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LANG=""; export LANG
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echo x - About.SETI_MOP
cat >About.SETI_MOP <<'@EOF'
RATIONALE  FOR  THE  NASA  MICROWAVE  OBSERVING
PROJECT  FOR  THE  SEARCH  FOR  EXTRATERRESTRIAL
                           INTELLIGENCE

BACKGROUND:  The National Aeronautics and Space Act of 1958
established NASA's mandate to conduct activities in space that
contribute substantially to the expansion of human knowledge, and
to preserve the United States as a leader in space science, among
other activities.  NASA's Office of Space Science and Applications
(OSSA) has always directed its energy toward advancing scientific
knowledge of Earth, the solar system, and the universe beyond.  A
goal of NASA's Exobiology program is to use the unique perspective
of the space sciences to understand the origin, evolution and
distribution of life in the universe.  (The term "exobiology" was
coined by Nobel prize winner Joshua Lederberg in 1957).  This
program has led to the development of major scientific insights on
the nature of life on Earth, and the prospects for life elsewhere.

The Earth is the only location known to have life, but as our
understanding of the nature of life has grown, so too have our
estimates of the likelihood of life outside of the Earth.  Some
locations can be searched directly for signs of life, as Mars was by
the Viking Project of the mid 1970's.  There are billions of other
locations outside this solar system that cannot be searched directly
because of the enormous distances involved.  In 1959, it was first
proposed that a method existed to accomplish an indirect search for
life by the use of radioastronomy techniques, to detect radio signals
that might be produced by intelligent life.  Such signals would
provide unique evidence of the existence of life elsewhere in the
universe.  In 1972, a National Academy of Sciences report on
astronomy and astrophysics stated that "a project with the goal of
detection of intelligent life elsewhere may, in the long run, be one
of science's most important and most profound contributions to
mankind and to our civilization."  Also in 1972, NASA published its
first report on this question of a Search for ExtraTerrestrial
Intelligence (SETI) that sought to determine how NASA-developed
technology could make such a search possible.  In the years between
1972 and 1988, NASA maintained a low-level research and
definition activity that resulted in the initiation of the Microwave
Observing Project in FY 1989, as the culmination of almost twenty
years of effort.

GOAL:  The goal of the SETI Microwave Observing Project is to
conduct a search for evidence of extraterrestrial intelligent life by
systematically searching the microwave radio spectrum for signals
indicating the existence of an extraterrestrial technology.

RATIONALE:   Modern astrophysical theories and recent
observations indicate that the processes that led to the formation of
the planet Earth are widespread, and that planets are probably
common around other stars in our galaxy.  Biological theories and
experiments predict that life, intelligence and technology may thus
evolve elsewhere.  The Earth provides an example that this sequence
has occurred at least once.  There is no reason to suspect that this
sequence is unique.  Current theory holds that planetary systems
around solar-type stars (stars similar to our own Sun in size,
temperature, etc.) are potential "life sites."  Within our own Milky
Way Galaxy, it is estimated that there are somewhere between 200
billion and 400 billion stars.  It is further estimated that as many as
30 billion of these stars may be "solar-type."  Even very pessimistic
assumptions result in a large number of good potential life sites in
our galaxy, and there are billions of galaxies in the universe.

STRATEGY:  The Project does not make any assumptions about the
specific nature of life elsewhere.  The Microwave Observing Project
will listen for microwave radio transmissions reaching the Earth
from extraterrestrial sources, and will attempt to detect signals
not produced by natural processes.  To do this, the Project will
complete the construction of specialized digital signal processing
equipment, and deploy it on large radio telescopes around the world
in a dual-mode search strategy involving a Targeted Search and a
Sky Survey.  The Targeted Search will examine some 800 nearby
solar-type stars over the frequency range of 1,000 to 3,000
megahertz (MHz) using the largest available radio telescopes to
achieve the highest possible sensitivity.  The specialized digital
signal processing equipment will provide the capability of
simultaneously studying the radio spectrum over tens of millions of
individual frequency channels, at resolutions ranging from 1 Hz to
30 Hz.  In this way, the equipment can automatically detect
continuous carrier waves or narrowband pulses whether they remain
constant in frequency or drift slowly because of some relative
acceleration between transmitter and receiver.  The Sky Survey will
use the 34-meter antennas of NASA's Deep Space Network (DSN) to
extend the search to cover the 1,000 to 10,000 MHz frequency range,
and all directions on the sky, while sacrificing some sensitivity.
The digital signal processing equipment will automatically examine
ten million frequency channels at 30 Hz resolution in order to detect
continuous narrowband carrier signals arriving from a fixed position
on the sky.  Both complementary search modes will be conducted
concurrently and provide an opportunity for independent signal
confirmation.  The new technology developed for this Project will
permit real-time signal recognition and the ability to search for a
much wider variety of signal types: two key abilities that have been
missing from all the searches carried out in the three decades of
effort since the first search carried out by Frank Drake in 1960.

        The Microwave Observing Project search will be almost
completely automatic in order to sift through the incoming data,
looking for signals at rates (over a hundred megabytes/second) that
are orders of magnitude beyond human capabilities, during a search
that will involve years of observing.  The automation will include
execution of all sky survey scanning patterns, target star sequence
selection, and the testing of signals for extraterrestrial origin.

PROJECT READINESS:  The Project completed a six-year research
and development phase in 1988.  After two successful NASA
Nonadvocate Cost Reviews, the Project Initiation Agreement for
Phase C/D activities was approved by NASA for initiation in FY 89,
officially establishing the SETI Microwave Observing Project.
Initial project-phase funding began in FY 90.  The basic technology is
highly developed.  There are no significant technological risks to the
Project.

FUNDING HISTORY:  The Microwave Observing Project, as part of
OSSA's Strategic Plan, was funded in FY 91 at a level of $12.1
million.  The total cost over the duration of the program, for both
development and operations over a decade, is $100 million, or an
average of $10 million per year.  With such an important potential
return, the Project is worth the cost of less than 1/10th of 1% of
NASA's budget per year.  This amounts to less than 5 cents per U.S.
taxpayer per year.  From 1975 through 1990 inclusive, the cost of
the research and development of the Project has been $21 million.

SCIENTIFIC STANDING:  The subject of SETI and NASA's Microwave
Observing Project has been reviewed and endorsed extensively by the
science community, including the National Academy of Sciences, the
NASA Life Sciences Strategic Planning Study Committee, the
National Commission on Space, and the international science
community (IAU, IAF, COSPAR, URSI).  In fact, 71 internationally
renowned scientists (including 8 Nobel laureates) signed a petition
published in the October 29, 1982 issue of Science, calling for "the
organization of a coordinated, worldwide and systematic search for
extraterrestrial intelligence."  It has repeatedly been urged that a
search be conducted to establish the bounds on the existence of life
elsewhere in the Galaxy, since this cannot be calculated from first
principles using known laws.  Only experimental evidence can
provide the answer.  The SETI Microwave Observing Project is, by
many orders of magnitude, the most comprehensive investigation of
this question to date.

WHY DO SETI NOW?  Mankind's constantly expanding technology,
especially as manifested in ever-increasing satellite transmissions
and Earth-based microwave communications, is methodically
obliterating the spectrum with day-to-day radio traffic.  This
technology, while useful to us here on Earth, produces signals that
SETI researchers must avoid in the attempt to detect very faint
signals from distant locations in the Galaxy.

ARE THERE ANY SIDE BENEFITS?  Yes.

Science Education:  SETI has been shown to be an exciting tool for
   educating young students about science and mathematics.  Its
   benefits are magnified because it is something that the United
   States can actually do now to address a fundamental question of
   scientific and public interest.  The interdisciplinary nature of the
   problem addressed by SETI provides a natural implementation for the
   AAAS Project 2061 recommendation on the cross-teaching of
   science.  SETI has already been included in the newly-revised
   Science Curriculum Framework produced by the Curriculum
   Commission of the California State Board of Education.  SETI
   encompasses physics, astronomy, planetology, chemistry, biology,
   evolution science, anthropology, sociology, communications
   engineering and mathematics.  These areas of science are
   fascinating subjects that catch the attention of children when
   taught in the context of their relation to the possible existence of
   extraterrestrial life.  Adults are eager to learn, as well:  during the
   Spring of 1990, the NASA SETI team worked with San Francisco
   State University's Extended Education Office to conduct a 10-part
   (20 hours) lecture series on SETI, with an average weekly
   attendance of 245 persons.  The program, attended by many science
   teachers, was highly successful and has created interest at other
   campuses around the country to conduct similar programs.  Finally,
   numerous education projects are in the development stages,
   including proposals for developing supplementary curriculum
   material and participation in the 1992-1993 International Space
   Year (ISY).

Technology Spinoffs:  The technologies developed to conduct the
   Microwave Observing Project have important potential spinoffs for
   electrical engineering, computer science, radio astronomy,
   diagnostic medicine (particularly computer aided tomography),
   materials science, aviation safety, geophysical research and failure
   analysis studies.

Public Interest:  The undeniable popularity of books, movies, and
   television programs dealing with extraterrestrial intelligence
   affords the SETI endeavor a wide popular appeal.  Over the years,
   repeated public opinion polls have shown strong sentiment in favor
   of SETI.  For example, a nationwide TV poll conducted by CNN on
   February 13, 1990, showed that 86% of the public believe there is
   extraterrestrial intelligent life.  Nonetheless, this opinion is not
   currently supported by experimental data.  The Microwave Observing
   Project is the first comprehensive experiment that can directly
   address this issue.

