20B Semester

20B Proposal Call

The Green Bank Observatory (GBO) invites scientists to
participate in the 2020B Semester
Call for Proposals for the Green Bank Telescope (GBT).

The submission deadline for Semester 2020B proposals is
Monday, 3 February 2020, at 17:00 EDT (22:00 UTC).

The entire proposal call can be found on this page.

Receiver availability for the 2020B semester will be determined by those highly ranked proposals accepted in Group A.

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.  There will not be a large proposal call for 2021A for the GBT.  The next large proposal deadline for the GBT after this call will be for the 2021B semester.  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
  • 8-20 and 23-50 GHz (Good weather)
    • Regular:  < 200 hours and lasting ≤ 1 year
    • Large: ≥ 200 hours or lasting >1 year
  • 20-23 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

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 for both open skies and sponsored time.    Prior commitments typically account for half of this time which leaves only 500 hours available for new requests 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.  Requests for GUPPI will not be considered.

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 3 February 2020 deadline is for the 2020B Semester observing period on the GBT:
1 August 2020 – 31 January 2021

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.

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.  There will not be a large proposal call for 2021A for the GBT.  The next large proposal deadline for the GBT after this call will be for the 2021B semester.  This new policy ensures equality for the reviews of all large proposals that can be scheduled across a full year.

Instrumentation News

The GBT receivers, backends, and observing modes that are available in Semester 2020B are listed in Tables 1 and 2 below.

ReceiverFrequency RangeNote
Prime Focus 1290 – 395 MHz
385 – 520 MHz
510 – 690 MHz
680 – 920 MHz
Prime Focus 2910 – 1230 MHz
L-band1.15 – 1.73 GHz
S-band1.73 – 2.60 GHz
C-band3.8 – 8.0 GHzlinear only, see below
X-band5 – 11.6 GHz
Ku-band12.9 – 15.4 GHz
K-band Focal Plane Array (KFPA)18 – 26.5 GHz7-pixel array
Ka-band26 – 39.5 GHz
Q-band38.2 – 49.8 GHz
W-band67 – 93.3 GHz
Argus75 – 115.3 GHz16-pixel array
MUSTANG-290 GHzshared-risk, private PI instrument
Table 1
BackendObserving ModeNote
VEGAScontinuum, spectral line, pulsar
MARK6 Disk RecorderVLBI
JPL Radar backendradarPrivate PI instrument, open for public use
Breakthrough ListenPrivate PI instrument, shared risk
Table 2

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: 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.

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 shared-risk observations during the 2020B 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) 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, 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 transition to reduced open skies 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:

The PFS radar backend (PI: Margot) is available only with prior agreement by the PI.
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.

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 VLBAHSA, and GMVA Proposal Call.


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 workshops will be held  January 22-24, 2020, October 13-15, 2020 and May 2020 (dates to be determined).

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 2020 workshop will be held in May 2020 (dates to be determined). 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 2020B and Semester 2021A.  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.

20B Proposal Call Results

A total of 82 proposals requesting NSF funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT)  for semester 20B.  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 20B semester that have been reviewed by the Green Bank Observatory Telescope Allocation Committee (TAC).

A description of the 20B proposals accepted can be found in our NSF Open Skies Science Program section below.

Total Proposals82
Statistics by Proposal Count
Requested Time7289 h
Available Time2465 h
Approved2053 h
Filler1701 h
Rejected3536 h
Statistics by Proposal Hours

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 18B 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.

20B Science Program

A total of 82 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 3, 2020 semester 20B 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 20B 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 20B can be found in the Proposal Call Results section above.

