Example 3: Separating a background EB from a foreground star

The likelihood of source confusion around any given target is high. One cannot be certain whether astrophysical variability across a Kepler light curve comes entirely from the target star. In order to resolve the sources of variability within a target mask, users should examine the Target Pixel File (TPF).

Step 1: Plot archived SAP data

For the purposes of this example, we will examine the light curve and pixel file of KIC 2449074, which we can download from the archive as follows:

$ wget http://archive.stsci.edu/missions/kepler/lightcurves/0024/002449074/kplr002449074-2009350155506_llc.fits

We can visualize the Simple Aperture Photometry (SAP) flux measured by the Kepler pipeline using the kepdraw tool:

$ kepdraw kplr002449074-2009350155506_llc.fits
../_images/kepdraw_sap.png

Step 2: Plot archived PDCSAP data

Kepler’s pipeline is able to remove systematic artifacts thorugh the Presearch Data Conditioning (PDC). The corrected light curve can be visualized with kepdraw by passing the desired keyword through --datacol argument:

$ kepdraw kplr002449074-2009350155506_llc.fits --datacol PDCSAP_FLUX
../_images/kepdraw_pdcsap.png

Step 3: Plot archived photometric time-series for individual target pixels

The next figure shows a calibrated flux time series of each target mask pixel collected over Q3. This figure was produced with the PyKE task keppixseries operating upon the TPF kplr002449074-2009350155506_lpd-targ.fits, as follows:

$ wget https://archive.stsci.edu/missions/kepler/target_pixel_files/0024/002449074/kplr002449074-2009350155506_lpd-targ.fits.gz

$ keppixseries kplr002449074-2009350155506_lpd-targ.fits.gz
--plotfile keppixseries.png --plottype local
../_images/keppixseries1.png

The figure reveals unambiguously that the target star is not the source of the “transit” features. A background eclipsing binary star is situated 10 arcsec from the target star (2.5 pixels to the left of KIC 2449074 on the figure) and is leaking into the optimal aperture.

Step 4: Define new optimal apertures for target and background binary star

By extracting the light curve manually using different pixels, we can either reduce the contaminating flux from the eclipsing binary in the target light curve or, alternatively, extract a separate light curve from the eclipsing binary. New mask files are created interactively from the TPF kplr002449074-2009350155506_lpd-targ.fits using the kepmask tool. The primary output from kepmask is an ASCII file defining the selected pixel aperture. The image associated with the 2,177th timestamp in the Target Pixel File is plotted on a linear intensity scale as follows:

$ kepmask kplr002449074-2009350155506_lpd-targ.fits.gz --frameno 2177 --maskfile mask_target.txt
--iscale linear
../_images/kepmask_target.png

Similarly, we can create an aperture mask for the eclipsing binary:

$ kepmask kplr002449074-2009350155506_lpd-targ.fits.gz --frameno 2177 --maskfile mask_eb.txt
--iscale linear
../_images/kepmask_eb.png

Step 5: Extract new SAP light curves from the TPF

The PyKE tool kepextract can be called to extract new SAP light curves from the TPF. We can create two new light curves as follows:

$ kepextract kplr002449074-2009350155506_lpd-targ.fits.gz --outfile kepextract_target.fits --maskfile mask_target.txt

$ kepdraw kepextract_target.fits
../_images/kepextract_target.png
$ kepextract kplr002449074-2009350155506_lpd-targ.fits.gz --outfile kepextract_eb.fits --maskfile mask_eb.txt

$ kepdraw kepextract_eb.fits
../_images/kepextract_eb.png

Step 6: Mitigate for systematic artifacts in new SAP light curves

The extracted light curves are constructed by simple pixel summation. Consequently artifacts resulting from target motion across the pixel aperture exist within the new light curves. Artifacts can be reduced or removed by fitting and subtracting the best fit ensemble of Cotrending Basis Vectors (CBVs). Users must ensure that they download CBVs from the MAST correctly corresponding to the quarter being analyzed. In the current case, the Q3 CBV is called kplr2009350155506-q03-d14_lcbv.fits. Artifact correction is performed by the kepcotrend tool. The corrected light curve is stored in an output file within a new FITS column called CBVSAP_FLUX.

$ kepcotrend kepextract_target.fits --outfile kepcotrend_target.fits
../cbv/kplr2009350155506-q03-d25_lcbv.fits 1,2,3,4,5,6 --sigmaclip 3.0 --plot

$ kepcotrend kepextract_eb.fits --outfile kepcotrend_eb.fits
../cbv/kplr2009350155506-q03-d25_lcbv.fits 1,2,3,4,5,6 --sigmaclip 3.0 --plot
../_images/kepcotrend_target.png ../_images/kepcotrend_eb.png