At the beginning of the last quarter of 1991 I worked on my poster 
         presentation for the conference on High Resolution Imaging by 
         Interferometry at Munich, October 14 to 18. I also held a short talk on 
         my work on binary star observations at the meeting of the Washington 
         area astronomers at the USNO. 
              After I came back from Munich, I spent most of my time preparing the 
         schedules for the binary star observations on Mt Wilson in November and 
         December. We decided to concentrate our efforts on the most important 
         stars since at that time of the season bad weather conditions are 
         likely. I wrote a little scheduling program which calculates the 
         visibilites of stars during a specified night of observing on Mt Wilson. 
              On November 12 I left for Los Angeles to meet A. Quirrenbach with 
         whom I went by car to Socorro, New Mexico, in order to reduce VLA data 
         that had been taken this year. I mapped two sources, the quasars 
         0836+710 and 0153+744, that I have been working on during my time in 
         Bonn. A paper on 0836+710 is in preparation. Though experienced in the 
         practice of mapping very long baseline interferometry data, it was the 
         first time I worked with VLA data and was helped by Andreas Quirrenbach. 
         I also gave a lunch time talk on my work at the USNO. 
              After Socorro, I started my two week term on Mt Wilson. The first few 
         nights yielded no observations, however, due to high winds (up to 68 
         mph) and snowfall. The weather improved subsequently and I was able to 
         obtain very useful data on binary stars on 5 nights. In addition to 
         Eta Andromedae, we now have sufficient data for publication on Theta 2 
         Tauri and Pi Andromedae. Shortly before I left Mt Wilson on December 8, 
         the weather deterioated and no binary observations were obtained during 
         the remainder of the binary star session. 
              Back in Washington, I started to work on the software and logistics 
         of the astrometry data reduction, which has become very urgent due to a 
         huge pile of unreduced data. I modified two programs for convenient use, 
         which were written originally by D. Mozurkewich and N. Elias. The first 
         one is a program to read raw astrometry data and to detect and integrate 
         data of the so called "central fringe". The second one reads data of the 
         position of a white light fringe pattern in order to correct measured 
         delays for hourly changes in the baseline geometry. I wrote a transfer 
         program, which applies the corrections to the delays and prepares the 
         standard input file for the least squares algorithm which determines the 
         star positions. Thus, we should be able to start astrometry data 
         reduction on a large scale with the beginning of next year. 
              On December 20, I left for Germany to take two weeks of vacation over 
         the holidays.