24B Proposal Call
The Green Bank Observatory (GBO) invites scientists to
participate in the 2024B Semester
Call for Proposals for the Green Bank Telescope (GBT).
The submission deadline for Semester 2024B proposals was
Wednesday, 31 January 2024, at 17:00 EST (22:00 UTC).
The deadline is for the 24B semester observing period on the GBT:
1 August 2024 – 31 January 2025
Virtual Proposal Planning Office Hours [4] will be held January 24 and 25.
The GBO would like to highlight the following:
- Low frequency (< 8 GHz) projects are encouraged
- Up to 200 hours per source or field is reasonable.
- No Large proposals requesting high frequencies (> 60 GHz) will be accepted at 24B deadline.
- Joint proposals with JWST [5] (new), NICER [6], XMM-Newton [7], Chandra [8], HST [9], Swift [10], and Fermi [11]
- Expected hours available: ~2300-3100 hours.
- Increase in open skies time of ~600 hours in the 24B semester
- Shutdown May-September in 2024 and 2025 (no observing) for infrastructure work
- Other shutdowns for infrastructure work may occur as necessary
- No more than 100 hours available for ν ≥ 50 GHz
- Monitoring observations will not be guaranteed cadence through shutdowns.
- UWBR remains shared risk.
- UWBR available for one (maybe two) short, weeklong campaigns at irregular intervals
- S, Q and W-bands will not be available.
- Multi-semester proposals will be considered. Proposals requesting observations lasting longer than one year will be considered but must be submitted as a large proposal.
- Undersubscribed LSTs
- Below 8 GHz in the 0-13h LST range
- 8-18 GHz and 27.5-50 GHz at all LSTs
A detailed timeline for the 24B Proposal Call is available here [12] and summarized in the table below:
| Date | Action |
|---|---|
| 03 January 2024 | GBO/NRAO Call for Proposals |
| 31 January 2024 | GBO/NRAO Proposal Deadline @ 22:00 UTC |
| 29 February 2024 | Individual Science Reviews Completed |
| 20 March 2024 | Science Review Panel (SRP) Meetings Completed |
| 16-17 April 2024 | Telescope time allocation committee (TAC) meeting |
| 10 May 2024 | Disposition Letters Sent |
The GBO 2024B Call for Proposals is for observations with the GBT; the corresponding call for the VLBA/HSA/GMVA and VLA can be found at the NRAO Call for Proposals [13].
What’s New in 2024B?
- Large Proposals. The GBT will accept large proposals at the 24B deadline. However, no large proposals requesting high frequencies (> 60 GHz) will be accepted at this deadline.
- Joint Programs with JWST. Starting in 24B, joint proposals may be submitted requesting time on the James Webb Space Telescope (JWST). A maximum time of 50 hours can be allocated per year on the JWST.
- Updated Dissertation Plans. Students that have dissertation plans as part of their NRAO profile will be REQUIRED to update their plans following a strict thesis template. The template is available in either Word or LaTex formats (see Section 7.2 of the NRAO and GBO Users’ Policies).
As stated in the Users’ Policies – While not a guarantee, the Observatory allows reviewers to consider elevating the proposal in the rankings if it is associated with an acceptable Plan of Dissertation. This is given in consideration to the time constraints students typically operate under, as having to resubmit a proposal due to minor criticisms may not be possible within the scope of their studies. Therefore, it is advantageous for students to provide a thoughtful and thorough Plan of Dissertation if their PhD research is reliant on the proposal data. - NRAO and GBO Users’ Policies. The policies have been substantially updated ahead of the 24B Call for Proposals.
- The requirements and policies concerning Joint Proposals have been significantly revised in Sections 3.2.1 and 3.2.3
- The policies for VLA and VLBA Resident Shared Risk Observing (RSRO) and Shared Risk Observing (SRO) have been significantly revised in Section 5.3. The policy for scheduling General Observing (GO) observations has been updated in Section 5.3.
- The requirements for student Dissertation Plans have been significantly revised in Section 7.2 (see above).
- See the NRAO and GBO Users’ Policies [14]page.
