                  SPACE SHUTTLE ENDEAVOUR

                          STS-67

                     MISSION PRESS KIT

                         MARCH 1995



PUBLIC AFFAIRS CONTACTS

For Information on the Space Shuttle

Ed Campion                 Policy/Management      202/358-1778
Headquarters, Wash., DC

Rob Navias                 Mission Operations     713/483-5111
Johnson Space Center,      Astronauts
Houston, TX

Bruce Buckingham           Launch Processing      407/867-2468
Kennedy Space Center, FL   KSC Landing Information

June Malone           External Tank/SRBs/SSMEs    205/544-0034
Marshall Space Flight Center
Huntsville, AL

Cam Martin            DFRC Landing Information    805/258-3448
Dryden Flight Research Center
Edwards, CA

     For Information on STS-67 Experiments & Activities

Don Savage                     ASTRO-2           202/358-1547
Headquarters, Wash., DC

Mike Braukus                   PCG               202/358-1979
Headquarters, Wash., DC

Tammy Jones                    GAS               301/286-5566
Goddard Space Flight Center
Greenbelt, MD

Jim Cast                       MACE, CMIX        202/358-1779
Headquarters, Wash., DC

Terri Hudkins                  SAREX             202/358-1977
Headquarters, Wash., DC


CONTENTS

GENERAL BACKGROUND
General Release                                      1
Media Services Information                           4
Quick-Look Facts                                     6
Shuttle Abort Modes                                  8
Summary Timeline                                     9
Payload and Vehicle Weights                         11
Orbital Events Summary                              12
Crew Responsibilities                               13

CARGO BAY PAYLOADS & ACTIVITIES
ASTRO-2                                             15
Get Away Special (GAS) Experiments                  33

IN-CABIN PAYLOADS
Commercial MDA ITA Experiments (CMIX)               35
Protein Crystal Growth (PCG) Experiments            39
Middeck Active Control Experiment (MACE)            43
Shuttle Amateur Radio Experiment (SAREX)            44

STS-67 CREW BIOGRAPHIES
Stephen S. Oswald , Commander (CDR)                 47
William G. Gregory, Pilot (PLT)                     47
John M. Grunsfeld, Mission Specialist-1 (MS-1)      48
Wendy B. Lawrence, Mission Specialist-2 (MS-2)0     48
Tamara E. Jernigan, Payload Commander/Mission 
                    Specialist-3 (MS-3)             48
Samuel T. Durrance, Payload Specialist-1 (PS-1)     49
Ronald Parise, Payload Specialist-2 (PS-2)          49




RELEASE:  95-18

ASTRO TELESCOPES MAKE SECOND FLIGHT ON STS-67 MISSION


     This March, Space Shuttle Endeavor will conduct NASA's 
longest Shuttle flight to date carrying unique ultraviolet 
telescopes that will give astronomers a view of the universe 
impossible to obtain from the ground.

     The mission, designated STS-67, also will see Endeavour's 
crew perform a wide range of microgravity processing 
experiments, continue efforts in understanding the structure 
of proteins and study active control of flexible structures in 
space.

     Launch of Endeavour is scheduled for March 2, 1995 at 
approximately 1:37 a.m. EST from NASA's Kennedy Space Center's 
Launch Complex 39-A.  Endeavour's flight will be 15 days, 13 
hours, 32 minutes.  A 1:37 a.m. launch on March 2, would 
result in a landing at Kennedy Space Center's Shuttle Landing 
Facility on March 17, at 3:09 p.m. EST.

     The STS-67 crew will be commanded by Stephen S. Oswald 
who will be making his third Shuttle flight.  William G. 
Gregory, who will be making his first space flight, will serve 
as pilot.  The three mission specialists aboard Endeavour will 
include John M. Grunsfeld, Mission Specialist-1 (MS-1) who 
will be making his first flight, Wendy B. Lawrence, Mission 
Specialist-2 (MS-2) who will be making her first flight and 
Tamara E. Jernigan, Payload Commander and Mission Specialist 3 
(MS-3) who will be making her third flight.  Rounding out the 
crew will be two payload specialists who flew on ASTRO-1 
during the STS-35 mission in December 1990.  Samuel Durrance 
will serve as Payload Specialist-1 (PS-1) and Ronald Parise 
will serve as Payload Specialist-2.  Both Parise and Durrance 
will be making their second space flight.

     The Astro Observatory, making its second flight aboard a 
Space Shuttle, is a package of three instruments mounted on 
the Spacelab Instrument Pointing System (IPS).  The Hopkins 
Ultraviolet Telescope will conduct spectroscopy in the far 
ultraviolet portion of the electromagnetic spectrum, allowing 
scientists to learn what elements are present in targeted 
celestial objects, as well as identify physical processes 
taking place. 

     The second instrument, the Ultraviolet Imaging Telescope, 
will take wide-field photographs of objects in ultraviolet 
light, recording the images on film for processing back on 
Earth.  The third instrument, the Wisconsin Ultraviolet Photo-
Polarimeter Experiment, will measure the intensity of 
ultraviolet light and its degree of polarization.  The 
instrument will give astronomers clues to the geometry of a 
star or the composition and structure of the interstellar 
medium it illuminates.

     Simultaneous observations by these three telescopes will 
complement one another as they provide different perspectives 
on the same celestial objects.  These observations also will 
complement those of ultraviolet instruments on other NASA 
spacecraft, such as the Hubble Space Telescope, the 
International Ultraviolet Explorer, and the Extreme 
Ultraviolet Explorer -- all currently in operation.  By 
combining research findings from these various instruments, 
scientists hope to piece together the evolution and history of 
the universe and learn more about the composition and origin 
of stars and galaxies.

     The flight also will see the continuation of NASA's Get 
Away Special (GAS) experiments program.  The project gives 
individuals an opportunity to perform experiments in space on 
a Shuttle mission.  Two GAS cans will be carried in the cargo 
bay in support of a payload from the Australian Space Office.  
The payload, coincidentally named Endeavour, is an Australian 
space telescope that will take images in the ultraviolet 
spectrum of violent events in nearby exploding galaxies.
  
     The third in a series of six Commercial MDA ITA 
Experiments (CMIX) payloads will also fly aboard Endeavour.  
CMIX-03 includes biomedical, pharmaceutical, biotechnology, 
cell biology, crystal growth and fluids science 
investigations.  These experiments will explore ways in which 
microgravity can benefit drug development and delivery for 
treatment of cancer, infectious diseases and metabolic 
deficiencies.  These experiments also will include protein and 
inorganic crystal growth, experiments on secretion of 
medically important products from plant cells, calcium 
metabolism, invertebrate development and immune cell 
functions.

     Endeavour will carry two systems in Shuttle middeck 
lockers to continue space-based research into the structure of 
proteins and other macromolecules.  The study of proteins, 
complex biochemicals that serve a variety of purposes in 
living organisms, is an important aspect of this mission.  
Determining the molecular structure of proteins will lead to a 
greater understanding of how the organisms function.  
Knowledge of the structures also can help the pharmaceutical 
industry develop disease-fighting drugs.  The two systems are 
the Vapor Diffusion Apparatus in which trays will be housed 
within a temperature-controlled Thermal Enclosure System and 
the Protein Crystallization Apparatus for Microgravity that 
will be housed in a Single-locker Thermal Enclosure System.

     The Middeck Active Control Experiment is an experiment 
designed to study the active control of flexible structures in 
space.  In this experiment, a small, multibody platform will 
be assembled and free-floated inside the Space Shuttle.  Tests 
will be conducted on the platform to measure how disturbances 
caused by a payload impact the performance of another nearby 
payload which is attached to the same supporting structure.

     The STS-67 crew will take on the role of teachers as they 
educate students in the United States and other countries 
about their mission objectives.  Using the Shuttle Amateur 
Radio Experiment-II, Shuttle Commander Stephen S. Oswald (call 
sign KB5YSR), pilot William G. Gregory, (license pending), 
mission specialists Tamara E. Jernigan (license pending) and 
Wendy B. Lawrence (KC5KII) and Payload Specialists Ron Parise 
(WA4SIR) and Sam Durrance (N3TQA) will talk with students in 
26 schools in the U.S., South Africa, India and Australia 
using "ham radio", about what it is like to live and work in 
space.

     The STS-67 mission will be the 8th flight of Space 
Shuttle Endeavour and the 68th flight of the Space Shuttle 
system.

                - end general release-


MEDIA SERVICES INFORMATION

NASA Television Transmission

     NASA Television is available through Spacenet-2 satellite 
system, transponder 5, channel 9, at 69 degrees West 
longitude, frequency 3880.0 MHz, audio 6.8 Megahertz.

     The schedule for television transmissions from the 
Orbiter and for mission briefings will be available during the 
mission at Kennedy Space Center, FL; Marshall Space Flight 
Center, Huntsville, AL; Dryden Flight Research Center, 
Edwards, CA; Johnson Space Center, Houston; NASA Headquarters, 
Washington, DC; and the NASA newscenter operation at Mission 
Control-Moscow.  The television schedule will be updated to 
reflect changes dictated by mission operations.

     Television schedules also may be obtained by calling 
COMSTOR 713/483-5817.  COMSTOR is a computer data base service 
requiring the use of a telephone modem.  A voice update of the 
television schedule is updated daily at noon Eastern time.

Status Reports

     Status reports on countdown and mission progress, on-
orbit activities and landing operations will be produced by 
the appropriate NASA newscenter.

Briefings

     A mission press briefing schedule will be issued prior to 
launch.  During the mission, status briefings by a Flight 
Director or Mission Operations representative and when 
appropriate, representatives from the payload team, will occur 
at least once per day.  The updated NASA television schedule 
will indicate when mission briefings are planned.

Access by Internet

     NASA press releases can be obtained automatically by 
sending an Internet electronic mail message to 
domo@hq.nasa.gov.  In the body of the message (not the subject 
line) users should type the words "subscribe press-release" 
(no quotes).  The system will reply with a confirmation via E-
mail of each subscription.  A second automatic message will 
include additional information on the service.

     Informational materials also will be available from a 
data repository known as an anonymous FTP (File Transfer 
Protocol) server at ftp.pao.hq.nasa.gov under the directory 
/pub/pao.  Users should log on with the user name "anonymous" 
(no quotes), then enter their E-mail address as the password.  
Within the /pub/pao directory there will be a "readme.txt" 
file explaining the directory structure.

  The NASA public affairs homepage also is available via the 
Internet.  The page contains images, sound and text (press 
releases, press kits, fact sheets) to explain NASA activities.  
It also has links to many other NASA pages.  The URL is: 
http://www.nasa.gov/hqpao/hqpao_home.html

Access by fax

     An additional service known as fax-on-demand will enable 
users to access NASA informational materials from their fax 
machines.  Users calling (202) 358-3976 may follow a series of 
prompts and will automatically be faxed the most recent 
Headquarters news releases they request.

