From mgurwell at cfa.harvard.edu  Fri Apr  6 12:42:36 2001
From: mgurwell at cfa.harvard.edu (Mark A. Gurwell)
Date: Fri, 6 Apr 2001 12:42:36 -0400 (EDT)
Subject: [asac] Re: ALMA Software
Message-ID: <200104061642.MAA03318@yoda.harvard.edu>

> Date: Thu, 29 Mar 2001 15:27:56 +0200
> From: Arnold Benz <benz at astro.phys.ethz.ch>
> To: "Mark A. Gurwell" <mgurwell at cfa.harvard.edu>
> Subject: ALMA Software  
> 
> Hi Mark,
> 
> The European Alma SAC wants to discuss data analysis plans at the next
> telecon of April 12. 
> 
> Has there been any discussion on this already?
> 
> Best regards,
> 
> Arnold Benz
> 

Dear Arnold,

Sorry that I have not been able to respond before now.  I got your phone
message today, so I am spurred to reply to you.

I do not believe that there are any final plans on how realtime data 
analysis will procede, in the sense of the use of a particular package
such as Aips or Miriad.  From the document on Use Cases for the Science
Software Requirements, it seems that the user may have some choice on
which packages to use for online analysis, though I am hazy about this
at the moment.  I think that this will be too difficult to implement in
a practical way (indeed I'm not certain it is even suggested by the
SSR Committee), and that a standard package for the realtime calibration 
and analysis will have to be chosen, just for expediency and consistency.

This does lead directly to the question of concern: how will this be
done?  I don't know what sort of discussion has taken place on this so
far, the person to ask would be Robert Lucas who chairs the Science
Software Requirements Committee.  I believe that he has been asked to
join in the 12 April telecon (right Al?) but I will include him in the
distribution of this email so that he gets a heads up for this line
of discussion.  

In a reply to me on our section of the latest ASAC report on the 
Science Software Requirements, Robert does respond to this specific
question.  He wrote:

   '2. Obviously pipeline data reduction is a huge task:  the preparation 
   of detailed pipeline and off-line data analysis requirements has been
   started; this  will be followed by a re-use analysis of existing
   packages.'

So, in response to your query, I would say that some people are thinking
about this task.  I know that Karl Menten, for example, expressed serious
concern about this facet of the software development at the Florence 
meeting.  We will see where the situation is during the 12 April meeting.

Best wishes,

Mark
--------------------------------------------------------------------------
Mark A. Gurwell                                                     
Harvard-Smithsonian Center for Astrophysics          voice: (617) 495-7292
Mail Stop 42                                         fax:   (617) 495-7345
60 Garden Street                           email: mgurwell at cfa.harvard.edu
Cambridge, MA 02138                   http://cfa-www.harvard.edu/~mgurwell
--------------------------------------------------------------------------





From jsr at mrao.cam.ac.uk  Mon Apr  9 08:44:56 2001
From: jsr at mrao.cam.ac.uk (John Richer)
Date: Mon, 09 Apr 2001 13:44:56 +0100
Subject: [asac] ALMA Calibration PDR
Message-ID: <E14mb2O-0007pR-00@grigori.ra.phy.cam.ac.uk>


Dear colleagues,

Please see the enclosed announcement from Stephane Guilloteau, Al
Wootten and myself, regarding the ALMA calibration PDR to be held this
summer. There is a draft agenda at

	http://www.alma.ac.uk/calpdr

More details will be posted here in due course.  Can you please
confirm if you will be attending to me, but note you must take care of
your own hotel accomodation bookings as described in the note below.

Comments on the agenda/attendance list should be sent to Stephane, Al
and myself. 
 
Regards

John Richer

----------------------------------------------------------------------

			 ALMA Calibration PDR
				   
		Thursday June 21st + Friday June 22nd

	      MRAO, Cavendish Laboratory, Cambridge, UK


We are making plans for an ALMA calibration PDR meeting for the above
dates.  We expect two full days of sessions.

This a very lively time of the year in Cambridge.   It is 'May Week'
(yes, in June!), when all the College summer balls take place, plus
there is the usual large influx of tourists.  So those attending must
make hotel reservations as soon as possible, and no later than 1 May
(sooner if you wish to stay for extra nights before or after the
meeting).  A block of hotel rooms has been reserved at the Arundel
House Hotel in Cambridge:
      
      http://www.arundelhousehotels.co.uk

PARTICIPANTS MUST RESERVE THEIR OWN ACCOMMODATION AND GUARANTEE IT
WITH A CREDIT CARD BY 1 MAY.

