FINAL AGENDA

INTRODUCTION

Dr. Huntress welcomed the Delegations to Florida and looked forward to an informative and useful meeting.

1. APPROVAL OF AGENDA

The draft agenda as distributed prior to the meeting was approved, following agreement to re-order several items of business as reflected in the final agenda.

2. Report of the Executive Secretary (C. Pilcher)

Dr. Pilcher, Executive Secretary of the IACG, noted that the minutes of the previous meeting at Sapporo, Japan had been approved by the Heads of Delegation, signed, and distributed to delegations. Some copies were available for this meeting. He also reported on his November 13, 1995 letter to Dr. Nishida, confirming the IACG's endorsement, agreed at Sapporo, of the conference "The Earth's Magnetotail: New Perspectives." The Executive Secretary also reported that Dr. Nishida had represented the IACG at the IAF meeting in Beijing.

3. Agency Reports

3.1 ESA (M. Huber, J. Credland, G. Cavallo)

Dr. Huber reported on the current status of missions in operation. ESA has completed and launched several missions. Giotto, Hipparcos, and IUE were complete; ISO and SOHO were launched in November and December 1995 respectively. Cassini/Huygens is to be launched next year. INTEGRAL will be launched in 2001, XMM in 1999, ROSETTA in 2003, and FIRST in 2006. Huber noted that IUE has worked well for 18 years, it has had a tremendous impact on astronomy, and has produced an archive that is used extensively.

The HIPPARCOS catalog, which gives the positions of 120,000 stars, was completed in August 1996 and will be released to the general public in

mid-1997.

Ulysses is now in its extended mission phase. Plots from the SWOOP instrument were presented. Huber also reported for the first time on the new ISO mission, a 2.4-ton satellite with a 60-cm telescope. With tracking support from ISAS and NASA, it will operate for two years at least, instead of 18 months as originally planned. Some results are already available. Images of enhanced star-forming regions in the Whirlpool galaxy provided new insights into the infrared (IR) world. One of most important findings is that there is water where it was thought carbon would consume all oxygen. Lines of hydrogen can also be seen. ISO has also shown that superluminous galaxies seen in the IR do not show evidence for a black hole, contrary to expectation. Last month the first results were published in Astronomy and Astrophysics.

It has a very complete payload for studying the Sun, with twelve instruments in all from several European countries and the U.S. As such, SOHO is providing the tools necessary to understand coronal holes and the origins of the solar wind. Dr. Domingo showed data from the EIT telescope with images in four lines: helium II 304 Å (60,000 degrees K) showing activity on the limb, Fe XV 284 Å, Fe IX/X 171 Å, and Fe XII 195 Å. Movies from SOHO show how plumes form and develop; spicules can be seen at 60,000 K. All operations are controlled at the Goddard Space Flight Center (GSFC). Due attention is paid to coordination with ground observatories (such as Big Bear Observatory) and other solar missions (such as Yohkoh). The SUMER and CDS instruments focus on determined areas of study showing particular regions at different temperatures so as to measure velocities, composition, densities, and temperature.

Investigators also want to look at coronal expansion into the solar wind. Dr. Domingo presented a composite image from EIT, LASCO, and UVCS which shows how solar wind streamers increase velocity on leaving the Sun and maintain acceleration at 35 solar radii. He also showed data from the CELIAS experiment, which measures isotopic composition of the solar wind.

The SWAN instrument measures the solar wind anisotropies by mapping the Lyman-alpha line over the sky. The intention is to map the solar wind evolution through the solar cycle. (This instrument also observed the Hyakutake comet in early April). Teams are now beginning to work on data analysis and the first SOHO publications will appear in Solar Physics in January, 1997. It is hoped to continue operations through solar maximum.

Mr. Credland then discussed ESA missions under development and the options for a Cluster recovery, including launching the single Phoenix spacecraft, still an open option. ESA has also looked at a 4-spacecraft Cluster-2 option involving the rebuilding of three spacecraft, followed by two launches each of two spacecraft, in late 1999 and 2000. In this case, Phoenix would become part of Cluster-2. Support for the essential Cluster-2 payload has been found in the ESA Member States and the US with one exception, and ESA could therefore launch the first pair of spacecraft in 1999, if a suitable launcher could be found. A decision by the Space Science Programme Committee is expected early next year. Construction of Phoenix is already under way.

Huygens-Cassini is under development and no problems are expected to emerge at the Flight Acceptance Review in March 1997. Launch is planned for October 6, 1997.

XMM is well into its Phase C/D construction phase, with launch advanced to August, 1999. XMM has a bus common to INTEGRAL and comprises three telescopes made up of metallic shells. Production is well under way achieving better-than-expected accuracy of 5 arcseconds.

INTEGRAL is a gamma-ray mission whose main instruments are a spectrometer and an imager. The use of a common bus with XMM has brought costs down to those of a medium-sized mission. However, there have been some difficulties, now solved, in ensuring timely funding and development of the instruments, which are procured from national agencies. INTEGRAL will be launched in early 2001 on a Proton vehicle.

ROSETTA, a cometary rendezvous mission, is an ambitious undertaking which will be done without RTGs. The mission is to be launched in January 2003, uses Mars and Earth gravity assists, and flies by two mainbelt asteroids before a 2011 rendezvous with the Comet P/Wirtanen. The spacecraft will hibernate between the years 2003 and 2011. A contractor will be formally selected in 1997. Power is an important consideration in this mission and the spacecraft's 64 sq. m. of solar panels represent a significant new development in solar power.

The Far Infrared Space Telescope (FIRST) was initially configured with Stirling coolers, but now an easier ISO-type cryostat design is being used. Various materials are under study for the antenna and decisions will be made late this year.

