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Computes and applies a linear function between a <b>reference</b> image and the loaded image.

The algorithm will ignore all reference pixels whose values are outside of the [<b>low</b>, <b>high</b>] range
104/2050 · 205

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Gets a value from the settings using its name, or list all with <b>-a</b> (name and value list) or with <b>-A</b> (detailed list)

See also SET to update values
 
Prints information about the reference image of the sequence given in argument. First image has index 0
 
Generalised hyperbolic stretch based on the work of the ghsastro.co.uk team.

The argument <b>-D=</b> defines the strength of the stretch, between 0 and 10. This is the only mandatory argument. The following optional arguments further tailor the stretch:
<b>B</b> defines the intensity of the stretch near the focal point, between -5 and 15;
<b>LP</b> defines a shadow preserving range between 0 and SP where the stretch will be linear, preserving shadow detail;
<b>SP</b> defines the symmetry point of the stretch, between 0 and 1, which is the point at which the stretch will be most intense;
<b>HP</b> defines a region between HP and 1 where the stretch is linear, preserving highlight details and preventing star bloat.
If omitted B, LP and SP default to 0.0 ad HP defaults to 1.0.
An optional argument (either <b>-human</b>, <b>-even</b> or <b>-independent</b>) can be passed to select either human-weighted or even-weighted luminance or independent colour channels for colour stretches. The argument is ignored for mono images. Alternatively, the argument <b>-sat</b> specifies that the stretch is performed on image saturation - the image must be color and all channels must be selected for this to work.
Optionally the parameter <b>[channels]</b> may be used to specify the channels to apply the stretch to: this may be R, G, B, RG, RB or GB. The default is all channels
 
Equalizes the mean intensity of RGB layers in the loaded CFA image. This is the same process used on flats during calibration when the option equalize CFA is used
 
Lists the available commands or help for one command
 
Calculates the histogram of the <b>layer</b> of the loaded image and produces file histo_[channel name].dat in the working directory.
layer = 0, 1 or 2 with 0=red, 1=green and 2=blue
 
Adds the image <b>filename</b> to the loaded image.
Result will be in 32 bits per channel if allowed in the preferences
 
Divides the loaded image by the image <b>filename</b>.
Result will be in 32 bits per channel if allowed in the preferences.

See also FDIV
 
Splits the loaded image in a nine-panel mosaic showing the image corners and the center for a closer inspection (GUI only)
 
Inverts a generalised hyperbolic stretch. It provides the inverse transformation of GHT, if provided with the same parameters, undoes a GHT command, possibly returning to a linear image. It can also work the same way as GHT but for images in negative
 
Inverts a midtones transfer function. It provides the inverse transformation of MTF, if provided with the same parameters, undoes a MTF command, possibly returning to a linear image. It can also work the same way as MTF but for images in negative
 
Inverts a modified arcsinh stretch. It provides the inverse transformation of MODASINH, if provided with the same parameters, undoes a MODASINH command, possibly returning to a linear image. It can also work the same way as MODASINH but for images in negative
 
Multiplies image <b>filename</b> by the loaded image.
Result will be in 32 bits per channel if allowed in the preferences
 
Subtracts the loaded image by the image <b>filename</b>.
Result will be in 32 bits per channel if allowed in the preferences, so capable of storing negative values. To clip negative value, use 16 bit mode or use the THRESHLO command
 
Analyses several stars with aperture photometry in a sequence of images and produces a light curve for one, calibrated by the others. The first coordinates, in pixels if <b>-at=</b> is used or in degrees if <b>-wcs=</b> is used, are for the star whose light will be plotted, the others for the comparison stars.
Alternatively, a list of target and reference stars can be passed in the format of the NINA exolpanet plugin star list, with the <b>-ninastars=</b> option. Siril will verify that all reference stars can be used before actually using them. A data file is created in the current directory named light_curve.dat, gnuplot plots the result to a PNG image if available
The ring radii for aperture photometry can either be configured in the settings or set to a factor of the reference image's FWHM if <b>-autoring</b> is passed.

