PLATO Stellar Light-curve Simulator (SLS): Simulate stochastically-excited oscillations and associated stellar and instrumental background noises
PSLS: the PLATO Solar-like Light-curve Simulator
PSLS simulates solar-like oscillators representative for PLATO observations. The simulator includes planetary transits, stochastically-excited oscillations, granulation and activity background components, as well as instrumental systematic errors and random noises representative for PLATO. The program also manages the existence of a time shift between groups of cameras. Planetary transits are included following Mandel & Agol (2002) equations (see http://adsabs.harvard.edu/abs/2002ApJ…580L.171M) and using the Python implementation by Ian Crossfield (http://www.astro.ucla.edu/~ianc/) at UCLA.
For more details see http://psls.lesia.obspm.fr and also Samadi et al (2019, A&A, in-press).
The package provides the code and two files storing the parameters describing the PLATO systematic errors: - PLATO_systematics_BOL.npy: End Of Life (EOL) systematic errors - PLATO_systematics_EOL.npy: Begining Of Life (BOL) systematic errors
The package also provides two working examples: - a main sequence star (0012069449.yaml) with its associated theoretical frequencies (0012069449.gsm) generated by ADIPLS pulsation code - a red giant star (0009882316.yaml), which does not require as input theoretical frequencies.
A couple of grids of models can be downloaded from the PSLS website (http://psls.lesia.obspm.fr).
If you use PSLS in your research work, please make a citation to Samadi et al (2019, A&A, in-press).
Changes history: - 0.9 (20/05/19): the NSR table was incorrectly interpolated. V mangitudes ranging between 12 and 13 were affacted. - 0.85 (23/03/19): minor changes to be make the code fully compatible with python3 - 0.8 (23/02/19): systematic errors are now modelled and simulated in the time domain. The jumps induced by the quasi-regular mask updates are now included. - 0.7 (10/12/18): inclusion of PLATO systematic errors and random noise as a function of the star V magnitude - 0.6: minor problems fixed (missing file, link problem) - 0.5: can perform simulation for a given input set of theoretical frequencies (i.e. from a given .gsm file) ; new parameters included in the configuration file .yaml ; various minor improvements - 0.4: minor changes - 0.3: first working version
Copyright (c) October 2017, Reza Samadi, LESIA - Observatoire de Paris
This is a free software: you can redistribute it and/or modify it under the terms of the GNU General Public License as published by the Free Software Foundation, either version 3 of the License, or (at your option) any later version.
This software is distributed in the hope that it will be useful, but WITHOUT ANY WARRANTY; without even the implied warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the GNU General Public License for more details.
You should have received a copy of the GNU General Public License along with this code. If not, see <http://www.gnu.org/licenses/>.
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