Speakers: Guilloteau, Baars, Wootten Writeup: Yun

Speakers: Brown Writeup: Evans and Cox

Speakers: Rafal and Kurz Writeup: Guilloteau and Wootten

Speakers: Guilloteau, Wootten, Yun, Sakamoto, Bronfman Writeup: Yun, Bronfman

Speakers: Wild (see below) Writeup: Blake and van Dishoeck

Speakers: Wilson, Richer Writeup: Wilson and Richer

Speakers: Chikada, Baudry, Wootten Writeup: Bachiller and Scoville

Speaker: Lucas Writeup: Gurwell

Speaker: Baars, Rafal Writeup: Welch and Walmsley

Speaker: Wootten, Shaver Writeup: van Dishoeck?

Speaker: Crutcher Writeup: Crutcher, Menten

Speaker: Kawabe Writeup: Kawabe

Speakers: Guilloteau, Welch Writeup: Richer and Wilson

Wolfgang has proposed he report on (as above):

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Report - Wootten

Another monthly report has been assembled!!

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Configurations

Details for the Configuration PDR

Minutes of Meeting 4 Jan 2001

PDR

Since the teleconference, both Lee Mundy (lgm@astro.umd.edu) of the University of Maryland BIMA Group, and Eric Anterrieu (Eric.Anterrieu@cerfacs.fr) of (Signal & Image Processing Team), CERFACS, at Toulouse have agreed to serve as external referees. Two are required, so the quota is met, though more opinions may be sought.

Simulations

There was considerable discussion on the error images and statistics which Steven has placed at his WWW site. Best to use Steven's report here:

SH:"I'll just summarise my verbal report from the last meeting, and say what my immediate workplan is.

"At the time of the previous telephone conference I had just presented arithmetic difference images, and we discussed displaying image statistics, FFTs of difference images, and fractional difference images. The fractional difference measures primarily discussed were fidelity image results as presented by Stephane in his example, and the measures proposed by John which are a series of ratios of (arithmetic difference image)and (smoothed model magic blanked at a certain level) which gives rise to a corresponding series of rms values [This is my understanding of it].

"As these measures have very similar implications for scripting an AIPS implementation, I pressed on with implementing the fidelity image as it was slightly better specified. I originally intended to present just a few examples for comment, but progress was better than I expected so I was able to provide a complete set of C array examples and B array examples for MPD, CYG and SDC (please ignore bad links to the MAR and M51 cases). These examples are just a first step so feedback was and is welcomed.

"Mark asked about negative values in the Fidelity plots and histograms- these arise because some of the initial model images have negative values in them, viz. M51, SDC and CYG. M51 and CYG have negative values which are of the order of 0.1% of the peak values in absolute terms, but the SDC model has negative values which are up 5% of the peak value in magnitude. The use of CLEAN boxes was suggested, and also the use of a prior model for images such as MAR. I raised the question as to whether or not the denominator in the fidelity image ( the absolute values of the arithmetic difference image, truncated at 0.7 x rms value of the difference image) should use the same rms value for each of the corresponding ring and spiral cases... and the answer seems to be no, although some are uneasy with the fidelity image as a whole rather than the details of its implementation.

"I reported that FFTs of difference images can be churned out if necessary.

"So bearing all this and the discussions from last Thursday's telecon in mind, I have a number of things to do...

"1) Truncate M51, CYG, SDC model images so that they are greater than or equal to zero. Someone commented that this would take about an hour, which is true, but the implication in all this is that the imaging, CLEANing, calculation of smoothed models, differencing and presentation of results for these models should be redone as well, which takes considerably longer.

2) Import the 10K (dots) model into AIPS, and create down sampled versions to avoid registration problems. I may as well put the 10K model through the same process as the others, as (apart from disk usage and cpu time) the only overhead it imposes is adding a line to the setup file for each batch job.

3) Archive results from AIPS disks to CD, and also text and PostScript files used in generation of the webpages.

4) Redo imaging, CLEANing, differencing etc. for B and C resolutions using M51, CYG, SDC and 10K

5) Perform imaging of M51 and and CYG for D resolution for later combination with B array results, by way of trying multiconfigurations.

6) Try out DBCON using results of 5)

7) Implement John's metric from his specification.

8) Look at obtaining off-source rms values

"Use of CLEAN boxes is still an open issue as is the use of a prior model for Mars. If the consensus is to do either of these in the current round, I will, obviously redoing everything for all models consistently."

And, on 18 Jan, Steven reported:

I have posted new results (CLEAN, difference, fidelity) for the B and C resolutions. These results replace the 18th December results. The main changes are that the M51, CYG and SDC model images have had any negative pixels truncated to zero, so that they and their smoothed counterparts as used in the difference and fidelity image calculations are wholly positive (or zero). These results should now be complete, i.e. the links for the MAR and M51 cases should now work for the B resolution.

The results are of course at my site.

I have calculated results for M51 and CYG for the D resolution for the quick look at the hybrid array (although I imagine I only needed to go as far as getting the UV data), and may post these as well. Actually combing these snapshots with B array data will follow.

I hope to start looking at the 10K dots tomorrow, as well.

Metrics

John suggested that we arrive at the metric iteratively and collected the emails to alma-config on the subject.

Next Meeting

Another phone meeting was suggested, to discuss the metrics.

Configuration PDR

1) Date and Place

Date: February 26 and 27

Location: IRAM, Grenoble

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Action Items 1 Aug2000

DECISION: Configurations--where are we? Next phone meeting plans...ACA/THzA?

DECISION: Implementation of 183 GHz WVR?

DECISION: Are the specs for a nutating secondary correct?

DECISION: What is the total power specification on the ALMA?

DECISION: What is the effect of 1/f noise in the HEMT amplifiers of SIS receivers upon our ability to combine total power and interferometric images into a faithful representation of the sky?

Year 2000

January	February	March	April
May	June	July	August
September	October	November	December

October 13

ACC Meeting

Paris, France

Nov 6-9	ALMA Photonics/Receiver	Tokyo, Japan
Nov 6	ALMA SSR Meeting	Teleconference
Nov, 13	ALMA SAC Meeting	Teleconference
Nov 15-16	Vertex Antenna CDR	Duisburg, Germany
Nov 28-29	EIE Antenna PDR	Venice, Italy

Dec 8

Project Book Frozen

Executive Fiat

Send comments to <tcontini@eso.org> Last modified: Tue Feb 22 09:55:07 MET

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Travel

Butler

oct 22-29 | pasadena (annual dps meeting)

nov 3-7 | CV (readhead meeting)

nov 12-19 | marrakech, morocco (IAU site testing meeting)

Radford

nov 5-7 | CV (readhead meeting) ------