Proposal Process and Opportunities
Joint GBO and NRAO Telescope Time Allocation Process
Proposals to the Green Bank Observatory (GBO [15]) and the National Radio Astronomy Observatory (NRAO [16]) for the scientific use of its telescopes are evaluated on the basis of scientific merit and technical feasibility using a panel-based proposal review system [17]. This joint process is run by the NRAO in accordance with its policy of non-discrimination and inclusion. [18]
The GBO 2024B Call for Proposals is for observations with the GBT; the corresponding call for the VLBA/HSA/GMVA and the VLA can be found at the NRAO Call for Proposals [13].
Low Frequency Science Opportunities
Low frequency (below 8 GHz) projects, especially those that may require significant amounts of observing time per source or field, are strongly encouraged. Observations up to 200 hours per source or field at low frequencies is not unreasonable for the less subscribed LST ranges. Please see the LST pressure plots in the Proposal Results for previous semesters located here [19].
Expected GBT time available in 24B
The GBT is expected to be shut down from May-September 2024 and May-September 2025. During this shutdown repairs to the GBT infrastructure will be performed. This includes azimuth wheel replacement, painting, and track, foundation and grout work.
Other shutdowns for infrastructure work may occur as necessary and with little warning.
It is expected that there will be about 2300-3100 hours of A and B ranked observing time that can be assigned to new projects. It is also expected that no more than 100 hours of excellent weather high frequency time can be assigned to new projects.
We cannot guarantee that monitoring projects can be scheduled due to the planned infrastructure work.
Receiver Availability
Ultra-wideband shared risk
The new Ultra-wideband Receiver (UWBR) will undergo engineering changes and commissioning in early 2024. Unfortunately, the UWBR will not be available for regular monitoring observations in the 24B semester. We still anticipate that the UWBR could become available for some observations in the near future. This would be for one (maybe two) short, weeklong campaigns occurring on irregular basis.
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.
For more information on the UWBR please visit here [20].
S, Q and W-bands not available
The S, Q, and W-band receivers will not be available in the 24B semester. The Q and W-band receivers are expected to be available for the 25A semester.
Receivers available only during campaigns
The Prime Focus 342 and 800 MHz feeds, and the UWB receivers will only be available for campaigns during the 24B semester. The 800 MHz feed will be available on a monthly basis.
Receiver available during entire semester
It is expected that the L, C, X, Ku, KFPA, Ka, Argus and Mustang2 receivers will be available during the entire 24B semester.
Continuing Opportunities
Joint Observing program
Access to the Joint Observing program will continue for the GBT, VLA, and VLBA for semester 24B. This includes joint observations with JWST, NICER, the XMM-Newton Project, the Chandra X-ray Observatory, the Hubble Space Telescope (HST), the Swift Gamma-Ray Burst Mission, and the Fermi Gamma-ray Space Telescope. For more details see the Joint Proposal page [21].
Director’s Discretionary Time Including Education and Public Outreach
Proposals for Director’s Discretionary Time (DDT) may be submitted at any time. They must be submitted through the PST [22]. DDT proposals are intended to address targets of opportunity [23], high-risk/high-return exploratory time [24], or other science opportunities deemed sufficiently urgent to justify prompt action.
DDT proposals may also be submitted for the purpose of education and public outreach—for example, to image an iconic source or to support an educational opportunity for students. Such proposals should clearly justify the requirements for the requested time allocation and observing mode on any given instrument, and should describe the anticipated impact of the observation.
While there is not an a priori limit to time that can be requested via DDT, it is expected that no more than 5% of the available science time on each telescope will be allocated for this purpose.
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. That the proposal is high risk/high reward should be designated both in the abstract and the science justification.
- Triggered Proposals: Observations for unknown sources that would be triggered by a celestial event (e.g., near Earth asteroid discovery, comet discovery, fast radio burst, etc.) can be submitted as a triggered proposal. Any accepted triggered proposal will have proprietary rights to observations over any Director’s Discretionary Time (DDT) proposal.
- Filler Programs: Some programs are not time critical or do not 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. The proposal should make clear in the abstract and early in the science justification that “filler” time is being requested. Filler time requests will be ineligible for scheduling priority A or B.