See also SEQPSF for operations on single star
 
Computes and applies a linear function between a <b>reference</b> image and the loaded image.

The algorithm will ignore all reference pixels whose values are outside of the [<b>low</b>, <b>high</b>] range
L'algorisme ignorarà tots els píxels de referència el valor dels quals caigui fora del rang [baix, alt].
Same as CONVERT but converts only FITS files found in the current working directory. This is useful to avoid conversions of JPEG results or other files that may end up in the directory. The additional argument <b>-date</b> enables sorting files with their DATE-OBS value instead of with their name alphanumerically
 
Stretches the image linearly to a new black point BP.
The argument <b>[channels]</b> may optionally be used to specify the channels to apply the stretch to: this may be R, G, B, RG, RB or GB. The default is all channels.
Optionally the parameter <b>-sat</b> may be used to apply the linear stretch to the image saturation channel. This argument only works if all channels are selected
 
Process the provided image for live stacking. Only possible after START_LS. The process involves calibrating the incoming file if configured in START_LS, demosaicing if it's an OSC image, registering and stacking. The temporary result will be in the file live_stack_00001.fit until a new option to change it is added
 
Loads the image <b>filename</b> from the current working directory, which becomes the 'currently loaded image' used in many of the single-image commands.
It first attempts to load <b>filename</b>, then <b>filename</b>.fit, <b>filename</b>.fits and finally all supported formats.
This scheme is applicable to every Siril command that involves reading files
 
Computes and applies a logarithmic scale to the loaded image, using the following formula: log(1 - (value - min) / (max - min)), with min and max being the minimum and maximum pixel value for the channel
 
Lists files and directories in the working directory
 
Dumps metadata and statistics of the currently loaded image in JSON form. The file name is required, even if the image is already loaded. Image data may not be read from the file if it is the current loaded image and if the <b>-stats_from_loaded</b> option is passed. Statistics can be disabled by providing the <b>-nostats</b> option. A file containing the JSON data is created with default file name '$(FITS_file_without_ext).json' and can be changed with the <b>-out=</b> option
 
Generates a PSF for use with deconvolution, any of the three methods exposed by RL, SB or WIENER commands. One of the following must be given as the first argument: <b>clear</b> (clears the existing PSF), <b>load</b> (loads a PSF from a file), <b>save</b> (saves the current PSF), <b>blind</b> (blind estimate of tke PSF), <b>stars</b> (generates a PSF based on measured stars from the image) or <b>manual</b> (generates a PSF manually based on a function and parameters).

No additional arguments are required when using the <b>clear</b> argument.

To load a previously saved PSF the <b>load</b> argument requires the PSF <i>filename</i> as a second argument. This may be in any format that Siril has been compiled with support for, but it must be square and should ideally be odd.

To save a previously generated PSF the argument <b>save</b> is used. Optionally, a filename may be provided (this must have one of the extensions ".fit", ".fits", ".fts" or ".tif") but if none is provided the PSF will be named based on the name of the open file or sequence.

For <b>blind</b>, the following optional arguments may be provided: <b>-l0</b> uses the l0 descent method, <b>-si</b> uses the spectral irregularity method, <b>-multiscale</b> configures the l0 method to do a multi-scale PSF estimate, <b>-lambda=</b> provides the regularization constant.

For PSF from detected <b>stars</b> the only optional parameter is <b>-sym</b>, which configures the PSF to be symmetric.

