22B Semester

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.

ReceiverFrequency RangeExpected AvailabilityNote
Prime Focus 1290 – 395 MHz
680 – 920 MHz
short campaigns with irregular intervals between
Prime Focus 1385 – 520 MHz
510 – 690 MHz
high rank proposal demand only
Prime Focus 2910 – 1230 MHzhigh rank proposal demand only
L-band1.15 – 1.73 GHzentire semester
S-band1.73 – 2.60 GHzshort campaigns every 2 months
C-band3.8 – 8.0 GHzmost of semester (except when S-band is available)linear only, see below
X-band5 – 11.6 GHzentire semester
Ku-band12.9 – 15.4 GHzcampaigns
K-band Focal Plane Array (KFPA)18 – 26.5 GHzentire semester7-pixel array
Ka-band26 – 39.5 GHzcampaigns
Q-band38.2 – 49.8 GHzcampaigns
W-band67 – 93.3 GHzshort campaigns
Argus75 – 115.3 GHzentire semester16-pixel array
MUSTANG-290 GHzentire semestershared-risk, private PI instrument
Table 1
BackendObserving ModeNote
VEGAScontinuum, spectral line, pulsar
CCBcontinuumKa-receiver only
MARK6 Disk RecorderVLBI
JPL Radar backendradarPrivate PI instrument, open for public use
Breakthrough ListenPrivate PI instrument, shared risk
Table 2

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 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.

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 Proposals70
Statistics by Proposal Count
Requested Time3334.25 h
Available Time1828.75 h
Approved694.75 h
Filler376.75 h
Rejected2134.75 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 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.