GBT Proposal Guide
GBT Proposal Preparation
All proposals should state why the GBT is necessary for the requested observations in both the abstract and science justification.
Virtual Proposal Planning Office Hours [4] will be held January 24, and 25.
Proposers are encouraged to look at past proposal call results, especially the LST pressure plots, which can be found in the TAC proposal result reports. This information can be found here [19].
All proposers, including pulsar proposers, should use the GBT Sensitivity Calculator [25]. The Sensitivity Calculator results can be cut and pasted into the Technical Justification section of the proposal. This will streamline the creation of your Technical Justification and will lessen the chances for error.
If you are planning on making maps with the GBT, you should use the GBT Mapping Calculator tool [26].
The GBT observing policies [27] 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 [28].
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 15.8-18.0 GHz, and 50.5-67.0 GHz).
Key science areas [29] include, but are not limited to:
- low column density HI (NHI ≈1017 cm-2 galactic and extragalactic)
- star formation
- fast radio bursts
- galaxy and cluster evolution
- pulsars (searches and timing)
- cosmology
- radio recombination lines
- astrochemistry
- solar system science
Details of all GBT observing modes are inThe Proposer’s Guide for the Green Bank Telescope [30]. Proposers should also consult the more general document The Performance of the GBT: A Guide for Planning Observations [31].
Large Proposals
The GBT only accepts large proposals once per year for the B semester proposal deadlines. Large GBT proposals are not accepted at the A semester proposal deadlines. This 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.
Regular and Large proposal size definitions for the GBO are as follows:
- 0-8 GHz (Any weather)
- Regular: < 400 hours and lasting ≤ 1 year
- Large: ≥ 400 hours or lasting >1 year
- 8-18 and 27.5-50 GHz (Good weather)
- Regular: < 200 hours and lasting ≤ 1 year
- Large: ≥ 200 hours or lasting >1 year
- 18-27.5 and > 50 GHz (Excellent weather)
- Regular: < 100 hours and lasting ≤ 1.5 year
- Large: ≥ 100 hours or lasting >1.5 year
- Fixed and Monitoring proposals
- Regular: < 200 hours and lasting ≤ 1 year
- Large: ≥ 200 hours or lasting >1 year
Proposers submitting Large Proposals should read the Large Proposal Policy [32] to ensure that they address all of the mandatory requirements.
Currently Large proposals comprise 50% of the available time for excellent weather projects. We do not anticipate accepting any Large proposals for excellent weather projects at the 24B proposal deadline.
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 420 hours available to be scheduled each semester. Due to mechanical issues encountered in the 22B and 23A semester, we expect the amount of high frequency carry over time to be larger than normal for the 24B semester. We anticipate that ≤ 100 hours of high frequency time will be available for new proposals in the 24B semester.
Starting with the 23B proposal, all A ranked excellent weather projects will be considered for scheduling for 3 semesters.
Instrumentation
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 | short campaigns with irregular intervals between | |
| Prime Focus 1 | 680 – 920 MHz | Monthly 2-3 week campaigns | |
| 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 | |
| UWB Receiver | 700 – 4200 MHz | short campaigns, irregular intervals | shared-risk in 24B |
| L-band | 1.15 – 1.73 GHz | entire semester | |
| S-band | 1.73 – 2.60 GHz | not available | |
| C-band | 3.8 – 8.0 GHz | entire semester | linear only, see below |
| X-band | 5 – 11.6 GHz | entire semester | |
| Ku-band | 12.9 – 15.4 GHz | entire semester | |
| K-band Focal Plane Array (KFPA) | 18 – 26.5 GHz | entire semester | 7-pixel array |
| Ka-band | 26 – 39.5 GHz | entire semester | |
| Q-band | 38.2 – 49.8 GHz | Not available | |
| W-band | 67 – 93.3 GHz | Not available | |
| Argus | 75 – 115.3 GHz | entire semester | 16-pixel array |
| MUSTANG-2 | 90 GHz | entire semester | shared-risk, private PI instrument; proposals must include instrument team |
| 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 |
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, interim site director, or the GBT schedulers before the proposal is submitted.
