dan; Dyson Sphere Search ,
Site Leuschner Observatory; optical SETI pulse search; Serendip IV; SETI@home
Instrument Size (m) 0.76
Search Frequency (MHz) 1420
Search Wavelength (nm) 390 – 700
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 32 stars from IRAS and 2MASS catalog
Flux Limit (W m-2) ~3 sigma above mean
Total Hours
Reference Conroy, Charlie, Werthimer, Dan, “Optical and Radio Searches on Dyson Sphere Candidates” preprint; personal communication.
Link
Comments A search for advanced civilizations exploiting Dyson Sphere type technology, that is the employment of shells around stars to extract solar energy. Partial Dyson Spheres are theorized to radiate waste heat. The infrared excess is gone by 60 micrometers, indicating that the excess is intrinsic to the system and not to systematic error. 33 Dyson Sphere candidates with excess 12 micron radiation no 60 micron excess ages greater than a gigayear were observed for SETI signals with the Leuschner Optical Telescope, SERENDIP IV at Arecibo and the SETI@home program. Stars were observed with measured ages of above 109 years, such that there is no protoplanetary disk, a known source of infrared radiation. This search is significant enough to warrant further investigation. [Data were taken with OSETI pulse detection system at Leuschner, and SERENDIP IV and SETI@home systems at Arecibo Observatory]
Date 2004-2009
Observer(s) Narusawa
Site NAYUTA telescope at Nishi-Harima Astronomical Observatory (NHAO)
Instrument Size (m) 2
Search Frequency (MHz)
Search Wavelength (nm) 487 – 577
Frequency Resolution (Hz)
Other Resolution 0.6 Angstrom
Objects (Hz) 13 F, G, K, M stars
Flux Limit (W m-2) 1016 W
Total Hours 56 nights
Reference
Link https://ndlonline.ndl.go.jp/#!/detail/R300000004-I10487843-00
http://www.nhao.jp/research/annual_report/docs/ar2007-1.pdf
http://www.nhao.jp/research/annual_report/docs/ar2011-1.pdf
Comments Search for ns pulses
Date 2005
Observer(s) Holder et. al.
Site VERITAS (Whipple)
Instrument Size (m) 10
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution Temporal resolution: a few ns
Objects (Hz) HIP 107395
Flux Limit (W m-2) 10 photons m-2
Total Hours 0.467
Reference Holder et. al 2015
Link https://arxiv.org/abs/astro-ph/0506758
Comments A search for optical pulses
Date 2005
Observer(s) Stone, R.P.S.; Wright, S.A.; Drake, F.; Munoz, M; Treffers, R.; Werthimer, Dan
Site Lick Observatory
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 4,605 stars of spectral types F and M within 200 light-years of Earth
Flux Limit (W m-2)
Total Hours 4.5
Reference Stone, P.R.S., Wright, S.A., Drake, F., Munoz, M., Treffers, R., Werthimer, Dan, “Lick Observatory Optical SETI: Targeted Search and New Directions,” Astrobiology, Volume 5, Issue 5, pp. 604-611 (2005).
Link
Comments Lick Observatory’s Optical SETI. They observed 14 candidate signals (“triple coincidences”), all but one of which are explained by transient local difficulties. Additional observations of the remaining cadidate have failed to confirm arriving pulse events.
Date 2006 – 2010
Observer(s) Montebugnoli, S.; Bortolotti, C.; Cattani, A.; Maccaferri, A.; Orlati, A.; Poloni, M.; Poppi, S.; Monari, J.; Roma, M.; Pari, P. P.; Teodorani, M.; Righini, S.; Maccone, C.; Caliendo, D.; Cosmovici, C. B.; D’Amico, N.; SETI-Italia,
Site Medicina
Instrument Size (m) 32
Search Frequency (MHz) 1400 – 23500
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) Target stars
Flux Limit (W m-2)
Total Hours
Reference Montebugnoli, S.; Bortolotti, C.; Cattani, A.; Maccaferri, A.; Orlati, A.; Poloni, M.; Poppi, S.; Monari, J.; Roma, M.; Pari, P. P.; Teodorani, M.; Righini, S.; Maccone, C.; Caliendo, D.; Cosmovici, C. B.; D’Amico, N., “SETI-Italia 2003 status report and first results of a KL transform algorithm for ETI signal detection,” Acta Astronautica, Volume 58, Issue 4, p. 222-229 (2006).
Link http://setiitalia.altervista.org/
Comments Ongoing since early 1998, SETI-Italia is the only continuous European SETI endeavor, and is run by the Instituto di Radioastronomia. Unlike other SETI programs, it uses the KLT, not the FFT.