The telephone number for reservations is +44 1223 367701, or you can
FAX them on +44 1223 367721.  Be sure to mention the meeting name
(ALMA) when you make your reservation.  Prices should be about 65 GBP
per night for a single room, and 85 GBP per night for a twin or double
room.

John Richer is taking the lead in the local organisation - feel free
to email him with any questions about logistics (jsr at mrao.cam.ac.uk).

Travel hints

Cambridge is about 55 miles from central London, and well served by
trains from London Kings Cross station (2-3 per hour, journey time
45-75 minutes depending on the train).

London Stansted is the closest large international airport (~35 miles
from Cambridge), and is quite well connected to many European cities
by several 'low-cost' airlines; the only transatlantic flight will be
Continental's New York-Stansted service which begins in May.  Buses
run approximately hourly to Cambridge from Stansted, taking about 45
minutes; a taxi takes 35 minutes in light traffic and costs about 44
GBP.

London Heathrow and Gatwick airports are more distant from Cambridge -
about 75 and 110 miles respectively. Both are served by trains and
buses. The scheduled bus journey time is about two hours from Heathrow
and three hours from Gatwick. Because of heavy traffic around London,
the actual departure times of these buses are sometimes very different
to the times listed in the timetable. You just have to locate the
correct bus stop and then wait for one to come. Alternatively, you can
take trains: from Heathrow, you can take a long underground ride to
Kings Cross; alternatively, pay more money and take the fast Heathrow
Express train to London Paddington, then the tube to Kings Cross.
>From Gatwick, a regular train service takes you into London, then a
tube across London takes you to Kings Cross.  Frm Kings Cross it's
then less than an hour to Cambridge.

>From Cambridge railway station it's a short taxi ride to the hotel
(about 2.5 miles); the bus station is more central - a little over 1
mile from the hotel.


--
John Richer,  Cavendish Astrophysics,  Madingley Road,  Cambridge CB3 0HE
Tel. 01223-337246         Fax: 01223-354599          Mobile: 07870-509599
jsr at mrao.cam.ac.uk  http://www.mrao.cam.ac.uk/~jsr  http://www.alma.ac.uk


From awootten at NRAO.EDU  Tue Apr 10 14:10:51 2001
From: awootten at NRAO.EDU (Al Wootten)
Date: Tue, 10 Apr 2001 14:10:51 -0400 (EDT)
Subject: [asac] Meeting 12 April 1415UT.
Message-ID: <200104101810.OAA06542@polaris.cv.nrao.edu>

Dear colleagues:

An agenda has been placed at:
http://www.cv.nrao.edu/~awootten/mmaimcal/asac/asacapr01agenda.html
which has some links for reading material for discussion.

Here's the dial-in information for the telecon:
Conference Date: 12 Apr 2001
Conference Time: 10:15 AM EASTERN TIME=14:15 UT
USA Toll Free Number: 888-791-2132
Non-USA Number: +1-415-228-4574
PASSCODE: ALMA
Conference Leader: Mr Al Wootten

Clear skies,
Al



From cwhite at NRAO.EDU  Wed Apr 11 16:48:52 2001
From: cwhite at NRAO.EDU (Carolyn White)
Date: Wed, 11 Apr 2001 16:48:52 -0400 (EDT)
Subject: [asac] [almanews] ALMA Memos 360, 361, and 362 Released
Message-ID: <Pine.SOL.3.91.1010411164808.20776A@polaris.cv.nrao.edu>

ALMA Memo #360

Design of Sideband Separation SIS Mixer for 3 mm Band

Vessen Vassilev and Victor Belitsky

As a part of Onsala development of a single sideband mixer for ALMA band 7
(275-370 GHz), we present design of a prototype sideband separation mixer
for 85-115 GHz.; The mixer employs a quadrature scheme with two
identical DSB SIS mixers pumped by a local oscillator with 90 deg phase
difference.; The mixer uses a new device, a double-probe coupler,
which splits the input RF signal and provides transition from a waveguide
to a microstrip line, allowing the integration of all mixer components on
the same compact substrate and thus ensure a high degree of similarity in
the SIS junction performance and the geometry of all the mixer elements
including integrated tuning circuitry.