C-band Polarization: Proposals wishing to use the GBT C-band receiver should only use linear polarization outputs. The circular polarization of the receiver is currently not performing correctly and we will not accept any proposals to use the circular polarization output of this receiver.
VLBI including the HSA and GMVA:Proposers should clearly justify the need for the GBT in the text of the proposal. All Very Long Baseline Interferometry (VLBI) proposals requesting the GBT should include any needed setup and overhead time in the time request of their proposals.
Proposals requesting the GBT as part of High Sensitivity Array (HSA [33]), and Global 3mm VLBI Array (GMVA [33]) should be submitted through the Very Long Baseline Array’s call (available here [34]).
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 [28]) for proposals for more details.
MUSTANG2-: The GBO will accept proposals for shared risk observations using the MUSTANG-2 instrument at the proposal deadline. More information on MUSTANG-2 can be found here [35]. 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. All MUSTANG-2 proposals must have permission from the instrument development team – contact Emily Moravec [36], Simon Dicker [37] or Brian Mason [38].
Breakthrough Listen backend: The Breakthrough Listen project is making its backend available for shared-risk observations during the 2024B 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 [39].
Continuum Observations: Proposers wishing to perform continuum observation should consult with a GBO scientist. Some information on continuum observations can be found here [4].
Observing and Scheduling Constraints
The GBT is scheduled by the Dynamic Scheduling System (DSS) [40]. The DSS system is fully described in the GBT Proposer’s Guide [41] and the GBT Observer’s Guide [42].
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.
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.
RFI
The most recent RFI monitoring scans for the GBT can be found here [43]. These scans provide information on the frequencies that may encounter RFI. Note that a Green Bank computing account is required to be able to view this information. If you do not have a computing account, please contact the helpdesk [44] to request the desired RFI plots.
Schools and Workshops
Observer Training Workshops: The Green Bank Telescope (GBT) Remote Observer Training Workshop will provide the essential skills and knowledge needed to use the GBT and maximize its scientific output. It is intended for experienced astronomers who need to learn the specifics of observing with the GBT. After completing the workshop, an attendee will be certified to use the GBT as a remote observer. The workshop will focus on hands-on training in the observing techniques most relevant to participants (e.g. high frequency map, continuum, pulsar, etc.).
These workshops will be held several times a year and will complement traditional on-site training. The next workshop will be held Feb 06-08, 2024. More information can be found here [45].
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 June 24-29, 2024.
Joint Proposals
Joint Proposals Between the GBT, VLBA and VLA
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.
Joint Proposals with External Facilities
Here we list opportunities for joint proposals with several external (non-AUI) facilities. Agreements for Joint Observations with external facilities were made at different times across the boundaries when the NRAO was split into multiple observatories (NRAO, GBO, and LBO) in 2017, and when the LBO was reintegrated back into the NRAO in 2019. Therefore, the agreements below will sometimes mention various combinations of the NRAO, GBO, and LBO. Regardless, access to the Joint Observing program will continue for the VLA, VLBA, and GBT for semester 24B.
Joint Observations with JWST
By agreement between the GBO and NASA, detailed in a Memorandum of Understanding [46], the GBO can award up to 50 hours of JWST observing time per year. In return, JWST can award up to 5% of the GBT open skies observing time. See the Joint Observations with JWST [5] page for details.
Joint Observations with NICER
By agreement between the GBO and NASA, detailed in a Memorandum of Understanding [47], the GBO can award up to 250 ksec of NICER observing time per year. In return, NICER can award up to 5% of the GBT open skies observing time. See the Joint Observations with NICER [6] page for details.
Joint Observations with XMM-Newton
By agreement with the Green Bank Observatory, detailed in a Memorandum of Understanding [48], 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 [7] 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 Chandra 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 [8] 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 [9] 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 [49]. 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 [10] 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 [11] page for details.
GBO and NRAO User’s Policy
The new users’ policy manual is available here [50].
