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Overhead view of the VLA in D-configuration   The Very Large Array  
  What's New at the VLA  
  Last Updated: 7 February 2002  
  New Hardware   New Software   Other News   Ongoing  
  Recent VLA Hardware Improvements
 
  • High-frequency developments:

    • New high-frequency status page: a new Web page from Debra Shepherd gives the current status of the new 7mm and 1.3cm systems on the VLA, including receiver and system temperatures, pointing errors, and known problems.

    • 7mm (Q-band): As of September 2000, 7mm receivers have been installed on 22 of the VLA antennas. We anticipate 25 antennas to be so equipped by the end of 2000. Thanks again to the NSF/MRI program and MPIfR for making this possible!

    • 1.3cm (K-band): As of September 2000, new 1.3cm front-ends have been installed on 14 of the VLA antennas. System temperatures are about 55 K, compared to the 160 K typical of the old system.

  • Other hardware improvements:

    • Pointing: A prototype of a new encoder system has been installed on antenna 24; the aim is to improve the blind rms pointing accuracy from 10 to below 6 arcseconds.

  • Calibration improvements:

    • Gain Curves: A calibration run was carried out on July 8, 2000 to update the antenna gain curve coefficients at K and Q bands. The results can be found at the VLA Gain Curve Archive Page. In spite of poor summer weather, updated elevation dependent gain correction factors were determined for most antennas, especially those upgraded over the past year. .

    • Tip Curves: Data on atmospheric opacity taken with the VLA in "tipper mode" (TE) are automatically reduced and archived on Bryan Butler's Tip Curve Archive Page. For more information on making and understanding VLA tip curve measurements, see Bryan's VLA Scientific Memo 170.

  • The Expanded VLA (EVLA) Project:

    • News: Brent Carlson and the gang at DRAO have proposed a novel digital wide-band correlator (WIDAR) for the EVLA. See the various EVLA technical memoranda for details.

    • Documentation: Please see the EVLA Home Page for more details.


  Recent Software Upgrades and Developments
 
  • Scheduling Software:

    • JOBSERVE: We are in the process of developing the next-generation JAVA-based scheduling program JOBSERVE, and complete reworking of the venerable OBSERVE program. See the JOBSERVE Home Page for details. Note that JOBSERVE is still in the testing stages and therefore we cannot enourage users to move from OBSERVE at this time - however, it is quite capable for scheduling most simple observing programs so you might want to be brave and give it a whirl!

  • Analysis Software:

    • AIPS++: The AIPS++ "Astronomical Information Processing System" is our major user-grade software development and eventual successor to classic AIPS. It is under continual development and testing, with public releases in April and October of each year - see the current public release documentation for information on how to obtain the latest version. See the AIPS++ Home Page for further details. Alas, AIPS++ is still under vigorous development and is not yet ready for widespread use in the community. However, there has been continual improvement and the interested user should keep an eye on the biannual releases for features that might be of interest.


  Miscellaneous Notices
 
  • Polarization monitoring program: Steve Myers & Greg Taylor have begun monitoring the polarization of about 10 compact calibrators, widely distributed in right ascension, primarily to allow better calibration of the VLBA. Each source is observed about once a month, with flux densities and polarization angles tied to observations of 3C48, 3C138, or 3C286. Currently calibration is available at 7mm, 1.3cm, 3.6cm, and 6cm.

  • Complex correlation: the VLA online software has been updated to make complex correlation of ungated continuum observations the default. Observers desiring gated observations OF ANY TYPE are advised to contact Joan Wrobel or Ken Sowinski at least two weeks before their observations. See NRAO Newsletter No. 76 (1 July 1998) for details.

  • Recent L-band tests show that the VLA performs better than expected from 1140--1250 MHz; see NRAO Newsletter No. 75 (1 April 1998) for details.


  Older News:
 
  • Low Frequency Data Reduction at the VLA: Namir Kassim and Rick Perley have written up a guide to dealing with 74/330 MHz VLA data, and the first draft is here! This is a working draft; please send comments or suggestions to Joseph Lazio (lazio@rsd.nrl.navy.mil). It's also available as postscript [346k]).

  • NRAO Electronic News Bulletin: NRAO has recently instituted an electronic news bulletin that is intended to supplement the regular NRAO Newsletter. This is an email service consisting of short descriptions of news stories, articles, meeting announcements, and so forth, together with web links to longer descriptions. If you wish to receive these e-mailings, please sign up!

  • OBSERVE bug: Past versions of OBSERVE (possibly all before the most recent release on 16 December 1998) had a bug which affected spectral line observers using the "no change" option (//FIN card). If you don't know what this is, you haven't used it! Choosing the "no change" option on the Local Oscillator page should produce a //FIN card in the resulting OBSERVE file; instead, no //FI card of any type was produced. This sets the local oscillators to their default settings, appropriate for wide-band continuum work but seldom desirable for spectral line observations. We have checked the past year's worth of OBSERVE files for this problem; only one file had this problem, and that observer has already been contacted. OBSERVE itself is now fixed (16Dec98), and the new corrected version 4.0.4 can be fetched from our anonymous ftp site. Please check with Michael Rupen mrupen@nrao.edu if you wish further details.

  • Very strong RFI near 1622 MHz: The Iridium constellation of satellites has begun transmitting almost continually at 1622 MHz. This has serious consequences for 1612 MHz OH observations, and for continuum observations near 1622 MHz.


  Regular News:
 

   
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Last modified 17 Jan 2001 - Steven T. Myers