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The Columbus Optical SETI Observatory

Progress in the Search for Extraterrestrial Life, Commission 51 Symposium, Santa Cruz, August 16-20, 1993, Astronomical Society of the Pacific, Vol. 74, pp. 387-396, 1995.





The Electromagnetic Search For Extraterrestrial Technologies
The Observatory
Optical SETI Bulletin Board (BBS)


Copyright , 1993, ETI Photonics
Copyright , 1995, Astronomical Society of the Pacific



ETI Photonics
545 Northview Drive
Columbus, Ohio 43209-1051
United States



The first Visible Optical SETI Observatory in North America is described.  This observatory is only one of three on this planet today.  The prototype facility is being designed to detect fast pulses from solar-type stars within a few hundred light years.

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This paper addresses the design for a prototype observatory that will Search for Extraterrestrial Intelligence (SETI) in the optical spectrum.1-9,11-17 In October 1992, to celebrate NASA's official switch-on of the High Resolution Microwave Survey (HRMS)10, the author commenced the construction of his own Optical SETI Observatory that will operate in the visible and near-infrared spectrum. The design and construction of what has been named The Columbus Optical SETI Observatory has so far been a self-funded activity. This is the first Visible Optical SETI (OSETI) Observatory in the United States, and when it comes on-line, will be only one of three on this planet. A second Visible SETI Observatory based on the former Soviet MANIA (Multichannel Analyzer of Nanosecond Intensity Alterations)4,9 system is presently under construction in San Juan province, Argentina14. By early 1995, The Columbus Optical SETI Observatory should be in a state to commence the optical targeted search of the sky.

The optical approach to searching for ETI technologies touches on a subject which for various reasons has yet to be accepted by the majority of the SETI community.12 This paper deals primarily with the superiority of interstellar optical (laser) beamed communications over their microwave counterparts.

The author has defined three types of Optical SETI:

(a) Professional Optical SETI employing large telescopes and coherent heterodyne detection.15

(b) Professional Optical SETI employing large telescopes and incoherent direct-detection/photon-counting.15

(c) Amateur Optical SETI employing small telescopes and incoherent direct-detection/photon-counting.15,16


In this paper we consider the subject of SETI in the optical spectrum using systems (b) or (c). The word Amateur is a bit of a misnomer, for there is nothing amateurish about what will be described herein. Rather, it is a reflection of the size of the receiving telescope aperture that warrants the use of the term. Indeed, the aperture size in the author's prototype Optical SETI Observatory or Optical Earth Receiving Station is 25.4 cm (10"); a little larger than the near-infrared (1.06 m m) ETI Uplinks proposed in NASA's 1971/73 Project Cyclops design study!3

This Optical SETI research is thus applicable to both categories (b) and (c); the degree of sophistication that the "amateur" wishes to employ being dependent on funds available. What is very exciting about Amateur Optical SETI (AMOSETI) is that there is a rare opportunity for amateur optical astronomers to participate in a field with virtually no competition at this time from professional organizations. Of course, one of the aims of the author's OSETI activities is to develop the techniques and procedures which will allow HRMS to be extended into the optical regime, early in the next century. For it is his strong contention, that successful detection of ETI signals will not occur in the microwave regime, rather as every sensible ETI knows, "lasers are far more effective for interstellar and SETI communications"!

Note that the word "Optical" is used here according to its modern definition as employed by photonics (optoelectronic) engineers and scientists throughout the world. It covers that part of the electromagnetic spectrum from the far-infrared to the ultra-violet. However, as with normal optical telescopes, The Columbus Optical SETI Observatory is restricted to operation in the visible and near-infrared regime. Thus, for the purposes of this study, "Optical SETI" means "Visible & Near-Infrared SETI".



This is not the first time, nor will it be the last, that the scientific community may have gone in the wrong direction because of mistaken assumptions. At first glance, the three decades-old idea that ETI signals will be found in the quietest region of the electromagnetic spectrum seems reasonable. Thus, the 21-centimeter hydrogen (H) line and the region of the microwave spectrum between the H and lowest OH resonance lines (1.420 to 1.662 GHz), which has come to be known as the "waterhole", has become a favored "magic frequency".10 The over-emphasis on the microwave approach to SETI is illustrated by the SETI Lore Time Pyramid of Figure 1.


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Figure 1. The  SETI lore time pyramid.  To the right are listed a few milestones in microwave SETI, while to the left are listed most of the optical SETI research activities to date.  The predominance of the present microwave SETI lore has been caused by mistaken assumptions about the transmitter gains and resulting Effective Isotropic Radiated Powers (EIRPs) available to ETIs.


