The PLATO Solar-like Light-curve Simulator (PSLS) is Python tool that aims at  simulating solar-like oscillators representative of PLATO targets. It includes planetary transits, stochastically-excited oscillations, granulation and activity background components, as well as instrumental systematic errors and random noises representative for PLATO.

For more details see PSLS in a nutshell.

If you use this simulator in your research, please cite Samadi et al (2019, A&A, 624, A117). Thanks !

New version 1.5 (01/07/22): IMPORTANT bug correction: since version 1.0 a wrong value for the (square) visibility of the l=1 modes was used (0.2 instead of the correct value of 1.5), this bug led to a large underestimation of the amplitude of the l=1 modes.

New version 1.4 (30/08/21): some improvements and bug corrections. For more details see Change history

New version 1.3 (18/12/20): New tables for systematic errors are provided. They are now based on simulations made with the Plato Image Simulator (PIS) for 24 cameras. The input files are now stored in appropriated sub-directories. Bug correction: LimbDarkeningCoefficients is now taken into account. For more details see PSLS_v1.3_release_notes.

New version 1.2 (25/05/20): New tables for systematic errors are included. Random noise can vary with mask shapes and with mask updates, mask updates are flagged, and the amplitude of the star drift can be controlled by the parameter DriftLevel.  Sytermatic errors representative for the imagette-based lightcurves (PSF fitting method, P1 sample) can now be considered (the previous code versions only consider the systematic error expected only with the aperture-based lightcurves i.e. the on-board lightcurves, P5 sample).  For more details see the release notes.

Previous versions: see the change history  HERE.

 Caution: this simulator is not an official product of the Plato Mission Consortium (PMC), it  is distributed under the terms of the GNU General Public License  in the hope that it will be useful, but WITHOUT ANY WARRANTY.

Power spectrum of a simulated solar-like pulsating dwarf star as it would be observed during 2 years by PLATO.

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