Microlensing, or Galactic Twinkling
  Microlensing has established itself as a powerful new method for the detection of baryonic dark matter in the Galaxy. The theory of microlensing is sketched and its similarity with the optical effect of twinkling is explained. The bulk of the article presents a new analysis of the data-set on microlensing towards the Large Magellanic Cloud. The extent, flattening and velocity anisotropy of the Galactic halo are unknown. So, it is vital to analyse the microlensing data-set with families of models that span the viable ranges of these structural parameters. Also crucial is proper modelling of the dark matter halo of the Large Magellanic Cloud. Despite all the unknowns, a robust conclusion is that the Galactic and LMC haloes cannot be primarily built from objects in the mass range 10^{-7} - 0.1 solar masses. The baryonic fraction of the Galactic halo probably lies in the range 0.4 - 0.5. The mass of the deflectors probably lies between 0.05 - 1.0 solar masses. Stronger claims concerning the masses of the dark objects are unwarranted because the estimates are sensitive to the uncertain velocity anisotropy. 
Wyn Evans (Theoretical Physics, Oxford)