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PRIMA AOS Simulator Jeroen de Jong, 30 sep 2004

PRIMA AOS Simulator Jeroen de Jong, 30 sep 2004. Requirements Design Implementation Issues. Goals (in timeline order). Simulate ideal interferometer Produce correctly formatted simulated raw data for testing the DRL infrastructure

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PRIMA AOS Simulator Jeroen de Jong, 30 sep 2004

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  1. PRIMA AOS SimulatorJeroen de Jong, 30 sep 2004 • Requirements • Design • Implementation Issues

  2. Goals (in timeline order) • Simulate ideal interferometer • Produce correctly formatted simulated raw datafor testing the DRL infrastructure • Add perturbations to the ideal case by turningon specific error source simulation modules • Produce data suitable for testing the data reduction and trend analysis algorithms (Scientific tests!)

  3. Scientific Requirements • The simulator computes the optical pathlength difference between science and reference source for a number of potentional observing conditions. • The physics of the PRIMA instrument is properly taken into account. • Perturbations are added sequentially along the optical path between the target and the detector. • These perturbations have dependencies and share a general database.

  4. Technical Requirements • The simulator needs proper APIs for inserting modules written in different languages. • Design should allow for significant increase in complexity. • Computing time should be minimized as much as possible by appropriate physical approximations. • Visualization is done by external tools. • The output must conform to the PRIMA FITS standards.

  5. Modules • Setup • Target position and ideal OPD computation • Applying several (wavelength dependend) perturbations (Astronomical, Atmospheric, VLTI, PRIMA) • Computation of FSU outputs • Writing the files of each OB in the PRIMA FITS format

  6. Configuration files • Hierarchical structure • They describe everything for computing a complete set of simulated data: • Targets and calibrators • Observation Schedule • Physical information of targets • Baseline configuration • Perturbations to include

  7. Data Model • Array of timestamps of the observations • Array of station coordinates (u,v,w format) • Stokes parameters as function of time, beam and wavelength • Apparant coordinates of target and reference for all four beams (two per star) • OPD for all for beams

  8. Perturbations • The ideal OPDs will be computed from the apparant positions and station coordinates • Each module gets access to all data in the Data Model via an API • The modules perturb the optical path in the layer to which they are applicable.

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