Welcome to the GSFC Exoplanet Modeling and Analysis Center (EMAC)
EMAC serves as a catalog, repository and integration platform for modeling and analysis resources focused on the study of exoplanet characteristics and environments. EMAC is a key project of the GSFC Sellers Exoplanet Environments Collaboration (SEEC).
If you've used EMAC in any part of your research, please cite our RNAAS paper either in your methods section or in the "Software used" portion of any manuscripts; see the FAQ for more information.
More Information on EMAC for first-time visitors...If you make use of tools linked or hosted on EMAC: please use the following statement in your publication acknowledgements: “This research made use of the NASA Exoplanet Modeling and Analysis Center (EMAC), which is funded by the NASA Planetary Science Division's Internal Scientist Funding Model.”
Stay up to date with EMAC!- Subscribe to our monthly RSS messages on new updates and tools.
- Check out the Bluesky account @exoplanetmodels.bsky.social (not an official NASA account), where new tools and features are highlighted.
- Email us with general feedback at and tell us what you'd change or improve.
- Click the
icon in a resource box to provide suggestions for an individual tool or tools.
- EMAC is intended as a clearinghouse for the whole research community interested in exoplanets, where any software or model developer can submit their tool/model or their model output as a contribution for others to use.
- EMAC provides a searchable and sortable database for available source code and data output files - both resources hosted locally by EMAC as well as existing external tools and repositories hosted elsewhere.
- The EMAC team also helps develop new web interfaces for tools that can be run “on-demand” or model grids that can be interpolated for more individualized results.
- If you would like to submit a new tool/model to EMAC, please visit our Submit a Resource page.
- For help with tutorials for select resources/tools use the “Demo” buttons below and subscribe to our YouTube channel.
- Watch this video for a walk-through of the whole EMAC site, including how to submit a new tool and how to access information for each resource.
EMAC co-leads are Joe P. Renaud and Eric Lopez; more information on EMAC staffing and organization can be found on Our Team page.
EMAC has launched a new community-supported curator program, and we need your help! Check out our curator page to learn how exoplanet experts like yourself can support EMAC's mission, and help us spread the word about this new initiative!
Eureka!: An End-to-End Pipeline for JWST Time-Series Observations
Bell, Taylor J. et al.
Eureka! is a data reduction and analysis pipeline for exoplanet time-series observations, with a particular focus on James Webb Space Telescope (JWST) data. The goal of Eureka! is to provide an end-to-end pipeline that starts with raw, uncalibrated FITS files and ultimately yields precise exoplanet transmission and/or emission spectra. The pipeline has a modular structure with six stages, each with intermediate figures and outputs that allow users to compare Eureka!’s performance using different parameter settings or to compare Eureka! with an independent pipeline.
eclipsoid: Open-source JAX-based Python package
Dholakia, Shashank; Dholakia, Shishir; Pope, Benjamin J. S.
Eclipsoid provides a general framework allowing rotational deformation to be modeled in transits, occultations, phase curves, transmission spectra and more of bodies in orbit around each other, such as an exoplanet orbiting a host star.
SSOF: StellarSpectraObservationFitting, Data-Driven Modeling of Telluric Features and Stellar Variability
Gilbertson, C. et al.
StellarSpectraObservationFitting.jl is a Julia package for measuring Doppler shifts and creating data-driven models (with fast, physically-motivated Gaussian Process regularization) for the time-variable spectral features for both the telluric transmission and stellar spectrum, while accounting for the wavelength-dependent instrumental line-spread function.
VLT-sphere: Automatic VLT/SPHERE data reduction and analysis
Vigan, Arthur
The high-contrast imager SPHERE at the Very Large Telescope combines extreme adaptive optics and coronagraphy to directly image exoplanets in the near-infrared. The vlt-sphere package enables easy reduction of the data coming from IRDIS and IFS, the two near-infrared subsystems of SPHERE. The package relies on the official ESO pipeline (ascl:1402.010), which must be installed separately.
Tiberius: Time series spectral extraction and transit light curve fitting
Kirk, James
Tiberius is a Python library for reducing time series spectra and fitting exoplanet transit light curves. This can be used to extract spectra from JWST (all 4 instruments), along with ground-based long-slit spectrographs and Keck/NIRSPEC echelle spectra (beta).
The light curve fitting routines can be used as as standalone to fit, for example, HST light curves extracted with other methods.
EXOTIC (EXOplanet Transit Interpretation Code): A Python3 package for analyzing photometric data of transiting exoplanets
A Python 3 package for analyzing photometric data of transiting exoplanets into lightcurves and retrieving transit epochs and planetary radii.
EXOTIC can run on a Windows, Macintosh, or Linux/Unix computer. You can also use EXOTIC via the free Google Colab, which features cloud computing, many helpful plotting functions, and a simplified installation. However, if you are a user with many images or large images, we recommend running EXOTIC locally on your own computer.
VIP: Vortex Image Processing package
Christiaens, V.; Gomez Gonzalez, C. A.; Farkas, R.; Dahlqvist, C.-H.; Nasedkin, E.; Milli, J.; Wertz, O.; Absil, O. More contributors here
VIP is a Python package for high-contrast imaging of exoplanets and circumstellar disks. The goal of VIP is to integrate open-source, efficient, easy-to-use and well-documented implementations of state-of-the-art high-contrast image processing algorithms. In addition, it also contains a number of routines for image preprocessing, performance assessment and the characterization of both point and extended sources.
