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:commandname:`unclipstars` |scriptable| |indexlink|
Re-profiles clipped stars of the loaded image to desaturate them, scaling the output so that all pixel values are <= 1.0
:commandname:`unselect` |scriptable| |indexlink|
Allows easy mass unselection of images in the sequence **sequencename** (from **from** to **to** included). See SELECT
Links: :ref:`select <select>`
:commandname:`unsetmag` |nonscriptable| |indexlink|
Resets the magnitude calibration to 0. See SETMAG
Links: :ref:`setmag <setmag>`
:commandname:`unsharp` |scriptable| |indexlink|
Applies an unsharp mask, actually a Gaussian filtered image with sigma **sigma** and a blend with the parameter **amount** used as such: out = in \* (1 + amount) + filtered \* (-amount).
See also GAUSS, the same without blending
Links: :ref:`gauss <gauss>`
:commandname:`visu` |nonscriptable| |indexlink|
Displays the loaded image with **low** and **high** as the low and high threshold, GUI only
:commandname:`wavelet` |scriptable| |indexlink|
Computes the wavelet transform of the loaded image on (**nbr_layers**\ =1...6) layer(s) using linear (**type**\ =1) or bspline (**type**\ =2) version of the 'à trous' algorithm. The result is stored in a file as a structure containing the layers, ready for weighted reconstruction with WRECONS.
See also EXTRACT
Links: :ref:`wrecons <wrecons>`, :ref:`extract <extract>`
:commandname:`wiener` |scriptable| |indexlink|
Restores an image using the Wiener deconvolution method.
Optionally, a PSF created by MAKEPSF may be loaded using the argument **-loadpsf=\ filename**.
The parameter **-alpha=** provides the Gaussian noise modelled regularization factor
:commandname:`wrecons` |scriptable| |indexlink|
Reconstructs to current image from the layers previously computed with wavelets and weighted with coefficients **c1**, **c2**, ..., **cn** according to the number of layers used for wavelet transform, after the use of WAVELET
Links: :ref:`wavelet <wavelet>`
Dynamic PSF
This section describes the two essential steps which are undertaken to detect stars in individual frames. The detection on a single image can be run or fine-tuned using :menuselection:`Burger Menu --> Image Information --> Dynamic PSF` or with shortcut :kbd:`Ctrl` + :kbd:`F6`.
dialog
Dynamic PSF running on a deep sky image.
The process is as follows:
make an initial detection of potential star candidates

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  1. Siril
  2. User documentation 1.2
  3. English
Computes the wavelet transform of the loaded image on (**nbr_layers**\ =1...6) layer(s) using linear (**type**\ =1) or bspline (**type**\ =2) version of the 'à trous' algorithm. The result is stored in a file as a structure containing the layers, ready for weighted reconstruction with WRECONS.
Computes the wavelet transform of the loaded image on (**nbr_layers**\ =1...6) layer(s) using linear (**type**\ =1) or bspline (**type**\ =2) version of the 'à trous' algorithm. The result is stored in a file as a structure containing the layers, ready for weighted reconstruction with WRECONS.
9 months ago
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Source string location
../siril-doc/doc/processing/atrouwavelets.rst:0 • ../siril-doc/doc/commands/wavelet.rst:1
String age
9 months ago
Last updated
3 months ago
Source string age
9 months ago
Translation file
po/siril-documentation.pot, string 668