OUTSIDE/INTERNATIONAL PARTICIPATION:  The Microwave
Observing Project affords substantial opportunities for outside
participation.  A NASA Research Announcement, issued in April
1990, solicited participation from the science community in the
Project's Investigators Working Group, which was appointed in
January 1991.  The SETI equipment, which is at the cutting edge of
technology, is being produced by first-class engineering teams in
the United States.  In order to cover the entire sky in both the
Northern and Southern hemispheres, observations will be conducted
around the world.  Observation sites outside the U.S. will include
DSN sites in Australia and Spain.  National observatories in
Australia, France and elsewhere may also be participants in the
Project.

CONCLUSION:  The United States has led the world in developing the
means to realistically address the question of life in the universe.
The visionary nature of SETI evokes interest and excitement at all
levels.  To quote the 1982 report of the National Academy of
Sciences Astronomy Survey Committee, "It is hard to imagine a more
exciting astronomical discovery or one that would have greater
impact on human perceptions than the discovery of extraterrestrial
intelligence."  Moreover, the Microwave Observing Project is being
undertaken at a relatively low cost without an additional burden to
space flight resources.

        NASA SETI observations will begin in October 1992 as part of
the Quincentennial celebrations of Columbus' discovery of America.
The detection of an extraterrestrial technological civilization -- to
know that we are not alone -- would be a major event in the history
of the human race.



For more information contact:


SETI Office, MS 239-22, NASA Ames Research Center,
      Moffett Field, CA 94035.
SETI Office, MC 303-401, Jet Propulsion Laboratory,
     4800 Oak Grove Drive, Pasadena, CA 91109.
SETI Institute, 2035 Landings Drive, Mountain View, CA 94043.

February 1991
@EOF

chmod 644 About.SETI_MOP

echo x - HRMS_Progress.Rept
sed 's/^@//' >HRMS_Progress.Rept <<'@EOF'
@From David Boulton:
------------------------------------------------------------------------

@From: baalke@kelvin.jpl.nasa.gov (Ron Baalke)
Newsgroups: sci.space,sci.astro,alt.sci.planetary
Subject: HRMS Update - January 1993
Date: 28 Jan 1993 17:10 UT
Organization: Jet Propulsion Laboratory
Message-ID: <28JAN199317103302@kelvin.jpl.nasa.gov>
Keywords: HRMS, ARC, JPL

Forwarded from the Spacelink BBS

NASA HIGH RESOLUTION MICROWAVE SURVEY (HRMS)
TARGETED SEARCH AND SKY SURVEY STATUS
INAUGURATION  +  60 DAYS

BACKGROUND

The High Resolution Microwave Survey (HRMS) is part of the Toward Other
Planetary Systems (TOPS) program in NASA's Solar System Exploration Division.
The HRMS looks for evidence of planets orbiting other stars through radio
emissions that may be produced by technological civilizations on any such
planets.  The HRMS has two search modes, a Sky Survey and a Targeted Search.
The Sky Survey, managed by the Jet Propulsion Laboratory, uses 34-meter
antennas in NASA's Deep Space Network to sweep the entire sky over a wide range
of frequencies for the presence of strong signals.  The Targeted Search uses
the largest available radio telescopes to observe nearby sun-like stars over a
narrower range of frequencies for weak signals.  The Targeted Search is managed
by NASA's Ames Research Center which is also the lead center for the HRMS. The
combination of the two search modes is millions of times more comprehensive
than the sum of all previous search programs.  The observational phase of the
HRMS was inaugurated at 1900 hours Universal Time on 12 October 1992, Columbus
Day, at the NASA Goldstone Deep Space Communications Complex in California and
the Arecibo Observatory in Puerto Rico. The Arecibo Observatory is part of the
National Astronomy and Ionosphere Center, operated by Cornell University for
the National Science Foundation. In a coordinated program, the Arecibo antenna
pointed at the star GL615.1A and the Goldstone antenna began to scan a small
area of sky that included the position of the target star.  The beginning of
the search generated world-wide interest in the media.  This report presents an
overview of the observations and results to date.

INAUGURAL OBSERVATIONS

Sky Survey

Initial observations began with the new 34-meter antenna at the Venus
Development Station at Goldstone. The project is using the available X-Band
receiver which can be tuned from 8200 to 8600 MHz, and the Sky Survey Prototype
System (SSPS).  The SSPS divides 40 MHz of the spectrum into two million 20JHz
channels and automatically looks for Continuous Wave signals as the search
progresses.  Each observation involves driving the antenna rapidly in a
"sliding racetrack" pattern programmed to cover a "sky frame," a rectangular
area of sky approximately 1 degree high and 30 degrees in length.

While observing, the SSPS temporarily stores data from channels with power
above a specified threshold level and excises data from channels affected by
terrestrial signals.  The scan pattern is designed so that each point in the
frame will be scanned by the antenna at least twice (with slightly different
offsets) at times separated by about 10 minutes.  Candidate signals drawn from
the temporary buffer are selected for verification tests at the completion of
the sky frame.  A total of 17 sky frames, including 4 repeat frames, have been
observed at X-Band. To date, no candidates have passed the verification tests
and the results are entirely consistent with the expected thermal noise
statistics.  Through January 1993, the SSPS will continue to observe about one
day per week on the 34-meter antenna at Goldstone with an increase in allocated
time later in the year.

A special set of three sky frames covering parts of the galactic plane were
observed repeatedly in the frequency bands 1600-1750 MHz and 1380-1430 MHz.
These observations, using the available L-Band receiver on the 26-meter antenna
at the Venus site, are designed to optimize radio astronomy data and improve
interference excision algorithms.

Targeted Search

The Targeted Search System (TSS) used the 305-meter antenna of the Arecibo
Observatory, the world's largest, for its initial observations.  The TSS
processed a 10 MHz bandwidth into more than 14 million channels simultaneously,
producing parallel channel resolutions ranging from 1 Hz to 28 Hz.  Data were
analyzed in real-time for the presence of Continuous Wave (CW) and Pulsed
signals that may drift in frequency by as much as 1 Hz per second.
Observations focused on a list of 25 stars within 100 light years.  Receivers
provided by the observatory allowed observations in four frequency bands
covering a total of about 300 MHz within the range from 1300 MHz to 2400 MHz.
Each "observation" of a star in a particular frequency band consisted of three
steps with the antenna first pointed at the star, then away from the star, and
then back at the star.  Each observing step lasted either 92 seconds or 299
seconds.  Signals that were present only when the telescope was pointed at the
star were considered potentially of extraterrestrial origin and were subjected
to further tests.  Signals that were present both "on" and "off" the star were
deemed to be terrestrial interference signals.  A total of 436 observations
were conducted during the 200 hours of assigned telescope time.  A large number
of interference signals were detected and cataloged.  Fifteen signals required
further verification tests but all proved to be intermittent terrestrial
signals.

Since returning from Arecibo, the TSS is being reassembled in the TS
development lab at NASA Ames. As expected, operational experience has indicated
the need for modifications to several circuit boards and improvements to the
control software.  Over the next year the capability of the system will also be
doubled to cover 20 MHz.  This work is in preparation for observations of
nearby sun-like stars in the Southern Hemisphere, scheduled to begin in 1994 at
the 64-meter antenna of the Parkes Observatory in Australia. Parkes is part of
the Australian Telescope National Facility operated by the Commonwealth
Scientific Industrial Research Organization. Analysis of the data collected at
Arecibo is now under way with the goal of developing better techniques for
quickly identifying, classifying, and perhaps even avoiding interference
signals.

RESULTS

No signals from beyond our Solar System have been detected yet.  Although many
signals have been detected, none appear to originate from a point on the sky as
determined by our observation and verification strategies.  Most of the signals
were recognized immediately as terrestrial interference by the software.  A few
observations and sky frames detected signals that required verification tests.
Nearly all verification tests have been performed at the site within minutes of
the original detection.  A few tests had to be performed on the following day.
No signal passed this level of testing.

The HRMS has successfully inaugurated its observational phase.  Both the
Targeted Search and the Sky Survey are using the lessons learned in the initial
observations to improve the hardware, software, and observation techniques of
the HRMS project.

