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This wiki is a brief guide on how to install, run, and troubleshoot barycorrpy (BCPy). BCPy is the Python version of Jason Eastman's IDL code BaryCorr based on Wright & Eastman 2014 . BCPy can be used to calculate the barycentric velocity correction for a star with an accuracy of < 1 cm/s . To do this, it takes into consideration the following -

1. Revolution of the Earth to consider position and velocity of the geocenter with respect to the Solar System barycenter
2. Rotation of the Earth
3. Precession, nutation and polar motion of the Earth, along with the above to calculate the position and velocity of the observatory with respect to the geocenter
4. Gravitational time dilation due to objects of the Solar System
5. Leap second offset
6. Proper motion and systemic radial velocity of the star
7. Parallax
8. Shapiro delay

There is also a video tutorial (courtesy of the Exoplanet Modeling and Analysis Center ) available here, describing how to get started with barycorrpy.

Contents :

• 1. Installation
• 2. Getting Started
• 3. Dependencies
• 4. FAQ
• 5. Leap Second Management
• 6. Error Management
• 7. Exposure Meter Calculation
• 8. JDUTC to BJDTDB converter
• 9. Barycentric correction for Solar RVs
• 10. Predictive Mode
• 11. USNO IERS servers are down

New Versions:

20180330: In v0.2 we have also added a JDUTC_to_BJDTDB converter. See 8. JDUTC to BJDTDB converter

202001yy: In v0.3 we include barycentric corrections for Solar observations, as well as reflected light observations from other Solar system objects such as Vesta, Ceres, etc. See 9. Barycentric correction for Solar RVs. We also introduce a Predictive Mode.

20210303: In v0.4 we deprecate the leap second management, as that is now implemented in astropy.

Citation

To cite using this code you can cite this paper - RNAAS.

Guidelines to cite this package can be found here.

To sign up for updates, please join the Google Group linked here - https://groups.google.com/forum/#!forum/barycorrpy