VIP started as the effort of Carlos Alberto Gomez Gonzalez, a former PhD student of the VORTEX team (ULiège, Belgium). Since 2020, Dr. Valentin Christiaens (ULiège) has been in charge of VIP's maintenance and development lead.
excalibuhr: A pipeline for high-resolution spectral data reduction
Zhang, Yapeng ; de Regt, Sam ; González Picos, Darío
excalibuhr is a Python package for data reduction of high-resolution spectroscopy of exoplanets and brown dwarfs. It has an end-to-end pipeline for VLT/CRIRES+.
GRIP: Generic data Reduction for nulling Interferometry Package
Martinod, Marc-Antoine; Defrère, Denis; Laugier, Romain
The Generic data Reduction for nulling Interferometry Package (GRIP) aims to provide a universal pipeline to all existing and future nullers. GRIP aims to provide self-calibrated null depth measurements by fitting a model of the instrumental perturbations to histograms of data. The model is generated using a simulator of the instrument, which can be provided by the user or is built into the package for the main operating nullers
tglc (TESS-Gaia Light Curve): TESS FFI light curve based on point spread functions
Han & Brandt 2023
TESS-Gaia Light Curve (TGLC) is a PSF-based TESS full-frame image (FFI) light curve product. Using Gaia DR3 as priors, the team forward models the FFIs with the effective point spread function to remove contamination from nearby stars. The resulting light curves show a photometric precision closely tracking the pre-launch prediction of the noise level: TGLC's photometric precision consistently reaches ≲2% at 16th TESS magnitude even in crowded fields, demonstrating excellent decontamination and deblending power.
tshirt: Time Series Helper & Integration Reduction Tool
Everett Schlawin ; Kayli Glidic
The Time Series Helper & Integration Reduction Tool tshirt is a general-purpose tool for time series science. Its main application is to process raw data on exoplanet systems. tshirt can:
- Reduce raw data: flat field, bias subtract, gain correct, etc. This has been demonstrated to work with merged CCD images from Mont4K imager on the Kuiper-61 inch on Mt Bigelow, AZ.
- Extract Photometry
- Extract Spectroscopy
IGRINS Transit
Megan Weiner Mansfield & Michael R. Line
IGRINS transit is a pipeline to take high-resolution observations of transiting exoplanets with Gemini-S/IGRINS and produce cross-correlation detections of molecules in the exoplanet's atmosphere.
kpic_pipeline
The KPIC Team
The data reduction pipeline for the Keck Planet Imager and Characterizer. It is used for processing high resolution spectroscopy data taken with KPIC to study exoplanet atmospheres. Designed to process and calibrate KPIC data to enable spectroscopic model fitting.
breads: Broad Repository for Exoplanet Analysis, Discovery, and Spectroscopy
Agrawal, Shubh et al.
breads, or the Broad Repository for Exoplanet Analysis, Detection, and Spectroscopy, is a flexible framework that allows forward modeling of data from moderate to high resolution spectrographs. The philosophy of breads is to have the users choose a data class, a forward model function, and a fitting strategy. Data classes normalize the data format, simplifying reduction across different spectrographs while allowing for specific behaviors of each instrument to also be coded into their own specific class. The forward model (FM) aims to reproduce the data (d) as d = FM + n, where n is the noise.
The Giants Pipeline: An open-source Python package to search for exoplanets around evolved stars
Saunders, Nicholas et al.
An open-source TESS FFI pipeline to access TESS data, produce noise-corrected light curves, and search for planets transiting evolved stars, with an emphasis on detecting planets around subgiant and RGB stars. The giants pipeline produces a one-page PDF summary for each target including the following vetting materials. Built with Lightkurve.
exovetter: Transiting exoplanet detection python vetter
The exovetter development team
The exovetter package provide statistical metrics and quick visualizations needed when evaluating a periodic transit found in time domain photometry, such as Kepler and TESS. This code wraps codes used to evaluate TESS, Kepler and K2 transit-like signals in order to remove obvious false positives.
TIKE: The Time Series Integrated Knowledge Engine
The MAST Team at STScI
The TIKE (Time series Integrated Knowledge Engine) is a new service being offered by STScI to support astronomers working with the time series data archived at MAST, such as data from NASA's TESS, Kepler and K2 missions. This tool is built on the Pangeo deployment of JupyterHub, using Kubernetes in AWS. TIKE is a platform where astronomers can make use of data science utilities, astronomy software, and community software packages to retrieve and analyze data sets without having to download the data to their machines or maintain their own set of python packages.
ATMOSPHERIX: Data Processing Tool
Klein, B. et al.
A simple tool to process near-infrared high-resolution spectra for the atmospheric characterisation of transiting exoplanets. The code remove the stellar and Earth atmosphere spectra and correct for systematics in a data-driven way (e.g. principal component analysis or auto-encoders). It contains a planet atmosphere retrieval (nested sampling algorithm). The code is initially designed to work with telluric-corrected SPIRou transmission spectra, but could be easily adapted to other instruments (e.g. GEMINI-IGRINS, VLT-CRIRES+, ESO-NIRP) and to emission spectroscopy.
CONTROL: CUTE Autonomous Data Reduction Pipeline
Sreejith, A. G. et al.
V1.0 of CUTE data reduction pipeline.
This software is intented to be fully automated, aimed at producing science-quality output with a single command line with zero user interference for CUTE data. It can be easily used for any single order spectral data in any wavelength without any modification.
exoTEDRF: exoplanet Transit and Eclipse Data Reduction Framework
Radica, Michael
Formerly known as supreme-SPOON, exoTEDRF is an end-to-end pipeline for the reduction of JWST exoplanet time series observations (NIRISS and NIRSpec currently supported, MIRI in development).
APPleSOSS: A Producer of ProfiLEs for SOSS. Application to the NIRISS SOSS Mode
Radica, M. et al.