The cosmic background mission, COBRAS/SAMBA, has been chosen as ESA's Medium 3 Mission. It is very advanced and requires further development on detector technology. It will be launched earlier than FIRST, in mid-2004. This is an effort of the "faster, cheaper" kind, a pilot experiment trying to give more responsibilities to industry.

Dr. Huntress commented that ESA had a very impressive program. SOHO

and ISO were real observatories doing fantastic science in which NASA was privileged to be a partner. He looked forward to continuing the Ulysses mission with ESA, to yet further collaborations, and stood ready to refly Cluster.

Dr. Huntress commended ESA on being the only agency that can contemplate the large cornerstone missions.

3.2 RSA (A. Galeev)

Dr. Galeev reported that six missions are currently being supported. The oldest of these is GRANAT, on which fuel will shortly be exhausted. This mission has provided much exciting data, with the latest result being an all-sky survey in different energy ranges.

The ROENTGEN-KVANT observatory, docked to MIR, studies the energy characteristics and variability of cosmic x-ray sources. The BURST experiment, underway since 1995, involves synchronous observations of gamma-rays bursts from the Conus instrument on the U.S. spacecraft WIND and the Conus-A instrument on Cosmos-2326.

Of solar-terrestrial missions, APEX (an active plasma experiment) is presently monitoring the ionosphere, while CORONAS-I is now in passive scanning mode, having lost pointing capability.

Dr. Galeev also described the success of the Interball mission. Interball-Tail was launched August 1995 and Interball-Auroral in August, 1996. Some interesting data have been acquired on plasma at the magnetopause, showing quite surprising distribution functions. Had Cluster been available, it would have been possible to see more detail of these distributions and of plasma evolution. Observations above the polar region showed the acceleration of particles (hydrogen, helium) and raised some questions about how oxygen is accelerated. Dr. Galeev showed correlations between data taken by IMP, Interball, and WIND on Day 248, 1995, when the three missions were in proximity.

Dr. Galeev noted that the program put forward and accepted in 1990 is still in place. Several missions have been launched; other launch dates might change. CORONAS-F is currently due to launch in 1997; PHOTON, a mission from the Moscow Institute of Physical Engineering, to study electron, proton and nucleus acceleration in the solar atmosphere and heliosphere, should launch in 1998; and RELIC-2, to study the large- and medium-scale anisotropy of relict radiation and the distant magnetospheric tail, is planned for launch in 2000.

The Russian Academy of Sciences will begin giving priority to the Spectrum series of spacecraft: SPECTRUM-X (a gamma-ray mission), planned for launch in 1998; SPECTRUM-Radioastron (1999) and SPECTRUM-UVT, a UV telescope, to be launched in 2000.

The Mars-96 loss was extremely painful. It is now necessary to find a way to continue planetary exploration, probably using smaller spacecraft. This issue will go to the Council of Space Experts of the Russian Academy of Science. There is no chance of repeating the Mars-96 mission.

Dr. Bonnet asked whether the small spacecraft mentioned by Dr. Galeev to refly the Mars-96 instruments already existed. Dr. Galeev responded that new developments are likely to be too costly. Dr. Huntress commiserated, saying that space was a risky business. That was accepted: there could be great rewards, deep lows at failures, and great highs at successes. Everyone appreciated the feelings of the Russian delegation and expressed support for continued Russian planetary exploration.

3.3 ISAS (A. Nishida)

Dr. Nishida introduced the ISAS program of ongoing missions. Sakigake, launched in 1985, is degrading, but still alive. AKEBONO, launched 1989, is still operating in the high-latitude magnetosphere.

He showed a composite of the first five years of Yohkoh images, beginning when solar activity was high, and continuing through the period of low solar activity. Highlights of Yohkoh data show discoveries of:

Dr. Nishida also presented Geotail data demonstrating reconnection in extended field lines in the magnetotail. Ground-based observations identified substorms, corroborated by Geotail data. A change in the orientation of the magnetic field, which signified magnetic reconnection, was demonstrated to precede the onset of substorms. Reconnection took place at 20 or 30 earth radii.

The lifetime of Geotail is limited only by the shadowing period: the spacecraft is designed to withstand two hours of shadowing. By 1998, the umbra period will exceed 120 minutes.

The ASCA mission offers high spectral resolution capability and Dr. Nishida presented ASCA data showing observations, in five different lines and continuum, of supernova remnant v 49B.

Dr. Okuda described the Infrared Telescope in Space (IRTS)/Space Flyer Unit mission, a successful collaboration with NASA involving UC-Berkeley and Ames Research Center. After its launch by the H-2 rocket on March 17, 1995, IRTS provided four weeks of observations to April 25, 1995, and was later retrieved by the Space Shuttle in January, 1996. Although data analysis is not yet complete, a special symposium was held October 1996 to present some results. One of the most interesting of the findings was the detection of organic aromatic hydrocarbons. A map of organic emissions has been made that shows organic compounds and dust particles well mixed in space. Okuda also showed CII emission distribution data from the FILM instrument and data on interstellar dust observed by the FIRP instrument.

Dr. Okuda also presented a few preliminary results obtained through ISO, such as an IR quintuplet near the Galactic Center and the infrared detection of a radio continuum source called "The Pistol".

Dr. Huntress commented that a new era of IR astronomy was opening and the results of IRTS/SFU and ISO demonstrated the potential of IR astronomy in space. He thanked Dr. Okuda for a very interesting presentation.

Nishida noted that the new rocket M-5 will launch the MUSES-B mission, VSOP, on February 7, 1997.

Dr. Uesegi described MUSES-C, a space engineering test mission. This is an ambitious mission, using cutting-edge technologies including solar electric propulsion (SEP), autonomous navigation and guidance, sampling techniques, and high-speed re-entry (12km/sec or more). The spacecraft will travel to the asteroid Nereus, with a back-up target of 1989 ML. MUSES-C is to be launched January 7, 2002 on the M-5 rocket and will arrive in September, 2003. Departure is scheduled for November 11, 2003, and return to Earth for January, 2006. During this time, the mission will map the asteroid, skimming the surface three times, using a touch-and-go approach. It will pick up samples by shooting a projectile at the surface and collecting ejected material. Instruments on board will include a sampler; a CCD camera (narrow and wideangle) for navigation and observations; LIDAR; a Landed Surface Package provided by the US; X-ray and near-infrared spectrometers.