Allen, RonGBT20B-014A GBT Search for an Extended Disk of OH Emission in M3370Regular
Andersson, B-GGBT20B-015Small Scale Selective Photo-Dissociation of CO isotopes in IC63 and IC5925Regular
Andreon, StefanoGBT20B-020A intermediate mass cluster kept at the epoch of entropy growth13Regular
Appleton, PhilipGBT20A-268Measuring the cold gas in super spiral galaxies to z < 0.3 with ARGUS50.25Regular
Archibald, AnneGBT20B-332Continued Timing of a Millisecond Pulsar in a Stellar Triple System25Regular
Beasley, AnthonyGBT17B-131GBT Observations of 36 GHz Methonal Masers Towards the Galactic Center24Regular
Brodwin, MarkGBT20A-091MUSTANG-2 Observations of the Highest-Richness MaDCoWS Clusters at 0.8 < z < 1.663Regular
Brodwin, MarkGBT20B-212MUSTANG-2 Observations of the Highest-Richness MaDCoWS Clusters at 0.8 < z < 1.656.5Regular
Busch, MichaelGBT20B-044Turbulent Motions, Mass Content and Distribution of Dark H2 in the Outer Galaxy130Regular
Butterfield, NatalieGBT20B-273Investigating the Star Forming Potential of the Galactic Bar Dust Lanes27Regular
Butterfield, NatalieGBT20B-371Molecular Inventory of Molecules in the Fermi Bubble Clouds7Regular
Cameron, AndrewGBT20A-060Continued observations of an eccentric, relativistic binary pulsar.57Regular
Candelaria, TierraGBT20A-277Highly Excited NH3 Localized in the Galactic Center20Regular
Cepeda-Arroita, RokeGBT20B-336Spinning Dust in the Lambda Orionis Ring36Regular
Chawla, PragyaGBT20B-353Searching for Low Frequency Emission and Short Periodicities in Repeating FRBs30Triggered
Chen, Che-YuGBT20A-322Characterizing the Internal Velocity Fields of Star-forming Cores with GBT-Argus228.5Large
Clarke, SeamusGBT20A-139A young, cold and quiescent giant molecular filament – G214.5-1.812.5Regular
Darling, JeremyGBT20B-148Toward Direct Measurement of the Cosmological Acceleration20Regular
Das, SanskritiGBT20B-360A deep search for HI in the CGM of NGC891 and NGC456558Regular
Demorest, PaulGBT20B-307The North American Nanohertz Observatory for Gravitational Waves870Large
Fillingham, SeanGBT20B-261Characterizing HI Emission in BreakBRD galaxies24Regular
Fuente, AsuncinGBT20B-152Probing the dust and gas evolution in starless cores12Regular
Gajjar, VishalGBT20B-394High-frequency followup of the first periodically active FRB with the GBT15Regular
Grossan, BruceGBT20B-327Multi-Frequency, Simultaneous Observations of FRB121102 – A New Approach49.5Triggered
Gusinskaia, NinaGBT20B-347Searching for radio pulsars in neutron star low-mass X-ray binaries7Regular
Henshaw, JonathanGBT20A-055Testing Accretion-Driven Turbulence in Central Molecular Zone Clouds2.5Regular
Issaoun, SaraGMVA20B-269Sharpening the Source Model for Sgr A* with GMVA+ALMA10Regular
Karunakaran, AnanthanGBT20B-045The HI content of Field Ultra-Diffuse Galaxies in SMUDGes: Final Campaign159Regular
Kim, Jae-YoungGMVA20B-204First subparsec-scale imaging of the new TeV gamma-ray radio galaxy 3C 2648Regular
Kino, MotokiGMVA20B-066Ultra-deep imaging of the stratified jet base of Cygnus A15Regular
Kramer, MichaelGBT20B-214Timing and General Relativity in the Double Pulsar System101Regular
Kumar, PravirGBT20B-248Uncovering and studying the southern repeating fast radio burst population57Regular
Lockman, FelixGBT20B-200Tracing the Neutral Gas in the Nuclear Wind387.5Regular
Lu, RusenGMVA20B-220Jet Meets Black Hole in M87: Breaking New Ground with GMVA+ALMA28Regular
Maccarone, ThomasVLBA20B-121A trigonometric parallax for a globular cluster7.5Regular
MacDonald, NicholasGMVA20B-145Disorder vs. Order: Discerning the nature of the magnetic field in PKS 1510-0895Regular
Margot, Jean-LucGBT20A-021Interior structure of Europa and Ganymede4.5Regular
Margot, Jean-LucGBT20B-197Venus: Moment of Inertia and Length of Day3.75Regular
McGuire, BrettGBT19B-047Continuing An Extremely Deep GBT Survey of TMC-1396Large
Michilli, DanieleGBT20A-293Triggered follow-up of repeating Fast Radio Bursts discovered by CHIME/FRB40Triggered
Nair, PreethiGBT20B-328HI gas properties of post-merger remnant galaxies68Regular
Okabe, NobuhiroGBT20B-082Joint SZE, X-ray and Weak-lensing Analysis for Closest-pair Mergers36Regular
Pisano, D.J.GBT20B-321Project AMIGA: The Circumgalactic Medium of M31 — Mapping the inner halo173.5Regular
Plume, ReneGBT20B-027Complex Organics Vs. Warm Carbon Chains in High Mass Star Forming Regions17.25Regular
Ransom, ScottGBT20B-333Long Term Timing of 60 Recycled Pulsars in Bulge Globular Clusters40Regular
Rivilla, Victor M.GBT20B-111Confirming selective collisional-pumped excitation of ethanimine in G+0.6933Regular
Salas, PedroGBT20B-352Measuring the density and temperature of photodissociation regions6Regular
Schmiedeke, AnikaGBT20B-087MUSTANG-2 mapping of the dense core Barnard 511Regular
Scibelli, SamanthaGBT20B-326High Resolution C18O ARGUS Mapping toward Prestellar Cores in Taurus20Regular
Stairs, IngridGBT20B-213Understanding the Magnetic Field Configuration in a Moding, Oscillating Pulsar27Regular
Stark, DavidGBT20B-033HI-MaNGA: HI Followup for MaNGA Galaxies580Large
Svoboda, BrianGBT20B-295Dense gas in cold clumps: a pilot GBT/Argus Galactic Plane survey40Regular
Swiggum, JosephGBT20B-362Completion of the GBT All-Sky 350-MHz Pulsar Survey440Large
Williams, GwenllianGBT20B-007Interaction of two IRDC hubs: A complete evolutionary study of the SDC13 region1.75Regular
Zhou, ChenlinGBT20B-289Tracing the temperature structure of three Prestellar Core candidates16.5Regular

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