For a <b>manual</b> PSF, one of <b>-gaussian</b>, <b>-moffat</b>, <b>-disc</b> or <b>-airy</b> can be provided to specify the PSF function, Gaussian by default. For Gaussian or Moffat PSFs the optional arguments <b>-fwhm=</b>, <b>-angle=</b> and <b>-ratio=</b> may be provided. For Moffat PSFs the optional argument <b>-beta=</b> may also be provided. If these values are omitted, they default to the same values as in the deconvolution dialog. For disc PSFs only the argument <b>-fwhm=</b> is required, which for this function is used to set the <i>diameter</i> of the PSF. For Airy PSFs the following arguments may be provided: <b>-dia=</b> (sets the telescope diameter), <b>-fl=</b> (sets the telescope focal length), <b>-wl=</b> (sets the wavelength to calculate the Airy diffraction pattern for), <b>-pixelsize=</b> (sets the sensor pixel size), <b>-obstruct=</b> (sets the central obstruction as a percentage of the overall aperture area). If these parameters are not provided, wavelength will default to 525nm and central obstruction will default to 0%. Siril will attempt to read the others from the open image, but some imaging software may not provide all of them in which case you will get bad results, and note the metadata may not be populated for SER format videos. You will learn from experience which are safe to omit for your particular imaging setup.

For any of the above PSF generation options the optional argument <b>-ks=</b> may be provided to set the PSF dimension, and the optional argument <b>-savepsf=<i>filename</i></b> may be used to save the generated PSF: a filename must be provided and the same filename extension requirements apply as for <b>makepsf save <i>filename</i></b>
Genera una PSF per a utilitzar amb la deconvolució. Un dels següents s'ha de proporcionar com a primer argument: <b>clear</b> (esborra la PSF existent), <b>load</b> (carrega una PSF des d'un fitxer), <b>save</b> (desa la PSF actual), <b>blind</b> (estimació cega de la PSF), <b>stars</b> (genera una PSF basada en estrelles mesurades de la imatge) o <b>manual</b> (genera una PSF manualment a partir d'una funció i paràmetres).

No són necessaris arguments addicionals quan s'utilitza l'argument <b>clear</b>.

Per carregar una PSF prèviament desada, l'argument <b>load</b> requereix el <filename> de la PSF com a segon argument. Això pot ser en qualsevol format amb el qual Siril hagi estat compilat amb suport, però ha de ser quadrada i preferentment senar.

Per desar una PSF generada prèviament, s'utilitza l'argument <b>save</b>. Opcionalment, es pot proporcionar un nom de fitxer (aquest ha de tenir una de les extensions ".fit", ".fits", ".fts" o ".tif"), però si no se'n proporciona cap, la PSF s'anomenarà en funció del nom del fitxer o seqüència oberta.

Per a <b>blind</b>, es poden proporcionar els següents arguments opcionals: <b>-l0</b> utilitza el mètode de descens l0, <b>-si</b> utilitza el mètode d'irregularitat espectral, <b>-multiscale</b> configura el mètode l0 per fer una estimació de PSF de múltiples escales, <b>-lambda=</b> proporciona la constant de regularització.

Per a PSF a partir d'<b>estels</b> detectats l'únic paràmetre opcional és <b>-sym</b>, que configura la PSF perquè sigui simètrica.

Per a una PSF <b>manual</b>, es pot proporcionar un dels següents arguments: <b>-gaussian</b>, <b>-moffat</b>, <b>-disc</b> o <b>-airy</b>, per especificar la funció de la PSF, sent la Gaussiana la predeterminada. Per a les PSF Gaussianes o de Moffat, es poden proporcionar els arguments opcionals <b>-fwhm=</b>, <b>-angle=</b> i <b>-ratio=</b>. Per a les PSF de Moffat, també es pot proporcionar l'argument opcional <b>-beta=</b>. Si aquests valors s'ometen, els valors per defecte seran els mateixos que en el diàleg de deconvolució. Per a les PSF de disc només és necessari l'argument <b>-fwhm=</b>, que en aquesta funció s'utilitza per establir el diàmetre de la PSF. Per a les PSF de l'Airy, es poden proporcionar els següents arguments: <b>-dia=</b> (estableix el diàmetre del telescopi), <b>-fl=</b> (estableix la longitud focal del telescopi), <b>-wl=</b> (estableix la longitud d'ona per calcular el patró de difracció d'Airy), <b>-pixelsize=</b> (estableix la mida de píxel del sensor), <b>-obstruct=</b> (estableix l'obstrucció central com a percentatge de l'àrea total de l'obertura). Si no es proporcionen aquests paràmetres, la longitud d'ona serà per defecte de 525 nm i l'obstrucció central serà per defecte del 0%. Siril intentarà llegir els altres paràmetres de la imatge oberta, però alguns programari d'imatge pot no proporcionar tots ells, en què obtindreu resultats incorrectes, i tingueu en compte que les metadades potser no estiguin disponibles per als vídeos en format SER. Amb l'experiència aprendreu quins paràmetres podeu ometre de forma segura per a la vostra configuració d'imatge en particular.