For more information, please contact:

SETI Office
NASA Ames Research Center
M.S. 244-11
Moffett Field, CA  94035-1000

                                      #####
     ___    _____     ___
    /_ /|  /____/ \  /_ /|     Ron Baalke         | baalke@kelvin.jpl.nasa.gov
    | | | |  __ \ /| | | |     Jet Propulsion Lab |
 ___| | | | |__) |/  | | |__   M/S 525-3684 Telos | Every once in a while,
/___| | | |  ___/    | |/__ /| Pasadena, CA 91109 | try pushing your luck.
|_____|/  |_|/       |_____|/                     |



---
 David A. Boulton                 | knowledge is just a polite
 boulton@netcom.com               | term for dead, 
 Peregrine Associates             | but not buried imagination.
 POB 1385 Redwood City, CA 94064  |           -- e.e. cummings


@EOF

chmod 644 HRMS_Progress.Rept

echo x - NASA_HRMS_Press_Info.Oct92
sed 's/^@//' >NASA_HRMS_Press_Info.Oct92 <<'@EOF'
BACKGROUND ON SETI PROJECT  (submitted by David Boulton)

-------------------- Begin Forwarded Message -----------------------

Newsgroups: sci.space.news
@From: baalke@kelvin.jpl.nasa.gov (Ron Baalke)
Subject: HRMS Press Kit (Repost)
Message-ID: <1992Oct13.055252.3668@news.arc.nasa.gov>
Followup-To: sci.space
Organization: Jet Propulsion Laboratory
Date: Mon, 12 Oct 1992 23:03:48 GMT

[I'm reposting this since the previous version contained garbled text.  
Thanks  to Andrew Yee for supplying a clean version. - Ron Baalke ]


HIGH RESOLUTION MICROWAVE SURVEY  (HRMS)

PRESS KIT

OCTOBER 1992

PUBLIC AFFAIRS CONTACTS

NASA HEADQUARTERS, WASHINGTON, D.C.
Office of Space Science and Applications
Michael Braukus

Ames Research Center, Mountain View, Calif.
Michael Mewhinney

Jet Propulsion Laboratory, Pasadena, Calif.
Mary Hardin


CONTENTS


General Release                  1
Media Services Information       3
Quick-Look Facts                 4
Project History                  5
Project Objectives               6
Targeted Search                  7
Sky Survey                       9
Signal Detection Plans           10
Project Management               11



GENERAL RELEASE

NASA TO BEGIN SEARCH FOR INHABITED PLANETS

RELEASE:  92-161


     On Oct. 12, NASA will begin the most comprehensive search ever 
conducted for evidence of intelligent life elsewhere in the universe.

     The search will use telescopes and antennas to detect radio 
transmissions from other planetary systems.  The search will commence 500 
years after Columbus landed in North America.

     "In the first few minutes, more searching will be accomplished than in 
all previous searches combined," according to Dr. John Billingham of NASA's 
Ames Research Center, Mountain View, Calif.

     "Over the past few decades, " Billingham added, "scientific opinion 
has increasingly supported the theory that complex life may have evolved on 
planets orbiting other stars in the galaxy and the universe.  In some 
cases, further evolution may have led to the emergence of intelligence, 
culture and technology."

     Billingham, the program chief at Ames, said the High Resolution 
Microwave Survey (HRMS) consists of two parts -- a Targeted Search and a 
Sky Survey.

     The Targeted Search will use the largest available radio telescopes 
around the world to search the frequency range from 1,000 to 3,000 
megahertz, seeking a variety of patterns that may indicate the presence of 
an artificially generated signal.  A megahertz is a unit of frequency equal 
to one million cycles per second.

      The Targeted Search will perform the most sensitive search ever 
conducted of solar-type stars less than 100 light-years distant.  The 
Targeted Search begins from the world's largest radio telescope at the 
National Astronomy and Ionosphere Center's Arecibo Observatory in Puerto 
Rico. It is operated for the National Science Foundation by Cornell 
University.

     The Sky Survey will use the 34-meter antennas at NASA's Deep Space 
Network sites in the northern and southern hemispheres to scan the entire 
sky over the frequency range from 1,000 to 10,000 megahertz.  The Sky 
Survey begins at the Goldstone, Calif., site.

     "Because of the large increase in the area of sky and frequencies 
covered, a signal will have to be stronger to be detected by the Sky 
Survey," Billingham said. "But it could detect signals emitted in distant 
regions from directions that would be overlooked if the search were limited 
to nearby solar- type stars," he added.

     Both elements of the HRMS are using specially developed digital signal 
processing systems capable of simultaneously analyzing tens of millions of 
radio frequency channels.

     The HRMS is managed by NASA's Ames Research Center, which also is 
responsible for the Targeted Search project.  The Jet Propulsion 
Laboratory, Pasadena, Calif., is responsible for the Sky Survey.

     The HRMS is part of NASA's Toward Other Planetary Systems program in 
the Solar System Exploration Division, Office of Space Science and 
Applications at NASA Headquarters, Washington, D.C.


- end -


MEDIA SERVICES INFORMATION

NASA SELECT TELEVISION TRANSMISSION

     There will be no live NASA Select coverage of the HRMS deployment on 
Oct. 12, 1992.  Video footage of the HRMS deployment will be taken for 
documentary and archival purposes.



HRMS QUICK LOOK

PROJECT DESCRIPTION:  The High Resolution Microwave Survey (HRMS) operates 
under the aegis of the Toward Other Planetary Systems (TOPS) program in the 
Solar System Exploration Division at NASA Headquarters.  The TOPS program 
will employ a variety of astronomical techniques, including microwave 
surveys, to search for planets around other stars.  The HRMS Targeted 
Search and the Sky Survey will begin concurrently at Arecibo, Puerto Rico, 
and Goldstone, Calif. The project's initiation is called the "Initial 
Deployment of the NASA High Resolution Microwave Survey."

INITIAL DEPLOYMENT DATE/SITES:  Oct. 12, 1992 - The National Astronomy and 
Ionosphere Center's 305-meter (1,000-foot diameter) radio telescope near 
Arecibo, Puerto Rico, will be used for the Targeted Search.  This telescope 
is operated for the National Science Foundation by Cornell University.  The 
new 34-meter (112-foot diameter) antenna at NASA's Goldstone Deep Space 
Communications Complex near Barstow, Calif., willbe used for the Sky 
Survey.

Time of Deployment: Targeted Search at 3 p.m.  EDT, Arecibo, Puerto Rico; 
Sky Survey at noon PDT, Goldstone, Calif.

Project Duration:  Expected to last until about 2001.


PROJECT HISTORY


     The Earth is the only location known to harbor life.  But as knowledge 
of the nature of life has grown, so too have estimates of the likelihood of 
life beyond Earth.  Some locations can be searched directly for signs of 
life as Mars was by the Viking Project of the mid-1970's.  There are 
billions of other locations outside of this solar system that cannot be 
searched directly because of the enormous distances involved.

     In 1959, it was first proposed that a method existed to accomplish an 
indirect search for life by the use of radio astronomy techniques to detect 
signals that might be produced on other planetary systems.  Such signals 
would provide unique evidence of the existence of intelligent life 
elsewhere in the universe.

     In 1972, a National Academy of Sciences report on astronomy and 
astrophysics stated that "a project with the goal of detection of 
intelligent life elsewhere may, in the long run, be one of science's most 
important and most profound contributions to mankind and to our 
civilization."  Also in 1972, NASA published its first report describing 
how NASA-developed technology could make such a search possible.

     In the years between 1972 and 1988, NASA maintained a low-level 
research and development activity that resulted in the initiation of the 
Search for Extraterrestrial Intelligence Microwave Observing Project (MOP) 
in FY 1989.

     In 1992, NASA established the High Resolution Microwave Survey (HRMS) 
as part of the Toward Other Planetary Systems (TOPS) program within NASA's 
Solar System Exploration Division.  The Sky Survey (scanning the entire sky 
for strong signals coming from any direction) will begin observations at 
noon PDT using a 34-meter antenna at NASA's Goldstone Deep Space 
Communications Complex near Barstow, Calif.

     The HRMS will be initiated on Oct. 12, 1992 in two concurrent phases, 
the Targeted Search, managed by NASA's Ames Research Center, Mountain View, 
Calif., and the Sky Survey, managed by the Jet Propulsion Laboratory, 
Pasadena, Calif.

     The Targeted Search (focusing with a very high degree of sensitivity 
on 1,000 nearby stars similar to the sun) will begin observations at 3 p.m. 
EDT using the National Science Foundation's National Astronomy and 
Ionosphere Center's 305-meter telescope near Arecibo, Puerto Rico.

     The Sky Survey (scanning the entire sky for strong signals coming from 
any direction) will begin observations at noon PDT using a 34-meter antenna 
at NASA's Goldstone Deep Space Communications Complex near Barstow, Calif.


PROJECT OBJECTIVES


     The detection and characterization of planetary systems around other 
stars is the goal of NASA's Toward Other Planetary Systems (TOPS) program.  
Earth's solar system is still the only known example of a planetary system, 
and Earth is the only known planet that sustains life.  Recent 
astrophysical observations suggest the existence of other planetary systems 
around distant stars.  The existence of these systems could support the 
hypothesis that life may exist beyond Earth in another solar system.

     Beginning in fiscal year 1993, NASA's Solar System Exploration 
Division will expand it TOPS program to include a new project called the 
High Resolution Microwave Survey (HRMS). The project will observe the 
microwave region of the electromagnetic spectrum in a manner that can 
detect signals produced by a distant technology.

     Potentially, there are billions of solar systems in the Milky Way 
galaxy at tremendous distances from Earth.  There are billions of locations 
outside Earth's solar system that may contain life but cannot be searched 
by robotic spacecraft.  By providing a means of locating and studying 
distant planetary systems for evidence of technology generated by life in 
those systems, the addition of HRMS to TOPS will expand and enhance this 
search for evidence of life.

The TOPS program originally was designed to be fully responsive to the 
document "Strategy for the Detection and Study of Other Planetary Systems 
and Extrasolar Material: 1990-2000," issued in 1990 by the Space Studies 
Board's Committee on Planetary and Lunar Exploration.  In the same year, 
the Space Studies Board's Committee on Planetary Biology and Chemical 
Evolution recommended the following four objectives in its report entitled 
"Search for Life's Orign":

   1) To determine the frequency and morphology of nearby planetary 
         systems.

   2) To determine the frequency of occurrence of conditions suitable to 
          the orign of life.