Date 2006 – 2015
Observer(s) Howard, Andrew; Horowitz, Paul; Mead, Curtis; Sreetharan, Pratheev; Gallicchio, Jason; Howard, Steve; Coldwell, Charles; Zajac, Joe; Sliski, Alan; Harvard OSETI Survey,
Site Oak Ridge Observatory
Instrument Size (m) 1.8
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) Survey of 80% of the sky
Flux Limit (W m-2) 10 photons per square meter per nanosecond
Total Hours 150
Reference Howard, Andrew; Horowitz, Paul; Mead, Curtis; Sreetharan, Pratheev; Gallicchio, Jason; Howard, Steve; Coldwell, Charles; Zajac, Joe; Sliski, Alan “Initial results from Harvard all-sky optical SETI” Acta Astronautica, Volume 61, Issue 1-6, p. 78-87, 06/2007.
Link
Comments
Date 2006 – 2010
Observer(s) Von Korff, J.; Demorest, P.; Heien, E.; Korpela, E.; Werthimer, D.; Cobb, J.; Lebofsky, M.; Anderson, D.; Bankay, B.; Siemion, A.
Site Arecibo
Instrument Size (m)
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 452 pulsars
Flux Limit (W m-2)
Total Hours 21600
Reference
Link http://adsabs.harvard.edu/abs/2013ApJ…767…40
Comments
Date 2007
Observer(s) Rampadarath, Hayden
Site Long Baseline Array; 64-m Parkes antenna of Australia Telescope National Facility (ATNF); ATNF Australia Telescope Compact Array; ATNF Mopra
Instrument Size (m)
Search Frequency (MHz) 1262, 1312, 1362, 1412, 1462, 1512
Search Wavelength (nm)
Frequency Resolution (Hz) 1953
Other Resolution
Objects (Hz) Gliese 581
Flux Limit (W m-2) 7 MW/Hz
Total Hours 8
Reference
Link http://adsabs.harvard.edu/abs/2014PhDT…….255
Comments
Date 2007 – 2010
Observer(s) Harp, G.R.; Backus, P.R.; Kilsdonk, T.N.; Jordan, J.C.; Tarter, J.C.
Site Allen Telescope Array
Instrument Size (m) 6.1 (42 antennas)
Search Frequency (MHz) 1400 – 1700, 2800 – 3400
Search Wavelength (nm)
Frequency Resolution (Hz) 0.7
Other Resolution
Objects (Hz) HabCat stars that could host habitable planets
Flux Limit (W m-2) 100 Jy
Total Hours 95.795
Reference (1.) Harp, Backus, Kilsdonk, Jordan, and Tarter, “Recent SETI Results with Observations at the ATA” Astrobiology Science Conference 2010: No. 1538, p.5558. (2.) Peter R. Backus, Jill C. Tarter, Gerry R. Harp, John Dreher, Jane Jordan, Ken Smolek, Tom Kilsdonk, John Ross, Jon Richards, Rob Ackermann, Samantha Blair, et al “SETI Observations of Exoplanets with the Allen Telescope Array: First Results” (Private Communication – unpublished as of yet…)
Link
Comments The HabCat search uses algorithms for narrow band sine waves and simple pulses. Two times the frequency of the Waterhole (1.4- 1.7 GHz)is a “magic frequency” search which starts with the frequencies of Hydrogen and Hydroxyl multiplied by a “magic” number
Date 2007 – 2015
Observer(s) Von Korff, J.; Siemion, A.; Korpela, E.; Werthimer, D.; McMahon, P.; Cobb, J.; Lebofsky, M.; Anderson, D.; Bankay, B.; Bower, G.; Foster, G.; van Leeuwen, J.; Mallard, W.; Wagner, M.; Astropulse,
Site NAIC, Arecibo
Instrument Size (m) 305
Search Frequency (MHz) 2.5
Search Wavelength (nm)
Frequency Resolution (Hz) 0.075
Other Resolution
Objects (Hz) Microsecond- millisecond radio pulses. Sensitive sky survey.
Flux Limit (W m-2) 60 x 10-26 J/m2
Total Hours
Reference Von Korff, J., Siemion, A., Korpela, E., Werthimer, D., McMahon, P., Cobb, J., Lebofsky, M., Aanderson, D., Bankay, B., Bower, G., Foster, G., Van Leeuwen, J., Mallard, W., Wagner, M., “New SETI Sky Surverys for Radio Pulses” eprint arXiv:0811.3046 (2008).
