WFIRST

WFIRST Simulations


Wide-Field Infrared Survey Telescope

WFIRST Coronagraph Instrument (CGI) Public Simulated Images


Summary

The WFIRST CGI instrument team at JPL has provided the following sets of simulated images in order to facilitate investigations of optimum image processing algorithms and expected scientific performance.

As the instrument, optics simulations and observing scenarios mature, we will keep this page updated with the latest sets of simulated images.




Observing Scenario (OS) 6

(2018-06-25)

These simulated CGI image time sequences (John Krist, JPL) are for direct imaging with the Hybrid Lyot Coronagraph (HLC) and the Shaped Pupil Coronagraph (SPC).

For HLC, speckle fields are produced in a 10% bandpass filter centered at 575 nm, with and without optical model uncertainty factors (MUFs).

For SPC, multiwavelength speckle fields are produced in a 18% bandpass centered at 770 nm, with and without optical MUFs.

The observing scenario is a combination of Reference Differential Imaging (RDI) and Angular Differential Imaging (ADI):

  • 2 hrs on reference star (eta UMa)
  • Four repeats of 2 hrs on target star (47 UMa) in two rolls
  • 13 repeats of the sequence above

Please see this PDF file for a more detailed description of the simulated data generation for the OS6 scenario.
In order to see the animations, view this pptx file in slideshow mode.


(Updated 2019-05-16)

Fixed offsets in some SPC source-offset images, see README for details.


Links to Images



HLC speckle field



Synthetic Optic Wavefront Error Maps, Synthetic Polarization Wavefront Error Maps, and Mask Design Files

(2019-10-17)

These files are used to model the performance of the WFIRST CGI. The optical WFE maps (John Krist, JPL) are a combination of mid-spatial-frequency and low-order errors representative of the WFIRST telescope and coronagraph optics as might be expected from manufacturing (polishing). The polarization aberration maps (John Krist, JPL) are wavelength-dependent combinations of low-order Zernike modes representative of what might be generated from the WFIRST telescope optics. The coronagraph mask files (A.J. Riggs and Dwight Moody, JPL) are for the two shaped pupil modes and one baselined hybrid Lyot coronagraph mode in the CGI. These files are meant to be used in the Phase B PROPER optical model maintained on Github at https://github.com/ajeldorado/proper-models/ in the wfirst_cgi subfolder. Refer to the "FALCO+PROPER" section at https://wfirst.ipac.caltech.edu/sims/Code.html for how to run closed-loop wavefront correction simulations of the WFIRST CGI.

Links to data:

The data can be found as a single zip file here.



Example of wavefront error map for primary mirror.



Coronagraph Performance Files

(2016-08-04)

These simulated CGI images (John Krist, JPL) are provided to evaluate the performance of the coronagraph. They represent optimal static dark hole fields (PSF and contrast) for the Shaped Pupil Coronagraph (SPC, over a 18% spectral bandpass centered at 800nm) and the Hybrid Lyot Coronagraph (HLC, over a 10% spectral bandpass centered at 550nm). These images correspond to the performance statistics and simulation results from Krist et al. and Traub et al. described at the WFIRST Coronagraph special section of JATIS 2016.

Links to Images



Example of PSF peak for SPC and HLP.





Observing Scenario (OS) 5, Angular Differential Imaging (ADI)

(2016-07-28)

These simulated CGI image time sequences (John Krist, JPL) are for direct imaging with the Hybrid Lyot Coronagraph (HLC), over a 15% spectral bandpass centered at 550 nm, and for the following observing scenario (please see additional details in the README files):

  • 25000 sec on 61 UMa to reach steady state.
    • no speckle fields generated for this stage
  • 600 sec slew to β UMa (V = 2.4, A1IV)
    • no speckle fields generated during slews or rolls
  • 30000 sec on the reference star β UMa at roll +13°, including 10000 sec settle
  • 600 sec slew to science target star 47 UMa (V = 5.0, G1V, has planets)
  • 50000 sec on 47 UMa at roll +13°, including 10000 sec settle
  • 100 sec to roll 26° around 47 UMa
  • 50000 sec on 47 UMa at roll -13°, including 10000 sec settle

Please see this (PDF) file for a more detailed description of the simulated data generation for the OS5 scenario.

SPOILER ALERT: this (PDF) file contains information about the planets injected into the simulated images. Do not look at this if your intent is to perform a blind retrieval exercise!


Links to Images



Speckle field time series.