Target Pixel Files (TPFs) are a file common to Kepler/K2 and the TESS mission. They contain movies of the pixel data centered on a single target star.
TPFs can be thought of as stacks of images, with one image for every timestamp the telescope took data. Each timestamp is referred to as a cadence. These images are cut out 'postage stamps' of the full observation to make them easier to work with.
TPFs are given in FITS files, which you can read more about here. Lightkurve includes tools for you to work directly with these files easily and intuitively.
In this tutorial we'll cover the basics of working with TPFs. In lightkurve there are classes to work with each mission. For example
KeplerTargetPixelFile deals with data from the Kepler (and K2) mission.
TessTargetPixelFile deals with data from the TESS mission. We'll use a Kepler TPF as an example.
To load a
KeplerTargetPixelFile from a local path or remote url, simply create a new object using the location of the file as the parameter:
from lightkurve import KeplerTargetPixelFile tpf = KeplerTargetPixelFile("https://archive.stsci.edu/pub/kepler/target_pixel_files/0069/006922244/kplr006922244-2010078095331_lpd-targ.fits.gz")
You can also search for the url automatically using the
search_targetpixelfile() function. This will search for the right file in the MAST data archive which holds all of the Kepler and K2 data.
In this case we want the Target Pixel File with Kepler ID 6922244 for Quarter 4 (Kepler's observations were split into quarters of a year):
from lightkurve import search_targetpixelfile tpf = search_targetpixelfile(6922244, quarter=4).download()
You can also pass the name of the target or its astronomical coordinates as a parameter to
The above code has created a variable named
tpf which is a Python object of type
KeplerTargetPixelFile Object (ID: 6922244)
We can access lots of meta data using this object in a simple way. For example, we can find the mission name, and the quarter that the data was taken in by typing the following:
The most interesting data in a
KeplerTargetPixelFile object are the
time values which give access to the brightness of the observed target over time. You can access the timestamps of the observations using the
array([352.37632485, 352.39675805, 352.43762445, ..., 442.16263546, 442.18306983, 442.2035041 ])
time is in the Kepler-specific Barycentric Kepler Julian Day format (BKJD). You can easily convert this into AstroPy Time objects using the
<Time object: scale='tdb' format='jd' value=[2455185.37632485 2455185.39675805 2455185.43762445 ... 2455275.16263546 2455275.18306983 2455275.2035041 ]>
In turn, this gives you access to human-readable ISO timestamps using the
array(['2009-12-19 21:01:54.467', '2009-12-19 21:31:19.895', '2009-12-19 22:30:10.752', ..., '2010-03-19 15:54:11.704', '2010-03-19 16:23:37.233', '2010-03-19 16:53:02.754'], dtype='<U23')
Beware: these timestamps are in the Solar System Barycentric frame (TDB) and do not include corrections for light travel time or leap seconds. To use a different time scale, such as the Earth-centered UTC system, you can use AstroPy's time scale conversion features. For example:
array(['2009-12-19 21:00:48.283', '2009-12-19 21:30:13.712', '2009-12-19 22:29:04.569', ..., '2010-03-19 15:53:05.518', '2010-03-19 16:22:31.048', '2010-03-19 16:51:56.568'], dtype='<U23')
Next, let's look at the actual image data, which is available via the
(4116, 5, 5)
flux data is a 4116x5x5 array in units electrons/second. The first axis is the time axis, and the images themselves are 5 pixels by 5 pixels. You can use the
plot method on the
KeplerTargetPixelFile object to view the data. (By default, this will show just one cadence of the data. But you can pass the cadence you want to look at to the
frame keyword if you would like to check a particular flux point for thruster firings, cosmic rays or asteroids.)
%matplotlib inline tpf.plot(frame=0);
The values shown in this image are also directly accessible as an array:
array([[ nan, 5.6079335e+00, 5.1491142e+01, 8.4241745e+01, 3.0221334e+01], [4.4045620e+01, 7.6861229e+01, 1.1227759e+03, 3.2262029e+03, 4.5486777e+02], [2.5911165e+01, 2.2907593e+02, 9.3626543e+03, 2.3606273e+04, 1.2087750e+03], [4.0100830e+01, 8.8543927e+02, 1.7102118e+03, 2.6254871e+03, 7.0796606e+02], [1.5719417e+02, 8.3713440e+02, 5.1021539e+02, 1.1501041e+03, 1.8313370e+02]], dtype=float32)
You can use normal
numpy methods on these to find the shape, mean etc!
We can now turn this Target Pixel File into a light curve, with a single flux value for every time value. Each of the pixels are 4 arcseconds across. The point spread function (PSF) of the telescope causes the light from the star fall onto several different pixels, which can be seen in the image above. Because of this spreading, we have to sum up many pixels to collect all the light from the source. To do this we sum up all the pixels in an aperture. An aperture is a pixel mask, where we take only the pixels related to the target.
The Kepler pipeline adds an aperture mask to each target pixel file. This aperture determines which pixels are summed to create a 1-D light curve of the target. There are some science cases where you might want to create a different aperture. For example, there may be a nearby contaminant or you may want to measure the background.
The standard pipeline aperture is easily accessed in a
KeplerTargetPixelFile object using
tpf.pipeline_mask, which is a boolean array:
array([[False, False, False, False, False], [False, False, True, True, False], [False, False, True, True, False], [False, True, True, True, False], [False, False, False, True, False]])
We can also plot this aperture over the target pixel file above to see if the flux of the star is all contained within the aperture.
Now that we have the aperture we can create a Simple Aperture Photometry light curve in the next tutorial.
Finally, note that you can inspect all the raw metadata of the target by taking a look at the 'header' of the FITS file, which contains information about the data set. Let's just print the first 10 lines:
SIMPLE = T / conforms to FITS standards BITPIX = 8 / array data type NAXIS = 0 / number of array dimensions EXTEND = T / file contains extensions NEXTEND = 2 / number of standard extensions EXTNAME = 'PRIMARY ' / name of extension EXTVER = 1 / extension version number (not format version) ORIGIN = 'NASA/Ames' / institution responsible for creating this file DATE = '2015-09-23' / file creation date. CREATOR = '917482 TargetPixelExporterPipelineModule' / pipeline job and program
We can look at the values in the second extension of the fits file by accessing the AstroPy FITS
HDUList object. For example, to look at all the column titles:
TTYPE1 = 'TIME ' / column title: data time stamps TTYPE2 = 'TIMECORR' / column title: barycenter - timeslice correction TTYPE3 = 'CADENCENO' / column title: unique cadence number TTYPE4 = 'RAW_CNTS' / column title: raw pixel counts TTYPE5 = 'FLUX ' / column title: calibrated pixel flux TTYPE6 = 'FLUX_ERR' / column title: 1-sigma calibrated uncertainty TTYPE7 = 'FLUX_BKG' / column title: calibrated background flux TTYPE8 = 'FLUX_BKG_ERR' / column title: 1-sigma cal. background uncertain TTYPE9 = 'COSMIC_RAYS' / column title: cosmic ray detections TTYPE10 = 'QUALITY ' / column title: pixel quality flags TTYPE11 = 'POS_CORR1' / column title: column position correction TTYPE12 = 'POS_CORR2' / column title: row position correction TTYPE13 = 'RB_LEVEL' / column title: rolling band level