Tips for Proposers
Scientific Justification
The NRAO proposal evaluation and time allocation process is panel based. That is, members of the scientific community are responsible for reviewing proposals based on their scientific merit through the Science Review Panels [17]. As a means of broadening the scientific perspective of its reviewers, and of increasing the participation of the wider astronomy and astrophysics community in the science program of NRAO facilities, SRP membership is deliberately selected to include some colleagues that are not necessarily experts in radio observational techniques. This being the case, we encourage proposers to consider the following when preparing their proposals:
- Avoid the use of radio astronomy jargon.
- Do not assume the reader is familiar with a particular observing technique – explain it briefly.
- Do not assume the reader is familiar with an earlier rationale for a developing line of research – provide adequate historical context and connect the dots as necessary.
- Describe previous observations and publications relevant to the proposed observations.
- If a particular point source or brightness temperature sensitivity is required, justify it.
Source Lists
The Observatory requires proposers to specify their source lists in full. This enables the Observatory to identify potential conflicts between observing programs and to better understand scheduling pressure on the instruments it operates. It may be the case that the final target list has not been selected at the time a proposal is submitted. In such cases, all potential targets and fields should be listed. The only exceptions to this requirement are for Triggered proposals to observe targets that are unknown a priori. Proposal source lists are not made public by the Observatory.
Dissertation Plans
The Plan of Dissertation is important in the proposal review process and should be well written; it is not a placeholder and should not be a replica of the proposal. The plan must be compliant with specific requirements, which includes following a Plan of Dissertation Research template. See Section 7.2 [51] of the NRAO Users’ Policy guide for details.
24B Proposal Call Results
A total of 99 proposals requesting NSF funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT [52]) for semester 24B. Proposals are reviewed on a competitive basis with a panel review system (see Proposal Review System [53]). 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 24B semester that have been reviewed by the Green Bank Observatory Telescope Allocation Committee (TAC).
A description of the 24B proposals accepted can be found in our NSF Open Skies Science Program [3] section below.
| Total Proposals | 99 |
|---|---|
| Approved | 48 |
| Filler | 15 |
| Rejected | 36 |
| Hold | 0 |
| Withdrawn | 0 |
| Oversubscription | 2.06 |
| Requested Time | 10772.21 h |
| Available Time | 1701.5 h |
| Approved | 4579.25 h |
| Filler | 1185.75 h |
| Rejected | 5006.71 h |
| Pressure | 6.33 |
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 black 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 24B semester.
GBT Observation Preparation
Please use the GBT Dynamic Scheduling System (DSS [54]) to enable observing sessions, select observers for your project, and enter your blackout dates. The DSS Home Page [55] has additional information about the DSS. See GBT Observing [56] 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.
24B Science Program
A total of 99 proposals requesting NSF funded “open skies” time were submitted to the Green Bank Observatory’s Robert C. Byrd Green Bank Telescope (GBT [52]) for the January 31, 2024 semester 24B 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 24B 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, HST, JWST, FERMI, NICER, SWIFT, and XMM-Newton.
For each approved program, the Proposal Finder Tool [57] will have access to its author, title, abstract and total approved hours.
A description of the Time Allocation Committee report for 24B can be found in the Proposal Call Results [2] section above.