   3) To search for presumptive evidence of life in other planetary 
          systems.

   4) To search for evidence of extraterrestrial technology.

     With the incorporation of the HRMS, the TOPS program will address each 
of these objectives and provide for an expanded comparative study of the 
universe.


TARGETED SEARCH


     Scientists at NASA's Ames Research Center will conduct the Targeted 
Search portion of the HRMS.

     The Targeted Search will examine 1,000 nearby solar-type stars within 
100 light years distance from Earth (one light year is approximately 5.9 
trillion miles).  The objective is to test the hypothesis that 
extraterrestrial technologies are transmitting radio signals whose 
characteristics are greatly different from natural sources of radio 
emissions and that the HRMS radio telescopes are sensitive enough to detect 
them.  Some stellar clusters and nearby galaxies also will be observed.  
The frequency range covered will be 1,000 to 3,000 megahertz (MHz).

     Scientists believe that electromagnetic radiation is the most 
efficient means for accompishing information transfer over interstallar 
distances.  All electromagnetic waves travel at the speed of light, but 
radio waves use lower energy photons than light or other radiation and are 
not absorbed by the interstaller medium.

     Of all possible electromagnetic frequencies, the radio portion of the 
spectrum suffers least from natural background noise.  Microwave radio 
frequencies between about 1,000 and 10,000 megahertz allow detection of the 
weakest signals because the background noise, due to our galaxy and the 
Earth's atmosphere, is least.

     To achieve the highest possible sensitivity, the largest available 
radio telescopes will be used to conduct the Targeted Search. The number of 
targets covered will be much larger than previous searches, and the range 
of frequencies covered will be thousands of times greater than all previous 
searches combined.

     To accomplish this, specialized digital signal processing equipment 
has been constructed to listen for microwave radio transmissions reaching 
the Earth from distant planetary systems.

     The specialized digital signal processing equipment will 
simultaneously study the radio spectrum over tens of millions of individual 
frequency channels, at spectral resolutions ranging from 1, 2, 4, 7, 14 and 
28 hertz (cycles per second).  The equipemnt can automatically detect 
continuous carrier waves or narrow band (limited range of frequencies) 
pulses whether they remain constant in frequency or drift slowly because of 
some relative acceleration between transmitter and receiver.  Low noise 
feeds and cryogenically cooled receivers will provide access to all 
frequencies between 1,000 and 3,000 megahertz.

     A special wide frequency bandwidth Multi Channel Spectrum Analyzer 
(MCSA) and real-time pattern recognition systems will be deployed at radio 
astronomy observatories with the largest existing antennas.  The MCSA is a 
spectroscope that dissects the incoming radio signal into a large number of 
very fine resolution frequency channels.  When combined with the NASA 
signal detectors built for the project, the sytem also is capable of 
detecting continuous wave signals as well as narrow band pulses, a likely 
form of interstellar transmission.  An automatic data analysis subsystem 
will be used to detect the presence of fixed frequency or drifting 
continuous wave (CW) signals or sequences of regularly spaced pulses.

     The Targeted Search will use the National Science Foundation's 
National Astronomy and Ionosphere Center's 305-meter (1,000-ft) diameter 
radio telescope located at the Arecibo Observatory near Arecibo, Puerto 
Rico, for the initial deployment of the HRMS on Oct. 12, 1992.  The system 
will have a total of 10 megahertz of bandwidth.  It will simultaneously 
analyze tens of millions of channels of spectral data at 1, 2, 4, 7, 14, 
and 28 hertz resolutions.  The system will be transported to other large 
radio telescopes around the world in a systematic fashion over the 10-year 
period of the search.  This will ensure that all target stars have been 
fully covered.

     In 1995, the National Radio Astronomy Observatory's (NRAO) 140-foot 
telescope in Green Bank, W. Va., will become a dedicated facility for the 
HRMS, permitting very large observations of each target at each frequency.  
It will serve as the logistical hub of the HRMS Targeted Search. Over the 
next 3 years, three more such systems will be built and packaged into two 
mobile research facility trailers for air transport to the observation 
sites.


SKY SURVEY


     The NASA Jet Propulsion Laboratory, Pasadena, Calif., will conduct the 
Sky Survey portion of NASA's HRMS to search for radio signals from other 
planetary systems.  The Sky Survey will scan all directions of the sky to 
cover a wide range of frequencies from 1,000 to 10,000 megahertz.

     NASA's HRMS will conduct a comprehensive, systematic search of a 
portion of the microwave radio spectrum to detect evidence of radio 
transmissions from other planetary systems.  An intentionally transmitted 
signal is easiest to detect in a frequency band where the background radio 
noise or static is minimal.  One of the quietest frequency bands is the 
"microwave window," which lies between 1,000 and 10,000 megahertz.  Since 
the quiet characteristic of microwave frequencies does not change 
throughout the galaxy, it is reasonable to assume that others might also 
choose this band.

     The Sky Survey observation technique involves automatically mapping 
small areas of the sky, called sky frames.  As the observations are 
completed, the sky frames will be assembled to form mosaic maps, one for 
each frequency band, of all the microwave detections over the entire sky.  
For each of the 31 frequency bands, the sky is divided into several hundred 
frames, as if the sky were a giant checkerboard.  Each frame takes 1 to 2 
hours to map.

     The Sky survey will initially use the 34-meter (112-foot) diameter 
antenna at the Goldstone Deep Space Communications complex of NASA's Deep 
Space Network in California's Mojave Desert. Toward the latter part of the 
survey, the search will move to a similar antenna near Canberra, Australia.

     In 1992, the Sky Survey will begin with a prototype system.  The 
prototype receiver, spectrum analyzer and signal processor will break up 
incoming microwave radio signals into 2 million separate frequency 
channels.  The system can be configured in a single polarization mode with 
40 megahertz total bandwidth or a dual polarization mode with 20 megahertz 
total bandwidth.  Specially designed digital hardware, operating at 
supercomputer speeds, will simultaneously process the 2 million channels to 
identify and separate interstallar signals that have "artificial" 
characteristics from background radio noise and terrestrial interference, 
such as Earth-orbiting satellites.  The most promising candidate signals 
will be subjected to detailed screening and will be saved for subsequent 
verification and study by the scientific community.

     The prototype will be used to test and verify the design of the Sky 
Survey control and data processing algorithms.  The operational Sky Survey 
system currently is being designed and constructed.  It will provide 16 
times the capability of the prototype and will feature a 32 million channel 
spectrum analyzer with a bandwidth of at least 320 megahertz.  Starting in 
1996, the system will begin to map the entire sky 31 times in both the 
northern and southern hemispheres during an observational phase that is 
expected to last 6 years and produce more than 25,000 sky frames.


SIGNAL DETECTION PLANS

     In the event that a signal is detected from another planetary system, 
a formal verification procedure will be implemented.  The procedure 
stipulates that before any public announcement is made, the signal 
detection must be independently onfirmed by other observers or research 
organizations.

     After the discovery has been verified, national and international 
authorities are to be informed.  News of the confirmed discovery then will 
be disseminated promptly, openly and widely through scientific channels and 
the news media.  All data necessary for the confirmation of the detection 
will be made available to the international scientific community through 
publications, meetings, conferences and other appropriate means.

     No response to any confirmed signal will be sent from Earth until 
appropriate international consultations have occurred.


PROJECT MANAGEMENT


NASA Headquarters, Washington, D.C.

Dr. Wesley Huntress    Director, Solar System Exploration Division
Dr. Nicholas Renzetti  Manager, Telecommunications and Data Acquisition 
                                Science Complex, Goldstone Deep Space 
                                Communications Complex
Dr. Michael J. Klein   JPL SETI Project Manager and HRMS Sky Survey Manager
Dr. Samuel Gulkis      HRMS Deputy Project Scientist
J. Richard Kolden      HRMS Sky Survey Implementation Manager


Arecibo Observatory, Puerto Rico

Dr. Daniel Altschuler  Director

     ___    _____     ___
    /_ /|  /____/ \  /_ /|     Ron Baalke         | 
baalke@kelvin.jpl.nasa.gov
    | | | |  __ \ /| | | |     Jet Propulsion Lab |
 ___| | | | |__) |/  | | |__   M/S 525-3684 Telos | Einstein's brain is stored
/___| | | |  ___/    | |/__ /| Pasadena, CA 91109 | in a mason jar in a lab
|_____|/  |_|/       |_____|/                     | in Wichita, Kansas.




@EOF

chmod 644 NASA_HRMS_Press_Info.Oct92

echo x - Newsgroup_HRMS_dialog
sed 's/^@//' >Newsgroup_HRMS_dialog <<'@EOF'
[FURTHER HRMS information culled from newsgroups sci.space, sci.astro]

Subject: HRMS/SETI Answers
Originator: eto@seti
Nntp-Posting-Host: seti.jpl.nasa.gov
Organization: HRMS Sky Survey, Jet Propulsion Laboratory
Date: Fri, 9 Oct 1992 14:55:36 GMT
Lines: 84

In response to David Harwood's direct questions in
<1992Oct9.054339.16971@ousrvr.oulu.fi>:


<Is NASA/HRMS going to investigate any previously detected signals, which
<it considers might possibly have been of ETI origin? Does NASA say that no
<such candidate ETI signals have been detected so far? (We all now that
<HRMS is beginning soon, but there have been previous surveys of far less
<scope.)

