The New Horizons Mission to Pluto-Charon and the Kuiper Belt is under development for launch in 2006. The experiment complement of eight sensors addresses fundamental issues of density, composition, albedo, geology, and atmospheric state, chemistry, and escape.

We report on current Mars mapping projects in support of NASA planetary exploration. This includes a summary of the current state and accuracy of such mapping at global, regional, and local (human) scales. The availability of Mars Orbiter Laser Altimeter data has revolutionized such mapping. Aside from its use as a global topographic dataset, images can easily be correlated to it with absolute uncertainties of ≈100 m horizontally. We are using this to create a revised version of the global Mars digital image mosaic (MDIM) that will have absolute errors of ≈231 m (one pixel) and improved cosmetic characteristics. We are undertaking stereo-topographic mapping at regional to local scales, using Viking and Mars Orbiter Camera Narrow Angle (NA) images, with horizontal resolutions of 600 to 5 m, and expected vertical precision of 200 to 1 m. Derived topography and altimetric information can also be used to calibrate shape-from-shading (photoclinometry) topographic models at down to single-pixel resolution (i.e. 1.4 m for NA images). Products of these efforts have a multitude of purposes, from assisting in large-scale geologic mapping, to characterizing the geology/safety of proposed landing sites. Plans are underway to also use THEMIS, HRSC, and HiRISE camera data in future efforts.

Planetary exploration is resulting in the creation of new archaeological sites, material and debris on planets and their moons, and in various orbits round the Earth, Mars, the Sun etc. The main off-Earth bodies with sites so far are the Moon and Mars. Although thousands of archaeological sites on Earth are protected for their heritage value, no sites off-Earth are properly protected as yet. Sites off-Earth need to be ranked for their comparative heritage significance and protocols developed for the conservation and protection of the more significant sites and artifacts, before specimens are collected and returned to Earth in an uncontrolled (from heritage points of view) manner. A new United Nations Space Heritage Treaty is needed, or at least appropriate IAU and WAC (World Archaeological Congress) protocols agreed by the various parties concerned. The UN Outer Space Treaty 1967 is very out of date and a product of the Cold War.

Using a three-dimensional numerical spectral model, we simulate the outermost layer of Jupiter’s convective envelope (two depth cases: 1-23 bars, 1-115 bars). The physical parameters (e.g. internal energy flux, rotation rate) are chosen to be close to those expected, but solar heating as well as dynamical influences from deeper layers are ignored. The model generates a wind field pattern remarkably similar to that observed. There is a narrow, super-rotating jet at the equator, and two prominent humps in temperature also develop in the subtropics. The strength of the jet streams does not change much over depth. The maximum wind speed occasionally reach 100 m/s, but the mean amplitude of the equatorial jet is about a factor of 2-3 lower than the nominal value. The latitudes of the secondary pro-grade jets are higher than those observed, but they are dependent on the depth of the model. Though the quantitative agreement is not quite satisfactory (as might have been caused by neglected physical effects like solar radiation), this model demonstrates, in principle, the feasibility of generating a Jovian type wind pattern through the interaction of fast rotation and convection in a thin shell.

