The second focus of discussion were the first detailed results from the Thermal Emission Spectrometer on the Mars Global Surveyor spacecraft -- an important instrument whose data has taken longer to analyze properly than that from the craft's other instruments.

The Thermal Emission Spectrometer (TES) takes spectra of mid-wavelength infrared radiation emitted by the soil and rocks of Mars' surface as a direct result of their warmth, and it can identify a large number of scientifically important minerals -- including many, such as carbonates, sulfates and other salts, which are indicators of areas where liquid water might have existed on the surface of ancient Mars and which would be promising hunting grounds for Martian fossils.

What the TES didn't find is as interesting as what it did find. J.L.Bandfield and V.E. Hamilton confirmed their recent report in the March 3 "Science" that TES has found that the volcanic rock which covers most of Mars' surface tends to fall into two general types:

• basalt in the rugged highlands that cover the southern hemisphere, and,
• andesite -- a volcanic rock with a higher silica content -- in the smoother northern lowlands.

The detection of andesite confirms the biggest surprise of the Mars Pathfinder mission, which found andesite rocks at its landing site.

Andesite was not expected to exist on Mars in large amounts because, on Earth, it is the product of sea water being drawn deep underground by crustal tectonics ("continental drift") and mixing with the magma (underground lava) there -- and crustal tectonics has never existed on Mars to any large degree.

Apparently some other process has been mixing water with magma deep under the surface of Mars. We're not sure of the details, but this does provide further evidence that ancient Mars had quite a lot of water stored in its crust, and may still have it.

Another puzzle in the TES data is that, so far, it shows no area on Mars with entirely the same infrared spectra as any of the 15 Mars meteorites that have been found on Earth.

These meteorites are known beyond doubt (for a variety of reasons) to have come from Mars; and all those recognized so far, judging from their rock formation dates, seem to have been ejected by only a few individual giant meteoroid impacts on the Martian surface -- which makes it possible that they may have come, by chance, from a few small areas of the Martian surface that just happen to be unusual.

Bandfield and Hamilton's "Science" article says that the famous ALH84001 meteorite and some others are probably from deep in the Martian crust -- which means that their material probably makes up only a very small part of the modern exposed surface -- and photos suggest that all the other known Martian meteorites may have come from two small craters on the relatively recent lava flows in the vicinity of Olympus Mons and Mars' other giant shield volcanoes.

But "Science" states that "The TES spectra from these regions apparently do not match the specific surface rock type", and Hamilton said at the LPSC that "A search for spectral signatures resembling those of [Martian meteorites] in TES data is ongoing."