A tool to produce empirical 2D point spread functions for JWST NIRISS/SOSS observations. These PSFs are necessary input for the ATOCA extraction algorithm implemented in the STScI calibration pipeline.
Difference Imaging Code and Visualization for TESS Full Frame Image Lightcurves
Oelkers, R. J.; Stassun, K.G.
This toolset includes a difference image analysis pipeline, which employs a delta-function kernel, useful for reducing TESS Full Frame Images. The data extracted using the pipeline for the first two years of TESS imagery is available for inspection at https://filtergraph.com/tess_ffi.
VCAL-SPHERE: Hybrid pipeline for reduction of VLT/SPHERE data
Christiaens, Valentin et al.
VCAL-SPHERE, for VIP-based Calibration of VLT/SPHERE data, is a versatile pipeline for high-contrast imaging of exoplanets and circumstellar disks. The pipeline covers all steps of data reduction, including raw calibration, pre-processing and post-processing (i.e., modeling and subtraction of the stellar halo), for the IFS, IRDIS-DBI and IRDIS-CI modes (and combinations thereof) of the VLT instrument SPHERE. The three main steps of the reduction correspond to different modules, where the first follows the recommended EsoRex (ascl:1504.003) workflow and associated recipes with occasional inclusion of VIP (ascl:1603.003) routines.
pycrires: Data reduction pipeline for VLT/CRIRES+
Stolker, Tomas; Landman, Rico
pycrires runs the CRIRES+ recipes of EsoRex. The pipeline organizes the raw data, creates SOF and configuration files, runs the calibration and science recipes, and creates plots of the images and extracted spectra. Additionally, it corrects remaining inaccuracies in the wavelength solution and the spectrum curvature. pycrires also provides dedicated routines for the extraction, calibration, and detection of spatially-resolved objects such as directly imaged planets.
DACE: Data & Analysis Center for Exoplanets
Ségransan, D. et al.
The Data & Analysis Center for Exoplanets (DACE) is a PlanetS web-platform located at the University of Geneva (CH) dedicated to extrasolar planets data visualization, exchange and analysis. DACE provides the research and education community with an enhanced access to exoplanet data with a suite of statistical tools for data analysis. Published observational data such as high resolution spectra, radial velocities, photometric light curves and high contrast imaging measurements are available online. Planetary systems formation and evolution can be studied as well as their long term dynamical evolution.
pycdata: A module to import datasets from various instruments in pycheops
Patel, Jayshil A.; Brandeker, Alexis; Maxted, Pierre
pycdata is a module to import datasets from various telescopes/instruments in pycheops. pycheops is a tool specifically designed to model CHEOPS observations of transits, eclipses and phase curves. While being a genius tool, what it lacks is a facility to model datasets from other telescopes/instruments, even the PSF photometry produced by PIPE. pycdata can be used to import datasets from PIPE, TESS and Kepler/K2 in pycheops thus enabling a joint lightcurve analysis of PIPE, TESS, Kepler/K2 data along with CHEOPS data in pycheops.
smart: Spectral Modeling Analysis and RV Tool
Hsu, Chih-Chun; Burgasser, Adam; Theissen, Chris; Birky, Jessica
The smart is a Markov Chain Monte Carlo (MCMC) forward-modeling framework for spectroscopic data, currently working for high-resolution spectrometers including Keck/NIRSPEC, SDSS/APOGEE, Gemini/IGRINS, Lick/HPF, Keck/HIRES and medium-resolution spectrometers including Keck/OSIRIS and Keck/NIRES.
For NIRSPEC users, required adjustments need to be made before reducing private data using NIRSPEC-Data-Reduction-Pipeline(NSDRP), to perform telluric wavelength calibrations, and to forward model spectral data. The code is currently being developed.
Applefy: Robust detection limits for high-contrast imaging
Bonse, Markus J.; Gebhard, Timothy D.
Applefy calculates detection limits for exoplanet high contrast imaging (HCI) datasets. The package provides a number of features and functionalities to improve the accuracy and robustness of contrast curve calculations. Applefy implements the classical approach based on the t-test as well as the parametric boostrap test for non-Gaussian residual noise. Written in Python, it computes contrast curves and contrast grids.
WATSON: Visual Vetting and Analysis of Transits from Space ObservatioNs
Dévora-Pajares, Martín
WATSON (Visual Vetting and Analysis of Transits from Space ObservatioNs is a lightweight software package that enables a comfortable visual vetting of a transiting signal candidate from Kepler, K2 and TESS missions. WATSON looks for transit-like signals that could be generated by other sources or instrument artifacts. The code runs simplified tests on scenarios including:
- Transit shape model fit
- Odd-even transits checks
- Centroids shifts
- Optical ghost effects
- Transit source offsets
PyMieScatt: The Python Mie Scattering package
Sumlin, B., Heinson, W., and Chakrabarty, R.
PyMieScatt is a comprehensive forward and inverse Mie theory solver for Python 3. This package calculates relevant parameters such as absorption, scattering, extinction, asymmetry, backscatter, and more. It also contains single-line functions to calculate optical coefficients (in Mm-1) of ensembles of particles in lognormal (with single or multiple modes) or custom size distributions.
The inverse calculations retrieve the complex refractive index from laboratory measurements of scattering and absorption (or backscatter), useful for studying atmospheric organic aerosol of unknown composition.
Read more in our JQSRT paper!
