Very Large Array (VLA) Proposals

VLA Configuration Plans and Science Time Available

The 1 February 2016 deadline covers the observing period 23 September 2016 through 23 January 2017 (Semester 2016B), corresponding to the A configuration. Multi-configuration proposals that include the A configuration may also be submitted. Additionally, proposals requesting only configurations that will fall in semester 2017A (or later) may be submitted if the Principal Investigator is a graduate student. NRAO offers this service to provide scientific and technical feedback for students, and to provide them with an opportunity to re-submit their proposals for their principal semester with this information in hand. Students should ensure that their status is up to date and correct in the NRAO User Database. Please refer to the VLA Configuration Plans for details and availability of upcoming configurations.

Note that semester 2016A was the last semester NRAO offered any hybrid configuration. Proposers with very southern or northern targets should consult the Array Configurations section of the Guide to Proposing for the VLA on how to combine principal configurations to obtain similar surface brightness sensitivity to the hybrids.

A plot of estimated available observing hours as a function of LST and weather conditions for the A configuration in semester 2016B is below. In this plot, engineering, maintenance, and testing cause the solid (upper) line to be less than the total number of LST days in the configuration; such activities occur predominantly during daytime.

Availability plot A config 2016B

Estimated science time available per LST hour is shown by the solid (upper) black line for all frequencies, the dashed (middle) line for K-band conditions, and dotted (lower) line for Q-band conditions. The colored bars show time already committed in previous proposal rounds, where green represents priority A, yellow priority B, and red priority C. For the net available time in 2016B per LST hour subtract the bars of the pre-committed time from the black curve.

Observing Capabilities for Semester 2016B

The capabilities offered for 2016B through our General Observing (GO) program are similar to those offered for 2016A, with the exception that recirculation by up to a factor of 64 can now provide as many as 1,048,576 channels (subject to the data rate limits noted below and the chosen subband bandwidth); details are given in the Proposing for the VLA section of the Observational Status Summary (OSS) and are summarized in the following table.  Several additional capabilities are available to proposers through the Shared Risk Observing (SRO) and Resident Shared Risk Observing (RSRO) programs, as described below.

CapabilityDescription

8-bit samplers

Standard default setups for:

    • 2 GHz bandwidth continuum observations at S/C/X/Ku/K/Ka/Q bands (16 × 128 MHz subbands)
    • 1 GHz bandwidth continuum observations at L-band (16 × 64 MHz subbands)
      • 256 MHz bandwidth continuum observations at P-band (16 × 16 MHz subbands)

      Flexible setups for spectroscopy, using two, independently tunable, 1 GHz baseband pairs, each of which can be split into up to 16 flexibly tunable subbands

      Single, dual, and full polarization products

      3-bit samplers

      Standard default setups for:

        • 8 GHz bandwidth continuum observations at K/Ka/Q-bands
        • 6 GHz bandwidth at Ku-band
        • 4 GHz bandwidth at C/X-bands

      Flexible setups for spectroscopy, using four, independently tunable, 2 GHz baseband pairs, each of which can be split into up to 16 flexibly tunable sub-bands

      Single, dual, and full polarization products

      Mixed 3-bit and 8-bit samplers

      Allows more flexibility for simultaneous continuum and high-resolution spectral line observing

      Sub-arrays

      Up to 3 independent subarrays using standard 8-bit continuum setups

      Phased array for VLBI

      See VLBA-HSA-VLBI section of this Call for Proposals

      Both single pointing and mosaics with discrete, multiple field centers will be supported. Data rates up to 25 MB/s (90 GB/hour) will be available to all users and, with additional justification, data rates up to 60 MB/s (216 GB/hour) will be available. Correlator integration time limits per band and per array configuration also apply as described in the OSS. The data rate and total data volume required by a proposal will be a consideration in its technical evaluation.

      There are some limitations on frequency settings and tuning ranges, especially at Ka-band; please consult the OSS for further details. Additionally, the Exposure Calculator has been updated and other special tools are available to assist users with the development of correlator setups for the proposal deadline (see VLA Proposal Submission Guidelines). All antennas employ electronics and receiver systems that provide continuous frequency coverage from 1–50 GHz in the following observing bands: 1–2 GHz (L-band); 2–4 GHz (S-band); 4–8 GHz (C-band); 8–12 GHz (X-band); 12–18 GHz (Ku-band); 18–26.5 GHz (K-band); 26.5–40 GHz (Ka-band); and 40–50 GHz (Q-band).