Access by Compuserve

     Users with Compuserve accounts can access NASA press 
releases by typing "GO NASA" (no quotes) and making a 
selection from the categories offered.

STS-67 QUICK LOOK

Launch Date/Site:     March 2, 1995/KSC Pad 39A
Launch Time:          1:37 a.m. EST 
Launch Window:        2 hours, 30 minutes
Orbiter:              Endeavour (OV-105) - 8th flight
Orbit/Inclination:    190 nautical miles/28.45 degrees
Mission Duration:     15 days, 13 hours, 32 minutes
Landing Time/Date     March 17, 1995
Landing Time:         3:09 p.m. EST
Primary Landing Site:    Kennedy Space Center, FL
Abort Landing Sites:     Return to Launch Site - KSC
            Transoceanic Abort Landing - Ben Guerir, Morocco
                                         Moron, Spain
            Abort Once Around - Edwards Air Force Base, CA

Crew:  Steve Oswald, Commander (CDR), Red Team
       Bill Gregory, Pilot (PLT), Red Team
       John Grunsfeld, Mission Specialist 1 (MS 1), Red Team
       Wendy Lawrence, Mission Specialist 2 (MS 2), Blue Team:
       Tammy Jernigan, Payload Commander, Mission 
       Specialist -3 (MS 3), Blue Team
       Sam Durrance, Payload Specialist 1 (PS 1), Blue Team
       Ron Parise, Payload Specialist 2 (PS 2), Red Team

Extravehicular Crewmembers:  Jernigan (EV 1), Grunsfeld (EV 2)

Cargo Bay Payloads:   ASTRO-2
                      Getaway Special Canisters

Middeck Payloads:     MACE
                      PCG-STES
                      CMIX
                      PCG-TES

In-Cabin Payloads:    SAREX-II


Developmental Test Objectives/Detailed Supplementary 
Objectives:

DTO 251:   Entry Aerodynamic Control Surfaces Test
DTO 254:   Subsonic Aerodynamics Verification
DTO 301D:  Ascent Structural Capability Evaluation
DTO 307D:  Entry Structural Capability
DTO 312:   External Tank Thermal Protection System Performance
DTO 319D:  Orbiter/Payload Acceleration and Acoustics Data
DTO 414:   APU Shutdown Test
DTO 667:   Portable In-Flight Landing Operations Trainer
                    (PILOT)
DTO 674:   Thermoelectric Liquid Cooling System Evaluation
DTO 700-8: Global Positioning System Developmental Flight Test
DTO 700-9: Orbiter Evaluation of TDRS Acquisition in Bypass
             Mode
DTO 805:   Crosswind Landing Performance
DSO 326:   Window Impact Observations
DSO 328:   In-Flight Urine Collection Absorber Evaluation
DSO 484:   Assessment of Circadian Shifting in Astronauts by
             Bright Light
DSO 487:   Immunological Assessment of Crewmembers
DSO 488:   Measurement of Formaldehyde Using Passive Dosimetry
DSO 603:   Orthostatic Function During Entry, Landing and
             Egress
DSO 604:   Visual-Vestibular Integration as a Function of 
             Adaptation
DSO 605:   Postural Equilibrium Control During Landing/Egress
DSO 608:   Effects of Space Flight on Aerobic and Anaerobic 
             Metabolism
DSO 614:   The Effect of Prolonged Space Flight on Head 
             and Gaze Stability during Locomotion
DSO 624:   Pre and Postflight Measurement of Cardiorespiratory
             Responses to Submaximal Exercise
DSO 626:   Cardiovascular and Cerebrovascular Responses to 
             Standing Before and After Space Flight
DSO 901:   Documentary Television
DSO 902:   Documentary Motion Picture Photography
DSO 903:   Documentary Still Photography 


SPACE SHUTTLE ABORT MODES

     Space Shuttle launch abort philosophy aims toward safe 
and intact recovery of the flight crew, Orbiter and its 
payload. Abort modes for STS-67 include:

     *  Abort-To-Orbit (ATO) -- Partial loss of main engine 
thrust late enough to permit reaching a minimal 105-nautical 
mile orbit with the orbital maneuvering system engines.

     *  Abort-Once-Around (AOA) -- Earlier main engine 
shutdown with the capability to allow one orbit of the Earth 
before landing at Edwards Air Force Base, CA.

     *  TransAtlantic Abort Landing (TAL) -- The loss of one 
or more main engines midway through powered flight would force 
a landing at either Moron, Spain, or Ben Guerir, Morocco.

     *  Return-To-Launch-Site (RTLS) -- Early shutdown of one 
or more engines, before the Shuttle has enough energy to reach 
Moron or Ben Guerir, would result in a pitch around and thrust 
back toward KSC until the Orbiter is within gliding distance 
of the Shuttle Landing Facility.


MISSION SUMMARY TIMELINE

Flight Day One:
Launch/Ascent
OMS-2 Burn
Astro/Spacelab Activation
Instrument Pointing System Activation
Astro Observations

Flight Day Two:
Astro Observations

Flight Day Three:
Astro Observations
MACE Operations

Flight Day Four:
Astro Observations
MACE Operations

Flight Day Five:
Astro Observations

Flight Day Six:
Astro Observations
Off-Duty Time for MS 3 and PS 1

Flight Day Seven:
Astro Observations
MACE Operations
Off-Duty Time for MS 1 and PS 2

Flight Day Eight:
Astro Observations

Flight Day Nine:
Astro Observations
MACE Operations

Flight Day Ten:
Astro Observations
MACE Operations

Flight Day Eleven:
Astro Observations
Off-Duty Time for MS 3 and PS 1

Flight Day Twelve:
Astro Observations
MACE Operations
Off-Duty Time for MS 1 and PS 2

Flight Day Thirteen:
Astro Observations
Crew News Conference

Flight Day Fourteen:
Astro Observations
Flight Control System Checkout
Instrument Pointing System Stow Check and Redeployment

Flight Day Fifteen:
Astro/Spacelab Deactivation
Instrument Pointing System Stow
Cabin Stow

Flight Day Sixteen:
Deorbit Prep
Deorbit Burn
Entry
KSC Landing

PAYLOAD AND VEHICLE WEIGHTS

Vehicle/ Payload                                   Pounds

Orbiter (Endeavour) empty and 3 SSMEs             173,910

ASTRO-2 (Instruments and Support Equipment)        17,384

Getaway Special Canisters                           1,000

CMIX                                                   69

MACE (Middeck Active Control Experiment)              258

Protein Crystal Growth Experiment                     205

Shuttle Amateur Radio Experiment                       28

Detailed Test/Supplementary Objectives                171

Shuttle System at SRB Ignition                  4,520,531

Orbiter Weight at Landing                         217,683


               STS-67 ORBITAL EVENTS SUMMARY
             (Based on a March 2, 1995 Launch)

EVENT                    MET                TIME OF DAY (EST)

Launch                 0/00:00              1:37 a.m., Mar. 2

OMS-2                  0/00:51              2:28 a.m., Mar. 2

IPS Activation         0/03:15              4:52 a.m., Mar. 2

Crew News Conference  12/11:10             12:47 p.m., Mar. 14

FCS Checkout          13/11:45              1:22 p.m., Mar. 15

Deorbit Burn          15/12:25              2:02 p.m., Mar. 17

KSC Landing           15/13:32              3:09 p.m., Mar. 17



CREW RESPONSIBILITIES

Payloads and Activities      Prime               Backup

ASTRO                      Jernigan              Grunsfeld,
                                              Durrance, Parise
Getaway Specials           Grunsfeld             Lawrence
MACE                       Oswald                Gregory
PCG                        Lawrence              Gregory
CMIX                       Gregory               Lawrence
SAREX                      Parise                Oswald



DTOs/ DSOs

DTO 251:   Entry Aerodynamics Test   Oswald        Gregory
DTO 312:   Tank TPS Performance      Grunsfeld     Lawrence
DTO 667:   PILOT                     Oswald        Gregory
DSO 484:   Circadian Shifting     Jernigan, Lawrence, Durrance
DSO 487:   Immunological Assessment      All
DSO 603C:  Entry Monitoring       Jernigan, Grunsfeld, 
                                  Durrance, Parise
DSO 604:   Head/Eye Movement      Grunsfeld, Parise, Oswald
DSO 608:   Aerobic/Anaerobic      Oswald, Gregory, Lawrence
DSO 605:   Postural Equilibrium       Oswald, Gregory
DSO 614:   Head and Gaze Stability    Gregory, Grunsfeld
DSO 624:   Submaximal Exercise        Durrance, Parise
DSO 626:   Extended Stand Test        Jernigan, Grunsfeld,
                                      Durrance, Parise

Other Activities:
Photography/TV          Grunsfeld          Lawrence, Gregory
In-Flight Maintenance   Gregory          Lawrence, Oswald
Earth Observations      Grunsfeld            Lawrence
Medical                 Oswald               Jernigan


Astro-2

     A cluster of unique telescopes will turn the Space 
Shuttle Endeavour into an Earth-orbiting ultraviolet 
observatory.  This set of mechanized "eyes" will give 
astronomers a view of the heavens impossible to obtain from 
the ground.

     The mission, which will study some of the most energetic 
events in the cosmos, builds on the experience and scientific 
data obtained on the first Astro flight in 1990.  This second 
mission will fill gaps in knowledge about ultraviolet 
astronomy, expand and refine existing data, and help 
astronomers better understand our dynamic universe.

     NASA's Marshall Space Flight Center in Huntsville, AL, 
supervised development of the Astro observatory and manages 
Astro missions for the Astrophysics Division of NASA's Office 
of Space Science, Washington, DC.

Why Ultraviolet Astronomy?

     Since the earliest days of astronomy, people have used 
the light from stars to test their understanding of the 
universe.  However, the visible light that can be studied from 
Earth is only a small portion of the radiation produced by 
celestial objects.  Other forms of radiation -- like lower 
energy infrared light and higher energy ultraviolet light and 
X-rays -- are absorbed by the atmosphere and never reach the 
ground.

     Seeing celestial objects in visible light alone is like 
looking at a painting in only one color.  To fully appreciate 
the meaning of the painting, viewers must see it in all of its 
colors.

     Getting above the atmosphere with space instruments like 
the Astro ultraviolet telescopes lets astronomers add some of 
these "colors"  to their view of stars and galaxies.

     The universe of ultraviolet astronomy is strikingly 
different from our familiar night sky. Most stars fade from 
view, too cool to emit much ultraviolet radiation.  But very 
young massive stars, some very old stars, glowing nebulae, 
active galaxies, quasars and white dwarfs stand out when 
observed with instruments sensitive to ultraviolet radiation.

      Before the advent of orbiting ultraviolet telescopes, 
scientists had to be satisfied with rocket-borne ultraviolet 
telescopes.  In fact, all three Astro telescopes are based on 
prototypes flown separately on sounding rockets.  A typical 
rocket flight might gather 300 seconds of data on a single 
object.  During Astro-2, scientists expect their three 
telescopes to gather hundreds of hours of data on a multitude 
of celestial objects.