PACMAN: A pipeline to reduce and analyze Hubble Wide Field Camera 3 IR Grism data
Zieba, Sebastian; Kreidberg, Laura
Here we present PACMAN, an end-to-end pipeline developed to reduce and analyze HST/WFC3 data. The pipeline includes both spectral extraction and light curve fitting. The foundation of PACMAN has been already used in numerous publications (e.g., Kreidberg et al., 2014; Kreidberg et al., 2018) and these papers have already accumulated hundreds of citations.
spaceKLIP: Pipeline for reducing & analyzing JWST coronagraphy data with the help of pyKLIP
JWST ERS 1386 Team
The spaceKLIP pipeline enables to reduce & analyze JWST NIRCam & MIRI coronagraphy data. It provides functions to run the official jwst stage 1 and 2 data reduction pipelines with several modifications that were made to improve the quality of high-contrast imaging reductions. It then performs PSF subtraction based on the KLIP algorithm as implemented in the widely used pyKLIP package, outputs contrast curves, and enables forward model PSF fitting for any detected companions in order to extract their properties (offset and flux). The pipeline is still under heavy development.
Molecfit: A general tool for telluric absorption correction
Molecfit is a tool to correct for telluric absorption lines based on synthetic modelling of the Earth’s atmospheric transmission. It can be used with data obtained with various ground-based telescopes and instruments. It combines a publicly available radiative transfer code, a molecular line database, atmospheric profiles, and various kernels to model the instrument LSF. The atmospheric profiles are created by merging a standard atmospheric profile representative of a given observatory’s climate, of local meteorological data, and of dynamically retrieved altitude profiles for temperature, pressure, and humidity.
Optimal BLS: Optimally-efficient code for transit searches in long time series
Ofir, Aviv
Explicitly including Keplerian dynamics in the transit search allows Optimal BLS to enhance transit detectability while allowing such searches to be done with much-reduced resources and time. By using the (standard) BLS, one is either fairly insensitive to long-period planets or less sensitive to short-period planets and computationally slower by a significant factor of ~330 (for a 3 yr long dataset). Physical system parameters, such as the host star's size and mass, directly affect transit search. This understanding can then be used to optimize the search for every star individually. The code is well-used by the community.
pyPplusS: Fast and precise light-curve model for transiting exoplanets with rings
Eden Rein and Aviv Ofir
The Polygon + Segments model allows modeling the light curve of an exoplanet with rings. This high-precision model includes full ring geometry as well as possible ring transparency and the host star’s limb darkening. Additionally, it can model oblate ringless planets as an opaque “ring” (same shape as a planet). pyPplusS is also computationally efficient, requiring just a 1D integration over a small range, making it faster than existing techniques. The algorithm at its core is further generalized to compute the light curve of any set of convex primitive shapes in transit (e.g. multiple planets, oblate planets, moons, rings, combination thereof, etc.) while accounting for their overlaps.
ATOCA: Algorithm to Treat Order Contamination. Used to decontaminate and extract spectra from image.
ATOCA is used to extract and decontaminate spectroscopic images with multiple sources or diffraction orders. The inputs are, for all orders and sources: the wavelength solutions, the trace profiles, the throughputs and the spectral resolution kernels. From this, ATOCA can model simultaneously the detector and extract the spectra. See Darveau-Bernier et al. (2022) for more details.
TESS-SIP: TESS Systematics Insensitive Periodogram
Hedges et al.
Tool for creating a Systematics-insensitive Periodogram (SIP) to detect long period rotation in NASA's TESS mission data. Read more in our published Research Note of the American Astronomical Society. SIP is a method of detrending telescope systematics (the TESS scattered light) simultaneously with calculating a Lomb-Scargle periodogram. This allows us to estimate of the rotation rate of variables with a period of >30days when there are multiple sectors. You can read a more in-depth work of how SIP is used in NASA's Kepler/K2 data here
IGRINS RV: A Radial Velocity Pipeline for IGRINS
Stahl, A. et al. 2021; Tang, S-Y. et al. 2021
IGRINS RV is a python open source pipeline for extracting radial velocities (RVs) from spectra taken with the Immersion GRating INfrared Spectrometer (IGRINS). It uses a modified forward modeling technique that leverages telluric absorption lines as a common-path wavelength calibrator. IGRINS RV achieves an RV precision in the H and K bands of around 25-30 m/s for narrow-line stars, and it has successfully recovered the planet-induced RV signals of both HD 189733 and τ Boo A. Visit Stahl et al. 2021 to see the published paper.
Prose: A Python framework for modular astronomical images processing
Garcia, L.
Built for astronomy, Prose is instrument-agnostic and allows the construction of data reduction pipelines using a wide range of building blocks, pre-implemented or user-defined. Using its modular architecture, it features basic reduction pipelines to deal with common tasks such as automatic reduction and photometric extraction.
dips: Detrending strictly periodic signals
Prsa, A.
dips is an algorithm for detrending timeseries of strictly periodic signals. It does not assume any functional form for the signal or the background or the noise; it disentangles the strictly periodic component from everything else. We use it in astronomy for detrending Kepler, K2 and TESS timeseries of periodic variable stars, eclipsing binary stars, exoplanets etc. The algorithm is described in detail in Prša, Zhang and Wells (2019), PASP 131, 8001. A new, generalized version of dips will be explained in Horvat and Prša (2022), currently in preparation.
SERVAL: Spectrum radial velocity analyser
Zechmeister, Mathias
Serval measures and analyses precise radial velocities in stellar spectra using least square fitting.
Nii: A Bayesian orbit retrieval code applied to differential astrometry
Jin, Sheng
Here we present an open-source Python-based Bayesian orbit retrieval code (Nii) that implements an automatic parallel tempering Markov chain Monte Carlo (APT-MCMC) strategy. Nii provides a module to simulate the observations of a space-based astrometry mission in the search for exoplanets, a signal extraction process for differential astrometric measurements using multiple reference stars, and an orbital parameter retrieval framework using APT-MCMC. We further verify the orbit retrieval ability of the code through two examples corresponding to a single-planet system and a dual-planet system. In both cases, efficient convergence on the posterior probability distribution can be achieved.
zeus: A Python implementation of ensemble slice sampling for efficient Bayesian parameter inference
Karamanis, M.; Beutler, F.; Peacock, J. A.
