The meeting began with a report on up-coming meetings of various working groups and committees. On February 21st through 23rd, there will be a meeting in Tucson of 12-13 European representatives with the MMA division heads and senior scientists to discuss the definition of the joint project. The first order tasks are to define the project in light of the European collaboration, divide tasks, define interfaces, and basically decide how to manage the project. A preliminary LO Multiplier design review will be held on Friday, February 19th. Neil Erickson from the MAC will attend this meeting. On March 5th, a meeting will be held to review the Request for Proposals (RfP) which will solicit designs that meet the specifications in the RfP. Presumably summaries of these meetings will be posted on the MMA webpages.

Most of the meeting was spent discussing the Science Workshop to be held September 23 - 24 at the Carnegie Institute in Washington D.C. The target science areas were discussed. There seemed to be a general concensus that the topics should follow those being emphasized by the Decadal Committee to the extent possible. A draft of a program is on the MMA web page and it is recommended that everyone read this and make whatever comments they have on it soon, as speakers need to be lined up fairly quickly. The point was made that the goals of this meeting need to be defined, as this will determine both the content of the program and the composition of the attendees. Several of us have sent comments about this to Al since the telecon.

Min Yun has simulated a MMA Deep Field image in the direction of the Hubble Deep Field and finds about 1600 galaxies in a 4'x4' field for a 2 hour integration. Jack Gallimore has incorporated a luminosity function to simulate a three dimensional distribution. The objects appearing in the MMA field are heavily weighted toward high-z objects. This is posted on the web at http://www.cv.nrao.edu/~awootten/mmaimcal/zlines.html. The final version of this is likely to be one of the center pieces of the science meeting. Demonstrating the ability of the MMA/LSA to obtain both accurate positions and redshifts simultaneously using the combination of CO transitions that could be redshifted into the 16 GHz bandpass of the MMA was strongly encouraged. Inclusion of CO intensity estimates in the MMA Deep Field is still under simulation for inclusion on the above www page when completed.

The present program for this meeting is expected to open with a keynote speaker who will review the overall capabilities of the facility. This will be followed by invited talks on high z observations of galaxies, AGNs, quasars, etc. The afternoon of the first day will be devoted to extra- solar planetary systems. The second day will focus on star formation in the morning and on element and isotopic abundance issues in the afternoon.

Work is proceeding on issues raised in the November MAC report such as fast switching/1/f noise, total power observing, 183GHz vs 23 GHz water vapor monitors,etc. These will appear in the memo series as the studies are completed.

Currently it is planned to have a MAC meeting on September 25th immediately following the Science Meeting so mark your calendars for the 23rd through 25th of September The NSF Oversight Committee would also like us to set the date for the MAC meeting for 2000. Al has suggested November 18, 2000. This is a Saturday two weeks before Thanksgiving. NRAO needs to have a date on the books to satisfy the NSF committee. The final date can be fine-tuned later if necessary.

The next MAC telecon will be on March 17th at the usual time and number.