Changelog & to-do

Changelog

v1.0.0 September 2019, R.G. van Holstein:
  • Added analysis of master flux frame to enable the user to express the final images in contrast/arcsec^2 or Jansky/arcsec^2
  • Restructered code and configuration file to allow for the separate execution of pre-processing, polarimetric differential imaging (previously referred to as post-processing) and angular differential imaging
  • Added plot of center coordinates of center frames vs time
  • Added possibility to open documentation through terminal command irdap --website
  • Confirmed that polarimetric data with dithering applied is correctly reduced
v0.3.0 July 2019, R.G. van Holstein:
  • Added command-line option to mean-combine final images of multiple observation blocks
v0.2.1 June 2019, R.G. van Holstein:
  • Added the possibility to reduce data taken with the narrowband filters using the existing model of the broadband filters
v0.2.0 June 2019, R.G. van Holstein:
  • Changed the definition of the tuple of the input parameters annulus_star, annulus_background and flux_annulus_background: width is replaced by outer_radius and the definition of start_angle and end_angle is now the same as in DS9
  • Replaced static flat in Ks by one with P0-90 inserted
v0.1.2 June 2019, R.G. van Holstein:
  • Release of IRDAP package on PyPI and GitHub
  • Documentation put online

To-do high priority

  • Add angular differential imaging (ADI) including principal component analysis (PCA) of total intensity images for pupil-tracking observations
  • Add ADI+PCA for polarimetric data reduction of pupil-tracking observations
  • Add accurate (calibrated) model correction for narrowband filters
  • Add option to apply accurate plate scale and distortion correction for data (especially important for pupil-tracking and bright sources; do we need calibrations?)
  • For pupil-tracking data mask bad pixel clusters when computing least squares solution to get rid off sectors of bad data; for field-tracking data set bad pixel clusters to NaN
  • Add detection limits (e.g. contrast curves)

To-do low priority

  • Add images and plots aimed at analysis of polarimetric data (R^2 scaling, AoLP arrows in polarized intensity or DoLP images, contrast curves etc.)
  • Add option to subtract DARK,BACKGROUND-frames if sky files are lacking (especially important for Ks; test effect first before completely implementing)
  • Add option for ‘stupid ADI’ for field-tracking data with derotator offset and option to subtract 180 deg rotated image if no derotator offset
  • Add warning if (part of the) data is taken at a low polarimetric efficiency, and perhaps make plot of efficiency vs file number
  • Make figures with sub-images horizontal, or make multiple lines of left and right images in a single figure
  • Add options for various methods to shift and rotate images (interpolate, ndimage-fourier, sci-image functions; similar to VIP)
  • When rotating images, make complete frame still visible to not cut out any parts of the data
  • Improve centering of non-coronagraphic data (center found depends a lot on first PSF and affects Qphi and Uphi images)
  • Test finding of satellite spots of center files when waffle pattern is ‘+’
  • Add weighted least-squares as option for model correction (depending on image quality or polarimetric efficiency)
  • Add multiprocessing for sigma filtering and centering of frames
  • Add option to scale the master sky frame to subtract from the object frames (especially for Ks; see also Gallicher et al. 2011)
  • Exclude saturated pixels in aperture to determine star polarization (same way as used in function fit_2d_gaussian)
  • Determine star polarization as a function of aperture radius
  • Add optional RDI for total intensity images
  • Make docstrings compliant with accepted conventions and create API doc on website