We introduce zeus, a well-tested Python implementation of the Ensemble Slice Sampling (ESS) method for Bayesian parameter inference. ESS is a novel Markov chain Monte Carlo (MCMC) algorithm specifically designed to tackle the computational challenges posed by modern astronomical and cosmological analyses. In particular, the method requires only minimal hand--tuning of 1-2 hyper-parameters that are often trivial to set; its performance is insensitive to linear correlations and it can scale up to 1000s of CPUs without any extra effort. Furthermore, its locally adaptive nature allows to sample efficiently even when strong non-linear correlations are present.
TRAN_K2: Search for planetary transits embedded in stellar variability and systematic effects
Kovacs, Geza
TRAN_K2 is standalone Fortran code to search for planetary transits under the colored noise of stellar variability and instrumental effects. Stellar variability is represented by a Fourier series and, when necessary, by an autoregressive model aimed at avoiding excessive Gibbs overshoots at the edges. For the treatment of systematics, a co-trending and an external parameter decorrelation are employed. The filtering is done within the framework of the standard weighted least squares, where the weights are determined iteratively, to allow a robust fit and to separate the transit signal from stellar variability and systematics.
TRIPPy: Python based Trailed Source Photometry
TRIPPy is a python package aimed to perform all the steps required to measure accurate photometry of both trailed and non-trailed (stationary) astronomical sources. This includes the ability to generate stellar and trailed point source functions, and to use circular and pill shaped apertures to measure photometry and estimate appropriate aperture corrections. Tools for source fitting with a model PSF (both MCMC and classical least-squares minimizers) are available.
Citation: If you use TRIPPy in your science works, please cite Fraser, W. et al., 2016, Astronomical Journal, 151. DOI at Zenodo.
PEP: The Planetary Ephemeris Program
Developed by many; original: Michael Ash; most recent and longest- time-involved: John Chandler
This Fortran computer program models orbital motion in the solar system, including almost 100 individual asteroids as well as all of the planets and some moons, along with a detailed model of our moon, and a model of pulsar motions and of distant radio sources. It takes as input diverse astrometric data: radio, radar, laser, timing of signal arrivals, and VLBI. The program can solve for well over 100 parameters, including orbital and (for some bodies) rotational initial conditions, sky coordinates for radio sources, plasma densities, the second harmonic of the Sun's gravitational field, and those related to tests of fundamental physics.
Deep-Transit: Identify Transit Signals with Deep Learning Based Object Detection Algorithm
Cui, K. et al.
Deep-Transit is an open-source Python package designed for transit detection with a deep learning based 2D object detection algorithm. For simple usage, Deep-Transit can handle your light curve and then output the transiting candidates' bounding boxes and confidence scores. Deep-Transit has already been trained for Kepler and TESS data, but can be easily extended to other photometric surveys, even ground-based observations. Deep-Transit also provides the interface to train on your own datasets.
RVLIN: A Fast Maximum Likelihood Method for Fitting Multiplanet Keplerian Curves to RV Data Coded in IDL
Jason Wright and Andrew Howard
An IDL routine for fitting multiple Keplerian curves (i.e. those that neglect planet-planet interactions) to radial velocity data. Handles heteroschedastic data, and constraints on P, e, phase, and transit timing. It is fast because it solves, via maximum likelihood, for all parameters other than P, e, and phase with a linear least-squares matrix inversion. It then determines the remaining 3*n parameters (where n is the number of planets) via a Levenberg-Marquardt optimization. The method is described in Wright & Howard ApJS 182, 205. Uncertainties in the fitted parameters can be determined via bootstrapping using BOOTTRAN (Wang et al. ApJ 761, 46).
Gemini Planet Imager Data Reduction Pipeline: Official data reduction pipeline for the GPI instrument integral field spectrograph
The Gemini Planet Imager Data Pipeline allows transformation of raw data from GPI into calibrated spectral and polarimetric data cubes. It also provides some basic capabilities for PSF suppression through differential imaging, and for astrometry and spectrophotometry of detected sources. See complete documentation here.
EDI-Vetter Unplugged: Transit Signal False Positive Vetting Tool
Zink, Jon K.
This program was originally designed to identify false positive transit signals in K2 photometry, but has been modified to play nicely with the Transit Least Squares software package. It contains several thresholds which mimic visual inspection and help automate the transit detection process.
MCMCI: MCMC-based analysis of light curves or RV time series with interpolation within stellar isochrones
Bonfanti A., Gillon M.
The MCMCI tool offers the opportunity to perform an integrated analysis of an exoplanetary system without splitting it into the preliminary stellar characterisation through theoretical models.The MCMCI combines the Markov chain Monte Carlo approach of analysing photometric or radial velocity time series with a proper interpolation within stellar evolutionary isochrones and tracks, to be performed at each chain step, to retrieve stellar theoretical parameters such as age, mass, and radius. This approach favours a close interaction between lightcurve analysis and isochrones, so that the parameters recovered at each step of the MCMC enter as inputs for purposes of the isochrone placement.
MAYONNAISE processing pipeline: A morphological components analysis pipeline for circumstellar disks and exoplanets imaging
Pairet, Benoît et al.