Link ***http://arxiv.org/PS_cache/arxiv/pdf/0811/0811.3046v2.pdf***
***http://www.seti.org/seti-institute/project/details/seti-ata-galactic-center-survey***
Comments Sources for the pulses may include black holes, neutron stars, cosmic strings, or ETI. Data from the 7 beam ALFA receiver at Arecibo is reduced by a distributed computing application that uses a coherent de-dispersion technique to look for short broad-pulses. The multibeam data is sent over the internet to the computers of millions of volunteers to be analyzed.
Date 2008
Observer(s) Von Korff, J.; Siemion, A.; Korpela, E.; Werthimer, D.; McMahon, P.; Cobb, J.; Lebofsky, M.; Anderson, D.; Bankay, B.; Bower, G.; Foster, G.; van Leeuwen, J.; Mallard, W.; Wagner, M.; Fly’s Eye,
Site Allen Telescope Array
Instrument Size (m) 6.1 (42 antennas)
Search Frequency (MHz) 210
Search Wavelength (nm)
Frequency Resolution (Hz) 1600
Other Resolution
Objects (Hz) Microsecond-millisecond radio pulses in 100 square degree field
Flux Limit (W m-2) 60 x 10-26 J/m2
Total Hours 450
Reference Von Korff, J., Siemion, A., Korpela, E., Werthimer, D., McMahon, P., Cobb, J., Lebofsky, M., Aanderson, D., Bankay, B., Bower, G., Foster, G., Van Leeuwen, J., Mallard, W., Wagner, M., “New SETI Sky Surveys for Radio Pulses” eprint arXiv:0811.3046 (2008).
Link ***http://arxiv.org/PS_cache/arxiv/pdf/0811/0811.3046v2.pdf***
Comments Sources for these pulses may include black holes, neutron stars, cosmic strings, or ETI. Each antenna points in a different direction. So far three pulsars (B0329+54, B0355+54, B0950+08) and six giant pulses from the Crab pulsar have been found.
Date 2009
Observer(s) Richard A. Carrigan Jr
Site Archival from IRAS
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm) 12000, 25000, 60000
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 1527 sources
Flux Limit (W m-2)
Total Hours
Reference Carrigan 2009 ApJ 698 2
Link http://iopscience.iop.org/article/10.1088/0004-637X/698/2/2075
Comments A search for Dyson spheres (IR excess) in IRAS
Date 2009
Observer(s) Narusawa, S.; Fujishita, M.; Inoue, Takeshi; Morimoto, Masaki; Team SAZANAKA,
Site Yamaguchi Univ.; Wakayama Univ./Misato Obs.; Takahasi Obs.; Kagami Obs.; Matsuo Obs.; Nishi-Harima Astro. Obs. Tokai Univ., Agawa Jovian Radio Obs. of Kochi College of Technology
Instrument Size (m) 13 radio telescopes (some with 2 antennas) (1.3, 2, 11, 5, 32, 8, 6, 1), 26 optical telescopes. Including 2 m Nayuta. 11m & 5m, 32m, 8m, 6m, Yagi antenna & Discone antenna, 1m & Dipole antenna, Log periodic antenna, Dipole & Yagi antenna.
Search Frequency (MHz) Yamaguchi and Wakayama- 8300 MHz, Takahashi- 1420 MHz, Kagami- 1420 and 31 MHz, Matsuo- 1420 and 38.2 MHz, Kochi- 30-35 and 38.2 MHz, Nishi-Harima- 38.0 and 22.0 MHz
Search Wavelength (nm)
Frequency Resolution (Hz) 0.05
Other Resolution
Objects (Hz) 30 arc-minute field of the Cassiopia constellation
Flux Limit (W m-2) 3.21 x 10-14
Total Hours 5
Reference Narusawa and Fujishita, Astrobiology Science Conferecne 2010 (2010) Narusawa, Shin-ya, Fujishita, Mitsumi, Inoue, Takeshi, Morimoto, Masaki, “Project SAZANKA,” (2009). http://www.nhao.jp/%7Enarusawa/oseti/project-sazanka.html
Link ***http://adsabs.harvard.edu/cgi-bin/nphdata_query?bibcode=2010LPICo1538.5074N&link_type=ARTICLE&db_key=AST&high=***
***2010LPICo1538.5074***
Comments It is thought that a narrow carrier signal is the most possible kind of signal from an Extra-Terrestrial Intelligence (ETI), because it needs only one parameter “frequency”. Therefore, it may be a possibility that other types of signals are used to inform their existence. For example, an Ultra-Wide Band (UWB) signal is one of the possible signals, because generally it is advantageous on the standpoint of signal to noise ratio as shown by the Global Positioning System. We carried out multisite and multi-frequency SETI observations based on similar idea. We also did the multi-site optical monitoring observations simultaneously. If radio antennas detect the candidate signals, we check these optical (CCD, Digital camera and Video) images. It gives a clue of clarification of radio events {e.g. natural phenomenon (flare of surface of the star, nova, GRB, meteor, microlens etc.), artificial signals (aircraft, artificial satellite, reflection off space debris etc.) and ETI}. This is the world’s first multi-site and multi-wavelength simultaneous SETI observation with 12 radio and 26 optical systems in Japan. World’s first multi-site and multi-wavelength simultaneous SETI observation. Detected radio signals were checked by optical images. Strategy: UWB signals may be used by ETI as narrow carrier signals have not yet yielded information. Data under reduction. No radio or optical candidate signals were detected.