1) NO. There are no believable previously detected signals.
2) YES. NASA says that no such candidate ETI signals have been
detected so far.

The NASA HRMS has no secret list of signals from previous searches.
The NASA HRMS will search in two modes: (1) a moderate sensitivity
all sky survey over the microwave spectrum between 1 GHz and 10 GHz
at 20 Hz resolution, and (2) a high sensitivity targeted search of all
solar type stars within 25 pc (there are nearly 800) over the
microwave spectrum between 1 GHz and 3 GHz at 1 Hz resolution.

The all sky survey must sweep the sky at high speed (about 0.2
deg/sec) to complete the survey within a 7 year period. Thus each beam
area on the sky will be looked at for a small period of time (of the
order of 1 second). The targeted search will dwell on each of the
chosen stars for up to 1000 seconds.

All previous surveys have had "hits", meaning signals above a preset
threshold.  The HRMS Sky Survey component will set an initial detection
threshold which will have a PFA (probability of false alarm, i.e., threshold
exceedence due to thermal noise fluctuations in the instrument) of
approximately 10**-5. In the case of the prototype system which will
be in the field at Goldstone, CA, which contains 2**21 channels and
which will apply that threshold to the spectral data every 0.1 second,
this means approximately 200 hits/second. Follow-on signal detection
algorithms will further winnow the data to a PFA of 10**-10 to
10**-12 to provide lists for immediate look back observations.

IT IS A REQUIREMENT THAT ANY ETI SIGNAL DETECTION BE REOBSERVABLE, NOT
ONLY WITH THE NASA HRMS SEARCH SYSTEMS, BUT ALSO BY SIMPLE
CONFIRMATION SYSTEMS. THIS REQUIREMENT FOR REOBSERVABILITY IS CRUCIAL
AND ALL PREVIOUS SEARCH "CANDIDATES" HAVE FAILED TO MEET IT.

<Is HRMS capable of detecting signals of power equivalent to terrestial
<broadcasts (different frequencies) at distances of say 50 light years or so?

YES or NO, depending upon which mode of NASA HRMS you are considering,
and more importantly, what terrestrial signals you choose to include
in your list of broadcast signals.

Neither component is capable of detecting the leakage of our
commercial broadcasts at interstellar distances. However, there have
been highly beamed, strong signals emitted from the Earth which both
components are capable of detecting. The strongest signal emitted from
the Earth is the Arecibo planetary radar, EIRP = 10**13 W. The strongest
commercial broadcasts eminate from UHF television stations, and have
EIRP = 10**6 W to 10**7 W. The sky survey could detect Arecibo at
approximately 50 ly, and the targeted search could do so at
approximately 1000 ly.

The strong military radars which have been used over the last decades
to detect possible bomber attacks and ICBM attacks are another source
of signals which HRMS could detect from nearby stars. Woody Sullivan
published an interesting article some time back in Science which
discussed this (Science, 199, pp377-388, 27 Jan 1978). Tarter and
Billingham also gave a paper at the 40th congress if the International
Astronautical Federation in 1989, whose publication reference escapes
me at this moment. These radars have EIRP levels of approximately
10**11 W. There is a torus around the north pole which has been
illuminated thusly for a few decades. Any advanced civilization within
20 ly within that torus would have been able to determine not only
that our solar system is inhabited by intelligences using the
electromagnetic spectrum, but would also have been able to determine
the parameters of our planetary orbit and rotation, our sun's mass
and infer the temperature of the earth.

Edward Olsen
HRMS

--
 Edward T. Olsen
 Mail Stop 169-506, Jet Propulsion Laboratory
 4800 Oak Grove Dr, Pasadena, CA  91109
 Phone: (818)-354-7604   INTERNET: eto@seti.jpl.nasa.gov (Node: 128.149.82.1)
End of article 8070 (of 8432)--what next? [^Nnpq]

**************************************

Article 8125 (359 more) in sci.astro:
@From: kchen@Apple.COM (Kok Chen)
Newsgroups: sci.space,sci.astro

Subject: Re: HRMS/SETI Answers
Keywords: spectrum, SETI, HRMS
Date: 11 Oct 92 20:22:30 GMT
Organization: Apple Computer Inc., Cupertino, CA
Lines: 22

sharma@nrcphy1.phy.nrc.ca (Rohit Sharma) writes:

>In article <1992Oct9.145536.19786@elroy.jpl.nasa.gov> eto@elroy.jpl.nasa.gov (E
dward T. Olsen) writes:
>
>>solar type stars within 25 pc (there are nearly 800) over the
>>microwave spectrum between 1 GHz and 3 GHz at 1 Hz resolution.
>                            ^^^^^^^^^^^^^^^^
> why this particular portion of the mw spectrum ?


This part of the microwave spectrum is the least noisy.  Moreover,
SETI folks being the poetic people they are, this band includes
the microwave "Water-hole." :-) :-)  (An H emission line exists at
1420 MHz and a set of four OH lines clustered about 1670 MHz, if
memory serves.)  Some searches in the past have been conducted inside
the water hole, and at other magic frequencies such as 2x 1420 MHz.

(Good luck, Ed.)


Kok Chen, AA6TY                         kchen@apple.com
Apple Computer, Inc.
End of article 8125 (of 8432)--what next? [^Nnpq]

****************************

Article 8236 (358 more) in sci.astro:
@From: dah@tko.vtt.fi (David Harwood)
Newsgroups: sci.space,sci.astro

Subject: Re: HRMS/SETI Answers
Date: 12 Oct 92 16:41:15 GMT
Organization: VTT
Lines: 54

In article <1992Oct9.145536.19786@elroy.jpl.nasa.gov> eto@elroy.jpl.nasa.gov (Ed
ward T. Olsen) writes:
[...]
>
><Is HRMS capable of detecting signals of power equivalent to terrestial
><broadcasts (different frequencies) at distances of say 50 light years or so?
>
>YES or NO, depending upon which mode of NASA HRMS you are considering,
>and more importantly, what terrestrial signals you choose to include
>in your list of broadcast signals.
>
>Neither component is capable of detecting the leakage of our
>commercial broadcasts at interstellar distances. However, there have
>been highly beamed, strong signals emitted from the Earth which both
>components are capable of detecting. The strongest signal emitted from
>the Earth is the Arecibo planetary radar, EIRP = 10**13 W. The strongest
>commercial broadcasts eminate from UHF television stations, and have
>EIRP = 10**6 W to 10**7 W. The sky survey could detect Arecibo at
>approximately 50 ly, and the targeted search could do so at
>approximately 1000 ly.
>
>The strong military radars which have been used over the last decades
>to detect possible bomber attacks and ICBM attacks are another source
>of signals which HRMS could detect from nearby stars. Woody Sullivan
>published an interesting article some time back in Science which
>discussed this (Science, 199, pp377-388, 27 Jan 1978). Tarter and
>Billingham also gave a paper at the 40th congress if the International
>Astronautical Federation in 1989, whose publication reference escapes
>me at this moment. These radars have EIRP levels of approximately
>10**11 W. There is a torus around the north pole which has been
>illuminated thusly for a few decades. Any advanced civilization within
>20 ly within that torus would have been able to determine not only
>that our solar system is inhabited by intelligences using the
>electromagnetic spectrum, but would also have been able to determine
>the parameters of our planetary orbit and rotation, our sun's mass
>and infer the temperature of the earth.
>
\\\\\\\\\\\

Thanks for your reply. I hope NASA will keep the international
community of scientists and engineers, many of whom read Usenet,
informed of technical developments and findings. For example, as
a specialist in computer pattern recognition (image analysis) I'd
be interested to hear about algorithms which discriminate signals.

Considering your examples, as well probable compression and EC encoding
of communications (images, linguistic data), is HRMS restricted to
detecting deep-space ranging signals, or perhaps synchronization signals?

[I suppose that inhabited planets would track all natural and artificial
objects of their solar systems, for which they might employ advanced
deep-space radar. For example, we will want to avoid being hit by large
meteors or asteriods here or elsewhere.]

D.H.
End of article 8236 (of 8432)--what next? [^Nnpq]

********************************


Article 8248 (357 more) in sci.astro:
Newsgroups: sci.space,sci.astro
@From: se_taylo@rcvie.co.at (Ian Taylor)

Subject: Re: HRMS/SETI Answers
Organization: Alcatel Austria - Elin Research Center, Vienna
Date: Wed, 14 Oct 1992 16:14:18 GMT
Lines: 24

In article <1992Oct9.145536.19786@elroy.jpl.nasa.gov> eto@elroy.jpl.nasa.gov (Ed
ward T. Olsen) writes:
>
>Neither component is capable of detecting the leakage of our
>commercial broadcasts at interstellar distances. However, there have
>been highly beamed, strong signals emitted from the Earth which both
>components are capable of detecting. The strongest signal emitted from
>the Earth is the Arecibo planetary radar, EIRP = 10**13 W. The strongest
>commercial broadcasts eminate from UHF television stations, and have
>EIRP = 10**6 W to 10**7 W. The sky survey could detect Arecibo at
>approximately 50 ly, and the targeted search could do so at
>approximately 1000 ly.
>
Why can't HRMS detect a current earth-like technology leakage at interstellar
distances? Isn't this the most likely case?

So is HRMS designed only to detect narrow beams directed our way?

