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 11pt or larger. Proposals that exceed
our page limit, are deemed poorly readable or are missing any required
sections will be penalized.
- 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
2016 NRA released: February 19, 2016.
2016 Appendix D.5 "Swift Guest Investigator Cycle 13"
- Notices of Intent: no NOIs are due for Swift Cycle 13
- Phase 1 proposals due: September 23, 2016, 4:30PM EDT
- Phase 1 proposal Review: early December 2016
- Phase 2 proposal due: February 2017
- Cycle 13 observations begin: April 1, 2017
- Cycle 13 observations end: March 31, 2018
Detailed information on how to submit
Swift Cycle 13 proposals and what is new in Cycle 13 can be found on
the Swift Cycle 13 web page.
Please also see the Swift GI Program FAQs for details on what
types of observations are permitted in Cycle 13.
Schedule for Swift Cycle 12 (Active)
2015 NRA released: February 13, 2015.
2015 Appendix D.5 "Swift Guest Investigator Cycle 12"
- Notices of Intent: no NOIs are due for Swift Cycle 12
- Phase 1 proposals due: September
25, 2015, 4:30PM EDT
- Phase 1 proposal Review: December 2015
- Phase 2 proposal due: February 2016
- Cycle 12 observations begin: April 1, 2016
- Cycle 12 observations end: March 31, 2017
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
will perform on your favorite source? Check out our Swift simulation
- Viewing To determine when, or if, a given
can be viewed by Swift, use the Viewing tool.
- XSPEC Response matrix files and ancillary
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
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 (email@example.com or
firstname.lastname@example.org) to discuss the observation before submitting your
- 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
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
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.