Dr. Huntress described this as an exciting and ambitious mission, a high-risk effort for high-value return.

Dr. Nishida then described some prospective missions on which decisions would be made by the end of the year. ASTRO-F will probably be approved. SELENE (Selenological and Engineering Explorer) proposed for 2003, is a joint lunar mission with NASDA. SELENE comprises an orbiter, lander and relay satellite. It is a relatively large spacecraft with about 14 different experiments being considered. Dr. Zelenyi, who asked about the plasma imager, was told it would make observations of the Earth from the Moon.

Two more candidate missions are under study in-house at ISAS: Solar-B, a follow-on to Yohkoh, and ATMOS, a mission to study the stratosphere and ionosphere. One of these missions will be proposed after a decision is made on the previous two.

Dr. Huntress noted that is was very exciting to hear about the science emerging from current missions. It had become clear after hearing the morning's presentations that space science around the world is very productive.

3.4 NASA (W. Huntress)

Dr. Huntress began by describing the downsizing under way at NASA. He reminded the meeting of the new science themes in the Office of Space Science (OSS). Each theme is based on a set of fundamental questions developed by the National Academy of Sciences, together with short- and long-term goals, current missions, and principal future missions.

The NASA program has been restructured to meet new budget realities. Large missions have been redirected towards smaller, less costly missions. NASA will also concentrate heavily on international missions, such as ASTRO-E with ISAS to recover science lost in the AXAF mission restructuring.

In the late 1980's through 1991, the space science budget had been experiencing double digit growth rates, leading to billion-dollar missions. More recently, the budget has been declining, with a considerable decline in the one year from 1996 to 1997. An illustration of NASA's response to this situation is the Mars Surveyor mission which will provide 80% of the science of the previous Mars Global Observer, but at one third the cost. NASA is ready to accept higher risk and use new technologies to achieve ambitious science mission goals.

The Office of Space Science Strategic Plan underwent a major revision in 1994, covering the period 1995-2000. This plan is revised every three years and so in 1997, OSS will be updating the plan with an emphasis on the period 2000-2004.

Turning to current activities, Dr. Huntress said that the SIRTF Phase C/D will start in 1998; that Cassini should be flying towards Saturn this time next year; and that Rosetta and Pluto Express should be progressing, the Pluto mission perhaps in collaboration with Russian colleagues. WIND and Polar have been launched. He noted that OSS has not had to cut off any operating missions and will continue ISTP through solar maximum. Of the remaining missions in the current Strategic Plan, Fire and Ice (Solar Probe and Pluto Express) remain under consideration. Europa is also another extremely interesting target for a future mission.

Dr. Huntress described the Hubble telescope as one of the most productive scientific missions in history and acknowledged the great contributions of ESA scientists. A sixty-hour exposure, looking as far back in time as possible, has begun to show how galaxies were constructed. Just beyond the resolution of the current telescope, one can observe an amorphous construction of sub-galactic size blue blobs that might provide more clues to the origins of galaxies.

Hubble is also showing us how stars are formed. Its images of the M16-Eagle nebula illustrate the beginning of star formation. In the Orion nebula, the telescope is observing the star-formation process at work, looking at protoplanetary disks of dust and gas. If these disks form planetary systems, then about half the stars in Orion will eventually have planets. Ground-based observations are also providing evidence of planets around other stars, indicating that planetary systems are fairly common. He noted that NASA is a one-sixth partner in the Keck observatory. The second Keck will be finished in 1997 and NASA will develop the facility as a testbed for space interferometry missions.

The Galileo probe has successfully investigated the Jupiter atmosphere. It appears to have entered an anomolously dry spot in the atmosphere. In orbit since December 7, 1995, the Galileo orbiter will pass Europa this month, with several other passes to come. Jupiter has a composition similar to our Sun.

Huntress went on to describe one of the most unexpected events from OSS's Research and Analysis program, evidence for ancient life on Mars stemming from research on a Martian meteorite. This extraordinary indication clearly requires more research. OSS will be soliciting additional research proposals in this area. The meteorite showing the evidence is very old - 4.5 billion years - compared to most Martian meteorites. A British group has confirmed the presence of organic carbon and suggested a biological origin.

Huntress pointed out that the goals of the Mars program will still stand even if evidence for life in the meteorite is not confirmed. There will be two missions (an orbiter and lander) at every launch opportunity. The intent is to have a very international program, with a sample return mission launched by 2005. He outlined the strategy of a paced mission set aimed at likely environments for life on Mars.

Huntress then described programs in Sun-Earth Connections. Three missions are still traveling out in the far reaches of the solar system. The Pioneer 10 mission ends in 1997, but the Voyagers will last until 2015 and NASA will continue to support those missions in hopes of penetrating beyond the heliopause. The SAMPEX mission has demonstrated that it is possible to learn something about the interstellar medium right here around Earth, with the discovery of the anomalous cosmic rays radiation belts. NASA's contribution to ISTP, the WIND and Polar missions, are both operating well; the fleet is up and the coordinated solar-terrestrial campaigns are beginning.

Dr. Huntress showed the same Yohkoh image, demonstrating the extreme variability of the Sun at high energies in x-rays, as had Dr. Nishida, to support the argument for the continuation of these missions through solar maximum. Such solar activity has important impacts on spacecraft, on electric power systems on Earth, and on astronauts in space. He noted that historic changes in solar irradiance seemed to track fairly well (except for volcanic activity) the change in global temperature, so it is possible that global change may come about through some combination of solar forcing and more recent anthropogenic activity. This, of course, was a rather controversial issue.

