Summary
The Roman Space Telescope 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) 11 Polarization Datasets for the Wide-field-of-view Shaped Pupil Coronagraph
- Observing Scenario (OS) 11 time series simulations for the Shaped Pupil Coronagraph (SPC) Modes
- Observing Scenario (OS) 11 time series simulations for the Hybrid Lyot Coronagraph Band 1
- Observing Scenario 9 Post-Processing report
- Observing Scenario (OS) 9
Observing Scenario (OS) 11 Polarization Datasets for the Wide-field-of-view Shaped Pupil Coronagraph
(2022-05-27)
Summary: To facilitate studies that rely on polarization, three datasets have been generated to complement John Krist’s Observing Scenario (OS) 11 time series simulations for the wide-field-of-view shaped pupil coronagraph in band 4: an x-polarized time series dataset, a y-polarized time series dataset, and a corresponding unpolarized time series dataset. The three polarization datasets were generated using the public version of CGISim, with some modifications to extract the electric fields and incorporate jitter, and they incorporate errors using the information provided in spc_wfov_os11_inputs.fits. The polarization datasets do not include LOWFS corrections (except for Z4), detector noise, or model uncertainty factors.
The presentation gives further details of the WFOV polarization datasets. A supplementary presentation describes how these datasets were generated.
Download Compiled_OS11_unpolarized, Compiled_OS11_xpolarized, Compiled_OS11_ypolarized.
Observing Scenario (OS) 11 time series simulations for the Shaped Pupil Coronagraph (SPC) modes
(2022-03-25)
SPC-Spec Band 3
Summary: These SPC-Spec Band 3 (16.7% band at 730 nm) simulations are for Observing Scenario 11 (John Krist, JPL). OS11 encompasses observations of a bright reference star (Zeta Pup) and a science target star (47 UMa), allowing for reference differential imaging. The science star is observed at each of 4 rolls alternating between +13 and -13 to allow for angular differential imaging. Time-dependent thermal and pointing jitter variations are included. OS11 and the provided files are described in the Powerpoint presentation. Each timestep is represented by a datacube of 31 monochromatic images spanning the bandpass and at 0.1 lam_c/D resolution (lam_c = 730 nm). They are intended to represent the field at the plane of the spectrographic slit.
The presentation gives further details of the files accessible via these scripts curl script and wget script.
Updated Mar. 20, 2024: (version 3) XCENTER and YCENTER header keyword values corrected (increased by 1.0 pixel each). Added Jul. 11, 2023: Revised (version 2) time series posted, incorporating the measured characteristics of the CGI flight deformable mirrors. These new files supersede the prior files.
SPC-WFOV Band 4
Summary: These SPC-WFOV (wide field of view) Band 4 (11.4% band at 825 nm) simulations are for Observing Scenario 11 (John Krist, JPL). OS11 encompasses observations of a bright reference star (Zeta Pup) and a science target star (47 UMa), allowing for reference differential imaging. The science star is observed at each of 4 rolls alternating between +13 and -13 to allow for angular differential imaging. Time-dependent thermal and pointing jitter variations are included. OS11 and the provided files are described in the Powerpoint presentation. The SPC-WFOV is very tolerant of low-order aberration variations and so the speckles are very stable over time.
The presentation gives further details of the SPC-WFOV simulations and files.
Updated Mar. 20, 2024: (version 3) XCENTER and YCENTER header keyword values corrected (increased by 1.0 pixel each). Added Jul. 11, 2023: Revised (version 2) time series posted, incorporating the measured characteristics of the CGI flight deformable mirrors. These new files supersede the prior files.
