------------------------------------------------------------------------ Source Code for NASA's Kepler Mission (jasonfrowe@gmail.com) ------------------------------------------------------------------------ !!!NEW!!! - There are now Python wrappers for some subroutines, ask for details. Requires: X11,PGPlot,CFITSIO libraries (-lX11 -lpgplot -lcfitsio) **If you use OS/X I recommend 'homebrew' to install pgplot and cfitsio and XQuartz for X11. **If you are a Linux fan, either use your favourite package installer (e.g., yum) or install pgplot/cfitsio from source. ------------------------------------------------------------------------ Quick INSTALL: ./configure make This should make binaries in the 'bin' directory. **I'm new to using autoconf, so if you run into trouble - let me know. ------------------------------------------------------------------------ If you find these codes useful please reference: Rowe et al. 2014 ApJ, 784, 45 Rowe et al. 2015 ApJs, 217, 16 --or-- Jason Rowe (2016). Kepler: Kepler Transit Model Codebase Release. [Data set]. Zenodo. http://doi.org/10.5281/zenodo.60297 Full documentation is a work in progress, but for now, have a look at the 'example' directory to get a start. I can also recommend: Uniform Modeling of KOIs: MCMC Data Release Notes http://adsabs.harvard.edu/abs/2015arXiv150400707R As a good resource to understand the file formats. ------------------------------------------------------------------------ TRANSITFIT5 - used to model planetary transits based on Kepler photometry -handles multi-planets, RVs and TTVs and deMCMC framework for posteriors. transitfit5: Uses Levenberg-Marquardt to fit a transit-model to photometry transitmcmc5: Uses deMCMC style MCMC to produce Markov-Chains for a transit-model transitsn5: estimates S/N of transit based on transit model transittiming5: calculates center of transit-times based on folded transit-model prdump5: data-dump routine for XML style output mcmcsetup: estimates Gibbs sampler factors to initialize MCMC routines transitdepth5: estimate transit-depth from a transit-model transitcut5: cuts out all observes beyond +/- 1 transit duration datadump5: removes all but one planet from a lightcurve (for multi-planet systems) transitdur5: estimates transit-duration from a transit-model transitremove5: removes transit-model from a light-curve transitchisq5: estimates chi-square from lightcurve and transit-model transitsigclip5: uses 3-sigma clipping to remove outliers based on transit-model fit plottimeseries: makes a plot of the time-series and marks location of transits transitplot5: plots the folded lightcurve and transit model mcmchistnew: produces histogram of a Markov-Chain and estimates median and posteriors mcmchist5: produces histogram of a Markov-Chain and estimates median and posteriors and uses stellar-parameter MCs to get absolute planet posteriors (e.g. Mp, Rp) mcmchist5bf: same as mcmchist5 but use best-fit for center of posterior TRANSITFIND - used to find transits or inverted transits in photometry. transitfind2: Uses an optimized BLS to search for transits/lensing in lightcurves DATATEST - routines to read FITS files retrieved from MAST and detrending detrend5: detrends lightcurves but preserves transit using a transit-model kfitsread: reads Kepler data FITS files from MAST sigclip: simple sigma-clip routine freqremove: Given a Fourier-decomposition solution, removes from lightcurve PERIOD - routines to calculate discrete Fourier transforms and Fourier decomposition keplerper: calculates a discrete Fourier transforms of photometric data. Can be unevenly sampled. Automatically calculates a Fourier decomposition that can be used by 'freqremove' ttper: same as keplerper but works with 'tt' files that come from a transting timing analysis outputted by 'transittiming5' freqmod: uses Fourier decomposition to fit for phase-changes of the frequency solution. This behaviour will be seen in a binary system with one or more components pulsating. The motion of the pulsator around the center of mass produces a timing delay in the observed pulsations. RHOSTAR - routines to calculate stellar parameters and posteriors rhostar: given some combination of Teff, log(g), [Fe/H] and rhostar estimate M*, R*, L and Age using the Yale-Yonsei Isochrones and output Markov-Chains. rhoboot2: displays histograms of Markov-Chain output from rhostar and calculate posterior distibutions of stellar parameters rhorand: simulate output of rhostar.