Kepler Ancillary Files

Kepler makes several ancillary data files available to users. Documentation regarding each file type may be found in the Kepler Archive Manual.

• Cotrending Basis Vectors (CBV) Files
  The CBVs may be used to mitigate instrumental signatures in Kepler light curves when the PDC light curve is inadequate for your science. One CBV is available each quarter and is listed with links to download the files along with documentation and sites describing how to use them.
  
  
• Focal Plane Characterization Models
  A collection of models that describe the properties of the CCD and the focal plane.
  
  
• Pixel Response Function Files
  These data were collected during Kepler commissioning in April, 2009, and used to build the focal plane characterization models for Focal Plane Geometry (FPG) and Pixel Response Function (PRF) (see Sections 2.3.5.16 and 2.3.5.17 of the Kepler Archive Manual). These data have now been recalibrated using the SOC 9.3 pipeline and packaged as target pixel files, making both the raw and calibrated pixel data available for the first time. The dither pattern and a discussion of the small differences between the original and current calibration are provided in the associated documentation ( KSCI-19100-001.pdf).

  The Files are stored online organized by channel number. A separate directory labelled tar_files contains a gzipped tar file for each channel.
  
  

• Fine Guidance Sensor Data (FGS) The FGS data collected throughout the Kepler mission are being made available to the user community for scientific analysis as flux and centroid time series, along with a limited number of FGS full frame images which may be useful for constructing a World Coordinate System (WCS) or otherwise putting the time series data in context.
  
  
• Full Frame Image (FFI) and Engineering Data Search
  Images of the entire Kepler Field are typically taken three times during the quarter and are used to confirm the proper orientation and placement of the detector and to assess photometer health. The FFI uncalibrated, calibrated and uncertainties files are available. FFIs may also be downloaded via anonymous ftp at /pub/kepler/ffi, or via the browser at https://archive.stsci.edu/missions/kepler/ffi . To display individual channels from any of the FFI images, and overlay various catalogs, see the FFI_Display page.

  The following engineering files may also be retrieved: Long and Short Cadence Collateral (COLL & COLS) files, Artifact Removal Pixel (ARP) files, Background Pixel (BKG) files, and Reverse Clock (RVC) files.
  
  

• SPICE Kernels for Kepler
  The latest SPICE kernels (i.e., the bsp and tsc binary files) are available for download here to calculate the Kepler spacecraft ephemerides. They are available via anonymous ftp at /pub/kepler/spice, or via the browser at https://archive.stsci.edu/missions/kepler/spice . See the Navigation and Ancillary Information Facility (NAIF) web site for information on using SPICE Kernels.
  
  
• Raw Cadence Data
  These raw cadence data consist of multiple components, including target pixels, collateral pixels, and pixel mapping reference files. For more information on format and usage, see the document KADN-26315.pdf, and consider using Kadenza to convert these raw data to a more user-friendly file format. We currently have raw cadence data for quarters 0 through 17 online.
  
  
• Simulated Light Curves
  The Kepler Simulated light curves (types INJ1, INJ2, & INJ3) and the average detection efficiency tables have been downloaded from NExScI and are now available online. The README file describes how the files are stored, and the Pipeline Detection Efficiency document describes how they were used to test DR25 detection efficiency.
  
  
• Commissioning Data: The 2.5 days of commissioning data used to measure the Pixel Response Function (PRF) and Focal-Plane Geometry (FPG) have been calibrated and formatted as target pixel files (see KAM 2.3.2). The models derived from this data are included in the set of Focal Plane Characterization Models described above, but some users may wish to build alternate models based on this unique data take, which is described in KSCI-19100-001.