Date 2009 – 2015
Observer(s) Harp et. al.
Site Allen Telescope Array
Instrument Size (m) 6.1 (42 antennas)
Search Frequency (MHz) 1000 – 9000
Search Wavelength (nm)
Frequency Resolution (Hz) 0.7
Other Resolution
Objects (Hz) 9293 stars
Flux Limit (W m-2) 1.8 – 3.1 x 10-26
Total Hours 19000
Reference Harp et. al. 2016 AJ 152 6
Link http://iopscience.iop.org/article/10.3847/0004-6256/152/6/181
Comments A search for narrowband radio signals from 9293 stars, including 2015 exoplanet stars and Kepler objects of interest and an additional 65 whose planets may be close to their habitable zones.
Date 2009
Observer(s) Hanna et al.
Site Solar Tower Atmospheric Cherenkov Effect Experiment (STACEE)
Instrument Size (m) 64 heliostats, 37m2 area
Search Frequency (MHz)
Search Wavelength (nm) 420
Frequency Resolution (Hz)
Other Resolution Temporal resolution: 12 ns
Objects (Hz) 187 stars
Flux Limit (W m-2) 10 photons m-2
Total Hours 31.17
Reference Hanna et. al. 2009
Link https://www.liebertpub.com/doi/abs/10.1089/ast.2008.0256
Comments A search for fast blue-green laser pulses
Date 2009 – 2015
Observer(s) Siemion, A.; Werthimer, D.; Chen, H.; Cobb, J.; Filiba, T.; Fries, A.; Howard, A.; Korpela, E.; Lebofsky, M.; Mallard, W.; Spitler, L.; Wagner, M.
Site NAIC, Arecibo; Leuschner Observatory
Instrument Size (m) 305, 0.762
Search Frequency (MHz) 1420
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) Multiple search strategies
Flux Limit (W m-2)
Total Hours
Reference Siemion, A., Werthimer, D., Chen, H., Cobb, J., Filiba, T., Fries, A., Howard, A., Korpela, E., Lebofsky, M., Mallard, W., Spitler, L., Wagner, M.. “Current and Nascent SETI Intruments in the Radio and Optical: SERENDIP V. v, OSPOSH and HRSS,” Astrobiology Conference 2010: Evolution and Life: Surviving Catastrophes and Extremes on Earth and Beyond, held April 20-26 2010 in League City, Texas. LPI Contribution No. 1538, p. 5378 (2010).
Link http://www.lpi.usra.edu/meetings/abscicon2010/pdf/5378.pdf
Comments This article describe ongoing efforts to develop high-performance and sensitive information to be used in SETI searches. These efforts are SERENDIP V.v, HRSS (Heterogenous Radio SETI Spectrometer) and OSPOSH (Open Sourse Pulsed Optical SETI Hardware). SERENDIP V.v uses an FPGA (field programmable gate array) based spectrometer. It looks for narrow-band signals and observes 2 billion channels acorss seven 3 arc-minute beams. OSPOSH looks for nanosecond scale light pulses that are not known to occur naturally. HRSS uses a high-speed analog-to-digital converter along with an FPGA. It digitizes, packets, and transmits CPUs and GPUs (graphic processing units) for spectroscopy. It will be available to researchers and students around the world.
Date 2010-2013
Observer(s) Project Dorothy
Site 29 institutions world wide
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz)
Flux Limit (W m-2)
Total Hours 29 nights
Reference
Link http://www.nhao.jp/~narusawa/oseti/project-dorothy.html
Comments Multifrequency search for artificial signatures
Date 2010
Observer(s) Montebugnoli, S.; Bartolini, M.; Bianchi, G.; Cosmovici, C.; Monari, J.; Orlati, A.; Perini, F.; Pluchino, S.; Pupillo, G.; Salerno, E.; Schillirò, F.; Zoni, L.
