Contact Information Agenda/Minutes for meeting Tuesday, 5 July at 4:00 pm EDT.

Date: 5 July 2005

Time: 4:00 pm EDT ( 2:00 pm Socorro, 1:00 pm Tucson)

Phone: Phone: (434)296-7082 (CV SoundStation Premier Conference phone 3rd floor). No Video planned.

Past minutes, etc on MMA Imaging and Calibration Division Page


  1. Rebaselining. A number of issues arose for the Science IPT and others. Front End, Site, Management left to go.
  2. Frequency Switching -- A document: Frequency Switching on ALMA SCID- is available at almaedm.
  3. ACA correlator PDR -- We are closing the issue on highest resolution modes.
  4. Nutator Requirements discussion continues. Comments to almaedm not wiki please. Finalize the Nutator Plan by 1 August.
  5. Early Science Modes: Our proposal for the TFB mode is a wideband mode for e.g. continuum simultaneous with a narrowband mode for e.g. a spectral line. Please comment; we don't have to be limited to one but without a specific group there could be nearly an infinite number. See ALMA Early Science Modes SCID-


  • Draft ALMA, ACA Configurations -- Holdaway

  • Characterization -- What needs to be done to get updated results posted? -- Wootten

  • Antenna news -- TBD Kickoff meeting 28-29 July Dallas.

  • Nutator Discussion -- see almaedm

  • Subarrays -- An option has arisen whereby the patch panel could accommodate any or all of the antennas available. See Subarray Wiki

Science Corner:

B6 Receiver results:


FITS images:
  • S. Wolf Simulation of ALMA imaging a young planet. ALMA fits images + readme file in a gzipped tar file. Wolf writes: "These fits files correspond to the images shown in Fig 2. in my paper with G. D'Angelo (2005, ApJ 619, 1114). All information concerning these images (simulations + the "instrument" function of ALMA + assumed observing conditions) are described in that paper.
  • G. Lodato Simulation of Massive Protostellar Disk. Lodato writes: "The resolution is 256x256. In this way the pixel size is also very close to the resolution length of the simulation. The value of each pixel is the surface density of the disc. What is missing in the header are the actual physical dimensions. This is because the simulations are scale-free and therefore can be scaled to different physical systems. One has to choose a unit length L and a unit mass M (which HAS to be the mass of the central star). The image then spans from -25*L to 25*L both in x and y and the surface density is expressed in the following units:


which means that if your central star has a mass equal to one solar mass and the disc radius is 25AU (L=1AU), then the surface density is in cgs units.



Events of Interest

(see also Al's ALMA Biweekly Calendar)

New! ALMA Calendar testing
Day Date Time Event location details
July 6-7
all day
Front End deltaPDR
July 13
ASAC Telecon
July 26-27
all day
System Requirements Review
Aug 4
ALMA Board telecon
August 26
2-3pm EDT
ANASAC Telecon
877-874-1919 PC=185064
Sep 22
ALMA Board telecon
October 28
2-3pm EDT
ANASAC Telecon
877-874-1919 PC=185064
Nov 1-2
ALMA Board Meeting
Dec 8
ALMA Board telecon

Upcoming Meetings

Star Formation in the Era of Three Great Observatories July 13-15, 2005 in Cambridge, Massachusetts

Astrochemistry throughout the Universe: Recent Successes and Current Challenges 2005 August 29 - September 2; Asilomar, California

Protostars and Planets V 24 - 28 October 2005 Hilton Waikoloa Village, The Big Island, Hawaii

Mm/submm Techniques and Science session, at the URSI General Assembly 2005 October 23-29, New Delhi, India

"IR Diagnostics of Galaxy Evolution". 14-16 November 2005, Pasadena, CA

50th anniversary of the founding of NRAO October 15-19, 2006; Charlottesville, Virginia

ALMA November 13-16; Madrid, Spain

See also NAASC listing

-- AlWootten - 05 Jul 2005
Topic revision: r3 - 2005-07-05, AlWootten
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