Once any dark anomalies in the data have successfully been dealt with, operating the Wipe module is fairly straightforward.
To get started quickly, a number of presets cover some common scenarios;
Internally, the module's engine models three stages of calibration similar to an image stacker's calibration stages;
Any issues specified and/or detected are modelled during the correct stage and its results feeds into the next stage.
The Wipe module is able to detect horizontal or vertical banding and correct for this. Multiple modelling algorithms are available to detect and mitigate banding.
A defective sensor column repair feature is also available that attempts to recover data that was transposed but not lost, rather than interpolating or 'healing' it using neighbouring pixels.
The Wipe module is able to quickly match and model a natural illumination falloff model to your dataset with correction for cropping and off-axis alignment.
Wipe discerns gradient from real detail by estimating undulation frequency. In a nut shell, real detail tends to change rapidly from pixel to pixel, whereas gradients do not. The 'Aggressiveness' specifies the undulation threshold, whereby higher 'Aggressiveness' settings latch on to ever faster undulating gradients. At high 'Aggressiveness' settings, be mindful of Wipe not 'wiping' away any medium to larger scale nebulosity. To Wipe, larger scale nebulosity and a strong undulating gradients can look like the same thing. If you are worried about Wipe removing any larger scale nebulosity, you can designate an area off-limits to its gradient detection algorithm, by means of a mask that masks out that specific area. See the 'Sample revocation' section for more details.
Because Wipe's impact on the dynamic range in the image is typically very, very high, a (new) stretch of the data is almost always needed. This is so that the freed up dynamic range, previously occupied by the gradients,can now be put to good use to show detail. Wipe will return the dataset to its linear state, however with all the cleaning and calibration applied. In essence, this makes a global re-stretch using AutoDev or FilmDev is mandatory after using Wipe. From there, the image is ready for further detail recovery and enhancement, with color calibration preferably done as one of the last steps.
Because Wipe operates on the linear data (which is hard to see), a new, temporary automatic non-linear stretch is reapplied on every parameter change, so you can see what the module is doing. The diagnostics stretch is designed to show your dataset in the worst possible light on purpose, so you can diagnose issues and remedy them. The sole purpose of this stretch is to bring out any latent issues such as gradient, dust donuts, dark pixels. That is, it is entirely meant for diagnostics purposes inside the Wipe module and in no way, shape or form should be regarded as a suggested final global stretch.
If Compose mode is engaged (see Compose module), Wipe processes luminance (detail) and chrominance (colour) separately, yet simultaneously. If you process in Compose mode (which is recommended), you should check both the results for the luminance and chrominance portion of your image. Before keeping the result, the Wipe module will alert you to this once, if you have not done so.
The Stereo 3D module can be used to synthesise depth information based on astronomical image feature characteristics.
It is up to you how you wish to approach image processing.
Preset buttons can be distinguished by their icons; they bear the icon of the module you launched.
You can convert everything you see to a format you find convenient. Give it a try!