Per a qualsevol de les opcions de generació de PSF esmentades anteriorment, es pot proporcionar l'argument opcional <b>-ks=</b> per establir la dimensió de la PSF, i l'argument opcional <b>-savepsf=<i>filename</i></b> es pot utilitzar per desar la PSF generada: s'ha de proporcionar un nom de fitxer i s'apliquen els mateixos requisits d'extensió de fitxer que amb <b>makepsf save <i>filename</i></b>.
Merges several sequences of the same type (FITS images, FITS sequence or SER) and same image properties into a new sequence with base name <b>newseq</b> created in the current working directory, with the same type. The input sequences can be in different directories, can specified either in absolute or relative path, with the exact .seq name or with only the base name with or without the trailing '_'
 
Flips the loaded image about the horizontal axis. Option <b>-bottomup</b> will only flip it if it's not already bottom-up
 
Flips the image about the horizontal axis, only if needed (if it's not already bottom-up). It takes the image file name as argument, allowing it to avoid reading image data entirely if no flip is required. Image is overwritten if a flip is made
 
Flips the image about the vertical axis
Encaixa la imatge a la finestra
Modified arcsinh stretch based on the work of the ghsastro.co.uk team.

The argument <b>-D=</b> defines the strength of the stretch, between 0 and 10. This is the only mandatory argument. The following optional arguments further tailor the stretch:
<b>LP</b> defines a shadow preserving range between 0 and SP where the stretch will be linear, preserving shadow detail;
<b>SP</b> defines the symmetry point of the stretch, between 0 and 1, which is the point at which the stretch will be most intense;
<b>HP</b> defines a region between HP and 1 where the stretch is linear, preserving highlight details and preventing star bloat.
If omitted LP and SP default to 0.0 ad HP defaults to 1.0.
An optional argument (either <b>-human</b>, <b>-even</b> or <b>-independent</b>) can be passed to select either human-weighted or even-weighted luminance or independent colour channels for colour stretches. The argument is ignored for mono images. Alternatively, the argument <b>-sat</b> specifies that the stretch is performed on image saturation - the image must be color and all channels must be selected for this to work.
Optionally the parameter <b>[channels]</b> may be used to specify the channels to apply the stretch to: this may be R, G, B, RG, RB or GB. The default is all channels
 
Applies midtones transfer function to the current loaded image.

Three parameters are needed, <b>low</b>, <b>midtones</b> and <b>high</b> where midtones balance parameter defines a nonlinear histogram stretch in the [0,1] range. For an automatic determination of the parameters, see AUTOSTRETCH.
Optionally the parameter <b>[channels]</b> may be used to specify the channels to apply the stretch to: this may be R, G, B, RG, RB or GB. The default is all channels
 
Changes pixel values of the currently loaded image to a negative view, like 1-value for 32 bits, 65535-value for 16 bits. This does not change the display mode
 

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  1. Siril
  2. Siril Application 1.2
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Computes and applies a linear function between a <b>reference</b> image and the loaded image.

The algorithm will ignore all reference pixels whose values are outside of the [<b>low</b>, <b>high</b>] range
L'algorisme ignorarà tots els píxels de referència el valor dels quals caigui fora del rang [baix, alt].
9 months ago
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Source string location
src/core/command_def.h:76
String age
9 months ago
Last updated
3 months ago
Source string age
9 months ago
Translation file
po/ca.po, string 2231