asteriks is an open source python to work with Kepler/K2 data and generate light curves of solar system objects.
asteriks is currently under development! If you try to use it and it breaks please open an issue above.
You can in install the most up to the minute version of
asteriks by executing the following commands in a terminal...
git clone https://github.com/christinahedges/asteriks.git cd asteriks python setup.py
Our most recent stable release is available on PyPI which you can install with
pip install asteriks
Note if you want to run this and generate movies with this code you will need to install ffmpeg:
sudo apt-get install ffmpeg
You can start learning to use
asteriks with the demos in the notebooks folder. (Note the docs folder builds out website!) The demos consist of jupyter notebooks which will show you how to build light curves and target pixel files.
You can see all our current published data products here.
asteriks provides two final products; a fits file with a light curve and a Target Pixel File of the object moving across the Kepler focal plane. Below is a description of the fits file.
There are several extensions in the fits files, where each extension is a different aperture. The first extension is the "optimum" aperture, as decided by the
asteriks pipeline. Other extensions have apertures of varying sizes, enabling the user to use visual inspection to determine the best aperture for their science.
The primary header of the file contains the origin (asteriks) and object name (use
OBJECT to find the name. The exposure start and end time are also in the header. The keyword
LDLGCORR is short for "Lead Lag Correction". If True, then the Lead Lag Correction has been applied to the object, providing more quality flags. (See further documentation for a full description of the Lead Lag Correction.) Finally, the asteriks version number is included in the primary header.
The first extension contains the optimum aperture, as decided by the pipeline. The following columns are included:
TIME: The time in JD of each observation
FLUX: The flux of the object as observed by Kepler
FLUX_ERR: The error in the flux of the object as observed by Kepler
RA_OBJ: The Right Ascention of the object at each exposure, as determined by JPL Small Bodies Database
DEC_OBJ: The Declination of the object at each exposure, as determined by JPL Small Bodies Database
LEAD_QUAL: Short for 'Lead Quality'. First quality flag for the flux of the object. This is the quality of the Lead Lag Correction. If False, the Lead Lag Correction could not be successfully applied. In such cases, the user may choose to mask out bad quality data.
NPIX_QUAL: Short for 'Number of Pixels Quality'. Second quality flag for flux of the object. This flag is True if all pixels of the aperture have real values (i.e. are not NaNs). Where e.g. an asteroid moves off the edge of the detector NPIX_QUAL will be False.
BKG_QUAL: Short for 'Background Quality'. Third quality flag for flux of the object. This flag is True if the pipeline determines the background to be static and corrected. The flag is False if the pipeline determines that there was variable background that was poorly corrected, such as from an object moving over a saturated star or through a halo of a bright star.
NPIX_APER: Number of pixels inside the aperture at each point in time
EXTNAME: Name of the extension. If extension one, is
PERC: Percentile cut used to create the aperture
NPIX: Number of pixels in the aperture.
LEADFLAG: Whether Lead Lag Correction was used.