Archibald, AnneGBT22A-358Continued Timing of a Millisecond Pulsar in a Stellar Triple System50Regular
Bastian, TimGBT22A-360Probing the Inner Heliosphere with Pulsars: a Pilot Study10Regular
Bhakta, DevenGBT22B-270Searching for Globular Cluster Pulsars10Regular
Bilous, AnyaGBT22B-266Zooming in on Pulsar Microstructure to understand Fast Radio Bursts18Regular
Bolatto, AlbertoGBT21B-024GBT EDGE: A Representative Survey of the z=0 Universe with Full IFU Spectroscopy300Large
Bublitz, JesseGBT22B-250Refining the Molecular Gas Enigma: Mapping NGC 6781 at 3mm16.5Regular
Busch, MichaelGBT22A-434SC:Mapping molecular clouds in OH from diffuse to high-mass star forming regions300Large
Caleb, ManishaVLBA22B-074Probing the local environment of FRB 20190714A6.5Regular
Calore, FrancescaGBT22B-112Follow-up of bulge MSP candidates detected by both Chandra and VLA24.5Regular
Cameron, AndrewGBT22A-118Continued observations of an eccentric, relativistic binary pulsar.57Regular
Dai, ShiGBT22B-030Monitoring the active repeater FRB 20190520B24Regular
Dong, AdamGBT22B-213GBT Follow-up of a Novel Repeating Galactic Transient Detected with CHIME/FRB32Regular
Emig, KimberlyGBT22B-170Recombination Lines from Diffuse Ionized Gas in the M82 Starburst8.75Regular
Fonseca, EmmanuelGBT22B-215Followup Timing of Low-declination GBNCC Pulsars10Regular
Frayer, DavidGBT22B-162GBT HI Observations of the GOALS LIRG 3C842Regular
Freire, PauloGBT22B-143Following two potentially super-massive pulsars in NGC 6624 and NGC 185113Regular
Gallimore, JackVLBA22B-148OH Masers in the Water Megamaser Disk of NGC 106812Regular
Goldsmith, PaulGBT22B-011A Novel Technique for Electron Density Determination18Regular
Gorai, PrasantaGBT22A-398Exploring Carbon Chain Chemistry of Massive Protostars22Regular
Gupta, HarshalGBT21B-316Molecular Exploration of the Diffuse Interstellar mediUM (MEDIUM)285.75Large
Huang, JaneGBT22B-085Mapping the Delivery of Material to a Planet-forming Disk – copy2Regular
Issaoun, SaraGMVA22B-249Resolving Polarization in Sgr A* with GMVA+ALMA10Regular
Jones, MichaelGBT22B-064Cold gas reservoirs of satellites in nearby Milky Way-like systems96.5Regular
Kooi, JasonGBT22A-404Probing Fluctuations in the Solar Wind with Pulsars: a Pilot Study17Regular
Kramer, MichaelGBT22B-231Timing and General Relativity in the Double Pulsar System101Regular
Lockman, FelixGBT22B-204The Ophiuchus Superbubble — Connecting the Disk to the Halo115.5Regular
Lowe, IanGBT22B-068A Multi-Scale, Multi-Wavelength Study of Dust in Molecular Cloud Filaments II21.5Regular
Luo, JingGBT22B-269PSR J2108+45 with a massive companion and dense circumstellar environment36.5Regular
Maan, YogeshGBT22B-104Transient radio emission from magnetars and connection with FRBs23.75Triggered
Margot, Jenan-LucGBT22B-209A search for technosignatures around newly discovered exoplanets
Mason, BrianGBT22B-242Measuring 3mm Source Contamination in the ACT Galaxy Cluster Sample18.75Regular
Maureira, Maria JoseGBT22B-180CO freeze-out across a filamentary dense cloud forming a quadruple system25.5Regular
McKean, JohnVLBA21B-289Resolving the nature of quasar flux-ratio anomalies in gravitational lenses60Regular
Naidu, ShantanuGBT22B-226Bistatic Goldstone-GBT Radar Imaging of Binary Near-Earth Asteroid Didymos25Regular
O’Neil, KarenGBT22B-065Hunting for Massive Low Surface Brightness Galaxies128.75Regular
Park, JonghoGMVA22B-100A Multicolor View of the Black Hole Environment in M8728Regular
Ransom, ScottGBT22B-256Long Term Timing of 65 Recycled Pulsars in Bulge Globular Clusters75Regular
Redaelli, ElenaGBT22B-052A crucial test for the mass of prestellar cores in a high-mass clump2Regular
Ribaudo, JosephGBT22A-430The Baryonic Tully-Fisher Relation for Galaxies with Supernova Distances132Regular
Roberts, HayleyGBT22B-060Understanding the role of dense gas in the most extreme OH megamasers34.75Regular
Roth, NathanGBT22B-176Measuring NH3 and OH in a Target of Opportunity Comet with the GBT7.5Triggered
Salas, PedroGBT22A-269Probing the C+/C interface in the Orion Bar16.5Regular
Salas, PedroGBT22A-437SC: GBT Diffuse Ionized Gas Survey at Low frequencies – GDIGS-Low826Large
Salome, QuentinGBT22B-049A survey of atomic gas in NLSy1 galaxies with X-ray Ultra Fast Outflows31.25Regular
Sanchez, MonicaGBT22B-228Observations of Marginal Arecibo HI 21cm Detections in the Zone of Avoidance4.5Regular
Schmiedeke, AnikaGBT22B-191Feeding a super-critical filament in a subsonic core17.5Regular
Scibelli, SamanthaGBT22A-435SC: Q- Band Chemical Complexity Survey of Prestellar Core L1544647Large
Singal, JackGBT19A-083How Bright is the Radio Sky? A 310 MHz Absolute Map30Regular
Song, YiqingGBT22B-248Mapping HCN and HCO+ in Local Luminous Infrared Mergers19.5Regular
Spekkens, KristineGBT22B-139Atomic Gas in the Host Galaxies of Gravitational Wave Events – LVK O440Triggered
Spezzano, SilviaGBT22B-040Exploring the chemistry of Sulfur towards the young starless core L1521E18Regular
Sridharan, T.K.GBT22A-366Path to Precision Astrochemistry with Magnetars II – mm-wave Observations33Regular
Stark, DavidGBT22A-325Understanding diverse HI depletion times in MaNGA star forming galaxies79.25Regular
Stark, DavidGBT22A-436SC: Robust Gas Measurements for BreakBRD Galaxies206.5Large
Traianou, EfthaliaGMVA21B-164Moving and stationary shocks interaction after a gamma-ray flare in TXS2013+37027Regular
Valdivia Mena, Maria TeresaGBT22B-163Mind the gap: connecting the scales between filaments and protostars18Regular
Wen, DiG22A001A magnified view of an ionised scattering medium in a z= 1.145 late- type galaxy36Regular
Wolszczan, AlexanderGBT22B-200A search for planets around white dwarfs18Regular
Yang, ChentaoGBT22B-020Confirming the nature of a 380GHz H2O maser disk in a lensed quasar at z=3.9114Regular

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