Swift Proposals & Tools
- The Swift Technical Handbook contains information about the Swift mission, instruments, performance, and technical feasibility.
Previously Accepted Targets:
Previously Accepted Swift proposals (with Abstracts):
Schedule for Swift Cycle 11
Detailed information on how to submit Swift Cycle 11 proposals and what is new in Cycle 11 can be found on the Swift Cycle 11 web page.
Please also see the Swift GI Program FAQs for details on what types of observations are permitted in Cycle 11.
2014 NRA released: February 18, 2013.
2014 Appendix D.5 "Swift Guest Investigator Cycle 11"
- Notices of Intent: no NOIs are due for Swift Cycle
- Phase 1 proposals due:
September 25, 2014, 4:30PM EDT
- Phase 1 proposal Review: early December 2014
- Phase 2 proposal due: early January 2015
- Cycle 11 observations begin: April 1, 2015
- Cycle 11 observations end: March 31, 2016
Schedule for Swift Cycle 10 (Active)
Swift Target of Opportunity Requests
The Swift MOC considers requests for Target of Opportunity
(TOO) observations on timely non-GRB targets of astrophysical interest.
For more information, and to submit a TOO request visit the Swift MOC's 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
- 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
- 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 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. 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
- UVOT Filter Modes UVOT filter settings are specified by an observing mode which groups the requested observations into filter groups. The UVOTfilter mode table will help you prepare your observations.
- 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.
- Viewing To determine when, or if, a given object can be viewed by Swift, use the Viewing tool.