Changelog & to-do¶
Changelog¶
- v1.1.0 October 2019, R.G. van Holstein & J. Milli
- Added angular differential imaging (ADI) including principal component analysis (PCA) of total intensity images for pupil-tracking observations
- Added mean combination of ADI final images to command-line option
irdap --meancombine
- v1.0.0 September 2019, R.G. van Holstein & J. Milli:
- No backward compatibility with previous versions
- Added analysis of master flux frames 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
irdap --meancombine
to mean-combine final images of multiple observation blocks
- Added command-line option
- 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 possibility to not collapse data of pre-processing so that ADI can be done more accurately.
- Add possibility to crop images when doing ADI to save time
- Add possibility to use CENTER-frames with a different exposure time than the OBJECT-frames
- Create contrast curves of final PDI-and ADI-images
- 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
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