PSLS in a nutshell

PSLS simulates solar-like oscillators representative for PLATO observations. It includes planetary transits, stochastically-excited oscillations, granulation and activity background components, as well as instrumental systematic error and random noises representative for PLATO. The program also manages the existence of the time shift between groups of camera. Planetary transits are included following Mandel & Agol (2002) equations and using the Python implementation by Ian Crossfield at UCLA.

Two different types of oscillation spectrum can be simulated depending of the type of star:

  •  Red-giant stars: oscillation spectra are based on the Universal Pattern (Mosser et al 2011) together with the mixed modes patterns derived from the asymptotic theory (see e.g. Mosser et al 2012)  ;
  •  Main-sequence and sub-giant stars: oscillation spectra based on a set of theoretical frequencies computed with the ADIPLS pulsation code.

Rotational mode splitting are implemented in a simplified manner.

Some illustrations are displayed here below.

Note the current limitations of the program: the parameters of the activity component still need to be specified by the user.  It is planned  in the near future to implement some prescriptions for the activity component as well as a spot modelling.


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.

(c) 2017 by Réza SAMADI, LESIA – Observatoire de Paris.

Main contributors: Alexis Deru (LESIA), Emmaunel Grolleau (LESIA), Daniel Reese (LESIA)


Power spectrum of a light-curve simulated for a red-giant star

Simulated light-curve with the presence of a planetary transit

 

 

 

 

 

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