THE ASTRO TELESCOPES

     The Astro Observatory is a package of three instruments, 
mounted on the Spacelab Instrument Pointing System.

     The Hopkins Ultraviolet Telescope (HUT), developed at The 
Johns Hopkins University, Baltimore, MD, conducts spectroscopy 
in the far ultraviolet portion of the electromagnetic 
spectrum.  Spectroscopy allows scientists to learn what 
elements are present in an object, as well as identify 
physical processes taking place there.

     The Ultraviolet Imaging Telescope (UIT), developed by 
NASA's Goddard Space Flight Center, Greenbelt, MD, takes wide-
field photographs of objects in ultraviolet light, recording 
the images on film for processing back on Earth.

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment 
(WUPPE), developed at the University of Wisconsin at Madison, 
measures the intensity of ultraviolet light and its degree of 
polarization.  When light waves are polarized, or vibrate in a 
preferred direction rather than randomly, they give 
astronomers clues to the geometry of a star or the composition 
and structure of the interstellar medium it illuminates.

     Simultaneous observations by the three telescopes 
complement one another, as they provide different perspectives 
on the same celestial objects.

     Astro-2 observations also complement those of ultraviolet 
instruments on other NASA spacecraft, such as the Hubble Space 
Telescope, the International Ultraviolet Explorer, and the 
Extreme Ultraviolet Explorer -- all currently in operation.  
By combining research findings from various instruments, 
scientists hope to piece together the evolution and history of 
the universe and learn more about the composition and origin 
of stars and galaxies.

Astro-1 

     The first flight of the Astro observatory took place in 
December 1990 and lasted nine days.  In addition to the 
ultraviolet telescopes, the observatory included an X-ray 
instrument called the Broad-Band X-ray Telescope mounted on a 
separate pointing system.

     During this mission the Astro team learned a number of 
valuable lessons about operating a Shuttle-based astronomical 
observatory in orbit -- lessons that will be put to good use 
during the Astro-2 mission.

     The Astro-1 instruments captured the first views of many 
celestial objects in extremely short ultraviolet wavelengths, 
took the first detailed ultraviolet photographs of many 
astronomical objects, and made the first extensive studies of 
ultraviolet polarization.  

     The end of 1994 saw more than 110 scientific articles 
published on Astro-1 results by these four instrument teams.

     One of the first-covered Hopkins Ultraviolet Telescope 
observations was designed to test a theory which had been 
proposed about the nature of so-called "dark matter," -- a 
substantial portion of the universe's mass that astronomers 
have been unable to account for.   The observation effectively 
disproved the theory, leaving the "missing mass" in the 
universe as mysterious as ever.

     Successive papers reveal an impressively wide range of 
scientific insights obtained by Astro-1.  Observations covered 
everything from solar system objects, nearby interstellar 
medium, distant quasars, star clusters, galaxies, individual 
nebulae and stars.  Each observation helps to fill in gaps in 
our understanding of the physics of these objects.

Astro-1 Results and Astro-2 Goals
     Many Astro-2 observations will build on discoveries from 
Astro-1, while others will seek to answer additional questions 
about the ultraviolet universe.

     * Stellar evolution.  Stars like Earth's Sun are the most 
common type, emitting most of their radiation in visible 
light.  But young stars being formed, and some old stars in 
later stages of their evolution, shine brighter in ultraviolet 
wavelengths.

     On Astro-1, UIT images identified rings of massive star 
formation in several galaxies, and roughly half of the 
instruments science program on Astro-2 is devoted to studies 
of star-forming galaxies.  A unique UIT contribution is the 
identification of thousands of individual hot stars in other 
galaxies for later study by NASA's Hubble Space Telescope.

     UIT also photographed globular clusters, where there are 
often so many stars grouped together that it is impossible to 
distinguish individual stars.  The ultraviolet images picked 
out hot stars in late stages of evolution, where hydrogen has 
been depleted from the cores and energy is provided by burning 
helium.  By comparing photographs taken in different 
wavelengths, scientists were able to measure the temperature 
as well as brightness of the individual stars.

     Observing more globular clusters is a high priority for 
the imaging telescope on Astro-2.  Astronomers will compare 
the observations to theoretical predications, to help fill in 
gaps in their knowledge about these late evolutionary stages.

     All three Astro-2 telescopes will study white dwarf 
stars.  These are old stars in a transition phase -- former 
giants which have shed their cool outer layers, leaving 
dormant cores containing a Suns worth of mass within a sphere 
the size of Earth.  The hottest white dwarf stars, perhaps as 
hot as 200,000 degrees Fahrenheit (110,000 degrees Celsius), 
are very unstable and pulsate every five to ten minutes.

     * Spinning stars.  One of the surprises from Astro-1 were 
observations of stars that are spinning very fast, called Be 
stars.  A Be star is thought to be surrounded by a disk of gas 
lost from the star.  WUPPE found that the amount of polarized 
light coming from these stars was less than is seen in visible 
light and less than expected in the ultraviolet, indicating 
that some of the ultraviolet polarized light was being removed 
by the gas in the disk around the star.  The wavelengths in 
the ultraviolet where polarized light was missing told 
astronomers that there are apparently atoms of gaseous iron in 
the disks close to Be stars.  The WUPPE team will try to learn 
more about the gaseous disks by viewing more Be stars during 
Astro-2.

     * Cataclysmic variables.  Astro-1 ultraviolet telescopes 
observed cataclysmic variables -- dual star systems which 
occasionally increase dramatically in brightness as a dense 
old star called a white dwarf pulls material from its 
companion normal star.  One particularly interesting 
observation was of a variable near the peak of its brightness, 
which Astro-1 was able to view after a support network of 
amateur astronomers using ground-based telescopes reported 
seeing an outburst in progress.  Results from the Astro-1 
observations did not match theoretical predictions, causing a 
re-evaluation of current theories about this type of star 
system.

     Scientists will use follow-up observations during Astro-2 
to learn more about what triggers the sudden outbursts of 
energy in cataclysmic variables, which can increase their 
brightness 100 times or more.

     * Supernova remnants.  Supernova remnants are the ghosts 
of dead stars, expanding gaseous nebulae created by stellar 
explosions.  Observing the young remnants of a supernovas 
explosion provides the only direct test of a process called 
nucleosynthesis, whereby lighter elements are manufactured 
into heavier elements in the centers of stars.  Observations 
of old supernova remnants actually probe conditions in 
interstellar space as the shock wave encounters clouds of 
interstellar material.

     During Astro-1, all three ultraviolet telescopes observed 
the Cygnus Loop, the remnant of an explosion some 40,000 years 
ago.  Observations detected a much higher temperature and 
therefore much greater velocity of its shock wave than had 
been predicted.  The telescopes also studied the Crab Nebula,  
a relatively young supernova remnant.

     Astro-2 observations will include the Cygnus Loop and 
several other supernovas as well.

     * Galaxy morphology.  Galaxies come in a variety of 
shapes and sizes, such as gigantic spirals like the Earth's 
Milky Way, egg-shaped ellipticals and irregular shapes with no 
preferred form.  Studying the shapes of galaxies in the 
ultraviolet is a key to the study of galaxy evolution in the 
early universe.

       Before Astro-1, there were only a handful of 
ultraviolet pictures of nearby galaxies available.  UIT images 
from that mission revealed that the shapes of galaxies seen in 
ultraviolet wavelengths are strikingly different for their 
familiar forms in visible light.  One UIT goal for Astro-2 is 
the construction of an ultraviolet atlas of spiral galaxies.

     * Active galaxies.  Observations of active galaxies by 
the Astro telescopes may help astronomers explain why the 
cores of galaxies give off large amounts of high-energy 
ultraviolet, X-ray and gamma-ray radiation.

     Most astronomers believe that the radiation is produced 
by a massive black hole in the center of the galaxy, 
surrounded by a torus, or doughnut-shaped cloud of material.  
The WUPPE instrument on Astro-1 confirmed the existence of a 
thick torus, while another instrument showed unexpectedly high 
temperatures near it.  These results support the idea that 
ultraviolet radiation is being absorbed by a disk of matter 
spiraling into a massive black hole.

     Astro-2 observations will help confirm or refute this 
picture of what is happening in the centers of active 
galaxies.

     * Elliptical galaxies.  Astro-1 observations by both HUT 
and UIT shed light on a 20-year-old mystery about the source 
of faint, ultraviolet emissions in elliptical galaxies.  Such 
galaxies are thought to consist almost entirely of old red 
stars, which do not emit large amounts of ultraviolet light.
However, early astronomical satellites showed that these 
elliptical galaxies increase in brightness at short 
ultraviolet wavelengths. 

     The Astro-1 studies ruled out some proposed explanations 
for the ultraviolet emissions, and they found strong evidence 
for a previously unknown stage of stellar evolution that 
apparently is occurring in these galaxies.  During Astro-2, 
both UIT and HUT will observe more elliptical galaxies to 
confirm and extend these ideas.

     *  Interstellar dust.  On Astro-1, WUPPE used half a 
dozen bright stars like flashlights to illuminate the 
interstellar medium, literally shedding new light on the 
chemical composition and physical nature of the "dust" between 
stars in our Milky Way galaxy.  Surfaces of these dust grains 
are thought to provide a safe haven for the formation of 
molecules, clouds of which are the "womb" for the formation of 
each generation of new stars.

     Astro-1 observations revealed that some parts of the 
galaxy seem to have dust grains that may look like tiny hockey 
pucks, while other parts seem to have a mixture of several 
sizes, shapes and kinds of dust grains.  Previously, 
astronomers had thought properties of this interstellar dust 
were the same wherever the dust was found.  A major Astro-2 
goal for WUPPE will be  to determine whether these different 
types of dust grains form because conditions in some parts of 
the galaxy are different than they are in other areas.

     *  Primordial intergalactic gas.  The primary Astro-2 
goal for the Hopkins telescope is to detect the existence of 
primordial intergalactic gas, an investigation it did not get 
to perform on Astro-1.

     This helium gas in the vast space between galaxies is 
thought to be left over from the "Big Bang," the primordial 
fireball which marked the beginning of the universe.  
Existence of the gas is a logical consequence of the "Big 
Bang" theory.

     HUT will look for evidence of intergalactic helium by 
observing the light of an extremely distant object called a 
quasar, located behind the gas, much as a hazy mist can be 
viewed when it is illuminated by the beam of a distant 
flashlight.  Helium in the intervening gas would absorb light 
of a specific frequency from the quasar, altering the chemical 
signature the quasar could normally be expected to produce.

     A recent Hubble Space Telescope observation found 
evidence of intergalactic helium in the spectrum of one 
quasar.  However, HUT's spectral region permits looking at 
more nearby quasars.  Positive results from Astro-2 
observations would not only verify the Hubble findings, but 
they could allow the density and ionization state of the gas 
to be measured as well.

