Swift Proposals & Tools

Science Justification Template: We encourage you to use the updated LaTeX template or the updated MS Word template for the scientific part of the proposal (i.e., the written text component of the proposal). The style files needed to compile the LaTeX file can be found here. If you use your own template, make sure that your proposal is readily legible, and that you include the same sections as in the template. It is strongly recommended to use a font size of 12pt or larger. Proposals that exceed our page limit, are deemed poorly readable or are missing any required sections will be penalized.

Schedule for Swift Cycle 21

ROSES 2024 NRA released: February 14, 2024
Neil Gehrels Swift Observatory Guest Investigator Cycle 21
Phase 1 proposals due: September 26, 2024 4:30 PM EDT
Phase 1 proposals review: early December 2024
Phase 2 proposals due: February 2025
Cycle 21 observations begin: April 1, 2025
Cycle 21 observations end: March 31, 2026

Detailed information on how to submit Swift Cycle 21 proposals and what is new in Cycle 21 can be found on the Swift Cycle 21 web page.

Please also see the Swift GI Program FAQs for details on what types of observations are permitted in Cycle 21.

Schedule for Swift Cycle 20 (Active)

ROSES 2023 NRA released: February 14, 2023
Neil Gehrels Swift Observatory Guest Investigator Cycle 20
Phase 1 proposals due: September 21, 2023 4:30 PM EDT
Phase 1 proposals review: early December 2023
Phase 2 proposals due: February 2024
Cycle 20 observations begin: April 1, 2024
Cycle 20 observations end: March 31, 2025

Swift Target of Opportunity Requests

Swift accepts requests for Target of Opportunity (TOO) observations on transient astrophysical sources (GRB and non-GRB targets). For more information, and to submit a TOO request visit the Swift TOO page.

Planning Tools

Want to get an idea of how the BAT, XRT and UVOT instruments will perform on your favorite source? Check out our Swift simulation tools!

Viewing To determine when, or if, a given object can be viewed by Swift, use the Viewing tool.
XSPEC Response matrix files and ancillary response files for BAT, XRT, and UVOT are available for download here. Example scripts for the generation of simulated spectral data using these calibration files and the X-ray spectral fitting package XSPEC are available here.
WebSpec To simulate spectra on-line, use WebSpec, the WWW interface to XSPEC. A variety of spectra models are available from the page. Use any of these to predict your Swift BAT, XRT or UVOT spectrum.
WebPIMMS If count rates are what you are after, visit WebPIMMS, a mission count rate simulator powered by PIMMS --- the Portable, Interactive Multi-Mission Simulator. Choose a flux, or count rate from any of a wide variety of previous and current missions, then convert it into Swift BAT, XRT and UVOT count rates.
Build XRT products: An online XRT product generator is provided at https://www.swift.ac.uk/user_objects/. This tool allows users to build X-ray light-curves, spectra and images of any point source object observed by Swift. All products are publication-quality, and account for all analysis issues such as pile-up and the presence of bad columns. Documentation and links to published papers about the system are available online at https://www.swift.ac.uk/user_objects/docs.php. These tools can also be used via the swifttools python module. In addition, for users who prefer to use the software directly to create the desired products, data analysis threads are provided at https://www.swift.ac.uk/analysis/xrt/, detailing the basic steps required for extracting data products. Among other topics, these webpages highlight how to account for pile-up and the best way to deal with background subtraction in WT mode. Information about known calibration and science analysis issues are listed on the XRT Digest Page.
XRT optical loading Bright optical sources can leak through the thin XRT optical blocking filter, causing "optical loading" that can severely complicate or compromise analysis of the X-ray data. There are several possible mitigations to this problem, but no good solutions. In general, objects with V < 8 mag should not be observed in PC mode. Objects with V < 5 mag should not be observed in any mode, as the data will be poorly calibrated and may be useless. The Optical Loading section includes a calculator to estimate how much a bright optical source may affect the X-ray spectrum. Swift data analysis queries can be sent to swifthelp@leicester.ac.uk.
The Swift Pyhton API Tools: The above XRT tools can also be used via the swifttools python module: https://www.swift.ac.uk/API/.
UVOT signal-to-noise calculator The UVOT instrument team at the Mullard Space Science Laboratory have developed a web-based tool for calculating S/N, background levels, and sensitivity limits.
UVOT Bright Star Checker Every PI needs to use the UVOT Bright Star Checker to see if there are bright sources in the UVOT field of view that might prohibit the use of UVOT or impact the scientific objectives of your proposed observation.
UVOT Filter Modes UVOT filter settings are specified by an observing mode which groups the requested observations into filter groups. The UVOT filter mode table will help you prepare your observations.
Roll Angle To determine the allowed range of roll angles for a given target use the Roll Angle Calculator.
BAT maps If it's the BAT Field of View you're interested in, check out the BAT partial coding maps made available by the BAT team.

National Aeronautics and Space Administration

Goddard Space Flight Center

Swift Proposals & Tools

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Schedule for Swift Cycle 21

Schedule for Swift Cycle 20 (Active)

Swift Target of Opportunity Requests

Planning Tools

Previously Accepted Targets:

Previously Accepted Swift proposals (with Abstracts):