We present the design of all the mixer components, detailed simulation
results using High Frequency Structure Simulator and measurements of the
double probe coupler.

View a pdf version of ALMA Memo 360 at URL:
     http://www.alma.nrao.edu/memos/html-memos/alma360/memo360.pdf

View a html version of ALMA Memo 360 at URL:
          http://www.alma.nrao.edu/memos/html-memos/alma360/memo360.html

-----------------------------------------------------------------------

ALMA Memo #361

PHASE CROSS-CORRELATION OF A 11.2 GHZ INTERFEROMETER
AND 183 GHZ WATER LINE RADIOMETERS AT CHAJNANTOR

Guillermo Delgado

The phase variation from a 300-m baseline 11.2 GHz interferometer was
cross-correlated with the phase variation estimated from the PWV
measurements using two radiometers operating near the water vapour line at
183 GHz at the ALMA site of Llano de Chajnantor in Northern Chile at an
altitude of 5,000 m. Care has been taken to have the radiometers observing
the same path of atmosphere as the interferometers, with both beams
matched as close as possible.

The result indicates that the cross-correlation varies during the day and
thus the phase correction possible to achieve using the radiometric method
at Chajnantor.

The results are discussed and comparisons are done with other
variables, specially the height of the turbulence layer. The later is
determined using two different methods: the first one is direct
measurements from radiosonde data, and the second method involves the
calculation of the time lag between the turbulence structures seen by the
two interferometers deployed at Chajnantor. A relation is proposed between
the height of the turbulence layer and the success of the
cross-correlation, with a better cross-correlation when the turbulence
layer is higher than about 300-400 m.

View a pdf version of ALMA Memo 361 at URL:
     http://www.alma.nrao.edu/memos/html-memos/alma361/memo361.pdf

Download a ps version of ALMA Memo 361 at URL:
          http://www.alma.nrao.edu/memos/html-memos/alma361/memo361.ps

-------------------------------------------------------------------------

ALMA Memo No. 362

ALMA Receiver Optics Design

J. W. Lamb (Caltech), A. Baryshev (SRON), M. C. Carter (IRAM),
L. R. D?Addario (NRAO), B. N. Ellison (RAL), W. Grammer (NRAO),
B. Lazareff (IRAM), Y. Sekimoto (NRO) , C. Y. Tham (U. Cambridge)

A detailed design for the optical configuration of the ALMA receivers is
presented.  Individual frequency bands are implemented as self-contained
cartridges holding two orthogonally polarized channels. The cartridges are
arranged on concentric circles round the center of a 970 mm diameter dewar
located on the telescope axis. The beams from them illuminate the
secondary mirror through windows on the top of the dewar, either directly
or via reflective optics. By having all the beams separate in the focal
plane, all bands view the sky simultaneously and selection of the
observing band simply requires re-pointing the antenna.

Where possible all the optical elements are integral with the
cartridge. For the lowest frequency bands, the optics are too large to go
on the cartridge and are located on the top of the dewar. There are no
optical elements inside the dewar that are not attached to a
cartridge. Since some of the cartridges are far off the telescope axis,
mirrors are used to bring the beam closer to the center to reduce
aberrations, polarization distortion, and vignetting by the hole in the
primary. Provision is made for a mirror to bring the beam of the water
vapor radiometer for atmospheric phase correction to the center of the
focal plane so it is close to all observing beams.

Several measures are taken to ensure low optical losses: the number of
elements is minimized; reflective optics are used where possible; large
beam clearances are maintained; and accurate fabrication and alignment
tolerances specified. A major driver was to generate minimal
cross-polarization, and this was realized by minimizing angles of
incidence on offset reflectors, and balancing cross-polarization between
consecutive mirrors.

Detailed calculations of the performance, including losses, noise, and
polarization have been carried out and are tabulated. There are also
estimates of the cryogenic loading. The principal uncertainties are the
optimum designs for the vacuum windows and infrared filters.