     *  Solar system objects.  HUT made several observations 
of the planet Jupiter and its moon Io during Astro-1, studying 
the dynamic nature of their relationship.  Io, the most 
volcanically active body in the solar system, spews out 
volcanic material into space, where it is ionized and swept up 
by Jupiter's strong magnetic field.  Ultraviolet observations 
permit a better understanding of the temperatures and 
densities of the resulting plasma.  Scientists were able to 
use HUT's more detailed spectra to reinterpret data gathered 
by the Voyager spacecraft in the late 1970s.

     More studies of Jupiter will be performed during Astro-2.
The observations will help determine the importance to 
Jupiter's atmosphere of extreme ultraviolet radiation from the 
Sun.  The telescopes also will look for changes in the 
planet's upper atmosphere resulting from recent impacts by 
fragments of Comet Shoemaker-Levy 9.

ASTRO-2 INSTRUMENTS
Hopkins Ultraviolet Telescope (HUT)

Principal Investigator:     Dr. Arthur F. Davidsen
                            The Johns Hopkins University
                            Baltimore, MD

     The Hopkins Ultraviolet Telescope conducts spectroscopy 
in the far ultraviolet portion of the electromagnetic 
spectrum.  During Astro-2, it will study a wide variety of 
objects, ranging from our own solar system and galactic 
neighborhood to very distant objects near the edge of the 
observable universe.

     The instrument team's highest priority for Astro-2 is the 
search for intergalactic helium thought to be left over from a 
primordial fireball that marked the birth of the universe 
about 10 to 20 billion years ago.  HUT astronomers will 
attempt to analyze light shining through this gas by observing 
distant quasars.

     The portion of the spectrum observed by the Hopkins 
telescope, coupled with the instrument's sensitivity, enables 
it to see a slice of the ultraviolet universe which other 
observatories are unable to detect.  HUT's spectral region 
covers wavelengths shorter than those observed by the Hubble 
Space Telescope and the International Ultraviolet Explorer and 
longer than the Extreme Ultraviolet Explorer satellite.

     HUT uses a 36-inch (0.9 meter) mirror, located in the 
back of the telescope tube, to focus ultraviolet light from 
astronomical objects into a spectrograph set in the middle of 
the telescope.  The spectrograph "spreads" ultraviolet light 
into a spectrum which can be studied in detail, in much the 
same way as a prism separates visible light into a rainbow of 
colors.  It then measures the brightness of the light at each 
wavelength.

     By analyzing how the brightness varies across the 
wavelengths, scientists can determine the elements present in 
the object, the relative amounts of each element, and the 
temperature and density of the object.  From this, astronomers 
can gain a better understanding of the physical processes 
occurring in or near the object being studied.

     HUT was designed and built by Johns Hopkins University 
astrophysicists and engineers at the university's Applied 
Physics Laboratory in Laurel, MD.  More than two dozen 
faculty, staff and students from Johns Hopkins currently are 
involved in the project.

     During Astro-1, HUT made numerous observations of active 
galactic nuclei, quasars, cataclysmic variables, nebulae, 
supernova remnants, solar system objects and other 
astronomical objects, many of which had never been studied 
before in the energy range unique to HUT.

     The telescope has been improved significantly for Astro-
2, and the science team expects it to be about three times 
more sensitive to the far ultraviolet spectrum than it was on 
its first mission.  This will allow them to obtain higher 
quality spectra and to observe fainter objects.  The primary 
mirror has been coated with silicon carbide, which is much 
more reflective to far ultraviolet light than the iridium 
coating on the original HUT mirror.  The spectrograph grating 
also has been coated with silicon carbide.

     Each time the Astro-2 telescopes point for a new 
observation, astronauts and ground controllers will use 
visible-light images on HUT's closed circuit TV camera to 
identify the desired targets and to verify that the telescope 
is pointing accurately.

     Spectra from the observations will be downlinked to the 
HUT science team in Huntsville, where Johns Hopkins scientists 
will record the data.  About 60 days after landing all of the 
science and engineering data will be sent to Baltimore.  
Scientists there will continue the detailed process of 
analyzing their collected information.



Hopkins Ultraviolet Telescope (HUT)

Telescope Optics:     Silicon carbide-coated parabolic mirror
Aperture:             36 inches (90 centimenters)
Focal Ratio:                f/2
Guide TV Field of View:     10 arc-minutes
Spectral Resolution:        3.0 Angstroms
Wavelength Range:           830 to 1860 Angstroms
            (limited sensitivity in 500 to 750 Angstrom range)
Magnitude Limit:            16
Detector:     Prime Focus Rowland Circle Spectrograph with 
                    microchannel plate intensifier 
                    and electronic diode array detector
Weight:         1,736 pounds (789 kilograms)
Dimensions:     44 inches (1.1 meter) diameter
                12.1 feet (3.7 meters) length


Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE)

Principal Investigator:     Dr. Arthur D. Code
                            University of Wisconsin
                            Madison, WI

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment 
(WUPPE) measures the polarization and intensity of ultraviolet 
radiation from celestial objects.

     Photometry is the measurement of the intensity 
(brightness) of the light, while polarization is the 
measurement of the orientation (direction) of the vibrating 
light wave.

     Light is made up of electric and magnetic waves that 
vibrate from side to side, up and down, and diagonally.  The 
polarization of light is a measure of how much more the waves 
vibrate in one direction than the others.

     Usually, light waves vibrate randomly, thus are said to 
be unpolarized.  The waves become polarized when they 
encounter a particular object or force which causes them to 
vibrate in a preferred direction.  For example, polarization 
occurs when light is emitted in the presence of a magnetic 
field or when it passes through clouds of dust grains aligned 
by an interstellar magnetic field.  The light from a comet's 
tail is reflected sunlight that becomes polarized when it is 
scattered by the ice and dust particles left in the comet's 
wake.  This is similar to the way that polarized sunglasses 
reduce the glare of scattered light.

     Determining the amount and direction of polarization and 
how these change with wavelength can tell scientists what 
caused the light waves to vibrate in a preferred direction  
indicators of a celestial object's geometry and other physical 
conditions, or about the reflecting properties of tiny 
particles in the interstellar medium along the radiation's 
path.

     The primary processes responsible for polarization within 
individual celestial objects are enhanced in observations of 
hotter, more energetic ultraviolet radiation.  The background 
clutter common in visible light studies is greatly reduced, 
which is important since polarization of the interstellar 
medium usually is not as strong in ultraviolet as in visible 
wavelengths.

     Natural light also can become polarized when it passes 
through a cloud containing dust grains aligned by an 
interstellar magnetic field.  From this scientists learn about 
the kinds of grains and can map out the magnetic fields in 
space.

     The Wisconsin Ultraviolet Photo-Polarimeter Experiment 
was built by scientists, engineers and students at the 
University of Wisconsin-Madison's Space Astronomy Lab in the 
1980s.

     Before the Astro-1 flight, only one single measurement of 
ultraviolet polarization had ever been made.  WUPPE 
observations from Astro-1 gave astronomers the first 
measurements of the ultraviolet polarization of many types of 
astronomical objects.  The instrument provided detailed 
spectral data on the polarization of some three dozen stars, 
interstellar clouds and galaxies, and ultraviolet spectra of 
an additional 20 stellar objects.

     A major Astro-2 goal for WUPPE is to follow up on Astro-1 
observations of the interstellar medium.  The science team 
hope to learn more about the causes of polarization and the 
nature of "dust" grains in the space between stars.  They also 
will follow up on observations of active galaxies and rapidly 
spinning stars.

     The WUPPE telescope examines ultraviolet radiation from 
1,400 Angstroms (around the mid-point of the far ultraviolet 
range) to 3,200 Angstroms (slightly shorter wavelengths than 
blue visible light ).  This is an area that has not been 
readily studied, especially for stars that are too bright for 
Hubble's Faint Object Spectrograph and for nebulae too large 
for Hubble's smaller spectrograph openings.

     The telescope is a classical Cassegrain-type, meaning 
that light enters the tube and strikes a large, parabolic 
mirror near the back.  The light then is reflected forward to 
a smaller, secondary mirror near the front of the telescope, 
which focuses the light back through a hole in the center of 
the large mirror.  The secondary mirror can be adjusted in 
precise increments to refocus the telescope, to allow it to 
look at objects slightly offset from those other Astro 
instruments are studying, and to perform rapid small 
corrections to the telescopes pointing direction.

     Behind the primary mirror, the beam passes through an 
ultraviolet spectrograph, a device which spreads out the 
radiation by wavelengths.  A beam-splitting prism divides the 
resulting spectrum into two perpendicular planes of 
polarization, and the two spectra are recorded simultaneously 
on two separate detectors.  Comparison of the two spectra is 
then used to study the polarization of the ultraviolet light 
as a function of wavelength.

Wisconsin Ultraviolet Photo-Polarimeter Experiment (WUPPE)
Telescope Optics:        Cassegrain system
Aperture:                20 inches (50 centimeters)
Focal Ratio:             f/10
Spectral Resolution:     6 Angstroms
Wavelength Range:        1,400 to 3,200 Angstroms
Magnitude Limit:         16
Detectors:     Spectropolarimeter with dual electronic diode 
                         array detectors 
Weight:         981 pounds (446 kilograms)
Dimensions:     28 inches (70 centimeters) diameter
                12.14 feet (3.7 meters) length


Ultraviolet Imaging Telescope (UIT)

Principal Investigator:     Theodore P. Stecher
                            NASA Goddard Space Flight Center
                            Greenbelt, MD

     The Ultraviolet Imaging Telescope makes deep, wide-field 
photographs of objects in ultraviolet light.  This type of 
imagery is a primary means for recognizing fundamentally new 
phenomena or important examples of known astrophysical objects 
in ultraviolet wavelengths.  Before Astro-1, very few 
ultraviolet images had been made and those that were available 
were taken during brief rocket flights. 

     The Ultraviolet Imaging Telescope observes a field of 
view two-thirds of a degree across, an area larger than the 
full Moon.  This is considered "wide field" for astronomers; 
each UIT photo covers an area more than 250 times the size of 
the Hubble Space Telescope's Wide Field/Planetary Camera, 
though at lower angular resolution and sensitivity.  For many 
galaxies or star clusters, this is large enough to encompass 
the entire object in a single photo frame.  In addition, the 
UIT suffers much less interference from visible light, since 
it is provided with "solar blind" detectors.

     Images made in the ultraviolet spectrum clearly show the 
dynamic events taking place beyond our world.  The clutter of 
objects which produce most of their radiation in visible light 
disappears.  Hot stars leap into prominence, the spiral arms 
of distant galaxies snap into clearer resolution, and the 
material hidden between the stars comes into view.
 