MAYO is a pipeline for exoplanet and disk high-contrast imaging from ADI datasets. For more information, please refer to Pairet, Benoît, Faustine Cantalloube, and Laurent Jacques. "MAYONNAISE: a morphological components analysis pipeline for circumstellar disks and exoplanets imaging in the near infrared.", Monthly Notices of the Royal Astronomical Society, 2021.
VARTOOLS: Command-line program for analyzing astronomical time-series data
Hartman, J.D.; Bakos, G.A.
The VARTOOLS program is a command line utility that provides tools for processing and analyzing astronomical time series data, especially light curves. It includes methods for calculating variability/periodicity statistics of light curves; for filtering, transforming, and otherwise modifying light curves; and for modeling light curves. It is intended primarily for batch processing a large number of light curves. The program is run by issuing a sequence of commands to perform actions on light curves, each command is executed in turn with the resulting light curves passed to the next command. Statistics computed by each command are sent to stdout as an ascii table.
TRICERATOPS: Bayesian Vetting and Validation Tool for Transiting Exoplanet Candidates
Giacalone, Steven et al.
TRICERATOPS is a Bayesian vetting and validation tool for TESS planet candidates. For a given planet candidate, the tool calculates the probabilities of several astrophysical transit-producing scenarios using the TESS light curve, information about nearby stars, and follow-up observations (e.g., high-resolution imaging, spectroscopy, and time-series photometry). Using these probabilities, TRICERATOPS calculates a false positive probability (the overall probability of the transit being caused by an astrophysical false positive) and a nearby false positive probability (the probability of the transit being caused by an off-target event around a nearby star).
xwavecal: A Blind Wavelength Calibration Algorithm for Echelle Spectrographs
Brandt, G. M. et al.
A library of routines for wavelength calibrating echelle spectrographs for high precision radial velocity work. Calibrates the instrument without any input for known emission line wavelengths and positions. A limited data-reduction pipeline is included.
Wotan: Remove Trends from Time-series Data
Hippke, Michael
Wotan offers free and open source algorithms to automagically remove trends from time-series data. Python open source.
Available detrending algorithms include: Time-windowed sliders with location estimates, splines, polynomials and sines, regressions, fitting a model that is a sum of Gaussian bases, Gaussian Processes. Available features: Filter lengths, break tolerances, edge cutoffs, tuning parameters, transit masks.
Juliet: A Versatile Modeling tool for Transiting and Non-transiting Exoplanetary Systems
Espinoza, N.; et al.
Juliet is a versatile modelling tool for transiting and non-transiting exoplanetary systems that allows to perform quick-and-easy fits to data coming from transit photometry, radial velocity or both using bayesian inference and, in particular, using Nested Sampling in order to allow both efficient fitting and proper model comparison. This pip-installable python library (pip install juliet) also allows to model these time-series using either simple linear models and/or more involved correlated noise on both photometry and radial-velocities through Gaussian Processes. Full documentation is available here
AAS - Timeseries: Read in and Manipulate Time Series in Astropy
Thomas Robitaille, American Astronomical Society (AAS)
The aas-timeseries package has been developed as part of a project between AAS Publishing and the Astropy Project. The goal of this project is to provide astronomers with all the tools needed to make it possible for astronomers to use Astropy to read in and manipulate time series data sets, such as exoplanet transit light curves, produce interactive figures, and easily embed these in a paper. The package is general enough to be usable in other contexts, for example to embed interactive time series figures in personal web pages, or for use in Jupyter notebooks and Jupyter Lab.
ARCHI: An expansion to the CHEOPS mission official pipeline
ARCHI, An expansion to the CHEOPS mission official pipeline, is an additional open-source pipeline to analyse the background stars present in CHEOPS images that are not tracked by the official pipeline. This tool opens a potential for the use of CHEOPS to produce photometric time-series of several close-by targets at once, as well as to use different stars in the image to calibrate systematic errors. Furthermore, there might be cases where the study of the companion light curve can be important for the understanding of contaminations on the main target .
Barycorrpy: Precise Barycentric Correction for Stellar and Solar Radial Velocities and Time-stamps
Shubham Kanodia, Jason Wright, Joe Ninan
Barycorrpy is an open source code written in Python based on Barycorr in IDL (Wright and Eastman 2014) to calculate the barycentric correction for any time series observations of stellar sources, and to convert JDUTC to BJDTDB time stamps (Kanodia and Wright 2018).
Update August 2020: It can now also be used to calculate the barycentric correction for Solar observations, as well as reflected light observations of solar system objects (Wright and Kanodia 2020).
PynPoint: Pipeline for Processing and Analyzing High-Contrast Image Data of Exoplanets and Brown Dwarfs
Stolker, Tomas; Bonse, Markus; Quanz, Sascha; Amara, Adam; et al.
PynPoint is a generic, end-to-end pipeline for processing and analysis of high-contrast imaging data of exoplanets and brown dwarfs. The software architecture has a modular and scalable design. A variety of pipeline modules are available for pre-processing, PSF subtraction with principal component analysis (PCA), photometric and astrometric measurements, and estimation of detection limits. The package supports post-processing with ADI, RDI, and SDI techniques.
eleanor: Python Package that Extracts TESS Target Pixel Files and Produces Systematics-Corrected Light Curves
Feinstein, A. D., Montet, B. T., Foreman-Mackey, D., et al.
Eleanor is a Python package that extracts target pixel files from TESS Full Frame Images and produces systematics-corrected light curves for any star observed by the TESS mission. In its simplest form, eleanor takes a TIC ID, a Gaia source ID, or (RA, Dec) coordinates of a star observed by TESS and returns, as a single object, a light curve and accompanying target pixel data. Paper: Feinstein et al., eleanor: An open-source tool for extracting light curves from the TESS Full-Frame Images, 2019
AstroImageJ: Image Display Environment and Tools for Calibration and Data Reduction
Collins, K.; Kielkopf, J.; Stassun, K.; Hessman, F.