OSS will have completed a new version of its strategic plan this time next year. There has been much interest in this activity, particularly in the Vice President's Office, reflected in the planned space summit with Congress in February on NASA's budget. It is hoped that this interest will stop the decline in the agency and space science budgets. The public popularity of space science has increased significantly. There have been numerous major magazine cover stories and, for example, an entire issue of Aviation Week devoted to planetary exploration.

Dr. Bonnet noted that Dr. Huntress had not mentioned the future of HST and the next generation space telescope. Dr. Huntress responded that a refurbishing mission is planned for February, 1997 to install two new instruments - a UV spectrometer and a near IR camera. Another mission in 1999 will reboost Hubble to higher altitudes to counteract atmospheric expansion at solar maximum; a new camera will be installed at that time. A further mission is planned for 2002 for which OSS is currently selecting instruments. It is clear that OSS will operate HST as long as it is a useful tool. The 2002 mission could be the last refurbishment. Discussions are beginning on what comes next and it is expected that a replacement for HST will be launched some time before the end of the next decade.

Dr. Zelenyi asked whether activities in space weather would go to another agency. Huntress said OSS will soon launch ACE, a spacecraft with space weather capability; the subject is still within NASA's purview.

Dr. Oraevskii asked about new smaller spacecraft programs. Dr. Huntress described the New Millennium program that will test new technologies and also perform some science. The Deep Space-1 mission, for example, will test ion propulsion. In addition, OSS runs the Explorer program, comprising the university (UNEX), small (SMEX), and medium-scale explorers (MIDEX). Thirdly, the Discovery program includes small missions such as Near-Earth Asteroid Rendezvous (NEAR) and Mars Pathfinder. Those programs will be open to international opportunities. He referred Dr. Oraevskii to the new NASA Announcement of Opportunity (AO) for SMEX.

Dr. Oraevskii followed up with a question about solar-terrestrial physics.

Dr. Huntress noted that the Explorer program included solar-terrestrial physics. He also expressed optimism about a New Start for the TIMED mission in 1998. He hoped to start a series of such solar-terrestrial missions but this will require Congressional approval.

Dr. Bonnet asked for more details on NASA's thinking about the post-Hubble era. Dr. Huntress explained that the next telescope after Hubble would fly in the 2005-2010 timeframe, dependent on the development of appropriate new technologies. NASA would not again be able to fly a Hubble-type spacecraft–it was too big and too expensive. So the next telescope will require the development of thinner or deployable mirrors, and/or adaptive optics, to reduce mass while providing increased aperture size.

Asked about the use of Space Station, Huntress said there is an opportunity for appropriate science experiments.

4. REPORTS FROM THE WORKING GROUPS

4.1 WG-1 Report (A. Pedersen)

Dr. Pedersen described the joint meeting held between WG-1 and WG-2 on December 9. He described the four coordinated campaigns and noted that now researchers were harvesting results. He very much regretted the loss of Cluster, which had been a major part of Campaign Two. He noted that the delays some of these missions had experienced also had advantages, as technology and methods of data exchange have advanced tremendously. Much useful material, such as the orbital elements of the main spacecraft, was now on the World Wide Web, accessible to a large community. There is a continued need for agency support to develop these data on the Internet and to bring the campaigns to a successful completion.

Campaign One: Dr. Pedersen described some of the results which have been shown at a number of workshops. For example, he showed Geotail data on 160 substorms at 50-200 Earth radii. These data were presented at the Chapman Conference on Geotail. Dr. Pedersen also presented figures from Dr. Zelenyi showing Geotail and Interball conjunctions providing opportunities for joint data-gathering.

Campaign Two: Dr. Pedersen commented that ACE will be able to support Cluster 2 once relaunched. SOHO will still be in orbit, as will Yohkoh, so several important missions will still be available to support Campaign Two at the later date.

Campaign Three: Data from SOHO and Yohkoh are being used to identify coronal mass ejections (CMEs). Dr. Pedersen presented a September 25, 1996 figure of a large filament precursor to a CME. He noted that Campaigns Three and Four are closely related: Campaign Three focuses on results of solar activity at the Earth, while Campaign Four focuses on the outward effects. An ESLAB symposium, "Correlated Phenomena at the Sun in the Heliosphere, and in Geospace," is planned for September 22-23, 1997 at ESTEC, Noordwijk, the Netherlands. This will present results from Campaigns Three and Four, concentrating on the data from the September, 1996 event. Dr. Pedersen asked for IACG endorsement of this symposium, which was later forthcoming.

He then presented the recommendations of the joint WG-1 and WG-2, which follow:

A fifth recommendation, on difficulties of using the Internet in certain areas, was withdrawn for further study of the issue. Dr. Bonnet asked that Recommendation 4 state more clearly what is required of the Heads of Delegation.

4.2 WG-2 Report (J. Green)

WG-2 Green: Dr. Green, as Lead Coordinator, reported on the first campaign, "Magnetotail Energy Flow and the Role of Non-Linear Dynamics". The first phase, "Structure of the Global Magnetotail System" had produced some exciting results, and investigators stood ready to initiate the second phase, "Dynamic Solar Wind/Magnetotail Interactions". He reminded the meeting of the objectives of the first campaign and of the intervals that had been selected at the IACG meeting in Sapporo, Japan, in 1995.

During the first interval, October 18-21, 1995, a major event occurred when a well-ordered magnetic field formed and passed around the Earth. WIND data from October 18-20, 1995 showed a stable structure, moving at a fairly constant speed. Yohkoh data indicates the solar origin of the cloud - a flux rope with a twined helical magnetic field. Yohkoh x-ray data showed flares produced in association with the cloud and observed by WIND. Many science presentations based on Campaign One, in particular on the Magnetic Cloud Event, have been given and there was a lot of interest at both the Fall and Spring AGU meetings in 1996.