+-- I -------- fax +43 1 391452 --------------------- voice +43 1 391621 169 --+
| T a y l o r  Alcatel-ELIN Research, 1-7 Ruthnergasse, Vienna A-1210 Austria  |
+-- n ---- ian@rcvie.co.at --- PSI%023226191002::SE_TAYLOR --- 20731::ian -----+

                               TBD


End of article 8248 (of 8432)--what next? [^Nnpq]

*********************************


Article 8280 (356 more) in sci.astro:
@From: nickh@CS.CMU.EDU (Nick Haines)
Newsgroups: sci.space,sci.astro

Subject: Re: HRMS/SETI Answers
Date: 14 Oct 92 22:38:25 GMT
Organization: School of Computer Science, Carnegie Mellon University
Lines: 20
In-Reply-To: se_taylo@rcvie.co.at's message of Wed, 14 Oct 1992 16:14:18 GMT
Originator: nickh@VOILA.VENARI.CS.CMU.EDU
Nntp-Posting-Host: voila.venari.cs.cmu.edu

In article <1992Oct14.161418.5759@rcvie.co.at> se_taylo@rcvie.co.at (Ian Taylor)
 writes:

   Why can't HRMS detect a current earth-like technology leakage at
   interstellar distances? Isn't this the most likely case?

Why is this the most likely case? We can't assign any probabilities to
levels of technology or power use by ETs. If we just look at human
history, we've been putting out _any_ signals for less than 100 years
and current levels for only a few decades. Any guesses on what powers
we'll be putting out (and at what frequencies) in 2092? 2992? 11992?
How directional will our signals be? What about our interstellar
probes?

I guess the reason HRMS wouldn't pick up BBC1 at 4 light-years is the
same reason why it won't spot a dim light-bulb at 4 gigaparsecs:
money.

(and it _would_ pick up military radar at ~5 light-years).

Nick Haines nickh@cmu.edu
End of article 8280 (of 8432)--what next? [^Nnpq]

**************************


Article 8302 (355 more) in sci.astro:
Newsgroups: sci.space,sci.astro
@From: se_taylo@rcvie.co.at (Ian Taylor)

Subject: Re: HRMS/SETI Answers
Organization: Alcatel Austria - Elin Research Center, Vienna
Date: Thu, 15 Oct 1992 09:49:25 GMT
Lines: 23

In article <NICKH.92Oct14173825@VOILA.VENARI.CS.CMU.EDU> nickh@CS.CMU.EDU (Nick
Haines) writes:
>In article <1992Oct14.161418.5759@rcvie.co.at> se_taylo@rcvie.co.at (Ian Taylor
) writes:
>
>   Why can't HRMS detect a current earth-like technology leakage at
>   interstellar distances? Isn't this the most likely case?
>
>Why is this the most likely case?
My assumption is that technologies using microwave communications will do so
primarily for their own benefit, not to send interstellar messages. Using
the one observation available as supporting evidence is clearly unfair, so
I won't :-)

>We can't assign any probabilities to levels of technology or power use by ETs.
Why not? Doing so of course is risky, but that is part of the fun :-)
BTW SETI work is partly justified by Drake's equation, which explicity assigns
probabilities to assumptions about the fraction of intelligently-inhabited
planets using radio technology.

+-- I -------- fax +43 1 391452 --------------------- voice +43 1 391621 169 --+
| T a y l o r  Alcatel-ELIN Research, 1-7 Ruthnergasse, Vienna A-1210 Austria  |
+-- n ---- ian@rcvie.co.at --- PSI%023226191002::SE_TAYLOR --- 20731::ian -----+

                                  TBD
End of article 8302 (of 8432)--what next? [^Nnpq]


   ********************** 


Article 8350 (354 more) in sci.astro:
Newsgroups: sci.space,sci.astro

Subject: Re: HRMS/SETI Answers
@From: rivero@mdcbbs.com (Michael Rivero)
Date: 15 Oct 92 12:31:27 PDT
Distribution: world
Organization: M&E (Division of EDS), Cypress CA
Nntp-Posting-Host: 134.244.5.151
Lines: 36

In article <NICKH.92Oct14173825@VOILA.VENARI.CS.CMU.EDU>, nickh@CS.CMU.EDU (Nick
 Haines) writes:
|> In article <1992Oct14.161418.5759@rcvie.co.at> se_taylo@rcvie.co.at (Ian Tayl
or) writes:
|>
|>    Why can't HRMS detect a current earth-like technology leakage at
|>    interstellar distances? Isn't this the most likely case?
|>
|> Why is this the most likely case? We can't assign any probabilities to
|> levels of technology or power use by ETs. If we just look at human
|> history, we've been putting out _any_ signals for less than 100 years
|> and current levels for only a few decades. Any guesses on what powers
|> we'll be putting out (and at what frequencies) in 2092? 2992? 11992?

  There's aother aspect. Already we are seeing mass communication moving from
carrier wave systems to cable based delivery. In light of studies which
suggest links between long term exposure to radio waves and certain
health problems in people living next to high powered transmitters,
we may see a trend of actual reduction of total planetary radio wave
output from Earth.

  That means that we might be searching for civilizations which are operating
in the narrow time perod between discovery of the radio spectrum and
the move to discreet cable communications, when their radio "noise" would
vanish from the heavens.


<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>
|  Michael Rivero rivero@mdcbbs.com  "Middle-aged Mutant Ninja Animator" |
@~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~~
|  "The great masses of people. . .will more easily fall                 |
|  victims to a big lie than to a small one."                            |
|                                          --Adolf Hitler                |
|                                                                        |
|   "All men are potential rapists, and that's _all_ they are!"          |
|                                 -- Susan Brownmiller                   |
<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<<>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>>

*********************

Article 8246 (352 more) in sci.astro:
@From: danwell@IASTATE.EDU (Daniel A Ashlock)
Subject: SETI spoiler?
Organization: Iowa State University
Date: Wed, 14 Oct 1992 15:52:18 GMT
Lines: 14

   I was talking about SETI with a colleage of mine who came up with an
interesting hypothisis.  An advanced civilization would want to make the best
possible use of it's communications resources.  It would therefore compress
it's communications traffic as much as possible on costly interstellar
channels.  Well-compressed signals are indistinguishable from noise unless you
know the decompression algorithm; if they are different from noise, there is
more room to compress.

   Thus, leakage from a putative galactic comnet would be indistinguishable
from background noise.  What a pisser, eh?  Has someone in the SETI effort
thought this through already?

Dan
Danwell@IASTATE.EDU
End of article 8246 (of 8432)--what next? [^Nnpq]



   ********************** 


Article 8404 (351 more) in sci.astro:
@From: killip@csc.liv.ac.uk (Mr. L.T. Killip)

Subject: Re: SETI spoiler?
Date: 16 Oct 92 12:37:35 GMT
Organization: Computer Science, Liverpool University
Lines: 29
Nntp-Posting-Host: ama.csc.liv.ac.uk

In article <1992Oct14.105218@IASTATE.EDU>, danwell@IASTATE.EDU (Daniel A Ashlock
) writes:
>
>    I was talking about SETI with a colleage of mine who came up with an
> interesting hypothisis.  An advanced civilization would want to make the best
> possible use of it's communications resources.  It would therefore compress
> it's communications traffic as much as possible on costly interstellar
> channels.  Well-compressed signals are indistinguishable from noise unless you
> know the decompression algorithm; if they are different from noise, there is
> more room to compress.
>
We want to contact people out there, right? That is what SETI is about,
right? People who compress their comms so that they are indistinguishable
from noise are not letting the newcomers find them by the most obvious
route, i.e., they _don't_ want to contact us. Let's try to find the people
who _do_ want to contavt us. The ones who don't compress their signals.
Oh, they are the one's we _can_ find. That's all right then.
--
______________________________________________________________________
Les Killip                JANET     : killip@uk.ac.liv.csc
Computer Science Dept,    Internet  : killip@csc.liv.ac.uk
University of Liverpool,
P.O. Box 147,             Phone     : 0(or 44)-51-794-3700
LIVERPOOL L69 3BX
United Kingdom
______________________________________________________________________
| The right of Mortuarius the Extremely  Violent to be identified as |
| the author of this posting has been very persuasively  asserted by |
| him in accordance with the  Copyright Designs and Patents Act 1988 |
----------------------------------------------------------------------
End of article 8404 (of 8432)--what next? [^Nnpq]

@EOF

chmod 644 Newsgroup_HRMS_dialog

echo x - SETI.Post_Detect_Protocol
cat >SETI.Post_Detect_Protocol <<'@EOF'
The following is from
Tarter, J. C. & Michaud, M. A.  "SETI Post Detection Protocol," a special
     issue of Acta Astronautica, Vol 21(2).  1990.

                              ****  INTRODUCTION  ****
Following the two years of joint meetings between the IISL and the IAA
SETI Committee, a drafting session resulted in the first crude draft of
a proposed protocol dealing with the activities that should properly
follow the first detection of a suspected ETI signal.  This draft was
then circulated for several rounds of comment and revision by Michael
Michaud, who presented it for consideration at the Bangalore IAF
Congress.  During their meetings in April 1989, the Boards of Trustees
of the IAA and IISL both approved the wording of the final version of a
protocol entitled "Declaration of Principles Concerning Activities
Following the Detection of Extraterrestrial Intelligence."  The approved
document appears in this final chapter.  During their summer meetings
in 1990-91, the scientific unions named therein shall be asked to
formally endorse this document.  Following this endorsement process,
the document will be sen, for information purposes, to the U. N. and will
be opened for signature by individuals and organizations conducting
SETI research.


