22B Proposal Call
The Green Bank Observatory (GBO) invites scientists to
participate in the 2022B Semester
Call for Proposals for the Green Bank Telescope (GBT).
The submission deadline for Semester 2022B proposals is
Tuesday, 1 February 2021, at 17:00 EST (22:00 UTC).
The entire proposal call can be found on this page.
The GBO would like to encourage low frequency (below 8 GHz) projects, especially those that may require significant amounts of observing time per source or field.
We would like to remind proposers that their submissions will be peer reviewed by a panel with a wide ranging background in astronomy.
Proposal preparation and submission remain via the NRAO Proposal Submission Tool (PST) available at NRAO Interactive Services. Proposers who need assistance with proposal preparation or have questions regarding the Call or GBT capabilities should contact Observatory staff via the Helpdesk. Note that use of the PST and Helpdesk requires registration.
News and Opportunities
The 1 February 2022 deadline is for the 2022B Semester observing period on the GBT:
1 August 2022 – 31 January 2023
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.
All proposals should state why the GBT is necessary for the requested observations in both the abstract and science justification.
Proposal preparation and submission remain via the NRAO Proposal Submission Tool (PST) available at NRAO Interactive Services. Proposers who need assistance with proposal preparation or have questions regarding the Call or GBT capabilities should contact Observatory staff via the Helpdesk. Note that use of the PST and Helpdesk requires registration.
A Virtual Proposal Planning Workshop will be held January 20 and 26. Learn more and register.
GBT Capabilities
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 50.5-67.0 GHz).
The GBO encourages the submission of:
- Low frequency (below 8 GHz) projects, especially those that may require significant amounts of observing time per source or field
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
Large Proposals
Beginning with the 2020B semester the GBT will only accept large proposals once per year at the February proposal deadlines. We will no longer accept GBT large proposals at the August proposal deadlines. This new policy ensures equality for the reviews of all large proposals that can be scheduled across a full year.
Recall that all large proposals are restricted to using no more than 50% of the open skies time available under any weather category (poor, good, excellent) at any LST during any semester.
New Regular, and Large proposal size definitions for the GBO:
- 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 year
- Large: ≥ 100 hours or lasting >1 year
- Fixed and Monitoring proposals
- Regular: < 200 hours and lasting ≤ 1 year
- Large: ≥ 200 hours or lasting >1 year
Proposers submitting Large Proposals should read the Large Proposal Policy to ensure that they address all of the mandatory requirements.
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 | Expected Availability | Note |
|---|---|---|---|
| Prime Focus 1 | 290 – 395 MHz 680 – 920 MHz | short campaigns with irregular intervals between | |
| Prime Focus 1 | 385 – 520 MHz 510 – 690 MHz | high rank proposal demand only | |
| Prime Focus 2 | 910 – 1230 MHz | high rank proposal demand only | |
| L-band | 1.15 – 1.73 GHz | entire semester | |
| S-band | 1.73 – 2.60 GHz | short campaigns every 2 months | |
| C-band | 3.8 – 8.0 GHz | most of semester (except when S-band is available) | linear only, see below |
| X-band | 5 – 11.6 GHz | entire semester | |
| Ku-band | 12.9 – 15.4 GHz | campaigns | |
| K-band Focal Plane Array (KFPA) | 18 – 26.5 GHz | entire semester | 7-pixel array |
| Ka-band | 26 – 39.5 GHz | campaigns | |
| Q-band | 38.2 – 49.8 GHz | campaigns | |
| W-band | 67 – 93.3 GHz | short campaigns | |
| Argus | 75 – 115.3 GHz | entire semester | 16-pixel array |
| MUSTANG-2 | 90 GHz | entire semester | shared-risk, private PI instrument |
| Backend | Observing Mode | Note |
|---|---|---|
| VEGAS | continuum, spectral line, pulsar | |
| DCR | continuum | |
| CCB | continuum | Ka-receiver only |
| MARK6 Disk Recorder | VLBI | |
| JPL Radar backend | radar | Private PI instrument, open for public use |
| Breakthrough Listen | Private PI instrument, shared risk |
Instrument Availability: The availability of GBT Gregorian receivers and prime focus feeds will be based on demand from the highly ranked (Group A) proposals. Some receivers and feeds may be available only for a few short, two or three week periods during the semester.
Availability of Receivers: The GBO plans on testing and commissioning new prime focus receivers during the 22B semester. These receivers will enhance the low-frequency capabilities of the GBT. However, the testing and commissioning of these new receivers will create significant scheduling pressure on the existing prime focus receivers. We will endeavor to accommodate proposals for prime focus receivers but encourage observers to make use of Gregorian receivers whenever scientifically feasible and to consider flexible observing strategies when requesting a prime focus receiver. This is especially true for proposals that request regular monitoring observations, phase connection observations, as well as any fixed date or temporally constrained observations.