During phase two of Campaign One, the optimal campaign period is between November 1996 and January 1997, with favorable months both at the beginning and the end of that period. Dr. Green expects the Campaign to be more productive now that the key missions are in place.

Dr. Huntress commented that it was gratifying to see results of the science campaign planning coming forth.

Dr. Green then turned to the WG-2 status report. There have been many presentations. The World Wide Web is now the method of data exchange. (The URL for IACG is http://iacg.org.) He noted that all spacecraft situation data is available on the WWW, together with key parameter data and retrospective data from different agencies. He demonstrated how the Web allows campaign participants to access images and line plots. In one month, September to October, 1996, there were well over 2000 accesses to the IACG pages.

Dr. Huntress commended WG-2 for its very valuable work.

4.3 WG-3 Report. (K. Uesugi)

Dr. Uesugi noted that almost all spacecraft involved in the IACG's current activities have now been launched. WG-3's Handbook was published a couple of years ago and the WG also produced the SPIN software on spacecraft orbits. Since the Sapporo meeting, however, there has been no activity, although the group stood ready for new tasks.

5. REPORTS FROM PANELS

5.1 Panel 1 - Space Very Long Baseline Interferometry (VLBI) (F. Jordan)

Dr. Jordan reported that the "synthesized aperture in space," the flagship VSOP mission would be launched on February 7, 1997 on the M-V launcher. A second mission, Radioastron, a Russian mission that includes international collaboration, is currently under development. Most of the payload is now in Russia undergoing integration testing. The antenna is made from carbon panels, parts of which will be thermal tested at ESTEC next year. The antenna fits within the Proton shroud above the Spectrum bus.

The VLBI Panel had been active in the development of both concepts. The Panel has worked over several years to encourage compatibility and standardization in observing and tracking frequencies, data transmission formats, and the like. Now the Panel was awaiting the VSOP launch and its results. The next generation VLBI mission was under discussion. One concept was ARISE (Advanced Radio Interferometry between Space and Earth). This concept would have a higher orbit, use higher frequencies, and offer twice the sensitivity and resolution of VSOP. The mission would use a lightweight, inexpensive, inflatable antenna, a 10m version of which has been tested with partial success. The dish did inflate, but not into the shape necessary for a radio astronomy antenna. Further collaboration with the Department of Defense is planned.

A Russian concept, Millimetron, is also under consideration. It offers a high-frequency precision antenna, with very long baselines, and might be a suitable candidate for the latter half of the next decade.

Once VSOP science is in hand, Panel One could have a role in determining what the next step might be. It will be important to maintain coordination with ground-based investigators.

Dr. Huntress asked what the high-frequency limit was using inflatable antenna technologies. Dr. Jordan responded that the goal of the inflatable technology program was to obtain 1 mm surface accuracy for a 25-m dish. This would support space VLBI to a frequency of 43 GHz. Submillimeter observations would probably require a different technology for at least the next decade.

5.2 Panel 2 - Planetary and Primitive Bodies (J. Rahe)

Dr. Rahe described many areas of collaboration, commenting particularly on Mars Exploration. A ten-year sustained, integrated Mars Surveyor Program has begun, and a Mars sample return mission is under consideration. In 1996, Mars mission objectives focused on surface morphology, geochemistry, and the atmosphere, through the Global Surveyor Orbiter and Mars Pathfinder (a Discovery mission). In 1998, science objectives will focus on the evolution of climate and volatiles, using the Mars '98 Lander and Orbiter. Dr. Rahe also noted the Japanese mission Planet-B. The 2001 Mars Surveyor mission will look at volatile and climate history; the 2003 mission will prepare for a sample return, the first of which is expected in 2005. He noted that two New Millennium missions also focus on planetary science: Deep Space-1 will undertake a flyby of an asteroid and a comet, and Deep Space-2 will send small probes to Mars. The approach involves collaboration within NASA, with the Europeans (whether ESA or member nations) and with both Russia and Japan. Dr. Rahe pointed out that of all the collaborative missions planned, none has more than two space agencies involved. He said that beginning in 1997, international workshops will be held to coordinate current and future Mars missions, similar to the coordination of Comet Halley activities.

Dr. Uesugi asked about the DS-2 Mars probe. Dr. Huntress explained that this would be a test of a lightweight penetrator.

5.3 Panel 3- High Energy Astrophysics (A. Bunner)

Dr. Bunner reported that all four instruments on the Compton Gamma Ray Observatory are operating in excellent condition. The Observatory provides pointed observations covering 60 keV to 100 GeV and all sky monitoring for gamma bursts and bright galactic sources for 15 keV to 1 MeV. Some 1500 gamma ray bursts have been observed, but their origins are still a mystery.

The Japanese satellite ASCA is providing x-ray spectroscopy with imaging over the spectral range 0.5 to 10 keV. All focal plane instruments are operating with excellent performance. He noted that strong gravity is becoming an observational science.

The Rossi X-ray Timing Explorer (XTE) was launched in December 1995 and all instruments are operating well, providing an x-ray all sky monitor capability and spectroscopy over 2-100 keV. This is a U.S. program but with international Guest Investigators. The mission is producing new results in relativistic astrophysics, as bursting pulsars are observed producing enormous bursts of x-rays at random times, which change the spin period and speed up the rotation of the crust of the star.

He noted the loss due to launcher failure of the High Energy Transient Experiment (HETE), in November 1996, which has left a gap in our ability to resolve the mystery of gamma-ray bursts. This mission had the power to provide accurate burst locations by means of simultaneous x-ray and possibly even optical signals. The Argentinean SAC-B spacecraft, carrying two gamma-ray burst experiments and a diffuse background experiment, was also lost.