     UIT's wide-field images are ideal for investigating 
astronomical questions such as the shapes of nearby galaxies 
as revealed in ultraviolet light, the properties of massive 
hot stars, the evolution of low-mass stars, and the nature of 
interstellar dust and gas.  UIT galaxy-wide images are sky 
surveys that can locate bright ultraviolet stars for further 
more detailed study by the Hubble Space Telescope.

     The Ultraviolet Imaging Telescope was developed at NASA's 
Goddard Space Flight Center, Greenbelt, MD.  During Astro-1, 
UIT obtained a large number of images, including clusters of 
young, hot massive stars; globular clusters containing old 
stars, some of which are unusually hot; spiral galaxies rich 
with star-forming activity; and smaller "irregular" galaxies 
that can experience sudden bursts of star formation.  Astro-2 
will continue the important work of imaging the ultraviolet 
sky.

     UIT is a powerful combination of telescope, image 
intensifier and camera.  Unlike data from the other Astro 
instruments, which will be electronically transmitted to the 
ground, UIT images will be recorded directly on very sensitive 
astronomical film.  The film will be processed and analyzed 
after Endeavour returns to Earth.

     Light is reflected from a 15-inch (38-centimeter) primary 
mirror, at the middle of the telescope tube, to a secondary 
mirror near the front.  The secondary mirror is linked to an 
image motion compensation system, which adjusts it slightly as 
necessary to offset any motion or jitter in the spacecraft.  
This is critical since any motions would blur the resulting 
photographs.

     Reflected from the secondary mirror, the light passes 
through filter wheels containing six filters each.  These 
different filters allow specific wavelengths of the 
ultraviolet spectrum to be selected.  By comparing two images 
of the same area with different filters, the UIT team can 
measure the temperature as well as the brightness of every 
object in the field.

     The light then enters one of the telescope's two image 
intensifier/film transport units.  The image intensifiers 
amplify and convert the ultraviolet light into a visible image 
that can be recorded on astronomical film.  Each unit contains 
1,000 film frames.

     A 30-minute exposure can record a blue star of 25th 
magnitude, about 100 million times fainter than the faintest 
visible light star which could be seen by the naked eye on a 
clear, dark night.  Developed after the mission, each frame of 
film is digitized to form an array of 2,048 x 2,048 picture 
elements, called pixels, for computer analysis.  This analysis 
produces quantitative information about the objects whose 
images appear on the film.



Ultraviolet Imaging Telescope (UIT)
Telescope Optics:       Ritchey-Chretien
Aperture:               15 inches (38 centimeters)
Focal Ratio:            f/9
Field of view:          40 arc-minutes
Angular Resolution:     2 arc-seconds
Wavelength Range:       1,200 to 3,200 Angstroms
Magnitude Limit:        25
Detectors:     Two image intensifiers with 70-millimeter film, 
                   1,000 frames each, IIaO 
astronomical film
Weight:                 1,043 pounds (474 kilograms)
Dimensions:             32 inches (81 centimeters) diameter
                        12.1 feet (3.7 meters) length


The Astro-2 Mission
     Like Astro-1, the Astro-2 observatory will be housed 
inside the Shuttle's payload bay, with astronomers serving as 
payload specialists operating the telescopes from the aft 
flight deck of the Shuttle.  As the Shuttle Endeavour orbits 
220 miles above Earth, a large contingent of scientists and 
engineers will guide the mission from NASA's Spacelab Mission 
Operations Control Center at Marshall Space Flight Center in 
Huntsville.

     The ultraviolet telescope assembly rests on two Spacelab 
pallets in Endeavour's cargo bay.  The Shuttle and Spacelab 
systems provide power, pointing and communications links for 
the observatory.

     The telescopes are mounted on the Instrument Pointing 
System (IPS), which was part of the Spacelab equipment 
developed for NASA by the European Space Agency.  It has been 
used twice before, on Spacelab 2 in 1985 and on Astro-1 in 
late 1990.

     The IPS furnishes a stable platform, keeps the telescopes 
aligned, and provides various pointing and tracking 
capabilities to the telescopes.  During Astro-1 the IPS had 
some difficulties locking onto guide stars properly, although 
an alternate technique allowed the astronauts to manually 
point the IPS and track targets.  In general, the astronauts 
were able to provide pointing stability of about 2 to 3 arc 
seconds or better.  However, in "optical hold", the IPS should 
be able to achieve sub-arc-second stability.  A special task 
team put together by mission management at Marshall has 
extensively modified and tested the IPS software and made 
other improvements to ensure the IPS works properly for Astro-
2.

     Marshall's image motion compensation system, designed to 
eliminate jitter caused by crew motions and thruster firings 
during observations, will refine pointing and stability even 
further for the photo-polarimeter and the imaging telescope.  
When the system senses unwanted motion in the instruments, it 
sends signals which adjust the telescopes' mirrors to reduce 
jitter. This is particularly important for UIT to maintain the 
quality of its imagery, since the pictures are recorded on 
film and a single exposure can last as long as 30 minutes.

     After launch, the plan calls for a roughly 20-hour 
checkout period, though fine-tuning the observatory could take 
somewhat longer.  Observations will begin immediately after 
checkout is complete and continue throughout the mission, with 
only brief interruptions for activities such as waste-water 
dumps and Shuttle tests.

     The night launch will allow the Shuttle Endeavour to pass 
through the so-called South Atlantic Anomaly, where high-
energy radiation dips closer to the Earth than usual, mainly 
on the daylit side of its orbit.  High energy particles affect 
instrument operation and increase the background levels in 
electronic detectors. The "natural" background, such as 
scattered light and ultraviolet residual airglow emissions, is 
also higher on the daylit side.  The nighttime launch 
therefore preserves orbital night passes  when Earth is 
between the Shuttle and the Sun  for observations of the 
faintest, and often highest priority, astronomical targets.
Brighter targets will be observed during the day.

     The mission timeline, a detailed "blueprint" of the 
flight's science activities, is divided into two-orbit (three-
hour) blocks.  One of the three telescope teams will have 
priority for the entire time block and will select the 
observations during that period.  Generally, the other two 
telescopes will observe the same object or something nearby, 
though some targets may be too bright for the imaging 
telescope to view.

     The seven-member Astro-2 crew will be split into two 12-
hour shifts, so astronomical observations can continue around 
the clock.

     To begin an observation, an Orbiter crew member will 
maneuver the Shuttle's payload bay to point toward the 
celestial object being studied.

     The two science crew members on each shift, a NASA 
mission specialist and a payload specialist (an astronomer 
chosen from among the experiment teams), will have the option 
of using a pre-programmed, automatic sequence to maneuver the 
Instrument Pointing System and lock onto guide stars, or they 
may choose to acquire the target manually using a joystick-
type device.  Generally, the mission specialist will be 
responsible for pointing the telescope assembly, and the 
payload specialist will control the actual instrument set-ups 
and observations.

     Astronomers on each instrument team will receive 
telescope data at Spacelab control and adjust their 
observations as needed to obtain the best possible results.
If the data reveal something unexpected, or if an unforeseen 
astronomical event occurs (like the cataclysmic variable 
outburst during Astro-1), the instrument teams will work with 
Marshall payload controllers to develop changes in the 
timeline.  This allows the investigators to explore the 
unexpected and take advantage of science opportunities that 
may arise during the mission.

Guest Investigators

     One new feature for Astro-2 is "community involvement."
Although each of the instruments was developed by a team of 
scientists and engineers at a particular university or 
government facility, "guest investigators"  also will use the 
Astro telescopes for their own observations.  In 1993 NASA 
solicited proposals from the general astronomical community 
for participation in the observatory's second flight.  After 
scientific and technical peer review, NASA selected ten 
proposals for inclusion into the scientific program.  This has 
produced an even broader range of observations that will be 
attempted and scientific investigations that will be carried 
out.

Astro-2 principal guest investigators and their experiments 
are:

The Near UV Properties of Galaxies Which Have Low Optical 
Surface Brightness (UIT)
Dr. Gregory D. Bothun
University of Oregon
Eugene, OR

Ultraviolet Extinction and Polarization of Interstellar Dust
in the Large Magellanic Cloud (HUT, WUPPE)
Dr. Geoffrey C. Clayton
University of Colorado
Boulder, CO

O-VI Emission and Broad-Band UV Spectra of Symbiotic Systems
(HUT, WUPPE)
Dr. Brian R. Espey
The Johns Hopkins University
Baltimore, MD

Investigations of Lyman Line Profiles in Hot DA White Dwarfs
(HUT)
Dr. David S. Finley
EUREKA Scientific, Inc.
Oakland, CA

An Ultraviolet Survey/Atlas of Spiral Galaxies (UIT)
Dr. Wendy L. Freedman
Carnegie Institution of Washington
Pasadena, CA

Astro-2 Observations of the Moon (UIT)
Dr. George R. Gladstone
Southwest Research Institute
San Antonio, TX

HUT Observations of the Lyman Continuum in Starburst Galaxies 
(HUT)
Dr. Claus H. Leitherer
Space Telescope Science Institute
Baltimore, MD

Far UV Observations of Interstellar Shocks (HUT)
Dr. John C. Raymond
Smithsonian Institution Astrophysical Observatory
Cambridge, MA

The Extended Atmospheres of Wolf-Rayet Stars (HUT, WUPPE)
Dr. Regina E. Schulte-Ladbeck
University of Pittsburgh
Pittsburgh, PA

A Reconnaissance of O3 Spectra in the 900-1200 Angstrom Region 
(HUT)
Dr. Nolan R. Walborn
Space Telescope Science Institute
Baltimore, MD

Astro-2 Management Team

Headquarters, Washington, DC
Program Manager                       James McGuire
Program Scientist                     Dr. Robert Stachnik

Marshall Space Flight Center
Mission Manager                       Dr. Robert Jayroe
Mission Scientist                     Dr. Charles Meegan
Deputy Mission Scientist              Dr. Eugene Urban
Assistant Mission Scientist           Dr. John Horack
Chief Engineer                        David Jacobson
Assistant Mission Manager             Stuart Clifton
Lead Payload Operations Director      Lewis Wooten



GET AWAY SPECIAL (GAS)

    The Get Away Special (GAS) project is managed by NASA's 
Goddard Space Flight  Center, Greenbelt, MD.  NASA began 
flying these small self-contained payloads in 1982.  The 
project gives an individual an opportunity to perform 
experiments in space on a Shuttle mission.  Students, 
individuals and people from private industry have taken 
advantage of this unique project.  Space is available for 
upcoming flights, and GAS presents an educational opportunity 
for students.  There is one experiment in two payloads on this 
flight.  Following is a brief description of the payloads.

G-387 & G-388
Customer:  Australian Space Office, Depart. of Industry 
Science & Technology Customer Manager:  Dr. John S. Boyd, 
Deputy Executive Director, Australian Space Office, NASA 
Technical Manager:  Charlie Knapp

    Endeavour, an Australian space telescope, is very 
significant to the Australian space program as it makes its 
second flight aboard Space Shuttle Endeavour on mission STS-
67.  The telescope previously flew in January 1992.

