Stages
PACMAN is separated into different stages, summarized here. Click on the hyperlinks below to see the python script for each stage. For an example of each stage applied to real data, check out Introduction.
Stage 00
read in the _ima_ fits files in the data directory
save important information from the header in a table
create a “work directory” to save all plots and files from the next stages
Stage 01
download the location of HST during the observations to prepare for the barycentric correction
Stage 02
perform the barycentric correction to convert from MJD (which is in the header) to BJD
Stage 03
download or generate a stellar spectrum that matches the spectral type of the host star. Options are: KURUCZ 1993, CASTELLI AND KURUCZ 2004, PHOENIX MODELS and a blackbody spectrum
smooth the stellar spectrum using a gaussian kernel to reduce the stellar spectrum’s resolution
multiply the stellar spectrum by the grism throughput (which is saved in PACMAN/src/data/bandpass) to make a reference spectrum for the wavelength calibration
saves the reference spectrum into the work directory
Stage 10
read in the direct images
fit the position of the star in each direct image
Stage 20
extract the spectra using the optimal extraction routine from Horne 1986
save the white light curve into “lc_white.txt” and the spectroscopic light curve information into “lc_spec.txt”.
Stage 21
bins the spectra in wavelength to create spectroscopic light curves (this step can be skipped if the user is only interested in the broadband light curve).
Stage 30