Site Medicina Radioastronomical Station
Instrument Size (m) 32
Search Frequency (MHz) 1400 – 22000
Search Wavelength (nm)
Frequency Resolution (Hz) 0.6
Other Resolution
Objects (Hz)
Flux Limit (W m-2)
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2010AcAau..67.1350
Comments
Date 2010
Observer(s) Williams, Peter K. G.; Bower, G. C.; Allen Telescope Array Team
Site Allen Telescope Array
Instrument Size (m) 6.1 (42 antennas)
Search Frequency (MHz) 1430, 2010
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) Galactic Center
Flux Limit (W m-2)
Total Hours Typically 3 hours per night / running ~4 nights per week for over six months
Reference
Link http://adsabs.harvard.edu/abs/2010AAS…21540303
Comments ATA Galactic Center Survey
Date 2010 – 2011
Observer(s) Harp et. al.
Site Allen Telescope Array
Instrument Size (m) 6.1 (25 antennas)
Search Frequency (MHz) 1000 – 10000
Search Wavelength (nm)
Frequency Resolution (Hz) 7 x 106
Other Resolution
Objects (Hz) 243 sources including quasars, pulsars, supernova remnants, and masers
Flux Limit (W m-2) 6.3 – 11.2 x 10-22
Total Hours ~ 40.5 hours
Reference Harp et. al. 2015
Link https://arxiv.org/abs/1506.00055
Comments A search for artificial nonsinusoidal periodic signals
Date 2010 – 2011
Observer(s) Bonin, Samuel; Barott, W. C.; Catanach, T.
Site Allen Telescope Array
Instrument Size (m)
Search Frequency (MHz) 6700
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 53 targets
Flux Limit (W m-2)
Total Hours Short (10 min) and long (60 minute) observations
Reference
Link http://adsabs.harvard.edu/abs/2012AAS…22052302
Comments
Date 2011
Observer(s) Siemion, Andrew P. V.; Demorest, Paul; Korpela, Eric; Maddalena, Ron J.; Werthimer, Dan; Cobb, Jeff; Howard, Andrew W.; Langston, Glen; Lebofsky, Matt; Marcy, Geoffrey W.; Tarter, Jill
Site Green Bank Telescope
Instrument Size (m)
Search Frequency (MHz) 1100, 1900
Search Wavelength (nm)
Frequency Resolution (Hz) 5
Other Resolution
Objects (Hz) 86 KOIs in Kepler field
Flux Limit (W m-2) 2 × 10-23 erg s^-1 cm-2
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2013ApJ…767…94
Comments
Date 2011
Observer(s) Davies, P.C.W.; Wagner, R.V.
Site Archival from Lunar Reconnaissance Orbiter
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution 5 meters
Objects (Hz) lunar surface
Flux Limit (W m-2)
Total Hours
Reference
Link https://www.sciencedirect.com/science/article/pii/S0094576511003249?via%3Dihu
Comments Search for artifacts on Moon
Date 2011 – ON
Observer(s) SETI Team at the SETI Institute
Site ATA
Instrument Size (m) array is equivalent in area to single dish 39m in diameter
Search Frequency (MHz) 1 x 109 – 10 x 109
Search Wavelength (nm)
Frequency Resolution (Hz) 0.7
Other Resolution
Objects (Hz) exoplanets
Flux Limit (W m-2) 80 Jy
Total Hours 13140
Reference
Link http://setiquest.info/data/obsreports
Comments observations made with 3 beamformers simultaneously. Total bandwidth per beam has increased from 20 MHz to 70 MHz due to the addition of more computers.
Date 2011
Observer(s) (1.) Siemion, Andrew P. V.; Demorest, Paul; Korpela, Eric; Maddalena, Ron J.; Werthimer, Dan; Cobb, Jeff; Howard, Andrew W.; Langston, Glen; Lebofsky, Matt; Marcy, Geoffrey W.; Tarter, Jill. (2.) Gautam, Abhimat Krishna; Siemion, Andrew; Korpela, Eric J.; Cobb, Jeff; Lebofsky, Matt; Werthimer, Dan
Site GBT
Instrument Size (m) 100
Search Frequency (MHz) 1100 – 1900
Search Wavelength (nm)
Frequency Resolution (Hz) 0.75
Other Resolution
Objects (Hz) 86 stars in the Kepler field including stars hosting candidates with 380 K > Teq > 230 K, stars with five or more detected candidates or stars with a super-Earth (Rp < 3 R⊕) in a >50 day orbit
Flux Limit (W m-2) 10 Jy
Total Hours 700
Reference (1.) Siemion, Andrew P. V.; Demorest, Paul; Korpela, Eric; Maddalena, Ron J.; Werthimer, Dan; Cobb, Jeff; Howard, Andrew W.; Langston, Glen; Lebofsky, Matt; Marcy, Geoffrey W.; Tarter, Jill “A 1.1-1.9 GHz SETI Survey of the Kepler Field. I. A Search for Narrow-band Emission from Select Targets” The Astrophysical Journal, Volume 767, Issue 1, article id. 94, 13 pp. (2013). (2.)Gautam, Abhimat Krishna; Siemion, Andrew; Korpela, Eric J.; Cobb, Jeff; Lebofsky, Matt; Werthimer, Dan “SETI Searches for Radio Transients from Kepler Field Planets and Astropulse Candidates” American Astronomical Society, AAS Meeting #224, #405.06, 06/2014.