    Coincidentally, the Australian payload has the same name 
as the Shuttle Endeavour.  Both were named after the sailing 
ship which the Captain James Cook commanded during an 
expedition to explore the Pacific Ocean.  In doing so he 
discovered the eastern coast of Australia and pioneered the 
way for the first settlement in Australia by Europeans.

    Endeavour is the most significant space payload built by 
the Australian space industry in more than two decades.  This 
is the program on which many Australian engineers learned 
their space skills.  This is particularly true for Auspace, 
the prime contractor for this project.  More than 200 
Australian companies also contributed to this pioneering space 
project.  The Australian Space Office of the Department of 
Industry Science and Technology, which administers the 
Australian space program, provided the funds for the Endeavour 
program.

    Outside the influence of the Earth's atmosphere, Endeavour 
will take images in the ultraviolet spectrum of targets which 
include star-forming regions, nearby galaxies and violent 
galactic events.  Such images cannot be taken from ground-
based telescopes because the radiation at these wavelengths is 
absorbed by the Earth's atmosphere.  The Australian Space 
Telescope is housed in two GAS canisters that are mounted on 
the side of the Shuttle cargo bay and are interconnected by 
means of a cable harness.  One of the canisters is fitted with 
a Motorized Door Assembly which protects the payload during 
launch and opens to allow observations to be made.  This 
canister houses the telescope, the detector and the control 
computer.

    Endeavour is a 100 mm binocular reflecting telescope.  One 
side of the telescope allows all the light from celestial 
targets to enter the other side allows only light in a narrow 
spectral band.  Thus, by the subtraction of the two signals, 
the narrow band image can be studied in detail as the brighter 
background is removed.

    The detector is a very sensitive photon counting array 
which comprises an image tube, a fiber optic image dissector 
and charged coupled arrays.  The detector counts individual 
photons, the smallest indivisible packet of light to obtain 
maximum efficiency at the low light level produced by these 
distant galaxies.

    The second canister contains the battery to supply 
electrical power to the payload and video cassette recorders 
to record the images for processing on the ground after 
landing.  The telescope has a field-of-view of two degrees and 
relies on the Shuttle for pointing.  Shuttle motion during 
exposures can be removed by subsequent ground image 
processing.

    The managing director of Auspace, Mr. T. Stapinski, said 
"Endeavour is a very important space project for Auspace.  It 
is a very complex payload of over 180 kg. (396 lbs.) and we 
learned a lot during its manufacture and testing.

    "The expertise learned on Endeavour has enabled Auspace 
engineers to make major contributions on other electro-optical 
space instrumentation such as the Along Track Scanning 
Radiometer for the European Remote Sensing satellite.  The 
Flight of Endeavour is very important as it will demonstrate 
the capability of the Australian space industry to produce top 
quality space hardware."

COMMERCIAL MDA ITA EXPERIMENTS (CMIX-03)

Overview

     The third in a series of six commercial experiments, 
known as CMIX, will fly aboard Endeavour during STS-67.  CMIX-
03 includes biomedical, pharmaceutical, biotechnology, cell 
biology, crystal growth and fluids science investigations. 

     These experiments will explore ways in which microgravity 
can benefit drug development and delivery for treatment of 
cancer, infectious diseases and metabolic deficiencies.  These 
experiments also will include protein and inorganic crystal 
growth, secretion of medically important products from plant 
cells, calcium metabolism, invertebrate development and immune 
cell functions.

     CMIX represents an innovative dual agreement program 
between NASA Headquarters and the University of Alabama in 
Huntsville (UAH) Consortium for Materials Development in Space 
(CMDS). UAH is one of NASA's eleven Centers for the Commercial 
Development of Space (CCDS).  The goals of the program are to 
provide increased access to space for NASA's CCDS 
investigators and their industry affiliates and to facilitate 
private sector utilization of space.  Through a subsequent 
agreement between UAH and Instrumentation Technology 
Associates (ITA), of Exton, PA, ITA provides flight hardware 
to UAH for its associated investigators and industry 
affiliates in exchange for flight opportunities.  ITA markets 
both the flight opportunity and hardware as a turnkey 
commercial service to both domestic and international users.

     On STS-67, UAH and ITA will fly more than 30 individual 
experiment investigations totaling some 400 samples on CMIX-
03.

     The most significant UAH CMDS/NASA CCDS experiments on 
this mission deal with microgravity research into aging, 
multi-drug resistance and neuro-muscular development.

     The most significant ITA commercial experiments on this 
flight involve the growth of urokinase protein crystals as the 
first step for use in developing an inhibitor drug to combat 
breast cancer metasis, and the microencapsulation of drugs as 
a drug delivery system for cancer therapy.


UAH CMDS Experiments

     Experiments being conducted by the UAH CMDS and 
collaborating scientists on the STS-67 CMIX-03 payload include 
aging, multi-drug effects on cells, neuro-muscular 
development, gravity sensing and calcium metabolism, 
production of plant cell products, and protein crystal growth.  
Some of the data expected from the CMIX-03 microgravity 
experiments can be used by industry to understand processes 
which can enhance the quality of life on Earth, and contribute 
to the health and welfare of the increasing numbers of persons 
spending time in space.

Aging

     Evidence from previous microgravity experiments indicates 
that gravity affects single cells.  No matter what effect any 
environmental factor produces on living systems, it begins 
with single cells or a group of single cells acting together.  
Microgravity appears to slow cell growth.  How this affects 
the aging process will be tested using human lymphocytes.


Multi-drug Resistance

     The broad objective of drug resistance experiments is to 
gain an understanding of the role of gravity and effect of 
microgravity on cell membranes.  Drugs must cross cell 
membranes to be effective;  however, many drugs lose their 
effectiveness after several years of use because patients 
develop multi-drug resistance.  Researchers believe that the 
mechanisms of multi-drug resistance may be more easily 
understood for cells in microgravity where cellular metabolism 
is slowed.  

Neuro-muscular Development

     There are a number of diseases which result from faulty 
nerve-muscle interactions and these disorders are a target for 
pharmaceutical and biotechnology industry research.  The 
development of nerve tissue is influenced by the communication 
between nerve and muscle cells and depends on membrane 
interactions.  Previous flight experiments have shown that 
microgravity slows the growth and development of these cells 
and significantly alters the cytoskeleton.  Frog cells will be 
flown as a model to investigate development of membrane 
associated interactions.

Gravity Sensing and Calcium Metabolism

     Calcium is known to regulate many cellular activities 
leading to growth, differentiation, and transduction of 
signals from the cell membrane to produce genetic responses.
The UAH investigation will fly an experiment using the 
Bioprocessing Modules to evaluate the development of gravity 
in understanding calcium dynamics in cells and has economical 
value in the area of calcium and bone metabolism.


Production of Plant Cell Products

     Pharmaceutical products from plants have been used for 
treatment of various types of cancer.  These plant products 
include vinblastin and taxol.  Cultured cells from soy bean 
plants will be flown in the MDA minilabs to assess the effect 
of microgravity on growth, development and production of 
secondary metabolites.  These cells, grown in ground-based 
tests, produce a product with strong anti-colon cancer 
activity.  Preliminary evidence suggests that microgravity may 
provide an advantage for higher production of this material.

Protein Crystal Growth

     Protein crystal growth experiments will be flown to gain 
information on the specific structure and growth 
characteristics of selected economically important proteins.  
Information will be used to develop more complex experiments 
on future missions.


Commercial ITA Experiments

     The private sector commercial experiments on CMIX-03 
utilizing the ITA hardware have three main thrusts: biomedical 
research involving the growth of protein crystals for cancer 
research;  the microencapsulation of drugs;  and an ITA-
sponsored student space education program.  

Urokinase Breast Cancer Experiment

     The most significant commercial experiment on the CMIX-03 
payload is an experiment to grow large protein crystals of 
urokinase for breast cancer research.  Urokinase is an enzyme 
which is present when breast cancer spreads (cancer 
metastasis).  ITA, with its team of scientists and engineers, 
will dedicate 60 to 90 space experiments to the growth of 
large protein crystals of at least 100 microns for analysis.  
Small urokinase protein crystals have been grown on the CMIX-
01 (STS-52) and CMIX-02 (STS-56) Shuttle flights.  The 
crystals were not large enough for analysis.  Urokinase 
protein crystals grown on the ground are not large enough for 
analysis.  If a 100+ micron protein crystal can be obtained on 
the CMIX-03 mission, the three-dimensional structure will be 
determined in the laboratories of crystallographers.  A cancer 
research center has agreed to try to develop and test drugs to 
inhibit urokinase and hence breast cancer metastasis.

     The scientists and engineers on the research team believe 
that the chance of achieving their goal of large urokinase 
crystals is enhanced because the STS-67 mission is twice as 
long (16 days) as the previous CMIX missions and the growth 
rate is believed to be linear.  In addition, the hardware has 
been modified to provide two temperatures and four separate 
crystal growth techniques.


Microencapsulation of Drugs

     The second major commercial thrust is experiments 
involving the encapsulation of drugs or living cells for new 
medical therapies.   This series of commercial 
microencapsulation experiments will continue the studies 
conducted on STS-52 (CMIX-01) and STS-56 (CMIX-02) wherein an 
antitumor drug (cis-platinum) was co-encapsulated with a 
radiocontrast medium into spherical, multilayer liquid 
microcapsules.  This is a commercial joint venture with the 
Institute for Research, Houston, TX.

     The objectives of the Microgravity Encapsulation of Drugs 
(MED) are for experiments on microcapsules to enable testing 
against tumors in mice as a necessary step towards clinical 
studies in cancer patients.

     Another separate group of microencapsulation experiments 
involves the mixing of polymer solutions which ultimately may 
be used to encapsulate pancreatic islet cells to facilitate 
transplantation into diabetic patients.

Student Space Education Program

     The third major thrust involves school students as part 
of ITA's Student Space Education Program to increase awareness 
and interest in science and space technology.  ITA is donating 
a portion of its hardware and personnel on every CMIX mission 
to flying student experiments as a "hands-on" experience for 
students.  To date, some 400 students and 30 teachers from 
seven states have participated in this private sector-
sponsored program for students to conduct Space Shuttle 
microgravity experiments on the CMIX payload.

CMIX-03 Payload Hardware

     The CMIX-3 hardware consists of four Materials Dispersion 
Apparatus (MDA) Minilabs, two of which will contain 
experiments developed by the UAH CMDS and its industry 
affiliates.  Additional hardware to fly on this mission 
includes ITA's Liquids Mixing Apparatus and UAH's 
BioProcessing Modules.  The other two MDA'S, commercially 
marketed by ITA, will contain experiments developed by ITA's 
customers, international users, and university research 
institutions.