Prediction of the occultations of the stars P126 and P131.1 by Pluto on 2002 July 20 (UT) and August 21 (UT), respectively (Clancy et al. 2002, BAAS 34, 1212) involved astrometric data sets spanning more than three months that were acquired on several telescopes. Pluto’s position in each frame was determined relative to a UCAC astrometric reference network (Zacharias et al. 2000, AJ 120, 2131) with a dual-source point-spread function (PSF) model that was fit to the blended Pluto-Charon image. The relative position of Charon from Pluto was fixed in the PSF using values from the JPL Horizons ephemeris, and the light ratio fixed at values from resolved photometric observations of Pluto and Charon presented in Buie, Tholen, and Wasserman (1993, Icarus 125, 233). Although the final predictions proved to be quite accurate (see http://occult.mit.edu/research/occultations/Candidates/Predictions/P126.html and http://occult.mit.edu/research/occultations/Candidates/Predictions/P131.1.html), empirical corrections were made to the offset of Pluto from its ephemeris. These corrections were based on the residuals of Pluto’s measured position from its ephemeris, which were sinusoidal. The consistency of the fitted residual phase and amplitude between all prediction data sets implies either an incorrect Charon to Pluto mass ratio was used for calculating Charon’s ephemeris, or that we used incorrect Charon/Pluto light ratios in this reduction. Resolved images of Pluto-Charon were taken over a period of six days (2003 April) in nine filters at the Magellan 6.5-m Clay telescope in order to uncover the cause of these residuals. Combined with other Magellan Pluto frames taken in 2001 and 2002, the images were fit with a dual-source PSF model. The Charon/Pluto light ratio determined from the PSF modeling was then plotted against orbital phase and fit with a sinusoidal model for each filter. A strong trend with wavelength was found for the mean light ratio of Charon to Pluto. This trend partially explains the residuals found, as the astrograph and CTIO data were taken in a filter of mean wavelength ~720nm, whereas the Buie et al. resolved light curve was obtained in the F555W filter of mean wavelength ~537 nm. This trend can account for 0.026” of the 0.053” residual amplitude. However, if the only other effect were an erroneous Charon/Pluto mass ratio, the remaining residual would imply a mass ratio of 0.086 rather than 0.120 (as used in the JPL Horizons ephemeris). A value of 0.086 does not agree with recent mass ratio measurements (0.157 ± 0.003 by Young et al. 1994, Icarus 108, 186; 0.124 ± 0.008 by Null and Owen 1996, AJ, 111, 1368; and 0.122 ± 0.008 by Olkin et al. 2003, Icarus 164, 254), thus more work must be done in these analyses to understand the cause of these residuals. This work was funded at MIT in part by NASA Grant NAG5-10444 and NSF Grant AST-0073447.

The asymmetry observed in the H-Lyα profiles measured near the Jovian equatorial limbs by the STIS/HST spectrograph is interpreted as due to H atoms propagating in the upper Jovian atmosphere with velocities ~ 80 km/s relative to Jupiter’s rotation. A qualitative scenario is suggested to correlate these energetic H atoms to energetic neutral particles recently detected by Cassini at higher altitudes.

Using the high-resolution images acquired by cameras onboard the MARS GLOBAL SURVEYOR orbiter made it possible to reveal the previously unknown objects on the Martian surface, which changed dramatically a notion of Mars as a dry, hydrologically dead planet (Malin and Edgett, 2000). Examination of new images shows that the nature of some extended dark formations on the slopes of craters and uplands may be associated with contemporary abundant sources of liquid water arising on the slopes at small depths below the level of surrounding plains.

ASTROD I with one spacecraft ranging optically with ground stations is a first step for a full ASTROD (Astrodynamical Space Test of Relativity using Optical Devices) mission. The goals are testing relativity with the relativistic parameter γ measured to 10~7, measuring solar-system parameters more precisely, and improving the present-day sensitivity for gravitational wave detection using Doppler tracking by radio waves. In this paper, we present the mission concept and the orbit design for ASTROD I with an emphasis on Venus flybys. The spacecraft is to be launched into an inner solar orbit with initial period about 290 days to encounter Venus twice to receive gravity-assistance for achieving shorter period (165 days or less) to reach the other side of the Sun for a sooner measurement of Shapiro time delay. For a launch on June 17, 2010, after two encounters with Venus, the orbital period can be shortened to 165 days and the spacecraft orbit reaches inside Mercury orbit. After about 400 days from launch, the spacecraft will arrive at the other side of the Sun and the relativistic parameter γ can be determined to 0.1 ppm or better. A simulation of the accuracy for determining the relativistic parameters γ and β, and the solar quadrupole parameter J2 gives 10−7, 10−7 and 10−8 for their respective uncertainties. In this simulation, we assume a 10 ps timing accuracy and 10−13 m/s2(Hz)1/2 at frequency f ~ 100μHz inertial sensor/accelerometer noise. Other orbits separated by synodic periods of Venus can readily be found. We discuss the sensitivity and noise reduction requirements, the atmosphere transmission noise, timing noise, spacecraft environmental noise, test-mass sensor back-action, and test mass-spacecraft control-loop noise and stiffness. In the second Venus flyby, the ASTROD I could also be swung into an elliptic 360-day orbit and stay near opposite side of the Sun for many good measurements of the Shapiro time delays — 19 times in 10 years. This is an interesting alternative. In the two Venus flybys, Venus multiple moments can be determined very precisely. In this paper, we also review ASTROD and discuss its gravitational-wave sensitivities.