Plans for the near future include a number of missions, most of which involve international collaborations. The first three (Spectrum-X-Gamma, AXAF and XMM) are "great observatories" with very different capabilities: AXAF offers very deep, high angular resolution imaging; Spectrum-X-Gamma provides polarimetery and Bragg spectroscopy; and XMM will provide very high collecting power and grating spectroscopy.

Dr. Bunner also discussed roadmappingwithin NASA for the Structure and Evolution of the Universe (SEU) theme, one of the four science themes in OSS that Dr. Huntress described earlier. The SEU science and technology roadmap outlines fundamental science quests for SEU, science campaigns, candidate missions, and requisite technology to address those missions.

One of these campaigns will focus on jets and outbursts, a common theme in high-energy astrophysics. These have been receiving increased attention and can be observed on all scales in the Universe. Hubble images have shown us super-relativistic outflow from an active galactic nucleus, and even at stellar scales, jets from young stars can be observed.

A recent cover of Nature had featured black holes, always a topic of interest with the general public. Dr. Bunner pointed out that there have been several interesting discoveries in this area and that the phenomenon had first been discovered by high-energy instruments.

Dr. Hudson asked about the prospects for gamma-ray bust monitors in future planning efforts. Dr. Bunner said that as these were light in weight and demanded a low data rate, there might be opportunities, although the cruise phase of missions was not usually designed to send back data.

Dr. Bonnet questioned the added value of Panel 3, contending that the coordinated observations would have happened naturally. Dr. Bunner felt that the Panel presented a useful forum for sharing future plans and to ensure that areas of coverage for all-sky monitors and mutual plans for data archiving, for example, were fully understood. It was pointed out that most discussions take place at bilateral meeting and not at specially convened Panel meetings.

Dr. Sunyaev referred to the recently announced discovery of new sources of gamma-rays and noted that spacecraft from the three space agencies should observe these sources. IACG is an extremely important forum for information exchange and the right forum to recommend lightweight gamma-ray burst monitors on many spacecraft. The Russian Space Agency is very sensitive to the opinions of other agencies, especially those of the IACG, and he felt that it would be a loss if the Panel were abandoned.

The meeting then adjourned for the day. On reconvening, Dr. Pilcher took the Chair as Dr. Huntress had left early that morning to attend a meeting with Vice President Gore in Washington D.C. on future space activities.

6. Conclusions on Recommendations

Dr. Pedersen presented WG-1's recommendation on combining WG-1 and WG-2. Dr. Pilcher noted that this was entirely consistent with a proposal discussed by Heads of Delegation, so this Recommendation was accepted.

Recommendation Two asked for IACG support for recovery of Cluster science. Dr. Galeev expressed his support as Cluster science was outstanding. Dr. Pilcher, while noting that ESA must be in the lead on this issue, expressed NASA's support of the recommendation. Dr. Bonnet said he would abstain on this issue. However, he explained that ESA was considering two options, not mentioned in the recommendation. The date of 2000 appearing in Recommendation Two implicitly selected Option 1, the only one which could be launched in 2000. However, he would not ask for a change of the written text. The recommendation was accepted as written by the other Heads of Delegation.

Recommendation Three on extending solar-terrestrial missions in operation through solar maximum was supported by all delegations. It was noted that NASA has budget concerns but will make every effort to resolve those to enable these mission extensions.

Recommendation Four, re-written at Dr. Bonnet's request, now read:

Dr. Pedersen understood there had been discussions on archiving in talks on the future of the IACG. This recommendation was accepted as entirely consistent with agreements at the Heads of Delegation meeting.

He also requested IACG endorsement of the ESLAB meeting on Campaigns Three and Four to enhance international collaboration. Dr. Pilcher agreed to write a letter of endorsement.

Dr. Pilcher then called for any other recommendations. Dr. Kardashev said that by next IACG meeting the first results from Muses-B would be available. Many problems were anticipated with this new and complex mission. At the next IACG meeting, Panel 1 will have prepared some recommendations for future work based on results from Muses-B. It was likely to discuss the future of Radioastron in light of these results. Dr. Pilcher said this topic would be taken up later in the afternoon.

Dr. Bunner, speaking for Panel 3, noted the agreed need for gamma-ray burst monitors on all missions to other planets and urged all agencies to consider this. Dr. Rahe commented that instruments for all NASA missions will be selected through an Announcement of Opportunity, so investigators could indeed propose such an instrument. Dr. Bonnet and Dr. Nishida agreed that the same held true for all agencies, so no promises could be made on flying these detectors.

7. UPDATE ON INTERNATIONAL SPACE SCIENCE INSTITUTE (ISSI)

Professor Geiss described activities at the Institute, which began work in the fall of 1995. The Chair of the Board, H.P Scheiter is an executive from the Swiss aerospace industry and all four IACG Heads of Delegation are on the Board and have visited the Institute. The Chair of the Science Committee is Dr. David Southwood of Imperial College, London.

ISSI will focus on a number of topics: the physics and chemistry of comets; the heliosphere; solar-terrestrial physics; solar wind and solar processes; planets; the origin of the solar system; cosmology and galactic evolution; and the Earth.

Prof. Geiss noted that ISSI is encouraging an interdisciplinary approach to science topics. One area of interest is the study of the environment both outside and inside the heliosphere and across the heliopause. Comets, for example, do not respect these boundaries and bring with them certain phenomena such as the transport of interstellar helium across the heliopause.

The Institute has three modes of operation: workshops, working groups, and teams. The need for publications gives discipline to meetings, and the goal is to publish quickly, still maintaining high quality. The first book,"The Heliosphere in the Local Interstellar Medium,"presented at the meeting, was published in November, 1996. In addition to achieving quick publication, the ISSI working groups develop recommendations from their studies and the Institute staff then works with spacecraft and instrument builders to try to achieve the recommendation.