     Dr. Marian Lewis, of the UAH/CMDS, is the Project Manager 
for the CMIX Program and Mr. John M. Cassanto, President of 
ITA, is the Program Manager for the commercial half of the 
CMIX payload.


Protein Crystal Growth Experiments

     The STS-67 mission will carry two systems in Shuttle 
middeck lockers to continue space-based research into the 
structure of proteins and other macromolecules.  Vapor 
Diffusion Apparatus trays will be housed within a temperature-
controlled Thermal Enclosure System, which fills the area 
normally occupied by two lockers.  The Protein Crystallization 
Apparatus for Microgravity will be housed in a Single-locker 
Thermal Enclosure System.

     Proteins are important, complex biochemicals that serve a 
variety of purposes in living organisms.  Determining the 
molecular structure of proteins will lead to a greater 
understanding of how the organisms function.  Knowledge of the 
structures also can help the pharmaceutical industry develop 
disease-fighting drugs.

     X-ray crystallography currently offers the best route to 
determine the three-dimensional structure of macromolecules, 
particularly proteins.  In this technique, researchers grow 
crystals of purified proteins, then collect X-ray diffraction 
data on the crystals.  The three-dimensional structure is then 
determined by analysis of this data.  Unfortunately, crystals 
grown in the gravity environment of Earth often have internal 
defects that make such analysis difficult or impossible.  

     As demonstrated on Space Shuttle missions since 1985, 
some protein crystals grown in space  away from gravity's 
distortions  are larger and have fewer defects.  The 
experiments help develop techniques and methods to improve the 
protein crystallization process on Earth as well as in space.

     Both systems will grow crystals using the vapor diffusion 
method, which has been highly effective in previous Shuttle 
experiments.  In vapor diffusion, water evaporates from a 
protein solution and is absorbed by a more concentrated 
reservoir solution contained in a wicking material.  As the 
protein concentration rises, the protein crystals form.

Vapor Diffusion Apparatus Experiments 
Dr. Larry DeLucas
University of Alabama at Birmingham
Birmingham, AL

     This investigation continues a very successful series of 
space-based protein crystal growth experiments, which has 
produced some of the highest-quality crystals of several 
proteins.  Previous experiments have helped determine the 
structures of porcine elastase, used to study emphysema; 
gamma-interferon, which stimulates the immune system and is 
used to treat cancer and viral diseases; and Factor D, 
important in understanding the bodys defenses against 
infection.

     On STS-67, the Vapor Diffusion Apparatus experiments will 
be contained in a Thermal Enclosure System (TES), which is the 
size of two mid-deck lockers.  The TES, set at 72 degrees 
Fahrenheit (22 degrees Celsius), will contain four vapor 
diffusion apparatus trays, each containing 20 individual 
crystallization chambers.  Each experiment chamber includes a 
double-barreled syringe containing protein solution in one 
barrel and precipitant solution in the other.  A reservoir of 
concentrated precipitant solution is contained in the wicking 
material lining the experiment chamber.

     To activate the experiments at the beginning of the 
mission, a crew member will turn a ganging mechanism on the 
side of each tray to push the syringe pistons forward and 
extrude the protein droplets onto the syringe tip.  During the 
course of the experiments, water molecules will migrate from 
the drops through the vapor space to the more concentrated 
reservoirs, increasing the protein and precipitant 
concentrations in the drops.  The increased concentration in 
the drops will initiate crystal growth.  At the end of the 
mission, the experiments will be deactivated by drawing the 
protein drops and crystals back into the syringes.

     [Vapor Diffusion Apparatus Experiments Graphic]

Protein Crystallization Apparatus for Microgravity
Dr. Daniel Carter
Marshall Space Flight Center
Huntsville, AL

     The Protein Crystallization Apparatus for Microgravity 
(PCAM) is the second test of a new design for growing large 
quantities of protein crystals in orbit.  It first flew aboard 
STS-63 in February 1995.  The apparatus holds more than six 
times as many samples as are normally accommodated in the same 
amount of space.

     A controlled-temperature enclosure occupying a single 
Shuttle mid-deck locker, called the Single-locker Thermal 
Enclosure System (STES), will hold six cylinders containing a 
total of 378 samples  one of the largest quantities in any 
single protein crystal growth experiment to date.  In most 
experiments of this type, a single locker accommodated a 
maximum of 60 samples.  The STES will maintain temperatures at 
72 degrees Fahrenheit (22 degrees Celsius).

     Each cylinder contains nine trays held in position by 
guide rods and separated from each other by bumper plates with 
springs. The trays are sealed by an adhesive elastomer. Each 
tray holds seven sample wells, surrounded by a donut-shaped 
reservoir with a wicking material to absorb the protein 
carrier solution as it evaporates.

     To start the experiment, a crew member will open the 
front of the thermal enclosure, then rotate a shaft on the end 
of the cylinder with a ratchet from an orbiter tool kit.  This 
will allow diffusion to start and protein crystal growth to 
begin.  Near the end of the mission, a crew member will rotate 
the shaft in the opposite direction to stop diffusion.

     A few of the candidate proteins for this flight of the 
PCAM are human cytomegalovirus assemblin (a factor in virus 
duplication), parathyroid hormone antagonist (a controlling 
factor in bone growth), pseudoknot 26 (a potential HIV 
inhibitor), human antithrombin III (a blood clotting factor), 
and an HIV protease/drug complex (a factor in viral 
replication).

MIDDECK ACTIVE CONTROL EXPERIMENT 

     The Middeck Active Control Experiment (MACE) is designed 
to study the active control of flexible structures in space.  
In this experiment, a small, multibody platform will be 
assembled and free-floated inside the Space Shuttle.  Tests 
will be conducted on the platform to measure how disturbances 
caused by a payload impacts the performance of another nearby 
payload which is attached to the same supporting structure.

     MACE consists of three separate hardware elements: The 
Multibody Platform, the Experiment Support Module, and the Ku-
Band Interface Unit.  The Multibody Platform consists of a 
long flexible polycarbonate structure.  A two axis gimballing 
payload is located at either end, and a three-axis torque 
wheel/rate gyro platform is located in the center. By swapping 
out certain components, the platform can be reconfigured into 
more complex geometries, thereby increasing the complexity of 
the control problem. Actuators consisting of 7 motors and two 
piezoelectric bending elements and sensors, consisting of rate 
gyros, strain gauges, and encoders, are distributed along the 
structure to  facilitate active control. The Experiment 
Support Module contains all the electronics necessary to 
conduct the experiment.  The Ku-Band Interface Unit allows 
downlink and uplink of data from the middeck.

     On-orbit, the astronaut will set-up the test article and 
attach it to the Experiment Support Module. A series of tests 
will be performed by using a hand-held terminal for selecting 
and controlling programmed test protocols. The astronaut will 
monitor the experiment and videotape its operation. At the end 
of each test day, the astronaut will select several of the 
test result data files for downlink via the Ku-Band Interface 
System. The MACE ground team will use this data to adjust the 
test protocols during the mission. These new protocols will be 
later uplinked and run on the hardware. MACE is expected to 
take 44 hours of on-orbit time.  Mission Commander Steve 
Oswald and Pilot William Gregory will operate the hardware on 
orbit.

     MACE is an IN-STEP (In-Space Technology Experiments 
Program) experiment, sponsored by NASA's Office of Space 
Access and Technology, that was developed by the Massachusetts 
Institute of Technology in collaboration with Payload Systems, 
Inc., NASA's Langley Research Center, and Lockheed Missiles 
and Space Company.  The experiment will provide a fundamental 
understanding of the effects of microgravity on the 
interaction between the dynamics of structures and attached 
payloads and validate control strategies and algorithms that 
will be applicable to a wide range of future space missions.


Shuttle Amateur Radio EXperiment (SAREX)

     Students from 26 schools in the U.S., South Africa, India 
and Australia will have a chance to speak via amateur radio 
with astronauts aboard Endeavour during the STS-67 mission.  
Ground-based amateur radio operators ("hams") will be able to 
contact the Shuttle through automated computer-to-computer 
amateur (packet) radio links.  There also will be voice 
contacts with the general ham community as time permits.  

     Shuttle Commander Stephen S. Oswald (call sign KB5YSR), 
pilot William G. Gregory, (call sign KC5MGA), mission 
specialists Tamara E. Jernigan (call sign KC5MGF) and Wendy B. 
Lawrence (KC5KII) and Payload Specialists Ron Parise (WA4SIR) 
and Sam Durrance (N3TQA)  will talk with the students.

     Students in the following schools will have the 
opportunity to talk directly with orbiting astronauts for 
approximately 4 to 8 minutes:

*  Brewton Elementary School, Brewton, AL (WD4SBV)
*  Watson Elementary School, Huntsville, AR (W5TM)
*  Fullbright Avenue Elementary, Canoga Park, CA (W6SD)
*  Tri City Christian Schools, Vista, CA (KK6FX)
*  Plymouth Center School, Plymouth, CT (KD1OY)
*  Bishop Planetarium & South Florida Museum, 
          Bradenton, FL (KB4SYV)
*  Renfroe Middle School, Decatur, GA (KM4LS)
*  Pearl City High School, Pearl City, HI (AH6IO)
*  Waihe'e Elementary School, Wailuku, HI (KH6HHG)
*  Highland Park H.S., Highland Park, IL (W9MON)
*  Kentucky Tech, Montgomery County Area Vocational 
           Education Center, Mt. Sterling, KY  (WD4EUD)
*  U.S. Naval Academy, Annapolis, MD (W3ADO)
*  Lutherville Elementary/Ridgely Middle School, 
           Lutherville, MD (WA3GOV)
*  Silver Spring/Burtonsville Schools, Silver 
           Spring, MD (N3CJN)
*  William Bryant Elementary, Blue Springs, MO  (WA0NKE)
*  Plank Road South School, Webster, NY  (KB2JDS)
*  Lockport H.S., Lockport, NY  (N2IQL)
*  Saint Peters School, Greenville, NC
*  Washington Senior H..S., Washington C.H., OH (N8MNB)
*  Bethany Middle School, Bethany, OK  (KB5KIJ)
*  Tarkington Middle School, Cleveland, TX  (N5AF)
*  Chisum Jr./Sr. H.S., Paris, TX  (KA5CJJ)
*  J.J. Fray Elementary School, Rustburg, VA (K4HEX)
*  Group of Scholars from South Africa, South Africa (ZS5AKV)
*  Little Lillys English School, Bangalore, India  (VY2RMS)
*  Cobram Secondary College, Cobram, Australia  (VK3KLN)


     The radio contacts are part of the SAREX project, a joint 
effort by NASA, the American Radio Relay League (ARRL), and 
the Radio Amateur Satellite Corp.   

     The project, which has flown on 15 previous Shuttle 
missions, is designed to encourage public participation in the 
space program and support the conduct of educational 
initiatives to demonstrate the effectiveness of communications 
between the Shuttle and low-cost ground stations using amateur 
radio voice and digital techniques.

