I could not find out what Dr. Stofan expects to be detected in that time. I also think that that is very overoptimistic. Let's see what an organism needs to metabolize and grow:
- Liquid water, to serve as a solvent and raw material: H2O
- Several other elements: C, N, P, S, various metal ions (can be trace amounts)
- Usable thermodynamic disequilibrium, like chemical disequilibrium or suitably-energetic photons
These are all extrapolated from the Earth's biota, but there are plausible arguments for the first two, and the third one is a necessity. It enables organisms to appear to violate the Second Law of Thermodynamics by metabolizing and growing and reproducing and moving and the like.
Organisms can alter their environments in various observable ways, sometimes massively, like photosynthesizers releasing large quantities of molecular oxygen into the atmosphere. This is in chemical disequilibrium with its producers and with the less-oxidized crustal rocks. Rocks with Fe++ instead of Fe+++. But there can be nonbiological processes that produce chemical disequilibria. Like serpentinization: FeO + (1/2)*H2O -> (1/2)*Fe2O3 + (1/2)*H2. FeO has Fe++ and Fe2O3 has Fe+++. The resulting hydrogen will be out of equilibrium with a neutral or oxidizing atmosphere. Neutral: lots of CO2 and/or N2. Oxidizing: lots of O2.
Mars
Its surface is borderline at best for liquid water, being cold with a thin atmosphere, though there is an abundance of evidence that it had oceans and rivers some 4 billion years ago.
However, a few km down may be more friendly to organisms, and there is possible evidence of their presence: methane. Tiny amounts of it have been detected in Mars's atmosphere. (
Mars methane detection and variability at Gale crater: Science magazine) It's typically a part per billion by volume, though it is sometimes greater.
It could be produced by 4H2 + CO2 -> 2H2O + CH4, where the H2 comes from serpentinization. It could be some nonbiological reaction alongside the serpentinization, or it could be organisms like Earth's methanogens. These organisms get their energy from the aforementioned reaction, and are a major source of methane in the Earth's atmosphere.
It might be possible to go further by finding the isotopic composition of Martian methane and comparing it to that of Martian water and Martian CO2. As a check, this ought to be done on Earth methanogens to see if they produce any distinctive signatures of isotopes.
Interior oceans of large icy moons
Moons like Europa, Ganymede, Callisto, Enceladus, and maybe also Titan, Triton, and Ceres (not a moon, but it has a similar size). They have the first two ingredients, but there is a serious question of whether any of them have the third ingredient: some usable disequlibrium like chemical disequilibrium.
There is a possibility for that. Several of them have rocky interiors, and they may get heated enough from radioactivity or tides to cause serpentinization and its production of hydrogen. This would likely be in disequilibrium with some of the contents the interior ocean.
Titan's surface
That would require some rather exotic biochemistry, starting with having hydrocarbons as a solvent. It would be biochemistry with H, C, N, but not much O or others. It doesn't look like it could make the necessary amount of complexity.
Extrasolar planets
The best chance here is doing spectroscopy and looking for out-of-equilibrium atmosphere gases like O2. That's going to be VERY difficult. For starters, one would have to do it in the infrared to get away from the bulk of the planet's star's light.