DECLARATION OF PRINCIPLES CONCERNING ACTIVITIES FOLLOWING THE
              DETECTION OF EXTRATERRESTRIAL INTELLIGENCE

We, the institutions and individuals participating in the search for
extraterrestrial intelligence,

Recognizing that the search for extraterrestrial intelligence is an
integral part of space exploration and is being undertaken for peaceful
purposes and for the common interest of all mankind,

Inspired by the profound significance for mankind of detecting evidence
of extraterrestrial intelligence, even though the probability of
detection may be low,

Recalling the Treaty on Principles Governing the Activities of States in
the Exploration and Use of Outer Space, Including the Moon and Other
Celestial Bodies, which commits States Party to that Treaty "to inform
the Secretary General of the United Nations as well as the public and
the international scientific community, to the greatest extent feasible
and practicable, of the nature, conduct, locations and results" of their
space exploration activities (Article XI),

Recognizing that any initial detection may be incomplete or ambiguous
and thus require careful examination as well as confirmation, and that
it is essential to maintain the highest standards of scientific
responsibility and credibility,

Agree to observe the following principles for disseminating
information about the detection of extraterrestrial intelligence:

1.  Any individual, public or private research institution, or
governmental agency that believes it has detected a signal from or
other evidence of extraterrestrial intelligence (the discoverer) should
seek to verify that the most plausible explanation for the evidence is
the existence of extraterrestrial intelligence rather than some other
natural phenomenon or anthropogenic phenomenon before making any
public announcement.  If the evidence cannot be confirmed as indicating
the existence of extraterrestrial intelligence, the discoverer may
disseminate the information as appropriate to the discovery of any
unknown phenomenon.

2.  Prior to making a public announcement that evidence of
extraterrestrial intelligence has been detected, the discoverer should
promptly inform all other observers or research organizations that are
parties to this declaration, so that those other parties may seek to
confirm the discovery by independent observations at other sites and so
that a network can be established to enable continuous monitoring of
the signal or phenomenon.  Parties to this declaration should not make
any public announcement of this information until it is determined
whether this information is or is not credible evidence of the existence
of extraterrestrial intelligence.  The discoverer should inform his/her
or its relevant national authorities.

3.  After concluding that the discovery appears to be credible evidence
of extraterrestrial intelligence, and after informing other parties to
this declaration, the discoverer should inform observers throughout the
world through the Central Bureau for Astronomical Telegrams of the
International Astronomical Union, and should inform the Secretary
General of the United Nations in accordance with Article XI of the
Treaty on Principles Governing the Activities of States in the
Exploration and Use of Outer Space, Including the Moon and Other
Bodies.  Because of their demonstrated interest in and expertise
concerning the question of the existence of extraterrestrial
intelligence, the discoverer should simultaneously inform the following
international institutions of the discovery and should provide them
with all pertinent data and recorded information concerning the
evidence: the International Telecommunication Union, the Committee on
Space Research, of the International Council of Scientific Unions, the
International Astronautical Federation, the International Academy of
Astronautics, the International Institute of Space Law, Commission 51
of the International Astronomical Union and Commission J of the
International Radio Science Union.

4.  A confirmed detection of extraterrestrial intelligence should be
disseminated promptly, openly, and widely through scientific channels
and public media, observing the procedures in this declaration.  The
discoverer should have the privilege of making the first public
announcement.

5.  All data necessary for confirmation of detection should be made
available to the international scientific community through
publications, meetings, conferences, and other appropriate means.

6.  The discovery should be confirmed and monitored and any data
bearing on the evidence of extraterrestrial intelligence should be
recorded and stored permanently to the greatest extent feasible and
practicable, in a form that will make it available for further analysis
and interpretation.  These recordings should be made available to the
international institutions listed above and to members of the scientific
community for further objective analysis and interpretation.

7.  If the evidence of detection is in the form of electromagnetic
signals, the parties to this declaration should seek international
agreement to protect the appropriate frequencies by exercising
procedures available through the International Telecommunications
Union.  Immediate notice should be sent to the Secretary General of the
ITU in Geneva, who may include a request to minimize transmissions on
the relevant frequencies in the Weekly Circular.  The Secretariat, in
conjunction with advice of the Union's Administrative Radio Conference
to deal with the matter, subject to the opinions of the member
Administrations of the ITU.

8.  No response to a signal or other evidence of extraterrestrial
intelligence should be sent until appropriate international
consultations have taken place.  The procedures for such consultations
will be the subject of a separate agreement, declaration or
arrangement.

9.  The SETI Committee of the International Academy of Astronautics,
in coordination with Commission 51 of the International Astronomical
Union, will conduct a continuing review of procedures for the detection
of extraterrestrial intelligence and the subsequent handling of the data.
Should credible evidence of extraterrestrial intelligence be discovered,
an international committee of scientists and other experts should be
established to serve as a focal point for continuing analysis of all
observational evidence collected in the aftermath of the discovery, and
also to provide  advice on the release of information to the public.  This
committee should be constituted from representatives  of each of the
international institutions listed above and such other members as the
committee may deem necessary.  To facilitate the convocation of such
a committee at some unknown time in the future, the SETI Committee
of the International Academy of Astronautics should initiate and
maintain a current list of willing representatives from each of the
international institutions listed above, as well as other individuals
with relevant skills, and should make that list continuously available
through the Secretariat of the International Academy of Astronautics.
The International Academy of Astronautics will act as the Depository
for this declaration and will annually provide a current list of parties
to all the parties to this declaration.
@EOF

chmod 644 SETI.Post_Detect_Protocol

echo x - SETI.Question_Answer
sed 's/^@//' >SETI.Question_Answer <<'@EOF'
SOME  FREQUENTLY  ASKED  SETI  QUESTIONS ... AND
                             ANSWERS



1.      What is SETI?

SETI is an exploratory research effort to Search for
Extraterrestrial Intelligence.  The objective of SETI is to
search for evidence of technological civilizations that may
exist on planets orbiting other stars.


2.      Why is the search being conducted?  What is the purpose?

Over the last half century, scientific discoveries have led to
a generally accepted theory of Cosmic Evolution.  One
prediction of this theory is that life is a natural phenomenon
and is likely to develop on planets with suitable physical
conditions.  Scientific evidence shows that life arose on the
Earth relatively quickly, suggesting that life will occur on
similar planets.  With the vast number of stars in our Galaxy,
and the probable number of earth-like planets, it is likely
that advanced technological civilizations are widely
distributed in space.  The NASA SETI Microwave Observing
Project will test this hypothesis by searching for the
technological manifestations of one form of life, intelligent
life.


3.      How is the search being conducted?

The search will use specially developed signal detection
equipment at existing radio astronomy observatories to
detect evidence of extraterrestrial technology.  Almost all
searches to date have tried to detect electromagnetic waves
that may have been emitted, either intentionally or
unintentionally, by technologically advanced societies.  These
electromagnetic waves are more commonly known by their
various types such as light, infrared, and radio.  The NASA
SETI Microwave Observing Project (MOP) will carry out its
observations in the microwave region of the radio spectrum;
i.e., from 1,000 MHz to 10,000 MHz, where there is the least
background noise from astrophysical sources.  The NASA MOP
relies on knowledge of universal physical laws in choosing its
search strategy.  These same laws would be known to
advanced technological civilizations and would suggest the
use of the microwave radio spectrum for them and for us.


4.      How will an ETI signal be recognized?

Artificial signals, those produced by technology, have several
characteristics that distinguish them from natural radio
emissions.  Natural signals tend to be spread over a wide
range of frequencies, are seldom polarized, and are not
coherent.  Artificial signals, produced by a transmitter and
antenna are often confined to a narrow range of frequencies,
highly polarized, and exhibit coherence (where the peaks of
the waves are in phase).  We also expect there will be
information coded on an ETI signal which does not occur with
natural signals.


5.      Why can't we just send a spacecraft out to look?

With our best current rocket technology we could send a
spacecraft to our Sun's nearest neighbor, Alpha Centauri, only
4 light years away.  The trip would take about 40,000 years
and would be very expensive.  There are about a thousand
stars like the Sun within 100 light years.  To search all of
them would take nearly a million years and vast amounts of
money.  Alternatively, we can search for radio waves now,
with state-of-the-art technology, at a cost of less than a
nickel per American per year.


6.      How long have we been searching for radio signals?

The first scientific proposal for using radio waves to
transmit information over interstellar distances appeared in
the journal Nature in 1959.  In the following year, Dr. Frank
Drake, using the 85 foot antenna of the National Radio
Astronomy Observatory, observed two nearby stars.  He called
the search Project Ozma.  Since that time, more than 50
searches have been conducted by dozens of astronomers in at
least eight countries.  All but a few of these searches have
been limited in duration, using only a fraction of a percent of
available radio telescope time.

The observational phase of NASA's Microwave Observing
Project has not begun.  After a six-year R&D phase NASA
began building the equipment in 1989 that will be used to
begin the operational observing phase in October 1992.  The
observing program will last five to seven years using one
dedicated radio telescope and several shared radio telescopes
(see description below).


7.      Have any previous searches found anything?

No -- and at this pioneering stage the chances were slim that
they would find anything.  All of the searches have been very
limited in one respect or another.  They have generally used
equipment that was designed for other purposes.  They also
faced limitations in sensitivity, the number of channels, the
types of signals, and the number of stars observed.