About 250 scientists have already attended extended study periods at ISSI and an increasing number of Russian and Japanese scientists also attend, despite travel expenses.

Dr. Pilcher, on behalf of Dr. Huntress, congratulated Prof. Geiss on the remarkable achievement of realizing the vision expressed to the IACG over a number of years. He knew that US participants have expressed appreciation for the work of ISSI.

8. INTERNATIONAL MARS EXPLORATION WORKING GROUP (IMEWG) REPORT (M. Coradini)

Dr. Coradini presented the IMEWG report on behalf of its Chairman, Dr. Waenke. At its meeting on December 2-3, 1996 at Cape Canaveral, Florida, IMEWG members discussed the loss of the Russian mission, Mars-96, and agreed on a two-fold resolution. First, it is important to recover the scientific objectives; it is also important to respect the different working methods of different space agencies. There was agreement on the priorities for science data recovery, the collection of high-resolution data and the study of the planet's internal structure. It was suggested that a small orbiter might be provided by a group of European countries (such as France, Germany, and Italy) that could use the flight spares of the existing payload. Key instruments were the high-resolution stereo camera (HRSC), the visible-near infrared spectrometer (OMEGA), and the planetary Fourier spectrometer (PFS) for atmospheric studies.

Secondly, IMEWG focused on the general scenario of Mars exploration. A huge scientific gap appears, as no Martian surface network mission is on any agency agenda. It is now necessary to redefine the strategic scenario of Martian exploration, from which all agencies can select the missions of interest. A small working group with one representative from each agency will be established to devise this framework by the end of 1997.

9. INTERNATIONAL LUNAR EXPLORATION WORKING GROUP (ILEWG) REPORT (H. Mizutani)

The major event for ILEWG was the organization of the Second International Lunar Workshop, October 15-17, 1996 in Kyoto, Japan, hosted by ISAS and NASDA. Over 140 representatives from 11 countries participated in four working groups: Science of the Moon; Science from the Moon; Utilization of the Lunar Environment and Resources; and Infrastructure Development.

A final declaration on the purposes and results of the meeting was issued (See Appendix 3). The issue of Science , November 1, 1996 carries a report of this meeting. Dr. Pilcher commented that the meeting was very well organized in a pleasant venue. The next meeting will be held in Moscow in 1998. Dr. Galimov, Director of the Vernadsky Institute for Geochemistry, will become the next chairman in 1997.

10. IACG after ISTP

Dr. Pilcher summarized discussions at the Heads of Delegation meeting on December 9, at which they had agreed on a number of items. He reported that several topics had been examined as potential foci for IACG after ISTP, with the central areas of attention on solar system exploration. The Heads of Delegation therefore proposed to form a new Working Group-1 within IACG to focus on solar system exploration. A new Working Group-2 would be formed by combining the existing WG-1, -2 and -3 to continue coordination of current solar-terrestrial missions. A new Working Group-3 would be formed to focus on data archiving. It was also proposed to form a new Panel on infrared astronomy.

It was proposed that the work of the new WG-1 include exobiology/life science as well as consideration of future solar missions, given that the Sun is part of the solar system. Coordination of current solar missions will remain with the new WG-2. No specific focus of solar system exploration was defined but a small definition team (M. Coradini, V. Moroz, C. Pilcher, and K. Tsuruda) will report back in one year on the proposed scope and terms of reference for the new WG-1.

Dr. Green proposed, and it was agreed, that Dr. Pedersen serve as Interim Chair of the new WG-2 and write new terms of reference.

During discussion Dr. Bunner proposed a slight change to the title of the new Panel 2, to "Infrared and Submillmeter Astronomy", which was agreed.

Dr. Bonnet noted that the IACG has always provided very good service to the scientific community when it had something to do. However, it should not perpetuate itself when there was no clear objective. He felt that Panel 1 on VLBI was dormant and should be terminated. Dr. Nishida proposed a compromise panel structure, which was agreed. Two panels would operate (Panel 1 on High-Energy Astrophysics - the former Panel 3; and the new Panel 2 on Infrared and Submillimeter Astronomy). The space VLBI community would report on suggested activities at the next plenary meeting. (See Appendix 4 for changes in Working Group and Panel structure).

11. WORKING GROUP AND PANEL MEMBERSHIP (C. Pilcher)

Rather than decide at the meeting on the scope of activities and membership, it was agreed to establish two more definition teams, one each for the new WG-3 and new Panel 2 to report back to the next meeting. By January 1, 1997, the Heads of Delegation would forward the names of members of these definition teams to Dr. Pilcher. The membership of Panel 1, High Energy Astrophysics, would remain unchanged from that of the previous Panel 3.

12. PROPOSAL TO ESTABLISH A SOLAR PHYSICS PANEL (M. Huber)

In raising the desirability of a solar physics panel, Dr. Huber noted that the Terms of Reference of the IACG (as of the November 1986 meeting in Padua, Italy) described exchanges of information on future plans as desirable, although no formal role was allowed in future mission planning. The scientific objective of any new solar panel would be to achieve a three-dimensional view of the Sun, normally observed from the ecliptic, and so multiple spacecraft would be required. A solar panel would:

Relevant missions and studies include TRACE, Solar-B, Close Fly-by missions, Inter-Helios, Solar Stereo, SOHO, Yohkoh, Coronas, and the Horizons 2000 solar missions.

Dr. Pilcher said everyone could agree on the scientific value of these issues but asked what the best forum was for discussing them. There were three options: i) a new panel, ii) the new WG-1, or iii) the new WG-2. Dr. Galeev said that this work was needed but that it should be conducted within the ISTP Working Group (new WG-2). Dr. Pilcher believed that since the old WG-1 had a solar physics membership, Dr. Huntress would agree with Dr. Galeev. Dr. Nishida said a solar physics panel could be useful. Dr. Bonnet expressed his concern at possibly creating a pressure group, while other disciplines would not have the same opportunity. He felt that either the new WG-1 or WG-2 could do this work. He would wait until new missions are approved before creating a new panel. Dr. Huber suggested its incorporation into the new WG-1 but Dr. Pilcher suggested that the meeting await the definition team's work on the new WG-1. A subset of WG-2 should work with that definition team for the new WG-1 to have the solar physics' view represented.