Link ***http://iopscience.iop.org/0004-637X/767/1/94/pdf/apj_767_1_94.pdf
***2013ApJ…767…94S***
***2014AAS…22440506***
Comments (1.) The stars searched were chosen based on the properties of their putative exoplanets, including stars hosting candidates with 380 K > T eq > 230 K, stars with five or more detected candidates or stars with a super-Earth (R p < 3 R ⊕) in a >50 day orbit. It is estimated that fewer than ~1% of transiting exoplanet systems host technological civilizations that are radio loud in narrow-band emission between 1 and 2 GHz at an equivalent isotropically radiated power (EIRP) of ~1.5 × 1021 erg s-1, approximately eight times the peak EIRP of the Arecibo Planetary Radar, and we limit the number of 1-2 GHz narrow-band-radio-loud Kardashev type II civilizations in the Milky Way to be {<}10^{-6}\ M^{-1}_\odot. (2.)We present a search for fast radio transients in targeted observations of planet candidates in the Kepler Field and candidate Astropulse sources. Kepler Field observations were conducted in the band 1.1 and 1.9 GHz using the Green Bank Telescope in Green Bank, West Virginia and are centered on 86 stars hosting candidate planets identified by the Kepler spacecraft. These stars were chosen based on the properties of their putative planetary system thought to be conducive to the development of advanced life, including all systems known (as of May 2011) hosting a Kepler Object of Interest (KOI) with a calculated equilibrium temperature between 230 and 380 K, at least 4 KOIs or a KOI with an inferred radius < 3.0 r and a period > 50 d. The Kepler Field is centered at an intermediate galactic latitude, b = 13.5°, which presents an additional opportunity to detect signals from the older population of millisecond and recycled pulsars located above the galactic plane.
Date 2011
Observer(s) Narusawa, S.; Fujishita, M.; Team Sazanka
Site Japan – 12 radio and 26 optical systems
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 30 arc-minute field of the Cassiopeia constellations
Flux Limit (W m-2)
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2010LPICo1538.5074
Comments
Date 2013
Observer(s) Covault, Corbin
Site Scanning Observatory for Optical SETI (SOFOS)
Instrument Size (m) 3.5 x 3.5
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz)
Flux Limit (W m-2) 10 photons/m2
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2013APS..APR.S2002
Comments search for nanosecond light pulses
Date 2014
Observer(s) Tingay et. al.
Site Murchison Widefield Array
Instrument Size (m) 3000
Search Frequency (MHz) 103 – 133
Search Wavelength (nm)
Frequency Resolution (Hz) 10000
Other Resolution
Objects (Hz) 38 planetary systems towards the Galactic center
Flux Limit (W m-2) 4 – 5 x 10-23
Total Hours 115 minutes
Reference Tingay et. al. 2016 ApJ 827 2 L22
Link http://iopscience.iop.org/article/10.3847/2041-8205/827/2/L22
Comments
Date 2014
Observer(s) Michael Hippke, John G. Learned2, A. Zee3, William H. Edmondson4, John F. Lindner5,6, Behnam Kia6, William L. Ditto6, and Ian R. Stevens7
Site Archival from Kepler data
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) KIC 5520878
Flux Limit (W m-2)
Total Hours
Reference
Link http://iopscience.iop.org/article/10.1088/0004-637X/798/1/42/meta
Comments search for irregular variability in RR Lyrae star
Date 2014
Observer(s) Gautam, Abhimat Krishna; Siemion, Andrew; Korpela, Eric J.; Cobb, Jeff; Lebofsky, Matt; Werthimer, Dan
Site Green Bank Telescope; Arecibo ALFA
Instrument Size (m)
Search Frequency (MHz) 1100, 1900, 1214 – 1536
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 86 KOIs in Kepler field
Flux Limit (W m-2)
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2014AAS…22440506
Comments
Date 2014 – 2015
Observer(s) Robert H. Gray and Kunal Mooley
Site Jansky VLA
Instrument Size (m) 25 (27 antennas)
Search Frequency (MHz) 1450, 1640
Search Wavelength (nm)
Frequency Resolution (Hz) 1953, 122 Hz, 15 Hz
Other Resolution
Objects (Hz) M31 (Andromeda)
M33 (Triangulum)
Flux Limit (W m-2) 1.995 – 2.93 x 10-25
Total Hours 200 minutes:
8 observations for 20 minutes and 8 observations at 5 minutes
Reference Gray and Mooley 2017 AJ 153 3
Link http://iopscience.iop.org/article/10.3847/1538-3881/153/3/110
Comments Searched 70% of the waterhole for narrowband radio signals
Date 2014 – 2016
Observer(s) Wright et. al.