Besides the issue of quantum noise at optical frequencies, the real reason that the SETI community has largely ignored the optical approach to detecting ETI signals and have generally claimed that lasers were poorer for SETI interstellar communications than the microwave counterpart, can be laid squarely at the process of derating and crippling the ETI transmitter uplink performance. The famous Cyclops Report3 must bear considerable blame for this. Unfortunately, the SETI community has attributed to ETIs the technical prowess of late 20th Century Earth. Just because we do not presently have precise peculiar proper motion data on nearby stars and don't know how to aim (point-ahead target) our lasers on such stars, is not a reason for suggesting that ETIs cannot do this. ETI civilizations may be millions of years ahead of us. However, even within the next 50 years we are likely to acquire the skills to respond to such signals with higher EIRP diffraction-limited beams that are a better match for the zones of life around nearby stars.

Figure 2 illustrates the range of microwave and optical transmitter gains that have been conjectured for ETIs by SETI researchers over the years. Figure 3 indicates the corresponding EIRPs. The graph of Figure 4 illustrates the expected sensitivity of a 32" aperture telescope as a function of the optical bandwidth, This assumes the use of continuous wave laser beacon signals at very high EIRP levels, and noise levels being set by the background stellar radiation of the targeted star.


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Figure 2. This is a graph showing the maximum usable gains that various SETI researchers have thought possible for ETIs over the past 34 years.   Generally, these researchers have limited the gains by the requirement to illuminate entire zones-of-life around stars and by point-ahead targeting difficulties.


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Figure 3. This is a graph of predicted maximum EIRPs that ETIs might produce.  It is based on the maximum usable gains shown in Figure 2, and the CW or pulsed powers predicted by the respective authors.  This author has speculated the highest EIRP levels - EIRPs that make optical SETI observations with small aperture telescopes a reasonable activity.


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Figure 4. Signal-to-noise ratio (SNR) versus optical bandwidth for OSU's 81 cm (32 in) Perkins Observatory Cassegrain with (incoherent) direct-detection optical receiver.  This graph is applicable to the reception of a continuous wave ETI beacon at a normalized range of ten light-years, and a wavelength of 656 nm.


Monte Ross13 has suggested that ETIs would find pulsed beacons and Pulse Position Modulation (PPM) data-streams for far more efficient for interstellar communications. Under this rationale, the peak EIRP may be so high as to make it possible to use incoherent photon-counting receivers, and/or smaller receiving telescopes, with little optical filtering.



Figure 5 shows a schematic of an observatory for both Professional and Amateur Optical SETI. The purpose of the conventional CCD is just to display the star-field on a TV or PC monitor and for precision star tracking. In this preferred design, it does not detect the ETI signal; that job is performed by the relatively fast single solid-state APD or PMT. APDs have the advantage of high quantum efficiency but usually have the disadvantage of higher dark-current; the converse being the case for photomultipliers. Though the imaging CCD can itself be used as the ETI detector, this approach would compromise detection sensitivity and bandwidth.


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Figure 5. Schematic of basic photon-counting optical SETI observatory.  The photodetector can be either an avalanche photodiode (APD) or a photomultiplier tube (PMT), depending upon the wavelength regime being investigated.   If ETI pulses of high EIRP are assumed, then the optical filter (or monochromator) can be relatively broadband.


The Meade LX200 is state-of-the-art in small computer-controlled Schmidt-Cassegrain Telescopes (SCTs). Figure 6 shows a photograph of the f/10 25.4 cm (10") Meade SCT that is employed at The Columbus Optical SETI Observatory. Interfacing and mains power (110 V) for the Meade LX200 is provided at the foot of the pole supporting the satellite dish. For the present time, a 2.3 m (9 ft.) square plinth consisting of concrete patio squares has been constructed in front of the dish to provide a level surface for the tripod. It takes about twenty minutes to set up the system for an observing session, but plans are in hand to either deploy a small permanent dome on the plinth, such as the HOME-DOME, or to relocate the observatory and new dome to the garage roof.


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Figure 6. Picture showing the first visible optical SETI observatory in North America, one of only three in the entire world.  Situated at the rear of the author's home, the 25.4 cm (10 in) Meade LX200 Schmidt-Cassegrain telescope (SCT) stands on a 9 foot square concrete plinth.  It is interfaced to its control computer via a serial port, the connections being at the foot of the pole that supports the satellite dish in the background.


The picture shows the telescope head with its dew-shield extension section, attached to the equatorial mount (Superwedge) on a fully-extended tripod. In practice, for Optical SETI observations, there is no need to use the equatorial mount, since field rotation is not a problem as it would be for astrophotography. Setting up the system as shown is a two-man job because of the weight of the telescope head (61 lbs). However, since the SCT can be used in the altazimuth-mode and the tripod legs do not have to be fully extended, it is possible for one person to set up the system.

Today, the Personal Computer (PC) has become ubiquitous in both the office and laboratory environments. Software and hardware for application in both professional and amateur photon-counting OSETI receivers will be the subject of future investigations. This is not to preclude the use of a scaled-down version of the MCSA (Multi-Channel Spectrum Analyzer) systems being employed for the HRMS project.10,12



In October 1991, the author set up a BBS for coordinating future world-wide AMOSETI activities. The idea is that when eventually the efficacy of the optical approach to SETI catches on with amateur optical astronomy societies and clubs, there will arise the opportunity to apply a "divide and conquer" approach to the targeted star search. In this way, different groups in the northern and southern hemispheres can be allocated stars and optical wavelength bands to search, that will allow for the most rapid and effective visible search of the stars that appear in the HRMS Targeted Star List. This BBS may one day be employed to allow users to download live Optical SETI data from The Columbus Optical SETI Observatory's control and signal processing computer.