      We continue to offer shared risk programs to our user community for those who would like to push the capabilities of the VLA beyond those offered for general use.

      VLA Shared Risk Observing

      The VLA Shared Risk Observing (SRO) program allows users access to capabilities that can be set up via the Observation Preparation Tool (OPT) and run through the dynamic scheduler without intervention, but are not well tested. The following capabilities are offered under the SRO program in Semester 2016B:

        • On-the-Fly (OTF) mosaicing (used when each pointing on the sky is no more than a few seconds)
        • 32 subbands per baseband with the 8-bit samplers

      See the VLA Proposal Submission Guidelines web page for information about tools and other advice on proposing for Shared Risk observing capabilities.

      VLA Resident Shared Risk Observing

      The VLA Resident Shared Risk Observing (RSRO) program provides access to extended capabilities of the VLA that require additional testing. This access is provided in exchange for a period of residence to help commission those capabilities. Examples of capabilities that would fall under the RSRO program in Semester 2016B include:

        • correlator dump times shorter than 50 msec, including integration times as short as 5 msec for transient detection;
        • pulsar observations;
        • data rates above 60 MB/s;
        • recirculation beyond a factor of 64 in the correlator;
        • P-band system (230–470 MHz) polarimetry and spectroscopy;
        • 4-band system (54–86 MHz; see Low Frequency Observing section below);
        • more than 3 subarrays, or sub-arrays with the 3-bit system;
        • complex phased array observations (e.g., pulsar and complex VLBI observing modes); and
        • frequency averaging in the correlator: a new capability for averaging to wider frequency channels in the correlator has been developed that will reduce the data volume for all continuum subbands

      A detailed description of the VLA RSRO program for semester 2016B and beyond is available at the VLA Proposal Submission Guidelines web page.

      Low Frequency Observing

      The new low frequency receiver system developed in collaboration with the Naval Research Laboratory is available for Stokes I continuum observations at P-band (230–470 MHz) through the GO program. Use of the P-band system for polarimetry and/or spectroscopy is through the RSRO Program. The new receivers also work at 4-band (54–86 MHz), and new feeds will be deployed on at least ten (and up to fourteen) VLA antennas. Both 4-band and P-band can be observed simultaneously, but access to the 4-band system is only available through the RSRO program.

      Finally, the commensal VLITE system will take data at P-band during regular observations that use bands other than P-band.  The VLITE system is deployed on ten VLA antennas.  Observers wishing to gain access to the commensal VLITE data taken during their VLA observations should follow the instructions on the VLITE web page for doing so.

      Proposal and Observation Preparation

      Proposal preparation and submission are via the Proposal Submission Tool (PST) at NRAO Interactive Services. Use of the PST requires registration in the NRAO User Database. There are various tools and documentation to help users in this process. Descriptions of all updated documentation and tools, along with an outline of the steps required to write a proposal, are available at the Guide to Proposing for the VLA web page.

      When constructing sessions in the PST, proposers should be cognizant of their use by the Time Allocation Committee (TAC). Specifically taking into account the time available as a function of LST, the TAC will assign a scheduling priority to each session in each proposal. The assigned scheduling priority will depend on the linear-rank score of the proposal from its scientific review, the LSTs involved in the session (daytime is harder to accommodate than nighttime), the total time requested in the session, and the competition from better-ranked proposals requesting time at similar LSTs. Please see the description of the VLA prioritizer for further details.

      All approved VLA observations are set up using the Observation Preparation Tool (OPT). Most, if not all, projects will be observed dynamically; users should submit scheduling blocks early in the configuration to maximize the opportunity of them being observed. Advice on the optimal length of scheduling blocks and other useful information may be found at the Observing FAQ web page.

      Information about VLA capabilities, proposal preparation and submission, observing strategies, and calibration overhead can be found in the VLA Observational Status Summary, at the Guide to Proposing for the VLA, at the Guide to Observing with the VLA, and at the Observing FAQ web page. Questions may also be directed to the NRAO Helpdesk.

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