Site Archival from WISE
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm) 3400, 4600, 12000, 22000
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) ~ 10 5 galaxies
Flux Limit (W m-2)
Total Hours
Reference
Link http://adsabs.harvard.edu/abs/2014ApJ…792…26
Comments A search for waste-heat in the infrared
Date 2015
Observer(s) Schuetz et. al.
Site Boquete Optical SETI Observatory
Instrument Size (m) 0.5
Search Frequency (MHz)
Search Wavelength (nm) 350 – 600
Frequency Resolution (Hz)
Other Resolution Temporal resolution: 25 ns
Objects (Hz) KIC 8462852
Flux Limit (W m-2) 67 photons m-2
Total Hours < 6 hours
Reference Schuetz et. al. 2016 ApJ 825 1 L5
Link http://iopscience.iop.org/article/10.3847/2041-8205/825/1/L5
Comments A search for optical pulses from KIC 8462852
Date 2015
Observer(s) Harp et. al.
Site Allen Telescope Array
Instrument Size (m) 6.1 (42 antennas)
Search Frequency (MHz) 1000 – 10000
Search Wavelength (nm)
Frequency Resolution (Hz) 1, 100000
Other Resolution
Objects (Hz) KIC 8462852
Flux Limit (W m-2) 1.8 – 3 x 10-24, 10-20
Total Hours 95.26 hours
Reference Harp et. al. 2016 ApJ 825 2
Link http://iopscience.iop.org/article/10.3847/0004-637X/825/2/155
Comments A search for narrowband radio signals from KIC 8462852
Date 2015
Observer(s) Abeysekara et. al.
Site VERITAS
Instrument Size (m) 12
Search Frequency (MHz)
Search Wavelength (nm) 300 – 500
Frequency Resolution (Hz)
Other Resolution Temporal resolution: 1 ns
Objects (Hz) KIC 8462852
Flux Limit (W m-2) 1 photons m-2
Total Hours 526 minutes
Reference Abeysekara et. al. 2016 ApJ 818 2 L33
Link http://iopscience.iop.org/article/10.3847/2041-8205/818/2/L33
Comments A search for optical pulses from KIC 8462852
Date 2015
Observer(s) Zackrisson et. al.
Site Archival from SFI++
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm) 21 x 108
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) 1359 disk galaxies
Flux Limit (W m-2)
Total Hours
Reference Zackrisson et. al. 2015 ApJ 810 1
Link http://iopscience.iop.org/article/10.1088/0004-637X/810/1/23
Comments A search for Kardashev type III civilizations based on outliers from the Tully-Fisher relationship
Date 2015 – ON
Observer(s) Breakthrough Listen Team
Site Automated Planet Finder (Lick Observatory)
Green Bank Telescope
Parkes Telescope
Instrument Size (m) 2.4, 100, 64
Search Frequency (MHz) 300 – 100000, 1200 – 1500
Search Wavelength (nm) 374 – 950
Frequency Resolution (Hz) 3
Other Resolution λ/Δλ = 10 5, Temporal Resolution: 18 seconds
Objects (Hz) 1649 main sequence and giant stars
123 galaxies of varying morphology: spirals, ellipticals, dwarf spherioidals, and irregulars
Flux Limit (W m-2) > 1013 W at 1.1-1.9 GHz, 1.7 x 10-25
Total Hours Ongoing, 400 hours published
Reference Isaacson, H. et. al. 2017 PASP 129 975
Enriquez, E. et. al. 2017 ApJ 849 2
Link http://iopscience.iop.org/article/10.1088/1538-3873/aa5800
http://iopscience.iop.org/article/10.3847/1538-4357/aa8d1b
Comments Searches for both continuous narrow-band transmission over a very broad range of frequencies, and for optical and near infrared laser light
Date 2015 – ON
Observer(s) SETIBURST (ALFABURST/SERENDIP VI)
Site Arecibo L-band Feed Array (ALFA)
Green Bank Telescope
Instrument Size (m) 305100
Search Frequency (MHz) 1225 – 1525
Search Wavelength (nm)
Frequency Resolution (Hz) 1, 300 x106
Other Resolution
Objects (Hz) Northern Sky (AGES) and Galactic Plane (PALFA)