View a pdf version of ALMA Memo 362 at URL:
     http://www.alma.nrao.edu/memos/html-memos/alma362/memo362.pdf
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From awootten at NRAO.EDU  Thu Apr 12 08:28:01 2001
From: awootten at NRAO.EDU (Al Wootten)
Date: Thu, 12 Apr 2001 08:28:01 -0400 (EDT)
Subject: [asac] Meeting 1615 UT today
Message-ID: <200104121228.IAA10742@polaris.cv.nrao.edu>

1615 UT is the time for the meeting.  I had a question mark by 
CEST and other civil times unknown to me
as  have no earthly idea what the people in Europe or elsewhere
do with their civil time.

Clear skies,
Al



From awootten at NRAO.EDU  Thu Apr 12 09:14:42 2001
From: awootten at NRAO.EDU (Al Wootten)
Date: Thu, 12 Apr 2001 09:14:42 -0400 (EDT)
Subject: [asac] Meeting 1415 UT today
In-Reply-To: <200104121302.PAA15113@strw.LeidenUniv.nl>
References: <200104121302.PAA15113@strw.LeidenUniv.nl>
Message-ID: <200104121314.JAA12643@polaris.cv.nrao.edu>

Too early in the morning here!!  I shouldn't try this before coffee.
Yes, 1415 UT.

Al


From tetsuo.hasegawa at nao.ac.jp  Thu Apr 12 09:32:26 2001
From: tetsuo.hasegawa at nao.ac.jp (Tetsuo Hasegawa)
Date: Thu, 12 Apr 2001 09:32:26 -0400
Subject: [asac] Meeting 1615 UT today - Are you sure?
In-Reply-To: <200104121228.IAA10742@polaris.cv.nrao.edu>
Message-ID: <v04010501b6fb5c15f402@nao.ac.jp>

Good evening, Al,

At 8:28 -0400 01.4.12, Al Wootten wrote:
> 1615 UT is the time for the meeting.  I had a question mark by
> CEST and other civil times unknown to me
> as  have no earthly idea what the people in Europe or elsewhere
> do with their civil time.

The meeting time was set at 10:15 EST (ref. minutes of the March telecon and
your reservation of today's telecon), and EST is now 4 (= 5 - 1) hours
behind UT because of day saving.
This means the telecon starts at 10 :15 EST + 4h = 14:15 UT, doesn't it.
If the above understanding is wrong, please let me know.  Otherwise, I will
call in at 14:15 UT anyway.

Regards,

Tetsuo
?_______________________________________________________________
Tetsuo HASEGAWA, D. Sc.   <tetsuo.hasegawa at nao.ac.jp>
ALMA-J Project Scientist
Professor, National Astronomical Observatory of Japan
2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
Phone +81-422-34-3843 / FAX +81-422-34-3764
_______________________________________________________________


From cwhite at NRAO.EDU  Tue Apr 24 11:07:05 2001
From: cwhite at NRAO.EDU (Carolyn White)
Date: Tue, 24 Apr 2001 11:07:05 -0400 (EDT)
Subject: [asac] [almanews] ALMA Memo 363 Released
Message-ID: <Pine.SOL.3.91.1010424110337.28348A-100000@polaris.cv.nrao.edu>

ALMA Memo #363

Velocity of the Effective Turbulence Layer at Chajnantor Estimated From
183 GHz Measurements

Guillermo Delgado and Lars-Ake Nyman

The cross-correlation of the precipitable water vapour (PWV) variation
of two water vapour radiometers placed at the ends of a 300-m baseline
along the E-W direction was used to measure the time lag between the
structures seen at each radiometer. With a fixed separation between the
two radiometers, and observing with parallel beams, we can determine the
effective speed of the turbulence layer.


A linear relation between the turbulence layer speed and the ground
wind speed was found indicating that the turbulence speed is roughly twice
as high as the ground measured wind speed.

The temporal phase structure function was calculated, showing that the
turbulence screen goes through a daily cycle associated with the
insolation, with a well-defined layer structure at the extremes of the
cycle.

The cross-correlation method allows the reliable measurement of the
effective turbulence speed for about 90% of the day, apparently associated
with the wind direction and the time when the turbulence layer is high up
(the definition of ?high up? is still uncertain). This implies that
with a variation of this method, by moving the beams in the sky, we can
continuously measure the height of the turbulence layer during most of the
day, providing a very useful tool to assess the dynamics of the turbulence
layer.