When The Columbus Optical SETI Observatory becomes fully operational, it will be employing a high-speed photometer to analyze starlight. It is almost inevitable that serendipity will apply to Optical SETI, where natural fast phenomenon will be discovered in the visible and near-infrared spectrum that have hitherto not been predicted by astrophysicists.

Future work will involve installing the telescope in an astronomical dome, building a dedicated control room, and devising means to efficiently extract the would-be ETI signals from the background and internal noise of the receiver. In many ways, The Columbus Optical SETI Observatory or AMOSETI Observatory is a small version of the late Shvartsman's "MANIA" system that is now being duplicated in Argentina.4,9,14 When this observatory comes on-line in 1995, will be simultaneously the only Amateur OSETI Observatory in the world, the only Visible OSETI Observatory in North America, and only the second (or third) Visible Optical SETI Observatory of any description, anywhere on this planet!



  1. R. N. Schwartz, and C. H. Townes, "Interstellar and interplanetary communication by optical masers", Nature, Vol. 190, No. 4772, pp. 205-208, April 15, 1961.
  2. M. Ross, "Search via laser receivers for interstellar communications", Proc. IEEE, Vol. 3, No. 11, p. 1780, November 1965.
  3. B. M. Oliver, and J. Billingham (Editors), "Project Cyclops - A design study of a system for detecting extraterrestrial intelligent life", NASA Publication CR 114445, 1971/1973.
  4. V. F. Shvartsman, "Communications of the Special Astrophysical Observatory", No. 19, p. 39, 1977.
  5. B. Zuckerman, "Preferred frequencies for SETI observations", Acta Astronautica, Vol. 12, No. 2, pp. 127-129, 1985.
  6. A. Betz, "A directed search for extraterrestrial laser signals", Acta Astronautica, Vol. 13, No. 10, pp. 623-629, 1986.
  7. B. Sherwood, "Engineering planetary lasers for interstellar communications", NASA Contractor Report 180780, May 1988.
  8. J. Rather, "Lasers revisited: Their superior utility for interstellar beacons", Journal of the British Interplanetary Society (JBIS), Vol. 44, No. 8, pp. 385-392, August 1991.
  9. V. F. Shvartsman, G. M. Beskin, S. N. Mitronova, S.I. Neizvestny, V. L. Plakhotnichenko, and L. A. Pustil'nik, "Results of the MANIA experiment: an optical search for extraterrestrial intelligence", Third Decennial US-USSR Conference On SETI, University of California, Santa Cruz, August 5-9, 1991, Astronomical Society of the Pacific Conference Series, Vol. 47, pp. 381-390.
10. F. Drake, and D. Sobel, "Is anyone out there?", Delacote Press, New York, 1992.
11. S. A. Kingsley, "The search for extraterrestrial intelligence (SETI) in the optical spectrum, The Electronic Journal of the Astronomical Society of the Atlantic (EJASA), Internet (anonymous ftp at chara.gsu.edu [], directory: /pub/ejasa), Vol. 3, No. 6, January 1992.
12. S. A. Kingsley, and M. Ross (Editors), "The search for extraterrestrial intelligence in the optical spectrum", OE/LASE '93 Symposium, SPIE Proceedings, Vol. 1867, Los Angeles, California, January 21-22, 1993.
13. M. Ross, "Large M-ary pulse position modulation and photon buckets for effective interstellar communications", SPIE Proceedings, The Search for Extraterrestrial Intelligence (SETI) in the Optical Spectrum, OE/LASE '93, Vol. 1867, pp. 161-177, 1993.
14. G. A. Lemarchand, G. M. Beskin, F. R. Colomb, and M. Mendez, "Radio and optical SETI from the southern hemisphere", SPIE Proceedings, The Search for Extraterrestrial Intelligence (SETI) in the Optical Spectrum, OE/LASE '93, Vol. 1867, pp. 138-154, 1993.
15. S. A. Kingsley, "The search for extraterrestrial intelligence (SETI) in the optical spectrum: a review", SPIE Proceedings, The Search for Extraterrestrial Intelligence (SETI) in the Optical Spectrum, OE/LASE '93, Vol. 1867, pp. 75-113, 1993.
16. S. A. Kingsley, "Amateur Optical SETI", SPIE Proceedings, The Search for Extraterrestrial Intelligence (SETI) in the Optical Spectrum, OE/LASE '93, Vol. 1867, pp. 178-208, 1993.
17. J.  Bebbington, "Hello, out there?", Columbus Monthly, pp. 77-80, January 1993.

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