20A Proposal Call
The Green Bank Observatory (GBO) invites scientists to
participate in the 2020A Semester
Call for Proposals for the Green Bank Telescope (GBT).
The submission deadline for Semester 2020A proposals is
Thursday, 1 August 2019, at 17:00 EDT (21:00 UTC).
The entire proposal call can be found on this page.
We have noticed for the GBT, that although proposals with female PIs have the same success rate as proposals with male PIs, over the past semesters female PIs tend to request half the amount of time that male PIs request. We are monitoring the situation and welcome suggestions.
New Regular, Large and Extra-Large proposal size definitions for the GBO:
- 0-8 GHz (Any weather)
- Regular: < 400 hours and lasting ≤ 1 year
- Large: 400-1000 hours or lasting 1-2 years
- Extra-Large: >1000 hours and/or lasting > 2 years
- 8-20 and 23-50 GHz (Good weather)
- Regular: < 200 hours and lasting ≤ 1 year
- Large: > 200 hours or lasting 1-2 years
- Extra-Large: not available
- Lasting > 2 years: not available
- 20-23 and > 50 GHz (Excellent weather)
- Regular: < 100 hours and lasting ≤ 1 year
- Large: > 100 hours or lasting 1-2 years
- Extra-Large: not available
- Lasting > 2 years: not available
- Fixed and Monitoring proposals
- Regular: < 200 hours and lasting ≤ 1 year
- Large: > 200 hours or lasting 1-2 years
- Extra-Large: not available
- Lasting >2 years: not available
The GBO encourages proposals that take advantage of the GBT’s unique capabilities across 0.29 to 116.2 GHz frequency range. (Coverage is not available for 2.65-4.0 GHz, 15.8-18.0 GHz, and 49.9-67.0 GHz)
Key science areas include, but are not limited to:
- Low column density HI (NHI ≈1017 cm-2 galactic and extragalactic)
- astrochemistry
- cosmology
- fast radio bursts
- galaxy and cluster evolution
- pulsars (searches and timing)
- radio recombination lines
- solar system science
The GBO also encourages the submission of high risk, high reward proposals requiring GBT observing time.
There are approximately 1000 hours of excellent weather (20-23 and > 50 GHz) available each semester. Prior commitments typically accounts for half of this time which leaves only 500 hours available for new proposals each semester.
Instrumentation news:
- Argus has become a GBO supported instrument and is open to all proposers without restrictions.
- The VEGAS Pulsar Modes have been fully released.
- GUPPI will be retired no later than May 2020. Only the continuation of pulsar timing projects may use GUPPI until then.
Filler time proposals which can take advantage of gaps in the GBT schedule are also encouraged.
Triggered proposals can be submitted for studies of transient objects such as fast radio bursts, near Earth asteroids, comets, and other transients.
All proposals should state why the GBT is necessary for the requested observations in both the abstract and science justification.
We strongly encourage proposers to carefully read through the “News and Opportunities” section of the proposal call.
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).
We wish to remind proposers of continuing opportunities for joint observations with the Chandra X-ray Observatory, the Hubble Space Telescope, the Swift Gamma-Ray Burst Mission, the Fermi Gamma-ray Space Telescope and XMM-Newton.
Proposal preparation and submission remain via the NRAO Proposal Submission Tool (PST) available at NRAO Interactive Services. Note that use of the PST requires registration. Proposers who need assistance with proposal preparation or have questions regarding the Call or GBT capabilities should contact Observatory staff via the Helpdesk.
News and Opportunities
The 1 August 2019 deadline is for the 2020A Semester observing period on the GBT:
1 February 2020 – 31 July 2020
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. Proposers should make sure that they are familiar with the latest versions of these documents before writing their proposal.
Instrumentation News
The GBT receivers, backends, and observing modes that are available in Semester 2018B are listed in Tables 1 and 2 below.