AstroImageJ (AIJ) provides an astronomy-focused image display environment and tools for image calibration and data reduction. AIJ maintains the general purpose image processing capabilities of ImageJ, but AIJ is streamlined for time-series differential photometry, light curve detrending and fitting, and light curve plotting, especially for applications requiring ultra-precise light curves (e.g., exoplanet transits). AIJ reads and writes standard Flexible Image Transport System (FITS) files, as well as other common image formats, provides FITS header viewing and editing, and is World Coordinate System aware, including an automated interface to astrometry.net for plate solving images.
pyKLIP: Tool for the Characterization of Directly-Imaged Exoplanets and Circumstellar Disk
Wang, Jason et al.
pyKLIP subtracts out the stellar PSF to search for and characterize directly-imaged exoplanets and circumstellar disks using a Python implementation of the Karhunen-Loève Image Projection (KLIP) algorithm. pyKLIP supports using ADI, SDI, and RDI observing techniques and parallelizes the KLIP algorithm to speed up the reduction. pyKLIP supports data from most high-contrast imaging instruments and provides libraries to both detect and characterize astrophysical sources in the data.
Other resources in the literature:
ASPIRED: Automated SpectroPhotometric Image REDuction
Lam, Marco C.; Smith, Robert J.; Steele, Iain A.
ASPIRED reduces 2D spectral data from raw image to wavelength and flux calibrated 1D spectrum automatically without any user input (quicklook quality), and provides a set of easily configurable routines to build pipelines for long slit spectrographs on different telescopes (science quality).
Published in "Automated SpectroPhotometric Image REDuction (ASPIRED)", 2020, Astronomical Data Analysis Software and Systems XXIX. ASP Conference Series, Vol. 527, proceedings of a conference held (6—10 October 2019) at the Martini Plaza, Groningen, the Netherlands.
Astrocut: Tools for creating cutouts of TESS images
Brasseur, Clara E. et al.
The Transiting Exoplanet Survey Satellite (TESS) produces Full Frame Images (FFIs) at a half hour cadence and keeps the same pointing for ~27 days at a time. Astrocut performs the same cutout across all FFIs that share a common pointing to create a time series of images on a small portion of the sky.
Published in "Astrocut: Tools for creating cutouts of TESS images", 2019, Astrophysics Source Code Library (ASCL).
CEERS NIRCam Reduction Pipeline
CEERS team
JWST NIRCam Reduction PipelineThe reduction process includes corrections for known prelaunch issues such as 1/f noise, as well as in-flight issues including snowballs, wisps, and astrometric alignment.
Published in "CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results", 2023, The Astrophysical Journal Letters, Volume 946, Issue 1, id.L12, 23 pp.
charis-dep: CHARIS reduction pipeline
Brandt, T. D. et al.
The charis pipeline is capable of extracting spectral data cubes from both the Subaru/CHARIS as well as the SPHERE/IFS integral field spectrographs for high-contrast imaging.
Published in "Data reduction pipeline for the CHARIS integral-field spectrograph I: detector readout calibration and data cube extraction", 2017, Journal of Astronomical Telescopes, Instruments, and Systems, Volume 3, id. 048002 (2017).
EVEREST: EPIC Variability Extraction and Removal for Exoplanet Science Targets
Luger, Rodrigo; Kruse, Ethan; Foreman-Mackey, Daniel; Agol, Eric; Saunders, Nicholas
EVEREST (EPIC Variability Extraction and Removal for Exoplanet Science Targets) removes instrumental noise from light curves with pixel level decorrelation and Gaussian processes. The code, written in Python, generates the EVEREST catalog and offers tools for accessing and interacting with the de-trended light curves. EVEREST exploits correlations across the pixels on the CCD to remove systematics introduced by the spacecraft’s pointing error.
Published in "EVEREST: Pixel Level Decorrelation of K2 Light Curves", 2016, ApJ, and "An Update to the EVEREST K2 Pipeline: Short Cadence, Saturated Stars, and Kepler-like Photometry Down to Kp = 15", 2018, ApJ
ExoTOM: A TOM implementation for observing exoplanet transits
Masur, Tim-Oliver et al.
ExoTOM is a target-observation-manager automating exoplanet transit follow-up.
Published in "ExoTOM: a target-observation-manager automating exoplanet transit follow-up", 2022, Proceedings of the SPIE, Volume 12186, id. 121861O 18 pp. (2022).
f3: Full Frame Fotometry for Kepler Full Frame Images
Montet, Benjamin T.; Tovar, Guadalupe; Foreman-Mackey, Dan
f3 is a package for extracting photometry from Kepler’s Full-Frame Images, a set of calibration data obtained approximately monthly during the primary Kepler mission.
Published in "Long-term Photometric Variability in Kepler Full-frame Images: Magnetic Cycles of Sun-like Stars", 2017, The Astrophysical Journal, Volume 851, Issue 2, article id. 116, 15 pp. (2017).
k2photometry: Read, reduce and detrend K2 photometry
Van Eylen, Vincent et al.
k2photometry reads, reduces and detrends K2 photometry and searches for transiting planets. MAST database pixel files are used as input; the output includes raw lightcurves, detrended lightcurves and a transit search can be performed as well.
Published in "k2photometry: Read, reduce and detrend K2 photometry", 2016, Astrophysics Source Code Library, record ascl:1602.014.
Used in "The K2-ESPRINT Project. II. Spectroscopic Follow-up of Three Exoplanet Systems from Campaign 1 of K2", 2016, The Astrophysical Journal, Volume 820, Issue 1, article id. 56, 8 pp.
