GBT Proposal Guide

Low Frequency Science Opportunities

Low frequency (below 8 GHz) projects, especially those that may require significant amounts of observing time per source or field, are strongly encouraged. Observations up to 200 hours per source or field at low frequencies is not unreasonable for the less subscribed LST ranges. Please see the LST pressure plots in the Proposal Results for previous semesters located here.

Expected GBT available time

The GBT is expected to be shut down from May-September during the summer of 2026. During this shutdown, repairs to the GBT infrastructure will be performed. This includes azimuth wheel replacement, painting, and track, foundation and grout work.  If funds for painting are not made available, then it may be possible to support one week of observing in May and June 2026.

It is expected that there will be around 2100 hours available for astronomy in the 26A semester with 169 hours available for high frequency observations requiring nighttime conditions (Mustang2, ARGUS and non-VLBI W-band).

We cannot guarantee that monitoring projects can be scheduled due to the planned infrastructure work. All monitoring requests are required to discuss how the infrastructure work will impact their science goals.

Receiver Availability

Receivers available

Proposal requesting the 342 MHz, 800 MHz, L, S, C, X, Ku, KFPA, Ka, Q, W, Mustang2, and Argus receivers will be considered for review as part of the 26A proposal call.  The accepted proposals will determine which receivers are made available during the 26A semester.

Ultra-wideband

Any proposal requesting the UWBR will be rejected without consideration for the 26A proposal call. 

GBT Capabilities

The GBO encourages proposals that take advantage of the GBT’s unique capabilities across 0.29 to 116 GHz frequency range. (Coverage is not available for 15.8-18.0 GHz, and 50.5-67.0 GHz).

Key science areas include, but are not limited to:

• low column density HI (NHI ≈10¹⁷ cm^-2 galactic and extragalactic)
• star formation
• fast radio bursts
• galaxy and cluster evolution
• pulsars (searches and timing)
• cosmology
• radio recombination lines
• astrochemistry
• solar system science

Details of all GBT observing modes are in The Proposer's Guide for the Green Bank Telescope. Proposers should also consult the more general document The Performance of the GBT: A Guide for Planning Observations.

The GBT will not accept Large Proposals

The GBT only accepts large proposals once per year for the B semester proposal deadlines. Large GBT proposals are not accepted at the A semester proposal deadlines.

Any Large proposal requesting the GBT will be rejected without consideration for the 26A proposal call. 

As a reminder the definitions of Regular and Large proposal for the GBO are as follows:

• 0-8 GHz (Any weather)
  • Regular: < 400 hours and lasting ≤ 1 year
  • Large: ≥ 400 hours or lasting >1 year
• 8-18 and 27.5-50 GHz (Good weather)
  • Regular: < 200 hours and lasting ≤ 1 year
  • Large: ≥ 200 hours or lasting >1 year
• 18-27.5 and > 50 GHz (Excellent weather)
  • Regular: < 100 hours and lasting ≤ 1.5 year
  • Large: ≥ 100 hours or lasting >1.5 year
• Fixed and Monitoring proposals
  • Regular: < 200 hours and lasting ≤ 1 year
  • Large: ≥ 200 hours or lasting >1 year

Instrumentation

 The GBT receivers, backends, and observing modes that are available for Semester 2026A proposals are listed in Tables 1 and 2 below.

Receiver	Frequency Range	Notes
Prime Focus 1	290-395 MHz
Prime Focus 1	680-920 MHz
Prime Focus 1	385-520 MHz and 510-690 MHz	Not available
Prime Focus 2	910-1230 MHz	Not available
Ultrawideband Receiver	700-4200 MHz	No proposals will be accepted.
L-band	1.15-1.73 GHz
S-band	1.73-2.60 GHz
C-band (linear polarization only – see below)	3.8-7.8 GHz
X-band	7.8-11.6 GHz
Ku-band	12.0-15.4 GHz
K-band Focal Plane Array (7 pixels)	18.0-27.5 GHz
Ka-band	26.0-39.5 GHz
Q-band	39.2-50.5 GHz
W-band	67-93.3 GHz
ARGUS	75-116 GHz	See The ARGUS Observer's Web Page for further information
MUSTANG2 (shared-risk – see below)	90 GHz, Shared Risk	Private instrument – proposals must include instrumentation team (see below).

Table 1

 

Backend	Observing Modes
Versatile Green Bank Astronomical Spectrometer (VEGAS)	Continuum (see below), spectral line, pulsar
Digital Continuum Receiver (DCR)	Continuum
Caltech Continuum Backend (CCB)	Continuum (Ka receiver only).
Mark6 Very Long Baseline Array Disk Recorder	Very Long Baseline Interferometry
JPL Radar backend	Private PI Instrument – Open for Public Use
Breakthrough Listen	Private PI Instrument, Shared Risk

Table 2

Permission required for instruments not listed as being available

Anyone requesting a receiver or instrument not listed as being available in the proposal call must have prior permission from the site director, or the GBT schedulers before the proposal is submitted.  Proposals that did not request permission will be rejected without consideration.