| Receiver | Frequency Range | Note |
|---|---|---|
| Prime Focus 1 | 290 – 395 MHz 385 – 520 MHz 510 – 690 MHz 680 – 920 MHz | |
| Prime Focus 2 | 910 – 1230 MHz | |
| L-band | 1.15 – 1.73 GHz | |
| S-band | 1.73 – 2.60 GHz | |
| C-band | 3.8 – 8.0 GHz | linear only, see below |
| X-band | 5 – 11.6 GHz | |
| Ku-band | 12.9 – 15.4 GHz | |
| K-band Focal Plane Array (KFPA) | 18 – 26.5 GHz | 7-pixel array |
| Ka-band | 26 – 39.5 GHz | |
| Q-band | 38.2 – 49.8 GHz | |
| W-band | 67 – 93.3 GHz | |
| Argus | 75 – 115.3 GHz | 16-pixel array |
| MUSTANG-2 | 90 GHz | shared-risk, private PI instrument |
| Backend | Observing Mode | Note |
|---|---|---|
| VEGAS | continuum, spectral line, pulsar | |
| DCR | continuum | |
| MARK6 Disk Recorder | VLBI | |
| JPL Radar backend | radar | Private PI instrument, open for public use |
| Breakthrough Listen | Private PI instrument, shared risk |
C-Band: Proposals wishing to use the GBT C-band receiver should only use linear polarization outputs. The circular polarization of the receiver is currently not preforming correctly and we will not accept any proposals to use the circular polarization output of this receiver.
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 Long Baseline Observatory call (available here) for proposals for more details.
VEGAS, Continuum: All modes of VEGAS may now be used for continuum observations. The Proposal Submission Tool has not been updated to reflect this situation. Proposers should use the spectral line modes of VEGAS to choose the desired bandwidth and then note in the technical justification that the observations will be for continuum measurements.
VEGAS, Pulsar: VEGAS pulsar modes have been released.
Argus: Observers interested in using the Argus instrument should see http://www.gb.nrao.edu/argus/ for further information.
VLBI: Time available for VLBI on the GBT will be extremely limited as open skies time has been greatly reduced as part of the divestment of the GBT by the NSF. Proposers should only include the GBT in the proposal if it is essential for the science. This should be clearly justified 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. C-band VLBI observers should see the C-band VLBI note above.
MUSTANG-2: The GBO will accept proposals for shared risk observations using the MUSTANG-2 instrument at the proposal deadline. The GBO cannot guarantee that MUSTANG-2 will be cold at the start of scheduled observing due to low observing elevations or rotations of the turret from prior observations. Cool down time for MUSTANG-2 observations should be included in the overhead for MUSTANG-2 observations. All MUSTANG-2 proposals must have permission from the instrument development team.
Breakthrough Listen backend: The Breakthrough Listen project is making its backend available for up to 50 hours of shared-risk observations during the 2020A semester. The instrument consists of a cluster of 32 Titan X and 1080 GPU-based servers capturing 8-bit baseband voltages over up to 5 GHz of instantaneous bandwidth. Data rates are typically tens of TB/hr but a pipeline is available to generate spectra with adjustable frequency (> 3 GHz) 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 at Berkeley SETI Research Center. 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 GBO policies.
More information including a technical description of the backend and team contact details can be found here.
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.
Session lengths: Proposers should be aware that long scheduling blocks (more than 6 hours) may be very difficult to schedule as a result of the reduced open skies time following the divestment of the GBT by the NSF. Proposers must make clear in the technical justification section how their project can be scheduled in small observing blocks that would more easily fit into the GBT scheduling constraints. This is especially critical for proposals that require fixed or coordinated observing dates, e.g. VLBI observations, pulsar monitoring, radar, etc.
Mapping If you are considering mapping with the GBT such that there are major turns or moves (end of rows in raster map, change 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.
“Fixed” and “Windowed” Observations: Due to varied pressures on the GBT’s scheduling resulting from the reduced open skies time as a result of the divestment of the GBT by the NSF, fixed time observations (e.g. VLBI, pulsar transit observations, etc.) and windowed observations (e.g. monitoring observations) will likely have to be ranked at least in or near the top 10-15% of all AUI telescope proposals in order to be accepted.
Instrument Availability:
Due to existing obligations, the Prime Focus 800 MHz feed will only be available for approximately two to three weeks each month. The Prime Focus 342 MHz feed will at most be available for one week each month.
The PFS radar backend (PI: Margot) is available only with prior agreement by the PI.
The availability of GBT Gregorian receivers will be based on demand from the accepted proposals. Some receivers may be available only for a few short, two or three week periods during the semester.
Observing Team Members: We would like to remind all project teams of the Green Bank Observatory policy that all observers must be listed as a member of the project team in the GBT Dynamic Scheduling System. Also, we would like to remind all observers that they should not log into any GBO computing system using another person’s account. Co-Is and students are required to have their own GBO login and account if they are to participate in observing and data reduction.
