[mmaimcal] Agenda: Meeting 1 Feb 99

[Al Wootten]

MMA Imaging and Calibration Group

Agenda for meeting Mon, 1 February 1999 at 4pm EST.

Date: 1 February 1999

Time: 4:00 pm EST (2:00 pm Socorro, 2:00 pm Tucson)

Phone: (804)296-7082 (CV SoundStation Premier Conference phone).

Past minutes, copy of this with hyperlinks, etc. on MMA Imaging and 
Calibration Division Page:
http://www.cv.nrao.edu/~awootten/mmaimcal/mmaimcal.html

Agenda

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URSI Site meeting - Radford

Simon will give us a report on the site testing meeting which was held at
the URSI meeting, along with an update on the activities.

Configurations -- Kogan and Helfer

Leonia has compared an optimal array (minimum sidelobes) with a non-optimal
one for two source classes. He simulated the UV data for the two array
configurations using two source classes as a model. The simulation was done
with different noise levels. In all cases the image was resrored by IMAGR
and compared with model. The image provided by the optimal array is better
in all cases considered. Leonia put the draft of MMA memo
(mma_memo_simul.ps) in the ftp.aoc.nrao.edu public area under
/pub/staff/lkogan.

We have been asked to provide example layouts of the antennas in the LMA,
using for example 50 x 12m antennas. These should be from the smallest
configuration up to 10 km in extent. The Europeans are interested in 20km; a
second step would be to investigate the practicality of this. Tamara has
estimated what these new antenna parameters mean for our standard
arrays--for example, the D array may expand to 135m in size. This has
ramifications, of course, for the HDF simulations and other work.

PR - Wootten

Let's discuss the simulation of the HDF some more. Examples are the SIRTF
simulation. Min has produced an effort at his page and Jack Gallimore has
also produced a simulation.  The WWW version of this agenda has hyperlinks.

I updated the MMA history, which I put at our site. Any comments? I will
abstract some point from this for a history slide.
The WWW version of this agenda has hyperlinks.

SKA diagram of M101. Is this a weak galaxy? Why does the MMA/LSA fare so
poorly here--or did they make a mistake. I thought we went to 7000 m^2 or
whatever just so we could get 'normal, unevolved' galaxies like this at z=3!
The WWW version of this agenda has hyperlinks.

Eurotasks -- Wootten

Looks like the European-US meeting in Tucson may occur 21-23 Feb 1999. What
MMA Imaging and Calibration tasks might the Europeans aid us in?

1. Investigation of 183 GHz phase correction systems. This would be a
continuation of the current program, in which one 183 GHz radiometer is
situated at each end of the 12 GHz interferometer baseline at Chajnantor.

2. Investigation of total power imaging modes. The continuing 'DREAM' mode
and related modes at the JCMT, as well as characterization of 1/f noise in
SIS receivers, could help us to understand problems associated with
sensitive total power observing modes.

3. Soil sampling.

4. Configuration studies. There has already been sizable interest in this
subject, resulting in several memos in the Memo Series. We need to put
prototype 50 x 12m antenna configurations down on a plat of the site, up to
10km in size, for purposes of example. European collaboration in this and in
imaging studies seems possible.

Fall 99 Meeting - Wootten

Note that the 12m '30th birthday meeting' will be of substantial interest to
our group:

6- 9 Jun 'Imaging at Radio through Submillimeter Wavelengths' meeting in
Tucson

As you may know, a meeting of U. S. and European scientists is being planned
for the Fall of 1999 in Washington, D. C. The goal of the meeting is to
review the scientific program planned for the joint array and how that
program interacts with the science goals of other astronomical facilities
expected to be operational at the time that the MMA/LSA becomes operational.

Please comment upon the prototype WWW page for the Science With A Large
Millimeter Array meeting at:

LMA99  The WWW version of this agenda has hyperlinks.

Science topics for this suggestion were drawn from those identified by the
1997 Thaddeus committee (Task Group on Space Astronomy and Astrophysics,
Committee on Astronomy and Astrophysics, Board on Physics and Astronomy,
Space Studies Board, Commission on Physical Sciences, Mathematics and
Applications, National Research Council) report A New Science Strategy for
Space Astronomy and Astrophysics", or by McKee:

McKEE's PROPOSED DRAFT SCIENCE PRIORITIES (12/98)

        o PRIMARY
        o -The large scale structure of the Universe
        o -The formation and evolution of galaxies
        o -The formation and evolution of stars
        o -The formation and evolution of planets, particularly habitable
          planets
        o SECONDARY
        o -The impact of the astronomical environment on the Earth
        o -The nature of dark matter
        o -The origin of the elements
        o -The formation and evolution of black holes
        o -The origin of high energy particles and photons
        o -The origin and evolution of magnetic fields

We might further limit them to those for which we thought that the MMA would
provide deep impact. Modifications and suggestions are welcome.

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Action Items 18Jan99

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Travel

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T. Helfer:

A. Wootten: 3-6 Feb (12m observing) 8-9 Feb (MMA talk at SPECS conference)
16 Feb (43m observing) 20-24 Feb Tucson 22-30 May househubby 9 - 13 Jun CSO

J. Mangum:

M. Yun:

B. Butler:

S. Radford: