Package: pyorbit-package
A code for exoplanet orbital parameters and stellar activity.PyORBITversion 10 by Luca Malavolta July 2023Documentation updateI have extensively updated the documentation and  several examples are now available in a new dedicated repository, check them out:PyORBIT10 DocumentationPyORBITexamples repositoryFor nostalgic people,PyORBIT8 and 9 are available as branches of the main repository:legacy_version8andlegacy_version9respectively.Updates on version 10Improved speedAfter several failed attempts, I finally managed to apply the advices from theemcee parallelization pageto the rather complex structure of PyORBIT. The speed up is noticeable for large datasets (e.g., photometry)Rossiter McLaughlinRossiter McLaughlin effect can now be precisely modelled using the CCF simulation approach employed inCovino et al. 2013.
When the rotation period is known - together with the stellar radius - the stellar inclination can be derived avoiding the bias reported byMasuda & Winn 2020Multidimensional Gaussian ProcessThe model has been introduced a few years back, but now it can finally take advante of imrpoved parallelizationtinyGP for better performancesWorking on bothclassicandmultidimensionalGaussian Process, although the former is showing some JAX problems when producing the output results.**No back-compatibility**
Version 10 is not compatible with the results obtained with version 9.
If you have been using the development version of V10, you may run into incompatibility issues as well.**Messed-up repository**
I must have done something wrong when upgrading to version 10, if you already downloaded the repository before the upgrrade then I advise to to delete the repo and clone it again.Updates on version 9Added celerite2 SHO termImproved output:spaces,bounds, andpriorsexplicitely written out at runtimeMinor changes:dataset_variablesandcommon_variableschanged todataset_parametersandcommon_parametersNew models addedAll instances namedvariablesrenamed toparametersfor internal
consistency. Backward compatibility ensured by new method inmodel_container_abstractPyORBITwill use the correct parametrization when a prior is assigned to a parameter and nested sampling is used (NS do not allow to assign priors to derived parameters).Many new models are now availableMultidimensional Gaussian Process (also known as GP Framework,Rajpaul et al. 2015,Barragán et al. 2022).New kernels for Gaussian Process regression: Quasi-Periodic with Cosine(Perger et al. 2021), Quasi-Periodic with first derivative.CHEOPS detrending (similar to FactorModel as inpycheops).Phase curve and secondary eclipse modelling withbatman(Kreidberg 2015)orspiderman(Louden et al. 2016).Rossiter-McLaughlin through analytical formulation byOhta et al. 2005.Celerite/Celerite2standardmodels, now better organized.Fit of individual time of transits (with automatic definition of boundaries) for TTV analysis.experimenting withtinygpMore options for parameters space exploration:Linear,Log_Natural,Log_Base2,Log_Base10.Some variables have been renamed, to improve clarity of results:DefinitionPyORBIT 8.xPyORBIT 9.xMean Longitudefmean_longScaled planetary radiusRR_RsScaled semi-major axisaa_RsPlanetary mass in Earth massesMM_MeStellar densityrhodensityAlso,batman_ld_quadraticandpytransit_ld_quadratichave been merged intold_quadratic.Note: the Mean Longitude is defined assuming the longitude of the ascending node $\Omega$ equal to zero, thus corresponding to the angle defined in section 4.3 of(Ford 2006)and simply calledphaseinMalavolta et al. (2016)Overall reorganization of the codeWarningLoss of backward-compatibilityYou cannot analyzes results obtain with previous versions (< 9) of PyORBIT. No worries, the old version is still available in thelegacybranch, you can download it from the Github page or switch to it through the terminal:gitcheckoutlegacyTo switch back to the current version, just execute:gitcheckoutmainWorking on itRossiter-McLaughlin throughstarry(Luger et al. 2019)Multi-component GP for light curves (Rotation + Granulation, Rotation + Granulation + Oscillations), followingBarros et al. 2020.SamplersBayesian evidence estimation can now be performed with:dynestyby Josh Speagledynesty documentation,code repositoryUltraNestby Johannes BuchnerUltraNest documentation,code repositoryMultinest and Polychord support is still there, but not supported anymoreJust substitute "emcee" with "dynesty" or "ultranest" to when running the code.WarningMCMC and Nested Sampling handle prior in a radically different way, as such it s not possible to directly translate some priors from one sampler to anotherDocumentationSome incomplete documentation is availablehere. For any doubt, feel free to contact me at luca.malavolta_at_unipd.it, I'll be happy to work out together any problem that may arise during installation or usage of this software.PyORBIThandles several kinds of datasets, such as radial velocity (RV), activity indexes, and photometry, to simultaneously characterize the orbital parameters of exoplanets and the noise induced by the activity of the host star. RV computation is performed using either non-interacting Kepler orbits or n-body integration. Stellar activity can be modeled either with sinusoids at the rotational period and its harmonics or gaussian process. Offsets and systematics in measurements from several instruments can be modeled as well. Thanks to the modular approach, new methods for stellar activity modeling or parameter estimation can be easily incorporated into the code.ModelsAny of these models can be applied to a dataset. The user can choose which models should be used for each dataset.Gaussian Processesfor RV or photometry (shared or independent hyperparameter)Transits, eclipses, phase curvesPolynomial trendswith user-defined orderCorrelationwith activity indexes (or any other dataset)Sinusoids(independent or shared amplitudes and periods)Harmonicsto test old results in the literaturePriorsThese priors can be applied to any of the parameters (it's up to the user to choice the appropriate ones):Uniformdefault prior for all the parametersGaussianJeffreysModified JeffreysTruncated RayleighWhiteNoisePriorBetaDistributionJeffreysandModified Jeffreyspriors are actuallyTruncated JeffreysandTruncated Modified Jeffreys, with truncation defined by the boundaries of the parameter space.Parameter explorationThe user can choice betweenLinearandLogarithmic. Note that in the second case the parameter space is transformed into base-2 logarithm.Most of the information can be found inMalavolta et al. (2016)andMalavolta et al. (2018).Papers using PyORBITGAPS XXXVII. A precise density measurement of the young ultra-short period planet TOI-1807 bNardiello et al. (2022)Investigating the architecture and internal structure of the TOI-561 system planets with CHEOPS, HARPS-N, and TESSLacedelli et al. (2022)Independent validation of the temperate Super-Earth HD79211 b using HARPS-NDiTommaso et al. (2022)Multi-mask least-squares deconvolution: extracting RVs using tailored masksLienhard et al. (2022)Kepler-102: Masses and Compositions for a Super-Earth and Sub-Neptune Orbiting an Active StarBrinkman et al. (2022)TIC 257060897b: An inflated, low-density, hot-Jupiter transiting a rapidly evolving subgiant starMontalto et al. (2022)A PSF-based Approach to TESS High quality data Of Stellar clusters (PATHOS) - IV. Candidate exoplanets around stars in open clusters: frequency and age-planetary radius distributionNardiello et al. (2021)An unusually low density ultra-short period super-Earth and three mini-Neptunes around the old star TOI-561Lacedelli et al. (2021)K2-111: an old system with two planets in near-resonanceMortier et al. (2020)GAPS XXIX. No detection of reflected light from 51 Peg b using optical high-resolution spectroscopyScandariato et al. (2021)GAPS XXVIII. A pair of hot-Neptunes orbiting the young star TOI-942Carleo et al. (2021)And many more I had no time to include here...