GBT Proposal Preparation
Proposers should consult the The Performance of the GBT: A Guide for Planning Observations and the GBT Observer’s Guide. All proposers, including pulsar proposers, should use the GBT Sensitivity Calculator. Please see the Calculator’s User’s Guide for instructions. 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 increase your chances of getting a positive technical review. 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.
RFI
RFI Monitoring Scans: The most recent RFI monitoring scans for the GBT can be found here. These scans provide information on the frequencies that may encounter RFI.
470-700 MHz RFI: Digital TV transmissions above 470 MHz will make observing very difficult with the 450 and 600 MHz feeds of the PF1 receiver. Available RFI plots do not show the strength of these signals as the RFI overpowers the system: the plot intensities are estimated to be too low by a factor of up to 10 to 50. Observers should consult the GBT support scientists before submitting a proposal for these feeds. Also, “TV Whitespace” usuage of these frequencies is expected to begin in 2018.
Potential for RFI: It is likely that there will be a major construction project near Green Bank in 2018-2019. For the safety of the workers, a portable radio system at 450 MHz is being proposed for use. Usage would be kept to a minimum, but there will be the potential for interference at 450 MHz and its harmonics during this time period. There remains the potential for RFI at other frequencies from other equipment used in this project.
Schools and Workshops
Observer Training Workshops: The Green Bank Telescope (GBT) Remote Observer Training Workshop will provide the essential skills and knowledge needed to use the GBT and maximize its scientific output. It is intended for experienced astronomers who need to learn the specifics of observing with the GBT. After completing the workshop, an attendee will be certified to use the GBT as a remote observer. The workshop will focus on hands-on training in the observing techniques most relevant to participants (e.g. high frequency map, continuum, pulsar, etc.).
These workshops will be held several times a year and will complement traditional on-site training. The next workshop will be held August 26-27, 2019. More information can be found here.
Single Dish Training School: The Green Bank Telescope (GBT) Single Dish Training School will provide graduate students, post-docs, and experts in other fields of astronomy with both knowledge and practical experience of the techniques and applications of single-dish radio astronomy using the GBT as the primary example. The school will be based around an intensive series of lectures from experts, as well as hands-on radio-astronomy projects and tutorials. Topics to be covered include radio telescope fundamentals, key single-dish science areas, observing and calibration techniques, the impact of weather, the GBT observing procedures and software, and data reduction.
The school will be held once per year. An intensive GBT remote observer training workshop will be held immediately following the school for those who wish to obtain remote observing certification. The 2019 workshop will be held August 19-23, 2019. More information can be found here.
Continuing Opportunities
Joint Observations with XMM-Newton
By agreement with the Green Bank Observatory, detailed in a Memorandum of Understanding, the XMM-Newton Project may award up to 3% of GBT open skies observing time. Similarly the GBT Time Allocation Committee may award up to 150 ks of XMM-Newton time per year. See the Joint Observations with XMM-Newton page for details.
Joint Observations with Chandra X-ray Observatory
In previous semesters, the community has had the opportunity to propose for observing time on NRAO facilities through a joint program with the Chandra X-ray Observatory. The Green Bank Observatory will continue with this program and will allocate up to 3% of the open skies time to highly ranked proposals that request time on both HST and the GBT. Proposers to the GBO will have the opportunity to request time on Chandra, to be awarded on the recommendation of the GBO Telescope Allocation Committee (TAC) and approved by the GBO Director. Up to 120 ksec will be made available to GBO/LBO/NRAO proposers annually. See the Joint Observations with Chandra page for details.
Joint Observations with the Hubble Space Telescope (HST)
By agreement between the NRAO (and continued honoring by GBO) and the Space Telescope Science Institute, STScI will be able to award up to 3% of the available open skies time to highly ranked proposals that request time on both HST and the GBT. In return, STScI has offered 30 orbits of HST time for allocation by the GBO/LBO/NRAO TAC to proposals submitted for the GBO deadlines for Semester 2019B and Semester 2020A. See the Joint Observations with HST page for details.
Joint Observations with Swift Gamma-Ray Burst Mission
To foster correlative observations, a joint Swift/NRAO observing program was established, detailed in a Memorandum of Understanding. The GBO will continue to honor this agreement. By this agreement, the Swift Program permits GBO/LBO/NRAO to award up to 300 kiloseconds of Swift observing time per year. Similarly, GBO/LBO/NRAO permits the Swift Guest Investigator (GI) Program to award GBO observing time. See the Joint Observations with Swift page for details.
