ALMA previous meeting     next meeting

Contact Information

  • 2005-1-25 15:30 UT
  • Duration: 1 hr
  • USA Toll Free Number: 877-874-1919
  • Toll Number: +1-203-320-9891
  • Passcode: 185064
  • Leader: Al Wootten

Calendar

11 Jan 2005 ALMA Town Meeting, AAS San Diego; Presentations
14-15 Jan 2005 CSV Discussion, Socorro; Presentations
25 Jan 2005 NA Board Telecaucus
27 Jan 2005 ALMA Board Telecon Dates for 2005
24-25 Feb 2005 ASAC Face-to-face Garching
24 Feb 2005 ALMA Board Telecon. Rebaselining to be discussed.
5-6 April 2005 ALMA Board Face-to-face meeting, Pasadena, CA.

Topics

  1. Old Business The enhanced Agenda from last month's meeting is available. Science IPT notes from last month's telecon.

DUSTY04 collection of papers relevant to ALMA.

  1. New Business--Project news/updates (Wootten, Wilson, Kawabe)
  2. Milestones--09.2.17.2 Complete draft ICD between Science and Site Planned 2303d Not Critical
  3. SolarObserving
  4. Group Activities (all)
  5. Next meeting is on February 15th (15:30 UT)

Science IPT Group Activity Reports

Please include your Group Activity Report here (How to Enter Your Report), or email it to AlWootten

1 Science IPT Statement of Work: Draft Document, Risk, Budget

2 ASAC news Next telecon 1 Feb, face-to-face meeting 24-25 Feb in Garching. Unapproved Minutes of January meeting

3 Antennas

4 Astronomer Outreach: NRAO Newsletter ESO Newsletter. NRAO ALMA Calendar

Emerson/Laing -- Instrument Scientists

EVLA Memo #88Quantization Noise, by A. R. Thompson and D. T. Emerson

John Conway -- Configuration

Congratulations to John on the birth of a son!

One aspect of rebaselining of the ALMA project for us may well be redesign of the array.

Japan has proposed to place the ACA in the western of the sites proposed by the project. The reasons are given in a document on almaedm. Please send your comments; the proposal seems well justified to those who have responded.

Jeff Mangum -- Calibration

Robert Lucas -- SSR

Michiel Hogerheijde -- DRSP

Robert Laing -- Commissioning and Science Verification

This has been a major focus over the last few weeks--please see the wiki page for details.

Mark Holdaway/Steve Myers -- Imaging

Calibrator Survey: We need versions of this at different levels of scope, as this will be new scope for the construction project.

L.-A. Nyman -- Site Characterization

Surveillance cameras have been operated for some time at the site. In the ALMA era, there are safety reasons for deploying surveillance cameras. We have used these for cloud cover studies (not terribly useful as they look at the horizon). Is there a scientific need for these--if so, what are the requirements. Discussions to date have suggested the usefulness of an infrared camera looking upward similar to that Japan has deployed at SUBARU but such a camera would have different requirements from those demanded by safety considerations.

The Altiplanic Winter has begun with a vengeance, we hear.

Science Corner:

Science Corner:  Sebastian Wolf writes: The new simulation was done for an observing wavelength of * 870mu *, instead of 330mu. These simulations show that the locally heated region around the (proto)planet is not visible anymore, even if the system is in a distance of only 50pc. The assumed system temperature is 220K (compared to 1200K at 900GHz - based on ALMA Memo 393). All other parameters (phase noise, pointing error/model, etc.) are the same as in Wolf & D'Angelo (2005; see http://xxx.uni-augsburg.de/pdf/astro-ph/0410064) The main reason for the negative result is the fact that the hot region around the planet has a small diameter only. Increasing the beam size, this signal is smoothed with the almost zero signal of the low-density gap and cannot be distinuished anymore from the bright region of the disk outside the gap. That's at least my understanding of the situation (which I found to be true in all other simulations I performed).

ALMA Planet Simulation

Fig. 2.— Simulation of ALMA observations of disk with an embedded planet of 1Mjup around a 0.5M⊙ star (orbital radius: 5AU). The assumed distance is 50 pc or 100 pc as labeled. The disk mass is set to that of the Butterfly Star in Taurus. Note the reproduced shape of the spiral wave near the planet and the slightly shadowed region behind the planet in the upper images.

See set of PPT slides from W. Wolf.

Upcoming Meetings

Dusty and Molecular Universe 27-29 October 2004, Paris Presentations Online

2005 IEEE International Conference on Acoustics, Speech, and Signal Processing March 19-23 2005, Philadelphia See Radio Astronomy Session; ALMA Article for ICASSP. Comments? Reviews welcomed.

IAU Symposium 227 Massive Star Birth: A Crossroads of Astrophysics May 16-20 2005, Acireale, Italy

Workshop on submillimeter wavelength astronomy in Cambridge (JUN 13-16).

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

URSI General Assembly 23-29 October 2005; New Delhi, India; "Mm/submm Techniques and Science" session 25-26 Oct.

-- AlWootten - 18 Jan 2005
Topic revision: r6 - 2010-08-03, ToddHunter
This site is powered by FoswikiCopyright © by the contributing authors. All material on this collaboration platform is the property of the contributing authors.
Ideas, requests, problems regarding NRAO Public Wiki? Send feedback