Kadenza: Kepler/K2 Raw Cadence Data Reader
Barentsen, Geert; Cardoso, José Vinícius de Miranda
Kadenza enables time-critical data analyses to be carried out using NASA's Kepler Space Telescope. It enables users to convert Kepler's raw data files into user-friendly Target Pixel Files upon downlink from the spacecraft. The primary motivation for this tool is to enable the microlensing, supernova, and exoplanet communities to create quicklook lightcurves for transient events which require rapid follow-up.
nirHiss
Feinstein, Adina D. et al.
A JWST NIRISS spectral extraction code.
Published in "Early Release Science of the exoplanet WASP-39b with JWST NIRISS", 2023, Nature, Volume 614, Issue 7949, p.670-675.
Notch and LoCoR
Rizzuto, Aaron C. et al.
The Notch and LOCoR pipelines for detrending TESS and K2 lightcurves and identifying planetary signals.
Published in "Zodiacal Exoplanets in Time (ZEIT). V. A Uniform Search for Transiting Planets in Young Clusters Observed by K2", 2017, The Astronomical Journal, Volume 154, Issue 6, id.224.
PACO ASDI
Flasseur, Olivier et al.
PACO ASDI produces detection maps with improved sensibility compared to existing methods.
Published in "PACO ASDI: an algorithm for exoplanet detection and characterization in direct imaging with integral field spectrographs", 2020, Astronomy & Astrophysics, Volume 637, id.A9, 29 pp.
PIPE: PSF Imagette Photometric Extraction
Brandeker, Alexis et al.
PIPE is a photometric extraction package for CHEOPS that is complementing the official Data Reduction Pipeline (DRP).
Published in "CHEOPS geometric albedo of the hot Jupiter HD 209458 b", 2022, Astronomy & Astrophysics, Volume 659, id.L4, 8 pp.
PLIA: The Planetary Laboratory for Image Analysis
Hueso, R. et al.
IDL based software for Planetary image processing and navigation developed at the Grupo de Ciencias Planetarias (GCP) in the University of the Basque country UPV/EHU.
Published in "The Planetary Laboratory for Image Analysis (PLIA)", 2010, Advances in Space Research, Volume 46, Issue 9, p. 1120-1138.
precision
Scicluna, P. et al.
A python pipeline to reduce astronomical IR imaging data, written with SPHERE data in mind.
Published in "precision: a fast python pipeline for high-contrast imaging - application to SPHERE observations of the red supergiant VX Sagitariae", 2020, Monthly Notices of the Royal Astronomical Society, Volume 494, Issue 3, pp.3200-3211.
pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets In TESS Primary Mission Photometry
Fernandes, Rachel B. et al.
pterodactyls builds on publicly available and tested tools in order to extract, de-trend, search, and vet
transiting young planet candidates.
Published in "pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry", 2022, The Astronomical Journal, Volume 164, Issue 3, id.78, 22 pp.
SPORK: SPectral cOntinuum Refinement for telluriKs (SPORK) & Iterative Smoothing
Rasmussen, K. C. et al.
SPORK is a spectrum normalization routine adapted from the stellar abundance determination software Spectroscopy Made Hard(er).
Published in "SPORK That Spectrum: Increasing Detection Significances from High-resolution Exoplanet Spectroscopy with Novel Smoothing Algorithms", 2022, The Astronomical Journal, Volume 164, Issue 2, id.35, 8 pp.
TCF: Transit Comb Filter periodogram
Caceres, G. A.; Feigelson, E. D.
Extreme Value Theory for comparing periodograms: Optimizing future transiting exoplanet surveys. TCF calculates a periodogram designed to detect exoplanet transits after the light curve has been differenced.
Published in "Autoregressive Planet Search: Methodology", 2019, The Astronomical Journal, Volume 158, Issue 2, article id. 57, 21 pp.
TERRA: Transit detection code
Petigura, E. A.; Marcy, G. W.
Published in "Identification and Removal of Noise Modes in Kepler Photometry", 2012, Publications of the Astronomical Society of the Pacific, Volume 124, Issue 920, pp. 1073 (2012).
TESSreduce: transient focused TESS data reduction pipeline
Ridden-Harper, Ryan
TESSreduce builds on lightkurve to reduce TESS data while preserving transient signals.
Published in "TESSreduce: Transient focused reduction for TESS data", 2021, Astrophysics Source Code Library (ASCL).
Used in "Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy", 2022, Monthly Notices of the Royal Astronomical Society, Volume 512, Issue 2, pp.2777-2797.
The Unpopular Package: A Data-driven Approach to De-trend TESS Full Frame Image Light Curves
Hattori, Soichiro et al.
An implementation of the Causal Pixel Model (CPM) de-trending method to obtain TESS Full-Frame Image (FFI) light curves.
Published in "The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves", 2022, The Astronomical Journal, Volume 163, Issue 6, id.284, 19 pp.
TIERRA: TransmIssion spEctRoscopy of tRansiting plAnets
Niraula, Prajwal
TIERRA is a 1D spEctRoscopy code that adopted the original Matlab by Julien de Wit (de Wit et. al 2016, 2018) and expanded it in python. Currently only 7 molecules are included in the code: methane, carbon-monoxide, carbon-dioxide, water, hydrogen, nitrogen and ozone as part of the study Niraula & de Wit et. al 2022).
transitspectroscopy
Espinoza, Nestor
transitspectroscopy is a package containing algorithms and wrappers useful for performing transit (transmission and emission) spectroscopy of exoplanetary systems.
Published in "TransitSpectroscopy", 2022, Zenodo.