We anticipate that the L-band, X-band, MUSTANG-2, Argus and KFPA receivers to be available most of the semester. We anticipate the following receivers to be available for short campaigns on an irregular basis: PF/342 MHz, S-band, C-band, Ku-band, Ka-band, Q-band and W-band. Other PF feeds would be made available for high ranking proposals. It is anticipated that PF/800 MHz will only be available on an irregular basis beginning in the 22B semester.
We anticipate commissioning the new 0.7-4 GHz ultrawideband (UWB) receiver during the spring and summer of 2022. If commissioning is successful we plan on making the UWB receiver available for the 23A proposal call (August 1, 2022 deadline). We will consider allowing some proposed observations the opportunity to switch from currently available receivers to shared-risk use of the UWB receiver in the 22B semester pending the successful commissioning of the receiver. Any proposal that wishes to be considered for this opportunity should include the following sentence in their technical justification under the section for “novel” observing: “We are interested in switching to the 0.7-4 GHz ultrawideband receiver for this project pending successful commissioning.”
We will contact projects that include this statement after commissioning is finished to re-confirm their interest and discuss observing procedures. We stress that we will not guarantee the availability of the UWB receiver in the 2022B semester, and projects must ensure that their scientific goals can be achieved without using the UWB receiver.
The UWB receiver is optimized for high-precision pulsar timing and wide-band observations of fast transients. VEGAS will support coherent and incoherent dedispersion, and pulsar searching and timing modes over the full bandwidth of the receiver. If you have questions about the predicted sensitivity of the receiver and supported observing modes, please contact Ryan Lynch.
High Frequency Observations: There are approximately 1000 hours of excellent weather (18-27.5 and > 50 GHz) available each semester for both open skies and sponsored time. Prior commitments typically account for slightly more than half of this time which leaves only 450 hours available to be scheduled each semester.
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 permission from the site director before the proposal is submitted.
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: TheGBO 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 are available for use.
Argus: Observers interested in using the Argus instrument should see http://www.gb.nrao.edu/argus/ for further information.
VLBI: 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. C-band VLBI observers should see the C-band VLBI note above.
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).
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 to submit a proposal and must include the instrument team on the proposal as co-investigators (see instrument team list and contacts here). For more information on MUSTANG-2 see: https://greenbankobservatory.org/science/gbt-observers/mustang-2/
Breakthrough Listen backend: The Breakthrough Listen project is making its backend available for shared-risk observations during the 2022B 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 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) become increasingly difficult to schedule as a result of the transition to reduced open skies time by the NSF. Proposers must clearly state in the technical justification section how their project could be scheduled in smaller observing blocks that would more easily fit within 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, 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.
Fixed, Windowed and Temporally Constrained Observations: Due to varied pressures on the GBT’s scheduling resulting from the transition to reduced open skies by the NSF, fixed time observations (e.g. VLBI, pulsar transit observations, etc.), windowed observations (e.g. monitoring observations) and temporally constrained observations (pulsar phase connection, orbit phase constraints, etc.) 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.
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.
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
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.
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 workshops will be held in February 2022, May 2022, and in the fall of 2022. 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 next school is tentatively set to occur in May 2022. More information can be found here.
Joint Observatory Observation Opportunities
Joint Observations with SOFIA
By agreement with the Green Bank Observatory, SOFIA may award up to 5% of GBT open skies observing time. Similarly the GBT Time Allocation Committee may award up to 3% of U.S. Guest Observer Time on SOFIA. See the Joint Observations with SOFIA page for details.
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/NRAO proposers annually.
Due to Chandra’s increasingly challenging thermal constraints, the amount of Chandra exposure time available for High Ecliptic Latitude (HEL) targets with |bGal| > 55deg is extremely limited. If you request joint time on Chandra, please avoid long exposures on such targets if at all possible. You must note explicitly the requested amount of Chandra HEL time in the body of your science justification.
N.B., Chandra ToO proposals are not supported under the Chandra-NRAO joint program. 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 per year of HST time for allocation by the GBO/NRAO TAC. See the Joint Observations with HST page for details.
N.B., HST “Snapshot” observations are not supported under the HST-NRAO Joint program since there is no guarantee that Snapshot targets will be completed.
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/NRAO to award up to 300 kiloseconds of Swift observing time per year. Similarly, GBO/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.
22B Proposal Call Results
A total of 70 proposals requesting NSF-funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT) for semester 22B. 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 22B semester that have been reviewed by the Green Bank Observatory Telescope Allocation Committee (TAC).
