At the beginning of the first quarter of 1996, I prepared my poster 
"A precessing radio jet in quasar 0153+744" for the AAS meeting in San Antonio,
which I attended from January 14 to 18. In collaboration with T. Armstrong, I
also presented a poster on "Double star astronomy with optical interferometers".
Time was spent in January on a variety of smaller tasks: preparation of a talk
at USRA's Science Council meeting, collaboration with S. Lundgren (NRL) on a
proposal to the VLBA for observations of an extra-galactic gamma-ray source,
tracking down a small bug in the NOVAS astrometry routines as supplied by
division AA of USNO, submission of the final version of a paper on "The masses
and radii of the eclipsing binary zeta Aurigae", a collaboration with 
P. Bennett, G. Harper, and A. Brown at the University of Colorado and JILA,
adding code to CONSTRICTOR which led to the first successful reading and
displaying of internal fringe data from NPOI, and writing code to determine
the effective wavelength of each channel in a NPOI spectrometer from bin
count rates.

During February, I added extensive code to CONSTRICTOR to process and pipe 
metrology data to the output file for reduction in INCHWORM. I also worked
on CHAMELEON on functions which will apply INCHWORM results to astrometric
delays for use in the global astrometric solutions computed in VOLVOX.

I was on vacation from 2/17 to 2/25. After this, I continued to work on a
new draft version of my paper on quasar 0153+744. I obtained three maps in 
the S/X bands from colleagues, which I analyzed and incorporated into the
paper. They seem to help answer a question as to the nature of one of the
emission components seen in 0153+744.

I attended the Washington Area Astronomers meeting in Baltimore (one day).

Extensive work on data reduction/software commenced with the first observation
of stellar closure phases with the NPOI in March. An improved group delay fringe
tracking algorithm, multiple input file processing, across packet boundary
integration were implemented in CONSTRICTOR. Data was read and edited in
CHAMELEON, an astrometric baseline solution for the night of March 19th 
yielded residuals smaller than 20 microns.