Improvement of astrometric accuracy is a major need of astrophysics today. A significant increase in the amount of information about the masses of stars, parallaxes, and proper motions is to be gained. Some improvements have been accomplished in the last few years such as the astrometric reflector like the 61-inch at Flagstaff, (K. Strand, 1967), and the McCormick 40-inch (under construction). Another direction of improvement has been automation of measuring devices such as the Strand Measuring Engine and the Grant Measuring Engine; but one of the large improvements of the future ought to be observations outside the Earth’s atmosphere to the level of diffraction limited images instead of seeing limited images. The concentration of light in a smaller image will then mean both a fainter magnitude reached and a high astrometric accuracy.