A description of the 22B proposals accepted can be found in our NSF Open Skies Science Program section below.
| Total Proposals | 70 |
|---|---|
| Approved | 30 |
| Filler | 19 |
| Rejected | 18 |
| Hold | 2 |
| Withdrawn | 1 |
| Oversubscription | 2.33 |
| Requested Time | 3334.25 h |
| Available Time | 1828.75 h |
| Approved | 694.75 h |
| Filler | 376.75 h |
| Rejected | 2134.75 h |
| Pressure | 1.8 |
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 22B 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.
22B Science Program
A total of 70 proposals requesting NSF-funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT) for the February 1, 2022 semester 22B 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 22B 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 proposals accepted via external agreements with CHANDRA, Hubble Space Telescope, FERMI, SOFIA, Swift, and XMM.
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 22B can be found in the Proposal Call Results section above.
| PI | ID | Title | Hours | Type |
|---|---|---|---|---|
| Archibald, Anne | GBT22A-358 | Continued Timing of a Millisecond Pulsar in a Stellar Triple System | 50 | Regular |
| Bastian, Tim | GBT22A-360 | Probing the Inner Heliosphere with Pulsars: a Pilot Study | 10 | Regular |
| Bhakta, Deven | GBT22B-270 | Searching for Globular Cluster Pulsars | 10 | Regular |
| Bilous, Anya | GBT22B-266 | Zooming in on Pulsar Microstructure to understand Fast Radio Bursts | 18 | Regular |
| Bolatto, Alberto | GBT21B-024 | GBT EDGE: A Representative Survey of the z=0 Universe with Full IFU Spectroscopy | 300 | Large |
| Bublitz, Jesse | GBT22B-250 | Refining the Molecular Gas Enigma: Mapping NGC 6781 at 3mm | 16.5 | Regular |
| Busch, Michael | GBT22A-434 | SC:Mapping molecular clouds in OH from diffuse to high-mass star forming regions | 300 | Large |
| Caleb, Manisha | VLBA22B-074 | Probing the local environment of FRB 20190714A | 6.5 | Regular |
| Calore, Francesca | GBT22B-112 | Follow-up of bulge MSP candidates detected by both Chandra and VLA | 24.5 | Regular |
| Cameron, Andrew | GBT22A-118 | Continued observations of an eccentric, relativistic binary pulsar. | 57 | Regular |
| Dai, Shi | GBT22B-030 | Monitoring the active repeater FRB 20190520B | 24 | Regular |
| Dong, Adam | GBT22B-213 | GBT Follow-up of a Novel Repeating Galactic Transient Detected with CHIME/FRB | 32 | Regular |
| Emig, Kimberly | GBT22B-170 | Recombination Lines from Diffuse Ionized Gas in the M82 Starburst | 8.75 | Regular |
| Fonseca, Emmanuel | GBT22B-215 | Followup Timing of Low-declination GBNCC Pulsars | 10 | Regular |
| Frayer, David | GBT22B-162 | GBT HI Observations of the GOALS LIRG 3C84 | 2 | Regular |
| Freire, Paulo | GBT22B-143 | Following two potentially super-massive pulsars in NGC 6624 and NGC 1851 | 13 | Regular |
| Gallimore, Jack | VLBA22B-148 | OH Masers in the Water Megamaser Disk of NGC 1068 | 12 | Regular |
| Goldsmith, Paul | GBT22B-011 | A Novel Technique for Electron Density Determination | 18 | Regular |
| Gorai, Prasanta | GBT22A-398 | Exploring Carbon Chain Chemistry of Massive Protostars | 22 | Regular |
| Gupta, Harshal | GBT21B-316 | Molecular Exploration of the Diffuse Interstellar mediUM (MEDIUM) | 285.75 | Large |
| Huang, Jane | GBT22B-085 | Mapping the Delivery of Material to a Planet-forming Disk – copy | 2 | Regular |
| Issaoun, Sara | GMVA22B-249 | Resolving Polarization in Sgr A* with GMVA+ALMA | 10 | Regular |
| Jones, Michael | GBT22B-064 | Cold gas reservoirs of satellites in nearby Milky Way-like systems | 96.5 | Regular |
| Kooi, Jason | GBT22A-404 | Probing Fluctuations in the Solar Wind with Pulsars: a Pilot Study | 17 | Regular |
| Kramer, Michael | GBT22B-231 | Timing and General Relativity in the Double Pulsar System | 101 | Regular |
| Lockman, Felix | GBT22B-204 | The Ophiuchus Superbubble — Connecting the Disk to the Halo | 115.5 | Regular |