Observing Scenario (OS) 11 time series simulations for the Hybrid Lyot Coronagraph Band 1
(2022-02-09)
Summary: These HLC Band 1 (10% band at 575 nm) simulations are for Observing Scenario 11 (John Krist, JPL). OS11 encompasses observations of a bright reference star (Zeta Pup) and a science target star (47 UMa), allowing for reference differential imaging. The science star is observed at each of 4 rolls alternating between +13deg and -13deg to allow for angular differential imaging. Time-dependent thermal and pointing jitter variations are included. OS11 and the provided files are described in the Powerpoint presentation. Note that OS11 is expected to be the last time series simulation prior to launch.
The Powerpoint presentation gives details on the generation and format of the OS11 results. Archive of HLC files and images.
Updated Mar. 20, 2024: (version 3) XCENTER and YCENTER header keyword values corrected (increased by 1.0 pixel each). Added Jan. 9, 2023: Included with the archive of files is “hlc_sky_transmission_oversampled.fits”, a 2D “sky transmission” of the Nancy Grace Roman Space Telescope Coronagraph Instrument when its Hybrid Lyot Coronagraph (HLC) is in the beam (John Krist, JPL). Each pixel in this map gives the relative intensity of the peak of an off-axis PSF centered on that pixel, normalized by the highest value in the field of view, so values span 0-100%. This map was made using the flight HLC design, and is intended be used in conjunction with Observing Scenario 11 (OS11) simulated images.
Results from HLC OS11 simulations for each star for the rolls with (left to right) Target and planets, Reference star, Difference, actual planets. The model Uncertainty Factors (MUFs) are included in these simulations.
Observing Scenario 9 Post-Processing report
(2021-02-03)
(Updated 2022-03-08)
Summary: The documents below report on findings from applying post-processing techniques to the Observation Scenario 9 (OS9) simulated data using the Hybrid Lyot Coronagraph (HLC) and Shaped Pupil Coronagraph (SPC) for the Roman Space Telescope Coronagraph Instrument. We measure the factor of contrast gain above classical PSF subtraction for the noiseless OS9 data and noiseless (no MUF) and noisy (MUF) data. This is on-going work and thus the information contained in this document is subject to future updates.
HLC OS9 Post-Processing Report and SPC OS9 Post-processing Report give details on the generation and format of the OS9 results.
Performing classical angular differential imaging (cADI) PSF subtraction on OS9 Hybrid Lyot Coronagraph data
Observing Scenario (OS) 9 time series simulations for the Shaped Pupil Coronagraph Band
(2020-05-14)
These SPC-Spec Band 3 (15% band at 730 nm) simulations are for Observing Scenario 9 (John Krist, JPL). OS9 consists of multiple cycles of reference star (Zeta Pup) and target star (47 UMa) observations, including two rolls on 47 UMa for ADI. This version only includes simulations including CGI aberration sensitivity modeling uncertainty factors (MUFs).
The Powerpoint presentation gives details on the generation and format of the OS9 results.
Use the curl script or wget script to obtain the SPC files and images.
The simulations demonstrate aspects of the SPC such as Band 3 is significantly impacted in terms of static dark hole contrast by the incoherent component (above)
Observing Scenario (OS) 9 time series simulations for the Hybrid Lyot Coronagraph Band 1
(2020-05-06)
(Updated 2020-05-19: The data are now provided at CCD resolution without noise.)
These HLC Band 1 (10% band at 575 nm) simulations are for Observing Scenario 9 (John Krist, JPL). OS9 consists of multiple cycles of reference star (Zeta Pup) and target star (47 UMa) observations, including two rolls on 47 UMa for ADI. Two versions are included, with and without CGI aberration sensitivity modeling uncertainty factors (MUFs).
By request, also included are separate archives containing the complex-valued electric fields instead of intensity images for those wishing to study wavefront sensing and control applications.
The Powerpoint presentation gives details on the generation and format of the OS9 results.
HLC archives of files and images: os9_hlc.zip, os9_hlc_efields.zip, os9_hlc_muf.zip, os9_hlc_muf_efields.zip. Please see the README files within each HLC archive.
HLC time series with and without MUFs (slide 16 from the presentation linked above)