In response to Dr. Bonnet's suggestion of a workshop on a 3-D study of the Sun, Dr. Huber said such a workshop is indeed planned for February, 1997. Dr. Pilcher said that the IACG could consider sponsoring this workshop.

It was agreed that a fourth definition team, consisting of the Chairs of old WG-1, -2 and -3 would work with the definition team for the new WG-1 concerning issues in solar physics.

13. ANY OTHER BUSINESS

Dr. Rahe showed a video animation of the landing of Mars Pathfinder on Mars which was very well received.

Dr. Bonnet commended the group for a useful, historical meeting, taking place on the edge of a new era. He congratulated NASA on the organization of meeting.

14. DATE AND PLACE OF NEXT MEETING

Dr. Galeev proposed to host the next IACG meeting somewhere in the Golden Ring cities around Moscow. Owing to the launch of Cassini on October 6, 1996, and the ESLAB meeting scheduled for September 22-25, 1997, it was agreed to meet the week of September 15, 1997.

The 1996 meeting then adjourned.

Dr. W. Huntress Dr. R. Bonnet

Head of the NASA Delegation Head of the ESA Delegation

Prof. A. Galeev Prof. A. Nishida

Head of the Russian Delegation Head of the ISAS Delegation

Appendix 1

ESA Russian Space Agency

R. Bonnet, Head of Delegation A. Galeev, Head of Delegation

G. Cavallo A. Boyarchuk

M. Coradini N. Kardashev

J. Credland V. Moroz

D. Dale R. Nazirov

V. Domingo V. Oraevsky

J. Geiss R. Sunyaev

M. Huber L. Zelenyi

A. Pedersen

R. Schmidt

ISAS NASA

A. Nishida, Head of Delegation W. Huntress, Head of Delegation

Y. Matogawa A. Bunner

H. Matsuo R. Carovillano

H. Mizutani G. Gloeckler

I. Nakatani J. Green

Y. Ogawara E. Huckins

H. Okuda H. Hudson

K. Tsuruda J. F. Jordan

K. Uesugi H. Lancaster

C. Pilcher

J. Rahe

G. Withbroe

Appendix 3

The Second International Lunar Workshop was held in Kyoto, Japan hosted by the Institute of Space and Astronautical Science and the National Space Development Agency of Japan from 15th through 17th October, 1996. The Workshop was held under the auspices of the International Lunar Exploration working Group which was formed by the world's space agencies in response to the first International Lunar Workshop in Beatenberg, Switzerland, 1994. Over 140 representatives from space agencies, industry and academia met and discussed means of better international communication, coordination and collaboration on both on-going and conceptual programs to explore and utilize the Moon. Several space agencies now have lunar missions in development and/or planning stages, such as Lunar-A, Lunar Prospector, and SELENE. The Workshop participants were enthusiastic about the progress made since Beatenberg in the first phase of lunar programs.

International cooperation and coordination are now increasingly important. International discussions are recommended in order to harvest the return from available data and to maximize the effectiveness of all projects.

It was emphasized that scientific exploration, infrastructure development, and use of the Moon are all important aspects of lunar programs. The workshop agreed that there should be increased international effort to study and coordinate a worldwide long term initiative to explore and use the Moon as an important step within the context of space exploration. Four working groups met to address various aspects of lunar exploration and utilization.

Working group #1, which examined "Science of the Moon" identified "Origin of the Moon and evolution of the Earth/Moon system" as principal theme underlying science of the Moon. The Moon is an accessible testbed or natural laboratory for fundamental processes active on planetary surfaces. A strategy for exploration initially includes missions which assesses the global composition and geophysical properties of the Moon. An international integrated strategy also includes a mix of advanced exploration and experiments involving landers with capable rovers, long-term network packages, and multiple sample return. Understanding the history of the sun and impact history of the Earth from lunar studies are important scientific issues.

Working Group #2, "Science from the Moon" emphasized the importance of the near term technology demonstrations on the lunar surface, which could lead to a variety of large scale astronomical instruments. Opportunities should be stressed in areas where the Moon provides unique advantages.

Working Group #3, "Utilization of lunar resources and environment" agreed that the Moon is a place where we can test the concept of using local resources, e.g. oxygen, in support of lunar activities and other activities in space. In addition, the feasibility of beaming solar power to Earth or providing lunar He3 for safe terrestrial fusion energy should be examined.

Working Group #4, "Lunar infrastructure development" agreed that an international lunar program should be based on the guidelines of the four-phase approach proposed at the Beatenberg Workshop. The acquisition of the necessary tools (basic data, technologies, infrastructure elements) should be pursued on a worldwide basis. The exploration of the Moon and the establishment of a permanent lunar infrastructure for a human-tended-base are crucial steps required to support and enable human expansion into space and missions to Mars and beyond.

It is expected that the work discussed and initiated at this Workshop will be continued through electronic communication and at future international workshops. The next International Lunar Workshop will be convened in Moscow, Russia in 1998.

Kyoto, Japan

17th October 1996

WG-1: Science

WG-2: Data Exchange

WG-3: Mission Design and Planning

P-1: Space VLBI

P-2: Planetary and Primitive Bodies

P-3: High-Energy Astrophyiscs

WG-1: Solar System Exploration

WG-2: ISTP (current WG-1, -2, and -3 combined)

WG-3: Data Archiving

P-1: High-Energy Astrophysics

P-2: Infrared/Sub-mm Astronomy

Space VLBI to report at next Plenary meeting