| PI | ID | Title | Hours | Type |
|---|---|---|---|---|
| Alexander, Kate | GBT23A-273 | Monitoring the Exceptional Jetted Tidal Disruption Event AT2022cmc | 17.5 | Regular |
| Anderson, Loren | GBT24B-329 | The Warm Ionized Medium of the Galactic Bar | 44 | Regular |
| Asali, Yasmeen | GBT24B-384 | Expanding the Sample of HI Measurements in Satellites of Milky Way Analogs | 60 | Regular |
| Balser, Dana | GBT24B-101 | Ionization State of the Warm Ionized Medium in the Inner Galaxy | 27 | Regular |
| Barcos-Munoz, Loreto | GMVA24B-356 | Arp 220: AGN or not AGN?, that is the question… | 16 | Regular |
| Bhakta, Deven | GBT24B-430 | The Search for New Cluster Pulsars | 25 | Regular |
| Bhakta, Deven | GBT24B-450 | Pulsar Searches on Steep Spectrum Radio Sources from Fermi Unassociated Sources | 5.25 | Regular |
| Blackmon, Victoria | GBT24B-374 | Continued observations of an eccentric, relativistic binary pulsar | 36.75 | 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 | GBT24B-320 | A Follow-up GBT Survey for OH in the Milky Way’s Nuclear Wind | 121 | Regular |
| Butterfield, Natalie | GBT23B-202 | BARFLYS: Investigating the Star Forming Potential of the Galactic Bar Dust Lanes | 227.5 | Large |
| Cannon, John | GBT24B-157 | Newly Discovered Local Volume Dwarf Galaxies | 43 | Regular |
| Cao, Jinhuang | GBT24B-291 | Following up two new FRBs discovered in FAST-CRAFTS drift-scan survey | 6 | Regular |
| Carleton, Timothy | GBT24B-009 | HI and UV Observations of an Quiescent Isolated Dwarf Galaxy Observed with JWST | 3.75 | Regular |
| Chen, Che-Yu | GBT20A-322 | Characterizing the Internal Velocity Fields of Star-forming Cores with GBT-Argus | 228.5 | Large |
| Cromartie, Thankful | GBT24B-427 | The North American Nanohertz Observatory for Gravitational Waves | 1723.5 | Large |
| Dicker, Simon | GBT24A-291 | Quantifying biases in selection functions of Sunyaev-Zel’dovich Effect surveys. | 16 | Regular |
| Di Gennaro, Gabriella | GBT23B-120 | SZ observations of MaDCoWS clusters with diffuse radio emission at z=0.8-1.34 | 14 | Regular |
| Di Gennaro, Gabriella | GBT24B-194 | SZ observations of MaDCoWS clusters with diffuse radio emission at z=0.8-1.34 | 45 | Regular |
| Di Teodoro, Enrico | GBT23A-131 | Measuring 12CO(1-0) emission in the Milky Way’s Nuclear Wind | 6.5 | Regular |
| Dong, Yuxin | GBT24B-390 | Exploring a New Pathway to Discover Fast Radio Bursts in Dwarf Galaxies | 66 | Regular |
| Feng, Yi | GBT24B-114 | Monitoring the active repeater FRB 20230607A | 10 | Regular |
| Fiore, William | GBT24B-393 | Search for Radio Pulsations from the Candidate Black Widow ZTF J1406+1222 | 2.75 | Regular |
| Gallardo Cava, Ivan | GBT24B-306 | Search for OH maseres in circumbinary-disk-containing post-AGB nebulae | 47.5 | Regular |
| Gao, Shijie | GBT24B-248 | Search for radio pulsations from exotic young pulsars in globular clusters | 30 | Regular |
| Ginsburg, Adam | GBT23A-268 | From ACES to TENS: The Central Molecular Zone with MUSTANG | 6 | 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 |
| Gusinskaia, Nina | GBT24B-435 | Continued Timing of a Millisecond Pulsar in a Stellar Triple System | 31 | Regular |
| Hunter, Laura | GBT24B-319 | Distances to Low-Surface Brightness Satellite Galaxies | 81 | Regular |
| Janssen, Michael | GMVA24B-054 | Precision astrometry of Sgr A* with 3mm VLBI observations of SiO stellar masers | 8 | Regular |
| Jones, Michael | GBT24B-251 | Origins of a new class of stellar system in the Virgo cluster | 42 | Regular |