However, in spite of these limitations, most of the searches
have found unexplainable signals.  Since in these searches the
data were often processed long after the observation, none of
the candidate signals could be immediately checked to see if
they were of extraterrestrial origin.  Subsequent
observations conducted months after the original
observations have never found any of the candidate signals.
In order for us to be sure that a signal is from another
civilization, it has to be independently verified and shown to
originate from a point beyond the Solar System.


8.      Who is supporting and carrying out these searches?

NASA is operating the Microwave Observing Project, with the
Ames Research Center leading the project and conducting a
"targeted search" and the Jet Propulsion Laboratory
performing a "sky survey."  The Planetary Society, an
independent, privately funded organization, operates Project
META at Harvard University and in Argentina.  The Ohio State
University conducts a search with a small grant from NASA
and a large volunteer effort.  Smaller scale, limited searches
have been and continue to be conducted by individual
scientists in the U.S. and other countries.


9.      Who "runs" the NASA search and who will participate?

As mentioned before, the NASA search is part of the
Exobiology Program in the Division of Life Sciences at NASA
Headquarters.  NASA's Ames Research Center in Mountain
View, California is the lead center for the SETI MOP and is
responsible for the Targeted Search.  The Jet Propulsion
Laboratory, Pasadena, California is responsible for the Sky
Survey.  Scientists from these centers and other institutions
who developed the SETI instrumentation, along with an
Investigators Working Group (IWG), will conduct the core
observations of the MOP.  Participation in the IWG was
solicited from the scientific community through a NASA
Research Announcement (NRA).  Proposals to the NRA were
reviewed and nine Investigators were selected in January
1991.  In the future, two more NRA's will solicit proposals
for other SETI and radio astronomy experiments using the MOP
instruments.


10.     Why is NASA planning a search?  Isn't NASA more interested
                               in spacecraft and planes?

Part of NASA's charter for research is to study the origin,
evolution, and distribution of life in the universe.  NASA has
an active Exobiology program in its Headquarters Division of
Life Sciences that includes:

- studies of the formation of biologically important
            atoms and molecules in space,
- research on the origin and evolution of life on Earth,
- the search for life on other planets in the Solar
             System, and
- the Search for Extraterrestrial Intelligence.


11.     Why is the planned NASA search different from previous
                                  searches?

The NASA SETI Project will have a number of features that
will distinguish it from previous and current searches:

- continuous coverage with narrow frequency channels
           over a wide range of frequencies;
- real-time processing of the data; i.e. searching for a
           signal immediately after the data are collected;
- a dual-mode search strategy:
- a Targeted Search will
- examine nearly 800 stars like the Sun
- use the largest available radio telescopes (45
          to 300 meters) to achieve high sensitivity
          (usage will amount to about 5% of the
           available time)
- use one dedicated 42-meter radio telescope
- search for either continuous or pulsed signals
- examine two billion channels over a frequency
            range of 1,000 to 3,000 MHz;
- a Sky Survey will
- search the entire sky
- use 34-meter antennas of NASA's Deep Space
           Network to achieve moderate sensitivity (at
           any particular time only one radio telescope
           will be in use)
- search for continuous signals
- examine nearly half a billion channels over a
           wider range of frequencies, 1,000 to 10,000
           MHz.


12.     How long will the NASA Microwave Observing Project last?

The observational phase of the NASA SETI MOP is expected to
span five to seven years.  The actual time needed will depend
on the availability of national observatory facilities and the
level of terrestrial Radio Frequency Interference.


13.     What will happen if we receive an ETI signal?

We expect that the NASA SETI Project will receive many
signals, but that the majority of them will be produced by our
own civilization.  In order to confirm that a signal is indeed
from another civilization, at least two observatories will
have to be able to detect it.  Once a signal is confirmed as
being of ETI origin, an announcement of the discovery would
be made as quickly and as widely as possible.  One way in
which the announcement could be made is described in a
>>>Declaration of Principles Concerning Activities Following
the Detection of Extraterrestrial Intelligence.<<<  This
document has been endorsed by five international space
organizations.


14.     How are we going to know what the signal means?

If the signal is intentional, it will be "anticryptographic,"
that is "easy to decode."  In order to either send or receive a
signal over interstellar distances, a civilization must
understand basic science and mathematics.  Knowing this,
they would probably compose the message with simple
tutorial pictures.  They would probably also use an
interstellar language based on universal mathematical and
physical principles.

Signals that a civilization uses for its own purposes may be
very difficult to decipher.  However, if such signals were
detected, we might still be able to deduce some facts about
the transmitting planet; e.g., the length of its day.


15.     Will the senders have any way of knowing that their signal is
                                  received?

Not right away.  We would have to send a message in reply.
The NASA SETI MOP has no plan for replying.  As part of an
International SETI Post-detection Protocol now under
consideration, the nations of the Earth would have to decide
whether and how to reply.


16.     If we are looking for a signal, are we also sending any
                                 signals?

The NASA SETI MOP is designed only to listen for signals, not
to send them.  However, since the early part of this century,
intelligent inhabitants of the planet Earth have been
unintentionally transmitting signals into space.  Among these
signals are our radio, television, and communications
transmissions as well as our military radar.  The earliest of
our TV transmissions have traveled out into space more than
forty light years.

A few mostly symbolic intentional messages have been sent.
Of particular note was a message sent in 1974 at the
rededication of the Arecibo Observatory.  The contents of the
message included a description of our Solar System, the
elements important for life, the structure of the DNA
molecule, and a depiction of a human figure.  The message
was transmitted in the direction of the globular star cluster,
M13, about 25,000 light years away.


17.     Does NASA plan to restrict information on the detection of a
                                       signal?

No.  One of the reasons for the Declaration of Principles
Concerning Activities Following the Detection of
Extraterrestrial Intelligence is to ensure that the news would
be distributed rapidly and widely.  The NASA Microwave
Observing Project, in order to confirm a potential signal, will
contact other observatories to investigate candidate signals.


18.     What if no signal is detected?

Even if the NASA Microwave Observing Project does not
detect an ETI signal it will provide many benefits to society.
The technology developed to search for faint signals from
distant planets can be applied to more down-to-earth
problems in medical diagnostic imaging, resource exploration,
and aircraft safety.  In the course of the search, the NASA
MOP will collect a uniquely detailed and complete set of
astronomical data; the potential for serendipitous
discoveries is large.  An important spin-off from the NASA
SETI Program will be in education.  SETI provides an almost
irresistible magnet for attracting young people to learn about
science and mathematics.


19.     What do scientists think of SETI?

>From the Report of the Astronomy Survey Committee.
National Academy of Sciences, 1972.

". . . More and more scientists feel that
contact with other civilizations is no longer
something beyond our dreams but a natural
event in the history of mankind that will
perhaps occur in the lifetime of many of us. .
@. .

In the long run, this may be one of science's
most important and most profound
contributions to mankind and to our
civilization."

>From the Report of the Astronomy Survey Committee.
National Academy of Sciences, 1982.

". . . It is hard to imagine a more exciting
astronomical discovery or one that would
have greater impact on human perceptions
than the detection of extraterrestrial
intelligence."


20.     How much will NASA's SETI Microwave Observing Project
                                       cost?

The cost for the ten-year period averages $10 million/year --
or less than 1/10th of 1% of NASA's budget per year -- less
than a nickel per American per year.


21.     Why should we spend millions on SETI when we face a huge
           budget deficit and there are homeless people on our streets?

Every society must manage its budget priorities, and of
course providing for the defense and welfare of its people are
of prime importance.  But a society also must invest in its
future.  Over the last few centuries, investment in scientific
research has dramatically improved the quality of life and led
to an improved understanding of our universe.  The NASA SETI
Program is based on recent discoveries in many fields of
science that indicate that extraterrestrial life is highly
probable.  As with many scientific programs, SETI research
has potential spin-offs of advanced technology that may
benefit the U.S. and its citizens.  The technology developed for
SETI may be of use in medical imaging, resource exploration,
airline safety, electronics, and radio astronomy.  Information
gathered from another civilization may provide important
practical as well as social and philosophical benefits.


22. Will the SETI Project search for UFO's?

No.  It is not the intention of SETI to search for UFO's; the
search strategy is designed to detect signals from
technological civilizations elsewhere in the Galaxy.  NASA's
approach to SETI has nothing to do with UFO's.





Glossary

DNA    Deoxyribonucleic Acid, the molecule of genetic inheritance.
ETI     Extraterrestrial Intelligence.
Light Year   The distance light travels in one year, about six trillion
                   miles.
IWG    Investigators Working Group, the team of scientists
                  participating in the SETI MOP.
META   Megachannel Extraterrestrial Assay, a SETI project
                  supported by the Planetary Society.
MHz     Megahertz, a unit of frequency, one million cycles per
                  second.
MOP     Microwave Observing Project.
NRA     NASA Research Announcement.
RFI      Radio Frequency Interference.
SETI    Search for Extraterrestrial Intelligence.


For more information contact:

SETI Office, MS 239-22, NASA Ames Research Center,
        Moffett Field, CA  94035      (415) 604-6505
SETI Office, MC 303-401,  Jet Propulsion Laboratory,
       4800 Oak Grove Drive, Pasadena, CA  91109   (818) 354-4518
SETI Institute, 2035 Landings Drive, Mountain View, CA  94043
       (415) 961-6633

April 22, 1991

@EOF

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