     Several audio and digital communication services have 
been developed to disseminate Shuttle and SAREX-specific 
information during the flight.

     The ARRL ham radio station (W1AW) will include SAREX 
information in its regular voice and teletype bulletins.

     The amateur radio station at the Goddard Space Flight 
Center, (WA3NAN), will operate around the clock during the 
mission, providing  SAREX information, retransmitting live 
Shuttle air-to-ground audio, and retransmitting many SAREX 
school group contacts.

     Information about orbital elements, contact times, 
frequencies and crew operating schedules will be available 
during the mission from NASA ARRL (Steve Mansfield, 203/666-
1541) and AMSAT (Frank Bauer, 301/286-8496).  AMSAT will 
provide information bulletins for interested parties on the 
Internet and amateur packet radio.

     Current Keplerian elements to track the Shuttle are 
available from the NASA Spacelink computer information system, 
computer bulletin board system (BBS) (205) 895-0028 or via the 
Internet: spacelink.msfc.nasa.gov., and the ARRL BBS (203) 
666-0578.  The latest element sets and mission information are 
also available via the Johnson Space Center (JSC) ARC BBS or 
the Goddard Space Flight Center (GSFC) BBS.  The JSC number is 
(713) 244-5625, 9600 Baud or less.  The GSFC BBS is available 
via Internet.  The address is wa3nan.gsfc.nasa.gov.


STS-67 SAREX Frequencies

     Routine SAREX transmissions from the Space Shuttle may be 
monitored on a worldwide downlink frequency of 145.55 MHz.  

The voice uplink frequencies are (except Europe):
144.91 MHz
144.93
144.95
144.97
144.99


The voice uplink frequencies for Europe only are:
144.70
144.75
144.80

     Note:  The astronauts will not favor any one of the above 
frequencies.  Therefore, the ability to talk with an astronaut 
depends on selecting one of the above frequencies chosen by 
the astronaut.

     The worldwide amateur packet frequencies are:

     Packet downlink          145.55 MHz
     Packet uplink            144.49 MHz

     The Goddard Space Flight Center amateur radio club 
planned HF operating frequencies are: 

     3.860 MHz          7.185 MHz
     14.295            21.395 
     28.650


STS-67 CREW BIOGRAPHIES

     Stephen S. Oswald, 43, will lead STS-67's seven-member 
crew, serving as Commander. This is his third space flight.

     Selected as an astronaut in 1985.  Oswald was born in 
Seattle, WA, but considers Bellingham, WA, to be his hometown.  
He received a bachelor of science degree in aerospace 
engineering from the U.S. Naval Academy in 1973 and was 
designated as a naval aviator in September 1974.  Following 
training in the A-7 aircraft, he flew the Corsair-II aboard 
the USS Midway from 1975-1977. In 1978, he attended the U.S. 
Naval Test Pilot School at Patuxent River, MD. Upon 
graduation, he remained at the Naval Air Test Center 
conducting flying qualities, performance and propulsion flight 
tests on the A-7 and F/A-18 aircraft through 1981.

     Oswald resigned from active Navy duty and joined 
Westinghouse Electric Corp. as a civilian test pilot.  During 
1983-1984, he was involved in developmental flight testing of 
various airborne weapons systems for Westinghouse, including 
the F-16C and B-1B radars.  He has logged over 6,000 flight 
hours in 40 different aircraft.  

     Oswald joined NASA in 1984 as an aerospace engineer and 
instructor pilot. Since being selected as an astronaut, he has 
served as Pilot for STS-42 and STS-56, flown in January 1992 
and April 1993, respectively.  The International Microgravity 
Laboratory-1, the primary payload on STS-42, included major 
microgravity experiments conducted over the eight-day flight 
in Discovery's Spacelab module.  STS-56 was the second 
Atmospheric Laboratory for Applications and Science mission.  
This nine-day flight also included the deployment and 
retrieval of the SPARTAN spacecraft.  With the completion of 
his second mission, Oswald has logged more than 400 hours in 
space.

     William G. Gregory (Lt. Col., USAF), 37, will serve as 
Pilot for STS-67. This is his first shuttle mission.

     Born in Lockport, NY., Gregory received a bachelor of 
science degree in engineering science from the Air Force 
Academy in 1979, a master of science degree in engineering 
mechanics from Columbia University in 1980 and a master of 
science degree in management from Troy State University in 
1984.

     Between 1981 and 1986, Gregory served as an operational 
fighter pilot flying the D and F models of the F-111.  In this 
capacity, he served as an instructor pilot at RAF Lakenheath, 
U.K., and Cannon Air Force Base, NM.  He attended the USAF 
Test Pilot  School in 1987.  Between 1988 and 1990, Gregory 
served as a test pilot at Edwards Air Force Base, flying the 
F-4, A-7D and all five models of the F-15.  He has accumulated 
more than 3,500 hours of flight time in more than 40 types of 
aircraft.  Gregory was selected for the astronaut corps in 
1990. 

     John M. Grunsfeld, Ph.D., 36, also will be making his 
first space flight on STS-67.  Grunsfeld will serve as Mission 
Specialist 1.

     Grunsfeld was born in Chicago, IL, and received a 
bachelor of science degree in physics from the Massachusetts 
Institute of Technology in 1980.  He earned a master of 
science degrees and a doctor of philosophy degree in physics 
from the University of Chicago in 1984 and 1988, respectively.

     Grunsfeld has held a variety of academic positions at 
institutions including the University of Chicago, California 
Institute of Technology and the University of Tokyo/Institute 
of Space and Astronautical Science.  His research has covered 
X-ray and gamma-ray astronomy, high energy cosmic ray studies, 
and development of new detectors and instrumentation.  He also 
has studied binary pulsars and energetic X-ray and gamma ray 
sources using NASA's Compton Gamma Ray Observatory, X-ray 
astronomy satellites, radio telescopes and optical telescopes.  
Grunsfeld was selected as an astronaut in 1992.

     Wendy B. Lawrence, Commander (Select), USN, will serve as 
flight engineer and will carry the designation Mission 
Specialist 2 during her first shuttle flight.

     Lawrence, 35, was born in Jacksonville, FL, and received 
a bachelor of science degree in ocean engineering from the 
U.S. Naval Academy in 1981.  She earned a master of science 
degree in ocean engineering from the Massachusetts Institute 
of Technology and the Woods Hole Oceanographic Institution in 
1988.

     Lawrence was designated as a naval aviator in July 1982 
and has more than 1500 hours of flight time.  She also has 
conducted more than 800 shipboard landings in six different 
types of helicopters.  While stationed at Helicopter Combat 
Support Squadron SIX, she was one of the first two female 
helicopter pilots to make a long deployment to the Indian 
Ocean as part of a carrier battle group.  In October 1990, she 
reported to the U.S. Naval Academy where she served as a 
physics instructor.  Lawrence is a member of the astronaut 
class of 1992.

     Tamara E. Jernigan, Ph.D., 35, will serve as the Payload 
Commander and Mission Specialist 3 during her third space 
flight.

     Born in Chattanooga, TN, Jernigan received a bachelor of 
science degree with honors in physics in 1981, and a master of 
science degree in engineering science in 1983, both from 
Stanford University.  She earned a master of science degree in 
astronomy from the University of California-Berkeley in 1985 
and earned her doctorate in space physics and astronomy from 
Rice University in 1988.

     After graduating from Stanford, Jernigan served as a 
research scientist in the  Theoretical Studies Branch at 
NASA's Ames Research Center from June 1981 to July 1985.  Her 
research interests have included the study of bipolar outflows 
in regions of star formation, gamma ray bursts and shock wave 
phenomena in the interstellar medium.

     Selected as an astronaut candidate in 1985, Jernigan has 
held a wide variety of technical assignments including 
software verification in the Shuttle Avionics Integration 
Laboratory, operations coordination on secondary payloads, 
spacecraft communicator for five shuttle flights, lead 
astronaut for flight software development, and chief of the 
Astronaut Office Mission Development Branch.

     Jernigan's first shuttle flight was STS-40 in June 1991, 
a nine-day mission called Spacelab Life Sciences-1, the first 
mission dedicated to investigating how the human body adapted 
to microgravity.  Her second mission, STS-52 in October 1992, 
was a 10-day flight during which crew members deployed the 
Laser Geodynamics Satellite and operated the U.S. Microgravity 
Payload-1.  Jernigan has logged about 455 hours in space. 

     Samuel T. Durrance, Ph.D., 51, will be returning to space 
for a second time as one of two payload specialists for the 
ASTRO-2 mission.  He first flew in that capacity on the ASTRO-
1 mission aboard Columbia on the STS-35 flight in December 
1990.  Durrance will carry the designation Payload Specialist 
1.

     Durrance was born in Tallahassee, FL, but considers 
Tampa, to be his hometown.  He earned a bachelor of science 
and mater of science degrees in physics from California State 
University, Los Angeles, in 1972 and 1974, respectively.  He 
then received a doctor of philosophy degree in astrogeophysics 
from the University of Colorado in 1980.

     Durrance is a Principal Research Scientist in the 
Department of Physics and Astronomy at Johns Hopkins 
University, Baltimore, MD.  He is co-investigator for the 
Hopkins Ultraviolet Telescope, one of the instruments flying 
as part of the ASTRO Observatory.

     Durrance has made International Ultraviolet Explorer 
satellite observations of Venus, Mars, Jupiter, Saturn and 
Uranus.  He has directed a program to develop adaptive optics 
instrumentation resulting in the design and construction of 
the Adaptive Optics Coronagraph, which is now being used at 
the Palomar Observatory in California.  In addition, he 
participated in the design construction, calibration and 
integration of the Hopkins Ultraviolet Telescope and the ASTRO 
Observatory.  His main astronomical interests are in the 
origin and evolution of planets, both in our own solar system 
and around other stars.

     Ronald Parise, Ph.D., rounds out the STS-67 crew as 
Payload Specialist 2. Parise will be making his second space 
flight, having first flown during the ASTRO-1 mission in 
December 1990.

     Parise, 43, was born in Warren, OH, and received his 
bachelor of science degree in physics with minors in 
mathematics, astronomy and geology from Youngstown State 
University in 1973.  He received a master of science degree 
and a doctor of philosophy degree in astronomy from the 
University of Florida in 1977 and 1979, respectively.

     Parise currently is a senior scientist in the Space 
Observatories Department of Computer Sciences Corporation in 
Silver Spring, MD.  He also is a member of the research team 
for the Ultraviolet Imaging Telescope, one of the ASTRO-2 
instruments.  Parise has been involved in all aspects of 
flight hardware development, electronic systems design and 
mission planning activities for the Ultraviolet Imaging 
Telescope.  He has studied the circumstellar material in 
binary star systems using the Copernicus satellite as well as 
the International Ultraviolet Explorer.  His current research 
involves the study of the later stages of the evolution of low 
mass stars in globular clusters.


                  -END STS-67 PRESS KIT-