| Kam, Minchul | GMVA24B-376 | Pinpointing the jet launching mechanism in 3C 84 with GMVA+ALMA+GLT | 20 | Regular |
| Kanekar, Nissim | GBT24B-340 | The Atomic Gas Content of Green Pea Galaxies | 92.5 | Regular |
| Karunakaran, Ananthan | GBT24B-330 | Understanding the Baryon Cycle of Ultra-Diffuse Galaxies | 63 | Regular |
| Kramer, Michael | GBT24B-407 | Timing and General Relativity in the Double Pulsar System | 44 | Regular |
| Kumar, Pravir | GBT24B-066 | Probing the dynamic environment of FRB20180301A | 30 | Regular |
| Ladu, Elisabetta | GBT24B-050 | Monitoring of the water megamaser in IC485: weighing the BH of a LINER galaxy II | 12 | Regular |
| Lin, Lingrui | GBT24B-167 | Resolving the turbulence-deficient molecular clouds in the outer Galaxy | 21 | Regular |
| Lorimer, Duncan | GBT24B-298 | GREENBURST Single Pulse Census of Nearby Galaxies | 32.5 | Regular |
| Lu, Rusen | GMVA24B-165 | Probing the dynamic jet-disk connection in M87 | 19 | Regular |
| Lynch, Ryan | GBT24B-373 | Continuing a Pilot GBT Pulsar Survey of the Galactic Plane | 216 | Regular |
| Margot, Jean-Luc | GBT24B-428 | Interior structure of Europa and Ganymede | 7.5 | Regular |
| Maureira, Maria Jose | GBT22B-180 | CO freeze-out across a filamentary dense cloud forming a quadruple system | 25.5 | Regular |
| McGuire, Brett | GBT23A-047 | Closing the Loop: PAHs Toward Cyg OB2-12 | 6 | Regular |
| McGuire, Brett | GBT24A-232 | The Dark Carbon Falls – An ARKHAM Pilot Project | 192 | Regular |
| McKee, James | GBT24A-255 | Broadband observations of giant pulses from PSR J0218+4232 | 8 | Regular |
| Minter, Anthony | GBT24A-237 | A Search for Dust-free Clouds in the Galactic Disk | 205.75 | Regular |
| Moravec, Emily | GBT23B-005 | Characterizing the Highest Redshift Shock in a Merging Galaxy Cluster | 35 | Regular |
| Morgan, Lawrence | GBT24B-253 | Methanol Maser COMBS: Completing the Original Multi-Beam Survey | 330 | Regular |
| O’Neil, Karen | GBT24B-415 | HI Properties of Low Surface Brightness Galaxies | 90 | Regular |
| O’Neil, Karen | GBT24B-417 | Exploring the Environment around J0613+52 | 160 | Regular |
| Ocker, Stella | GBT24B-290 | An Ultra-Wideband Study of Repeating Fast Radio Bursts | 27.5 | Triggered |
| Orlowski-Scherer, John | GBT24B-184 | Investigating Anomalous Flux from the Asteroids (511) Davida and (423) Diotima | 15 | Regular |
| Parent, Emilie | GBT24B-027 | Pinpointing the onset of radio pulsations in a new transitional pulsar candidate | 6 | Triggered |
| Park, Jongho | GMVA24B-153 | Peering into M87’s black hole in multiple colors | 28 | Regular |
| Patil, Swarali Shivraj | GBT24B-423 | Search and Follow-up of Scintillation Arcs in NANOGrav Binary Pulsars | 6 | Regular |
| Pearlman, Aaron | GBT24B-310 | Exploring the Origins of Nearby Repeating FRBs via Multiwavelength Observations | 20 | Triggered |
| Perez, Karen | GBT24A-351 | Establishing the Energetics of the Luminous Gamma-Ray Redback: PSR J0212+5321 | 22 | Regular |
| Pilia, Maura | GBT24B-225 | Searching for the elusive optical counterpart of repeating fast radio bursts | 31.5 | Triggered |
| Pineda, Jaime | GBT23A-199 | Ions vs Neutrals in a Dense Core – copy | 18 | Regular |
| Polisensky, Emil | GBT24B-365 | Searching for Pulsations from VLITE Neutron Star Candidates | 24 | Regular |
| Possenti, Andrea | GBT24A-023 | The magnetar-FRB link: simultaneous Radio/X-Ray monitoring of active magnetars | 21 | Triggered |