View a pdf version of the file at URL:

     http://www.alma.nrao.edu/memos/html-memos/alma363/memo363.pdf


Download a ps version of the file at URL:

         http://www.alma.nrao.edu/memos/html-memos/alma363/memo363.ps




</font>
<P><EM> Last modified: April , 2001</EM></P>
<P><ADDRESS><A HREF="mailto:alma-memos at nrao.edu">alma-memos at nrao.edu</A></ADDRESS></P></BODY>

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From awootten at NRAO.EDU  Tue Apr 24 17:39:30 2001
From: awootten at NRAO.EDU (Al Wootten)
Date: Tue, 24 Apr 2001 17:39:30 -0400 (EDT)
Subject: [asac] minutes-2nd-corr-informal-meeting
Message-ID: <200104242139.RAA13601@polaris.cv.nrao.edu>

Folks,

Sachiko K. Okumura and Alan Baudry forward the appended minutes, bounced owing
to length (versions in plain text and in html) by our mailer.

Clear skies,
Al

Bounced message:
------------------------------------------------------------------
Dear ALG and ASAC members,

We send you the minute of the second
informal meeting of enhanced/future correlator at
Florence 2001 according to ALG request on early April.
Japanese and European teams plan to
talk further progress about the following Action items
with US team on 10 and 11 May in Paris.

Best wishes,

Sachiko K. Okumura and Alan Baudry
------------------------------------------------------------------
Second Informal Meeting
on Europe/Japan Cooperation on Correlators and
High Speed Samplers

Minutes of 24 February 2001
Florence, Italy

Approved by: European and Japanese participants
Distributed by: A. Baudry (baudry at observ.u-bordeaux.fr)


Participants:
Europe: A. Baudry, A. Bos, M. de Vos, S. Guilloteau
Japan: Y. Chikada-san, M. Ishiguro-san,M. Momose-san, S. Okumura-san

Agenda:
- Status of the FX Correlator Project
- Status of the Digital Hybrid XF Correlator/European Future Correlator
- Areas Open to Possible Joint Cooperation
- Status of High Speed Sampler Developments in Japan & Europe
- 3-way Partnership

0. Introduction

The second informal meeting on European and Japanese plans for the Enhanced
Correlator and High Speed Samplers was held on 24 February 2001 in
conjunction with the ASAC face-to-face meeting in Florence (23/24 February
2001).
It follows a first meeting held in Berkeley in September 2000; see:

http://www.eso.org/projects/alma/committees/backwg/minutes10sept_correl.doc

1. Financial Context and Enhanced Correlator

Ishiguro-san presented the Japanese proposal for their contribution to ALMA
in which the enhanced correlator is ranked as of major value. We discuss the
correlator issues in the context of the Enhanced ALMA. The total cost for
the correlator would include the Baseline correlator and the Enhanced
correlator. The first quadrant of the Baseline correlator can accomodate up
to 32 antennas (and thus can be used for the ACA) with a cost of about 8 M$.
The Enhanced correlator cost based on the Japanese FX architeture is
estimated to be around 43 M$. The present Japanese financial model is at the
35 M$ level and could evolve in the future. Prototyping the European Future
Correlator design requires more than 3 M$ with personnel costs included;
however, the total cost estimate for 64 antennas or more is not firmly known
at the moment (ongoing task).

Several financial scenarios are possible at this stage in the frame of
Europe-Japan cooperation and of the 3-way partnership for a second
generation correlator. Baudry and De Vos mention that they cannot make any
statement on financial issues since this depends on the ASAC
recommendations, ACC decisions and involvement of the European Science
organizations. However, they feel certainly committed, on behalf of the
European correlator team, to further
collaboration regardless of the approach chosen for the final architecture
of the Enhanced correlator.
We thus desire and agree to go ahead with joint cooperation and exchange of
information (see Section 4).

2. Report on FX Correlator and Japanese Work on Digitizers

Okumura-san and Chikada-san report on the main characteristics of the
Japanese FX design: high number of channels, flexible channel smoothing in
the X-part, etc. See details in:

http://www.nro.nao.ac.jp/~sokumura/eALMAcorr/FeasibilityofHPFXforE-ALMA3.pdf

System and board architectures (8 LSIs on one FFT board, 0.18-micron LSI
technology, 128 MHz frequency clock, etc.) have been defined and prototype
development is well underway. A test system (2GHz, 2 digitizers, 128
kilochannels, 1 baseline) will be delivered to Nobeyama at the end of
September 2001.