Flux Limit (W m-2) SERENDIP VI: 1 x 10-25
ALFABURST: 7.8 x 10-21
Total Hours ONGOING
Reference Chennamangalam et. al. 2017 ApJS 228 2
Foster et. al. 2018 MNRAS 474 3847
Link http://iopscience.iop.org/article/10.1086/498335
https://academic.oup.com/mnras/article/474/3/3847/4662633
Comments Looks at data from ALPHABURST (a search for pulsars and fast radio burst transients) and SERENDIP VI (search for narrowband signals)
Date 2015 (A), 2017 (B)
Observer(s) Nathaniel K. Tellis and Geoffrey W. Marcy
Site Keck-I/HIRES
Instrument Size (m) 10
Search Frequency (MHz)
Search Wavelength (nm) 364 – 789
Frequency Resolution (Hz)
Other Resolution λ/Δλ = 60000 (5.6 km/s)
Objects (Hz) (A) 2796 F, G, K and M stars
(B) 5600 F, G, K and M stars
Flux Limit (W m-2) (A) > 90 W and < 100 lightyears or > 1kW if < 1000 lightyears (B) > 3 kW – 13 MW (independent of distance)
Total Hours (A) Varying, SNR ~100-200
(B) Varying, decade worth of data
Reference (A) Tellis N. and Marcy G. 2015 PASP 127 540
(B) Tellis N. and Marcy G. 2017 AJ 153 6
Link (A) http://iopscience.iop.org/article/10.1086/681966
(B) http://iopscience.iop.org/article/10.3847/1538-3881/aa6d12
Comments Search for laser emission: extremely narrow emission lines that are monochromatic and coming from an unresolved point in space
Date 2016
Observer(s) Ermanno F. Borra and Eric Trottier
Site Archival from Sloan Digital Sky Survey spectra
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) Solar-type stars
Flux Limit (W m-2)
Total Hours
Reference
Link http://iopscience.iop.org/article/10.1088/1538-3873/128/969/114201/meta
Comments search for periodic spectral modulations
Date 2016 – ON
Observer(s) Gerald R. Harp/SETI Institue
Site Allen Telescope Array
Instrument Size (m) 6.1 (20 antennas)
Search Frequency (MHz) 1000 – 10000
Search Wavelength (nm)
Frequency Resolution (Hz) 0.7
Other Resolution
Objects (Hz) 20000 red dwarfs
Flux Limit (W m-2) 1.5 x 10-24
Total Hours 12 Hr/Day every day
Reference Harps 2017, Presentation at AASTCS 5
Link http://files.aas.org/aastcs5/aastcs_5_300_04.pdf
Comments Three methods: look for narrowband signals, observe planets during transit/occulation, observe multuplanet systems during conjunction
Date 2016 – ON
Observer(s) Maire et. al. (NIROSETI)
Site Lick Observatory/Nickel Telescope
Instrument Size (m) 1
Search Frequency (MHz)
Search Wavelength (nm) 950 – 1650
Frequency Resolution (Hz)
Other Resolution Temporal resolution: 0.4 ns
Objects (Hz) 1340 objects, including main-sequence and giant stars, 20 spirals, 36 ellipticals, 15 dwarf spheroidals, 9 irregulars, and 2 SO galaxies
Flux Limit (W m-2) 380 photons m-2
Total Hours ONGOING
Reference Maire et. al. 2016 SPIE 91474K
Link https://www.spiedigitallibrary.org/conference-proceedings-of-spie/9908/1/A-near-infrared-SETI-experiment–commissioning-data-analysis-and/10.1117/12.2232861.short?SSO=
Comments A search for nanosecond pulsed near-infrared pulses
Date 2016 – ON
Observer(s) Villarroel et. al. (VASCO)
Site Archival from USNO-B1.0
Instrument Size (m)
Search Frequency (MHz)
Search Wavelength (nm)
Frequency Resolution (Hz)
Other Resolution
Objects (Hz) ~2.9 x 105 stars published
Flux Limit (W m-2)
Total Hours ONGOING
Reference Villarroel et. al. 2016 AJ 152 3
Link http://iopscience.iop.org/article/10.3847/0004-6256/152/3/76/meta
Comments A search for disappearing stars present in POSS plates but missing in SDSS and recent photometric surveys