Extremely metal-poor stars are now being discovered in the Galactic dSph satellite galaxies. Remarkably, the least luminous dSph seem to have the most extreme metal-poor stars, and to have a huge abundance dispersion. Are these faint dSph survivors of the first systems? Does their chemistry record the enrichment of the first supernovae, those which probably reionized the Universe? What was their internal chemical evolution? Are they surviving building blocks of galaxies, recording the early chemical enrichment of the proto-Milky Way? We have discovered the most metal-poor carbon-rich star known in any dSph in Segue I, the lowest luminosity dSph, and identified several other extremely metal-poor stars (with [Fe/H] < -3) in each of Segue I and Bootes I. Remarkably, there also apparently exists a large internal metallicity spread in these systems, indicating self-enrichment with dark matter haloes. We have a programme to obtain high-resolution spectra with the aim of determining elemental abundances of these intriguing systems and initial results are consistent with pre- enrichment with a normal massive-star IMF, just as the bulk of the field stellar halo. I will present our derived [Fe/H] and [C/Fe] distributions for stars in Segue I and in Bootes I, together with alpha-elemental abundances for a particularly interesting star in Bootes I. I will discuss implications for high-redshift star formation and galaxy formation.