MIRI Simulation

Spec Sim

Simulation of MIRI-MRS - Purpose

• Generate FITS frames which are a good approximation to the frames which will be taken by the Medium Resolution Spectrometer (MRS) on orbit.
• Give the MIRI community a preview of the data products the MRS will produce (sensitivity - spectral/spatial resolution/coverage - data artefacts).
• Provide test frames for the Data Reduction Software.
• A tool for fine-tuning the calibration plan.
• A means of communicating the performance of and illustrating trades for MRS components (telescope, dichroics, detectors).

The Model (IDL)

• Input
  • The sky and telescope background
  • Model astronomical targets
  • (Written as 12 fully resolved FITS data cubes (α,δ,λ))
• Filtering/transformation of input
  • Image slicing
    • Sky to detector coordinate transformation/Diffractioneffects
  • Dichroics
    • Spectral passbands/Ghosts
  • Detector performance
    • Expected flat field response
    • Bad pixels
    • Image latency
• Output
  • 2 x 1k square FITS frames per data cube

Simulated Source

The pictures below show the difference of the source images sampled by the IFU in the two dither positions.

Simulated Channel 2B Spectrum - Position A

Simulated Channel 2B Spectrum - Position B

Difference Spectrum