Joint Observations with Fermi Gamma-ray Space Telescope
We remind the community that it is possible to propose for observing time on the GBT through the Fermi Gamma-ray Space Telescope Joint Proposal Opportunity or the Cooperative Proposal Opportunity. See the Joint Observations with Fermi page for details.
Joint Proposals Between the GBT and NRAO
Observing programs that require combinations of the GBT, VLBA, and/or the VLA should submit a proposal for each of the requested telescopes, with a clear justification for each, as has been the case to date. The proposals will be reviewed as before and considered jointly by the Time Allocation Committee. VLBI proposals which request the GBT or VLA (or the HSA, for example) as elements of the VLBI array do not need separate proposals—those telescopes can be selected as separate VLBI stations from a VLBA/HSA proposal.
Other Proposal Opportunities
The GBO would like to make users aware that there are additional proposal opportunities as follows:
High Risk Proposals: As a means of maximizing its scientific impact through cutting-edge observations, the Observatory encourages the submission of high-risk/high-reward proposals. The high risk/high reward should be designated in the abstract of the proposal and in the science justification.
Filler Programs: Some programs that are not time critical or require highly subscribed LST ranges can request designation as a “filler program.” Such programs may be able to take advantage of gaps in the GBT schedule, but there no guarantee that any GBT time will be allocated. Proposals requesting a designation as filler should do so in the proposal abstract and in the science justification. All filler programs will be given a ranking of C.
Triggered Proposals: Observations for unknown sources that would be triggered by a celestial event (e.g. near Earth asteroid, comet, fast radio burst, etc.) can be submitted as a triggered proposal. Any accepted triggered proposal will have proprietary rights to observations over any DDT proposal.
Further information about each of these programs can be found here.
20A Proposal Call Results
A total of 97 proposals requesting NSF funded “open skies” time were submitted to the Green Bank A total of 68 proposals requesting NSF funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT) for semester 20A. Proposals are reviewed on a competitive basis with a panel review system (see Proposal Review System). Below are the statistics by proposal count and hours. The oversubscription is the ratio of the number of submitted proposals to the number of approved proposals. The pressure is the ratio of the requested time to the available time in hours. Here we only include proposals submitted for the 20A semester that have been reviewed by the Green Bank Observatory Telescope Allocation Committee (TAC).
A description of the 20A proposals accepted can be found in our NSF Open Skies Science Program section below.
| Total Proposals | 68 |
|---|---|
| Approved | 23 |
| Filler | 12 |
| Rejected | 32 |
| Hold | 0 |
| Withdrawn | 1 |
| Oversubscription | 2.6 |
Statistics by Proposal Hours, table unavailable.
GBT Pressure Plots
Observations in high frequency bands require better weather conditions than observations in lower frequency bands. The GBT uses three weather categories:
- poor – for observations below 8 GHz
- good – for observations between 8-18 GHz and 26.5 – 50 GHz
- excellent – for observations in the 18-26.5 GHz band and above 50 GHz
The first three figures below show the pressure plots for each these weather categories. The last figure includes all weather categories. The grey horizontal line shows the total available hours. The letters A, B, and C correspond to the priorities assigned by the TAC where A and B are approved time and C is filler time. Carryover is time allocated by a TAC from a previous semester that is being executed in the 20A semester.
GBT Observation Preparation
Please use the GBT Dynamic Scheduling System (DSS) to enable observing sessions, select observers for your project, and enter your blackout dates. The DSS Home Page has additional information about the DSS. See GBT Observing for information about how to prepare for your observations.
Please note that the DSS uses the average Right Ascension (RA) and Declination (Dec) of all sources within a session. The average RA and Dec will be used to determine when the session can be scheduled. You will need to carefully check the RA and Dec, along with the minimum and maximum session lengths, to make sure that these values are satisfactory and will allow all your sources to be observed before enabling the session.
20A Science Program
A total of 68 proposals requesting NSF funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT) for the August 1, 2019 semester 20A deadline . The table below summarizes the approved observing programs. Listed are the PI name, proposal ID, proposal title, maximum hours approved and proposal type (Regular, Triggered, Large or External). Proposals from previous semesters that were awarded time in the 20A semester are included. The table also includes HSA and GMVA proposals that were awarded time on the GBT as a VLBI station as well as proposal accepted via external agreements with CHANDRA, Hubble Space Telescope, FERMI and Swift.