The observed distribution of trans-Neptunian objects (TNOs) implies that they originally orbited in a narrow ring of radius 41 AU. The mass of the largest TNO was around 1 — 4 x 1026 g.

A new model for the origin and bulk chemical composition of the inner planets, especially for their water content, is reported.

Dynamics of Venus’ mesosphere (70-110 km) is characterized by the coexistence of two different wind regimes: (1) between 70 and 85 km the vertical amplitude decrease of Venus’ zonal retrograde super-rotation; (2) between 85 and 110 km, a stable, sub-solar to anti-solar (SSAS) flow, driven by solar EUV heating. On July 7-14, 2001 and July 31 – August 4, 2002 we observed Venus with the Aurélie spectrometer on the 1.5-m telescope at Observatoire de Haute-Provence, France. The spectra cover the visible 8660-8730 Å range, in the 5v3 band of 12C16O2, at a resolving power of about 120,000. Seven regions were observed on Venus’ illuminated side at ~ 75° phase angle. About 28 lines from the P and R branches of the 5v3 band were detected and used for wind velocity measurements with an accuracy of 15 to 25 ms-1.

The motivation for holding Special Session 2 at the 25th IAU GA is described, together with an outline of the rational for pursuing astronomy in Antarctica.

A brief review of astroparticle activities in Antarctica is presented including balloon cosmic rays detectors and use of the clear ice sheet for large neutrino telescopes.

Totality at the eclipse of 23 November 2003 will cross land only on Antarctica. Details of the path and contact information for safe observation are provided.

Analysis of sky images obtained from an automated experiment at Dome C, Antarctica, at 2-hourly intervals from February to November 2001 show cloud-free conditions 74% of the time. This augurs well for the prospects of future astronomical observatories at this site.

Results relative to three campaigns at Dome Concordia, aimed to measure the millimetric sky noise, are presented. The atmospheric noise during summer seems to be definitely lower with respect to that measured with the same instrumentation in other geographical locations. We illustrate the scientific results obtained.

The SPIREX telescope, located at the Amundsen-Scott South Pole Station, was a prototype system developed to exploit the excellent conditions for IR observing at the South Pole. Observations over two winter seasons achieved remarkably deep, high-resolution, wide-field images in the 3-5 μm wavelength regime. Several star forming complexes were observed, including NGC 6334, Chamaeleon I, η Chamaeleontis, the Carina Nebula, 30 Doradus, RCW 57, RCW 38, as well as the Galactic Center. Images were obtained of lines at 2.42/μm H2, 3.29/μm PAH and 4.05/μm Br α, as well as 3.5/μm L-band and 4.7 μm M-band continuum emission. These data, combined with near-IR, mid-IR, and radio continuum maps, reveal the environments of these star forming sites, as well as any protostars lying within them. The SPIREX project, its observing and reduction methods, and some sample data are summarized here.

AST/RO is a 1.7m diameter submillimeter-wave telescope at the geographic South Pole. A key AST/RO project is the mapping of CI and CO J = 4→3 and J = 7 → 6 emission from the inner Milky Way (Martin et al. 2003). These data are released for general use.

Cosmic ray observations related to Antarctica commenced in the austral summer of 1947-48 from sub-Antarctic Heard and Macquarie Islands and from the HMAS Wyatt Earp. Muon telescope observations from Mawson station, Antarctica, followed from 1955. The International Geophysical Year was the impetus for the installation of a number of neutron monitors around Antarctica, observing the lowest energy cosmic rays accessible by ground based instruments. In 1971 a new observatory was built at Mawson including the only underground muon telescope system at polar latitudes in either hemisphere. Over more than half a century, cosmic ray astronomy has been undertaken from Antarctica and its surrounding regions and these observations have been critical to our growing understanding of the heliosphere.

Solving the century-old puzzle of how and where cosmic rays are accelerated mostly drives the design of high-energy neutrino telescopes. It calls, along with a diversity of science goals reaching particle physics, astrophysics and cosmology, for the construction of a kilometer-scale neutrino detector. This led to the IceCube concept to transform a kilometer cube of transparent Antarctic Ice, one mile below the South Pole, into a neutrino telescope.