| Lowe, Ian | GBT22B-068 | A Multi-Scale, Multi-Wavelength Study of Dust in Molecular Cloud Filaments II | 21.5 | Regular |
| Luo, Jing | GBT22B-269 | PSR J2108+45 with a massive companion and dense circumstellar environment | 36.5 | Regular |
| Maan, Yogesh | GBT22B-104 | Transient radio emission from magnetars and connection with FRBs | 23.75 | Triggered |
| Margot, Jenan-Luc | GBT22B-209 | A search for technosignatures around newly discovered exoplanets | ||
| 2 | ||||
| Mason, Brian | GBT22B-242 | Measuring 3mm Source Contamination in the ACT Galaxy Cluster Sample | 18.75 | Regular |
| Maureira, Maria Jose | GBT22B-180 | CO freeze-out across a filamentary dense cloud forming a quadruple system | 25.5 | Regular |
| McKean, John | VLBA21B-289 | Resolving the nature of quasar flux-ratio anomalies in gravitational lenses | 60 | Regular |
| Naidu, Shantanu | GBT22B-226 | Bistatic Goldstone-GBT Radar Imaging of Binary Near-Earth Asteroid Didymos | 25 | Regular |
| O’Neil, Karen | GBT22B-065 | Hunting for Massive Low Surface Brightness Galaxies | 128.75 | Regular |
| Park, Jongho | GMVA22B-100 | A Multicolor View of the Black Hole Environment in M87 | 28 | Regular |
| Ransom, Scott | GBT22B-256 | Long Term Timing of 65 Recycled Pulsars in Bulge Globular Clusters | 75 | Regular |
| Redaelli, Elena | GBT22B-052 | A crucial test for the mass of prestellar cores in a high-mass clump | 2 | Regular |
| Ribaudo, Joseph | GBT22A-430 | The Baryonic Tully-Fisher Relation for Galaxies with Supernova Distances | 132 | Regular |
| Roberts, Hayley | GBT22B-060 | Understanding the role of dense gas in the most extreme OH megamasers | 34.75 | Regular |
| Roth, Nathan | GBT22B-176 | Measuring NH3 and OH in a Target of Opportunity Comet with the GBT | 7.5 | Triggered |
| Salas, Pedro | GBT22A-269 | Probing the C+/C interface in the Orion Bar | 16.5 | Regular |
| Salas, Pedro | GBT22A-437 | SC: GBT Diffuse Ionized Gas Survey at Low frequencies – GDIGS-Low | 826 | Large |
| Salome, Quentin | GBT22B-049 | A survey of atomic gas in NLSy1 galaxies with X-ray Ultra Fast Outflows | 31.25 | Regular |
| Sanchez, Monica | GBT22B-228 | Observations of Marginal Arecibo HI 21cm Detections in the Zone of Avoidance | 4.5 | Regular |
| Schmiedeke, Anika | GBT22B-191 | Feeding a super-critical filament in a subsonic core | 17.5 | Regular |
| Scibelli, Samantha | GBT22A-435 | SC: Q- Band Chemical Complexity Survey of Prestellar Core L1544 | 647 | Large |
| Singal, Jack | GBT19A-083 | How Bright is the Radio Sky? A 310 MHz Absolute Map | 30 | Regular |
| Song, Yiqing | GBT22B-248 | Mapping HCN and HCO+ in Local Luminous Infrared Mergers | 19.5 | Regular |
| Spekkens, Kristine | GBT22B-139 | Atomic Gas in the Host Galaxies of Gravitational Wave Events – LVK O4 | 40 | Triggered |
| Spezzano, Silvia | GBT22B-040 | Exploring the chemistry of Sulfur towards the young starless core L1521E | 18 | Regular |
| Sridharan, T.K. | GBT22A-366 | Path to Precision Astrochemistry with Magnetars II – mm-wave Observations | 33 | Regular |
| Stark, David | GBT22A-325 | Understanding diverse HI depletion times in MaNGA star forming galaxies | 79.25 | Regular |
| Stark, David | GBT22A-436 | SC: Robust Gas Measurements for BreakBRD Galaxies | 206.5 | Large |
| Traianou, Efthalia | GMVA21B-164 | Moving and stationary shocks interaction after a gamma-ray flare in TXS2013+370 | 27 | Regular |
| Valdivia Mena, Maria Teresa | GBT22B-163 | Mind the gap: connecting the scales between filaments and protostars | 18 | Regular |
| Wen, Di | G22A001 | A magnified view of an ionised scattering medium in a z= 1.145 late- type galaxy | 36 | Regular |
| Wolszczan, Alexander | GBT22B-200 | A search for planets around white dwarfs | 18 | Regular |
| Yang, Chentao | GBT22B-020 | Confirming the nature of a 380GHz H2O maser disk in a lensed quasar at z=3.91 | 14 | Regular |