For each approved program, the Proposal Finder Tool will have access to its author, title, abstract and total approved hours.
A description of the Time Allocation Committee report for 18B can be found in the Proposal Call Results section above.
| Seymour, Andrew | GBT19B-228 | Exploring the Burst Structures of FRB121102 at High Frequencies | 28 | Regular |
|---|---|---|---|---|
| Appleton, Philip | GBT20A-268 | Measuring the cold gas in super spiral galaxies to z < 0.3 with ARGUS | 50.25 | Regular |
| Battistelli, Elia | GBT19B-095 | MUSTANG2 SZ study of the filamentary structure between cluster pair A401-A399 | 66 | Regular |
| Beasley, Anthony | GBT17B-131 | GBT Observations of 36 GHz Methonal Masers Towards the Galactic Center | 24 | Regular |
| Bordoloi, Rongmon | GBT20A-253 | A high-latitude HI cloud in the Fermi Bubble Wind | 70 | Regular |
| Brodwin, Mark | GBT20A-091 | MUSTANG-2 Observations of the Highest-Richness MaDCoWS Clusters at 0.8 < z < 1.6 | 63 | Regular |
| Butterfield, Natalie | GBT20A-168 | Investigating the Star Forming Potential of the Galactic Bar Dust Lanes | 13 | Regular |
| Cameron, Andrew | GBT20A-060 | Continued observations of an eccentric, relativistic binary pulsar. | 57 | Regular |
| Candelaria, Tierra | GBT20A-277 | Highly Excited NH3 Localized in the Galactic Center | 20 | Regular |
| Chantzos, Johanna | GBT19B-096 | The first steps of Interstellar Phosphorus Chemistry | 40 | Regular |
| Chen, Che-Yu | GBT20A-322 | Characterizing the Internal Velocity Fields of Star-forming Cores with GBT-Argus | 228.5 | Large |
| Clarke, Seamus | GBT20A-139 | A young, cold and quiescent giantmolecular filament – G214.5-1.8 | 12.5 | Regular |
| Codella, Claudio | GBT20A-135 | Large carbon chains in the early stages of Solar-type forming systems | 24 | Regular |
| Das, Sanskriti | GBT20A-398 | A deep search for HI in the CGM of NGC891 and NGC4565 | 21 | Regular |
| DeCesar, Megan | GBT20A-309 | A Continued Search for Pulsed Emission from Candidate MSPs in Globular Clusters | 20 | Regular |
| DeCesar, Megan | GBT20A-388 | Optimizing Pulsar Timing Array Sensitivity to Single Gravitational Wave Sources | 36 | Regular |
| Deller, Adam | VLBA19A-154 | Characterizing Neutron Star Mergers with VLBI Afterglow Observations | 104 | Triggered |
| Demorest, Paul | GBT18B-226 | The North American Nanohertz Observatory for Gravitational Waves | 78 | Large |
| Fonseca, Emmanuel | GBT20A-350 | Timing of GBNCC Pulsars in Relativistic, Intermediate-Mass Binary Systems | 15.25 | Regular |
| Fox, Andrew | GBT20A-238 | GBT 21cm HI Observations toward UV Sources in the Fermi Bubbles | 35.75 | Regular |
| Gallimore, Jack | VLBA20A-190 | The Water Megamaser Disk of NGC1068: Self-Gravitation or Keplerian Rotation? | 6 | Regular |
| Ginsburg, Adam | GBT20A-108 | MUSTANG Galactic Plane survey: The inner Galaxy | 96 | Regular |
| Gupta, Harshal | GBT20A-383 | An Absorption-line Survey of C3H+ in Diffuse Molecular Clouds | 56 | Regular |
| Henshaw, Jonathan | GBT20A-055 | Testing Accretion-Driven Turbulence in Central Molecular Zone Clouds | 2.5 | Regular |
| Ju, Mengting | GBT20A-227 | Starburst in a BCD trigged by gas accretion? | 8.5 | Regular |
| Karunakaran, Ananthan | GBT20A-089 | The HI content of Field Ultra-Diffuse Galaxies in SMUDGes | 141 | Regular |
| Kepley, Amanda | GBT17B-151 | Extragalactic GBT+ARGUS Gas Density Survey | 85.5 | Large |
