The HEASARC welcomes your participation in a brief survey
to capture how users access and utilize HEASARC data, software, and services. The outcome(s) of this survey will be used to guide, prioritize, and plan our activities and development in the coming years. It contains 18 questions, generally takes just a few minutes to complete, and your answers will remain totally anonymous. We thank you in advance for your valuable feedback.
Swift Proposals & Tools
The Swift Technical Handbook contains information about the Swift mission, instruments, performance, and technical feasibility.
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 11pt or larger. Proposals that exceed our page limit, are deemed poorly readable or are missing any required sections will be penalized.
Previously Accepted Targets:
Previously Accepted Swift proposals (with Abstracts):
Schedule for Swift Cycle 15
Detailed information on how to submit Swift Cycle 15 proposals and what is new in Cycle 15 can be found on the Swift Cycle 15 web page.
Please also see the Swift GI Program FAQs for details on what types of observations are permitted in Cycle 15.
Schedule for Swift Cycle 14 (Active)
- ROSES 2017 NRA released: February 14, 2017
- ROSES 2017 Appendix D.5 "Swift Guest Investigator Cycle 14"
- Phase 1 proposals due: September 28, 2017, 4:30PM EDT
- Phase 1 proposal Review: early December 2017
- Phase 2 proposal due: February 2018
- Cycle 14 observations begin: April 1, 2018
- Cycle 14 observations end: March 31, 2019
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.
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.
- XRT data simulations The ASI Science Data Center in Italy have provided a web-based XRT Data Simulation tool. The tool creates science-like event FITS files from simulated or real sky fields.
- 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. To determine whether optical loading is likely to contaminate your dataset use the Optical Loading Calculator. If you have an extremely compelling science case that requires such an observation, we strongly suggest that you contact the Swift XRT team (firstname.lastname@example.org or email@example.com) to discuss the observation before submitting your proposal.
- 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.