Japanese work on digitizers is summarized in a note distributed during our
informal meeting. Okumura-san presents the Allan variance results obtained
for their 1-bit, 8 GHz digitizer in the range 1-2 GHz. The note can be found
in:

http://www.nro.nao.ac.jp/~sokumura/eALMAad/8G-AD-iguchi.pdf

The Japanese 2-bit design obtained by combining two 1-bit systems is in
progress.

3. Report on DHXF Correlator (Future Correlator) and European Work on
Digitizers

Baudry uses his transparencies presented at the ASAC meeting to discuss some
characteristics of the European design and to outline the system
architecture. Various issues or options related to system architecture,
delay tracking, fringe stopping, system synchronization, etc. are briefly
commented by Bos.

Okumura had a comment on the cooling of the DHXF correlator board whose
power consumption might be more than 100 W per board.

Chikada asks about the effects of computational errors in the FIR filters
due
to internal quantization effects. De Vos mentions this has to be handled
in the quantization studies at ASTRON (see Andre Gunst's contribution in the
February meeting on the European Future Correlator). Other work has been
made in this field by the European team and Baudry will send some
references, including Gunst's contribution, to Chikada.

Baudry presents the major milestones of the European digitizer plan
including the Test Bench to be used for Allan variance and spectral analysis
of the fabricated multi-bit samplers. The first European 2-bit, 4 GHz,
bandpass sampling ASIC design has been accepted by the foundry and further
fabrications will be submitted in May and August this year. The European
team expects that qualification tests of the Test Bench will start in the
Summer.

4. Conclusions and Actions

Developments in both Japan en Europe have similar goals: wide band
correlation, high resolution and sensitivity with large number of channels,
flexibility.

The schedules and milestones until mid-2003 or the end of 2003 could
possibly be brought together more closely to ease the selection of a final
concept for the Enhanced Correlator.

It was agreed that we need to define some common test criteria to evaluate
the European and Japanese concepts.

The following Actions are to be completed before the next face-to-face ASAC
meeting and made public as soon as possible.

Action 1: Propose an initial set of common test procedures and performance
indicators [initiated by Bos for circulation to participants]
Action 2: Propose a joint timeline based on the current schedules to ease
synchronization and comparison of tasks in both teams [initiated by Okumura
for circulation to participants]
____________________________________________________________________________
____


From awootten at NRAO.EDU  Wed Apr 25 10:28:32 2001
From: awootten at NRAO.EDU (Al Wootten)
Date: Wed, 25 Apr 2001 10:28:32 -0400 (EDT)
Subject: [asac] Draft April Minutes 
Message-ID: <200104251428.KAA04951@polaris.cv.nrao.edu>

The ASAC draft minutes, including the statement of the software liaison,
may be found at:
http://www.cv.nrao.edu/~awootten/mmaimcal/asac/asacapr01minutes.html

Please send further corrections if necessary.

Clear skies,
Al


From cwhite at NRAO.EDU  Fri Apr 27 16:43:34 2001
From: cwhite at NRAO.EDU (Carolyn White)
Date: Fri, 27 Apr 2001 16:43:34 -0400
Subject: [asac] [almanews] ALMA Memo 364 Released
Message-ID: <3AE9D9F6.B96D0BDE@nrao.edu>

ALMA Memo 364

An Antenna Location Mask for Configuration Designs for ALMA

Bryan J. Butler

2001-Apr-19

It is not practically feasible to place antennas at any location
in our science preserve. Topographic constraints cause large
areas of the science preserve to be undesirable for antenna placement, 
due to the cost of putting antennas in those locations. In
addition, the existing pipelines and roads provide further constraints 
for possible antenna locations. Given the guidance of the
report of the review committee from the configuration PDR (Guilloteau 
et al. 2001), a new antenna location mask specifying where antennas 
should not be placed on the preserve has been created for use by those 
designing the ALMA configurations, and is presented herein. 


View a pdf version of ALMA Memo 364 at URL:
     http://www.alma.nrao.edu/memos/html-memos/alma364/memo364.pdf

View a html version of ALMA Memo 364 at URL:
          http://www.alma.nrao.edu/memos/html-memos/alma364/memo364.html

Download an html version of ALMA Memo 364 at URL:
          http://www.alma.nrao.edu/memos/html-memos/alma364/memo364.ps
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