| Kim, Jae-Young | GMVA19B-233 | Imaging Jet and Magnetic Field near the Spinning SMBH in M87 | 14 | Regular |
| Koch, Eric | GBT19B-221 | Dense Gas Formation through a Spiral Arm | 41 | Regular |
| Kramer, Michael | GBT19B-199 | Timing and General Relativity in the Double Pulsar System | 101 | Regular |
| Lim, Jeremy | GBT20A-140 | Neutral Atomic Hydrogen in the Cooling-Flow Nebula of NGC 5044 – copy | 6 | Regular |
| Luisi, Matteo | GBT20A-149 | Radiative and mechanical feedback in regions of massive star formation | 27.75 | Regular |
| Luisi, Matteo | GBT20A-342 | Diffuse Ionized Gas in the Sagittarius Arm Tangency | 65.5 | Regular |
| Marcum, Pamela | GBT20A-378 | Neutral Hydrogen in Extremely Isolated Early-Type Galaxies – 4 | 119.75 | Regular |
| Margot, Jean-Luc | GBT20A-021 | Interior structure of Europa and Ganymede | 4.5 | Regular |
| Margot, Jean-Luc | GBT20A-375 | A search for technosignatures around Sun-like stars near the plane of the Galaxy | 2 | Regular |
| McGuire, Brett | GBT20A-038 | Is Aromatic Chemistry Everywhere? | 112 | Regular |
| McGuire, Brett | GBT19B-047 | Continuing An Extremely Deep GBT Survey of TMC-1 | 396 | Large |
| Michilli, Daniele | GBT20A-293 | Triggered follow-up of repeating Fast Radio Bursts discovered by CHIME/FRB | 40 | Triggered |
| Morgan, Lawrence | GBT20A-250 | Methanol Maser Monitoring for Variability and Periodicity | 33 | Regular |
| Murphy, Eric | GBT19B-012 | MUSTANG-2 SFRS: 3mm Maps of Star Formation in Nearby Galaxies | 25 | Regular |
| Oslowski, Stefan | GBT20A-117 | Continuing follow-up of ASKAP FRBs | 126 | Regular |
| Ransom, Scott | GBT19B-263 | Continued Timing of a Millisecond Pulsar in a Stellar Triple System | 50 | Regular |
| Ransom, Scott | GBT19B-264 | Long Term Timing of 59 Recycled Pulsars in Bulge Globular Clusters | 75 | Regular |
| Sayers, Jack | GBT20A-290 | Diagnosing the AGN-Driven Bubbles and Shocks in Abell 2052 | 18 | Regular |
| Schmiedeke, Anika | GBT19B-182 | Testing the dissipation of turbulence in dense cores | 15 | Regular |
| Seymour, Andrew | GBT19B-228 | Exploring the Burst Structures of FRB121102 at High Frequencies | 28 | Regular |
| Singal, Jack | GBT19A-083 | How Bright is the Radio Sky? A 310 MHz Absolute Map | 0 | Regular |
| Spekkens, Kristine | GBT18B-246 | Atomic Gas in the Host Galaxies of Events Gravitational Wave | 20 | Triggered |
| Spekkens, Kristine | GBT20A-273 | Atomic Gas in the Host Galaxies of Gravitational Wave Events – The End of O3 | 2 | Triggered |
| Spingola, Cristiana | G19A001 | Confirming the first detection of a merging dual SMBH system at high-z | 14 | Regular |
| Stairs, Ingrid | GBT20A-254 | Understanding the Magnetic Field Configuration in a Moding, Oscillating Pulsar | 13.5 | Regular |
| Stinebring, Daniel | GBT19B-170 | Pulsar Scintillation Arcs – An L-band Follow-up to Previous GBT Detections | 19.5 | Regular |
| Straal, Samayra | GBT19B-063 | Confirming the pulsar that formed PWN G141.2+5.0 | 4 | Regular |
| Svoboda, Brian | GBT19B-253 | GBT-JVLA-ammonia and ALMA-dust measure the origins of the IMF | 3.25 | Regular |
| Swiggum, Joseph | GBT17B-325 | Continuing the GBT All-Sky 350-MHz Pulsar Survey | 230 | Large |
| Williams, Gwenllian | GBT19B-169 | Interaction of two IRDC hubs: A complete evolutionary study of the SDC13 region | 3 | Regular |
| Zhou, Ping | GBT20A-406 | Searching for pulses from a pulsar candidate in supernova remnant G7.7-3.7 | 1.5 | Regular |