C-band Polarization

Proposals wishing to use the GBT C-band receiver should only use linear polarization outputs.  The receiver is not optimally designed for circular polarization and we will not accept any proposals to use the circular polarization output of this receiver.

VLBI including the HSA and GMVA

Proposers should clearly justify the need for the GBT in the text of the proposal.  All Very Long Baseline Interferometry (VLBI) proposals requesting the GBT should include any needed setup and overhead time in the time request of their proposals. 

Proposals requesting the GBT as part of High Sensitivity Array (HSA), and Global 3mm VLBI Array (GMVA) should be submitted through the Very Long Baseline Array's call (available here).

C-band VLBI on the GBT

The GBO will only accept proposals using the GBT C-band receiver for VLBI Stokes I continuum observations (the observations will need to be done using full Stokes just to calibrate Stoke I).  Please see the HSA section of the VLBA call (available here) for proposals for more details.

MUSTANG2

The GBO will accept proposals for shared risk observations using the MUSTANG2 instrument at the proposal deadline.  More information on Mustang2 can be found here.  All MUSTANG2 proposals must have permission from the instrument development team – contact Emily Moravec, Simon Dicker or Brian Mason. 

Breakthrough Listen backend

The Breakthrough Listen project is making its backend available for shared-risk observations during the 2026A semester.  The instrument consists of a cluster of 64 Titan X and 1080 GPU-based servers capturing 8-bit baseband voltages over up to 12 GHz of instantaneous bandwidth.  Data rates are typically tens of TB/hr but a pipeline is available to generate spectra with adjustable frequency (> 3 Hz) and time (> 350 μs) resolutions, with possible science applications including fast radio transients, pulsar observations, stellar flares, SETI, etc.  Before submitting a proposal, proposers must obtain permission from the Breakthrough Listen team.  The team will consult on proposal preparation and data analysis.  Any data acquired using the backend will be proprietary to the proposer per the standard policies.

More information including a technical description of the backend and team contact details can be found here.

Continuum Observations

Proposers wishing to perform continuum observation should consult with a GBO scientist. 

RFI

The most recent RFI monitoring scans for the GBT can be found here.  This tool allows you to explore scans that provide information on the frequencies that may encounter RFI.  Note that a Green Bank computing account is required to be able to view this information. 

If you do not have a Green Bank computing account please look here for pre-made RFI plots.You will not be able to manipulate these plots to obtain more detailed information.

If you wish to obtain more information on RFI near your desired frequencies, please contact the helpdesk to request the desired plots.  This should be done well before the proposal deadline as we cannot guarantee rapid responses on the proposal deadline date.

Observing and Scheduling Constraints

The GBT is scheduled by the Dynamic Scheduling System (DSS). The DSS system is fully described in the GBT Proposer's Guide and the GBT Observer's Guide.

Mapping

If you are considering mapping with the GBT such that there are major turns or moves (end of rows in raster map, petals in daisy maps, changes in position for pointed maps, etc.) that occur with a cadence faster than every 30 seconds, you will need to consult with a GBT support scientist to ensure that the GBT can safely withstand the stresses induced by the mapping motions.

Scheduling Increments

Please note that the GBT is scheduled in 15 minute (0.25 hour) increments and that all proposals should request time appropriately.   Time requests will be rounded down to the nearest 0.25 hour increment. 

GBT Proposal Preparation

All proposals should state why the GBT is necessary for the requested observations in both the abstract and science justification.

Proposers who need assistance with their proposal should submit a helpdesk ticket via https://help.nrao.edu/.  Proposers needing significant help should submit their requests to the helpdesk well before the deadline.

Proposers are encouraged to look at past proposal call results, especially the LST pressure plots, which can be found in the TAC proposal result reports located here.

 All proposers, including pulsar proposers, should use the GBT Sensitivity Calculator. The Sensitivity Calculator results can be cut and pasted into the Technical Justification section of the proposal. This will streamline the creation of your Technical Justification and will lessen the chances for error. 

If you are planning on making maps with the GBT, you should use the GBT Mapping Calculator tool.

The GBT observing policies describe the telescope's remote observing restrictions.

Proposers requesting GBT participation in High Sensitivity Array (HSA), Very Long Baseline Array (VLBA), or Global Millimeter Very Long Baseline Interferometry (GMVA) observations should consult the VLBA, HSA, and GMVA Proposal Call.