| Ransom, Scott | GBT24B-410 | Long Term Timing of 76 Recycled Pulsars in Bulge Globular Clusters | 210 | Large |
| Redaelli, Elena | GBT24B-271 | Nitrogen chemistry in prestellar gas | 9 | Regular |
| Robishaw, Timothy | GBT24A-397 | Confirmation of Magnetic Field Detection in CRRL Emission from DR 21 | 41 | Regular |
| Romero, Charles | GBT23A-086 | SZ Constraints of Shocks in CIZA J2242.8+5301 | 40 | Regular |
| Roth, Nathan | GBT24B-396 | First Maps of Cometary NH3: VLA + GBT Spectra of Exceptional Comet C/2023 A3 | 6.5 | Regular |
| Rugel, Michael | GBT24B-314 | GBT HI follow-up observations for THOR-GC | 65 | Regular |
| Salas, Pedro | GBT24B-288 | Complete the Drift S Scan Survey for Gas in Galaxies, the Milky Way, PSRs and FRBs | 0 | Large |
| Sarazin, Craig | GBT23A-028 | Bridges of Intergalactic Gas Connecting ACT Cluster Pairs | 35 | Regular |
| Schmiedeke, Anika | GBT23A-360 | Exploring the kinematics in a filamentary infrared dark cloud | 40 | Regular |
| Schmiedeke, Anika | GBT22B-191 | Feeding a super-critical filament in a subsonic core | 17.5 | Regular |
| Scibelli, Samantha | GBT24B-077 | A Quest for More GLUCOSE: the GBT L1544 Unbiased Complex Organics SurvEy | 556 | Large |
| Sengar, Rahul | GBT24B-378 | Confirming New PALFA Survey Candidates from Einstein@Home | 9.5 | Regular |
| Shirley, Yancy | GBT23A-161 | PROBING DUST OPACITY VARIATIONS: MUSTANG-2 IMAGING OF THE PRESTELLAR CORE L183 | 12 | Regular |
| Shroyer, Jordan | GBT23B-262 | Polarized Ku-Band Observations near G107.2+5.20 for CMB Foregrounds Study | 55 | Regular |
| Shull, Michael | GBT24B-075 | 21cm HI Column Densities Toward High Galactic Latitude AGN | 3.25 | Regular |
| 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 |
| Squillace, Reynier | GBT23A-263 | A Survey of 15-Nitrogen Fractionation in Prestellar Cores | 36 | Regular |
| Stark, David | GBT24B-263 | HI-MaNGA: HI Followup for MaNGA Galaxies | 379.5 | Large |
| Stephens, Ian | GBT23A-288 | Mapping Ammonia in Bones: Understanding our Magnetized Spiral Potential | 132 | Regular |
| Stephens, Ian | GBT24B-106 | Mapping Ammonia in Bones: Understanding our Magnetized Spiral Potential | 13 | Regular |
| Stroyer, Jordan | GBT24A-262 | Polarized Ku-Band Observations near G107.2+5.20 for CMB Foreground Study | 55 | Regular |
| Tang, Ningyu | GBT24B-304 | OH 18 cm Survey Towards OB Stars with Detected OH Absorption in the UV Waveband | 13.25 | Regular |
| Tremblay, Chenoa | GBT24B-234 | Magnetic Properties in Star Formation through observations of CH and OH | 10 | Regular |
| Tu, Tianyu | GBT23B-090 | Probing the cosmic-ray-ionized dense gas associated with supernova remnant HB9 | 12 | Regular |
| Turner, Jacob | GBT24B-039 | Cyclic Spectroscopy of Three Pulsars with Considerable Pulse Broadening | 45 | Regular |
| Turner, Jacob | GBT24B-040 | Multi-Hour Scintillation Studies by the PSC: GBT Follow-up to GBO 20m Campaign | 50 | Regular |
| Urquhart, James | GBT23A-350 | Search of Hypercompact HII Regions Towards Methanol Masers | 56.25 | Regular |
| van Marrewijk, Joshiwa | GBT24A-249 | Resolving SZ-selected clusters in the epoch of most rapid cluster growth | 42 | Regular |
| van Marrewijk, Joshiwa | GBT24B-002 | Resolving SZ-selected clusters in the epoch of most rapid cluster growth | 42 | Regular |
| Wilde, Aurora | GBT24B-092 | Mapping NH2D Emission in Starless Cores | 23 | Regular |
| Yang, Zonglin | GBT24B-003 | Looking for the companion of PSR J1922+1512g | 2.5 | Regular |