Zen

Translation

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>
3558/31800 · 3180

Sign in to save the translation.

English Catalan Actions
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 exoplanet 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, Siril 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
 
Creates a new image filled with zeros with a size of <b>width</b> x <b>height</b>.

The image is in 32-bit format, and it contains <b>nb_channel</b> channels, <b>nb_channel</b> being 1 or 3. It is not saved, but becomes the loaded image and it is displayed and can be saved afterwards
 
Replaces null values by <b>level</b> values. Useful before an idiv or fdiv operation, mostly for 16-bit images
 
Adds the constant <b>value</b> (specified in ADU) to the current image. This constant can take a negative value.

In 16-bit mode, values of pixels that fall outside of [0, 65535] are clipped. In 32-bit mode, no clipping occurs
 
Parses the string <b>str</b> using the information contained in the header of the image currently loaded. Main purpose of this command is to debug path parsing of header keys which can be used in other commands.
Option <b>-r</b> specifies the string is to be interpreted in read mode. In read mode, all wilcards defined in string <b>str</b> are used to find a file name matching the pattern. Otherwise, default mode is write mode and wildcards, if any, are removed from the string to be parsed.

If <b>str</b> starts with <i>$def</i> prefix, it will be recognized as a reserved keyword and looked for in the strings stored in gui_prepro.dark_lib, gui_prepro.flat_lib, gui_prepro.bias_lib or gui_prepro.stack_default for <i>$defdark</i>, <i>$defflat</i>, <i>$defbias</i> or <i>$defstack</i> respectively.
The keyword <i>$seqname$</i> can also be used when a sequence is loaded
 
Run the Photometric Color Correction on the loaded plate-solved image.

The limit magnitude of stars is automatically computed from the size of the field of view, but can be altered by passing a +offset or -offset value to <b>-limitmag=</b>, or simply an absolute positive value for the limit magnitude.
The star catalog used is NOMAD by default, it can be changed by providing <b>-catalog=apass</b> or <b>-catalog=gaia</b>. If installed locally, the remote NOMAD (the complete version) can be forced by providing <b>-catalog=nomad</b>
Background reference outlier tolerance can be specified in sigma units using <b>-bgtol=lower,upper</b>: these default to -2.8 and +2.0
 
Plate solve the loaded image.
If the image has already been plate solved nothing will be done, unless the <b>-force</b> argument is passed to force a new solve. If WCS or other image metadata is erroneous or missing, arguments must be passed:
the approximate image center coordinates can be provided in decimal degrees or degree/hour minute second values (J2000 with colon separators), with right ascension and declination values separated by a comma or a space (not mandatory for astrometry.net).
focal length and pixel size can be passed with <b>-focal=</b> (in mm) and <b>-pixelsize=</b> (in microns), overriding values from image and settings. See also options to solve blindly with local Astrometry.net

Images can be either plate solved by Siril using a star catalog and the global registration algorithm or by astrometry.net's local solve-field command (enabled with <b>-localasnet</b>).

The following options are common to both solvers:
Unless <b>-noflip</b> is specified, if the image is detected as being upside-down, it will be flipped.
For faster star detection in big images, downsampling the image is possible with <b>-downscale</b>.
The solve can account for distortions using SIP convention with polynomials up to order 5. Default value is taken form the astrometry preferences. This can be changed with the option <b>-order=</b> giving a value between 1 and 5.
When using Siril solver local catalogues or with local Astrometry.net, if the initial solve is not successful, the solver will search for a solution within a cone of radius specified with <b>-radius=</b> option. If no value is passed, the search radius is taken from the astrometry preferences. Siril near search can be disabled by passing a value of 0. (cannot be disabled for Astrometry.net).

The following options apply to Siril's plate solve only:
The limit magnitude of stars used for plate solving is automatically computed from the size of the field of view, but can be altered by passing a +offset or -offset value to <b>-limitmag=</b>, or simply an absolute positive value for the limit magnitude.
The choice of the star catalog is automatic unless the <b>-catalog=</b> option is passed: if local catalogs are installed, they are used, otherwise the choice is based on the field of view and limit magnitude. If the option is passed, it forces the use of the remote catalog given in argument, with possible values: tycho2, nomad, gaia, ppmxl, brightstars, apass.
If the computed field of view is larger than 5 degrees, star detection will be bounded to a cropped area around the center of the image unless <b>-nocrop</b> option is passed.

The following options apply to Astrometry.net solver only:
Passing options <b>-blindpos</b> and/or <b>-blindres</b> enables to solve blindly for position and for resolution respectively. You can use these when solving an image with a completely unknown location and sampling
Resolució astronòmica d'una seqüència. Es crearà una nova seqüència amb el prefix "ps_".
Si les imatges ja han estat resoltes astronòmicament, només es copiaran, llevat que s'indiqui l'argument <b>-platesolve</b> per forçar una nova resolució. Si les WCS o altres metadates d'imatges són errònies o falten, s'han de passar arguments:
es poden proporcionar les coordenades aproximades del centre de la imatge en graus decimals o valors de grau/hora minut segon (J2000 amb separadors de dos punts), amb valors d'ascensió recta i declinació separats per una coma o un espai (no és obligatori per a astrometry.net).
la distància focal i la mida dels píxels es poden passar amb <b>-focal=</b> (en mm) i <b>-pixelsize=</b> (en microns), sobreescrivint valors d'imatge i de configuració.

A no ser que <b>-noflip</b> sigui especificat, si les imatges es detecten cap per avall, seran girades.
Per a una detecció d'estels més ràpida en imatges grans, és possible reduir la mida de la imatge amb <b>-downscale</b>.

Les imatges es poden resoldre astronòmicament per Siril utilitzant un catàleg d'estels i l'algoritme de registre global o per astrometry.net amb l'ordre local de resolució de camps (habilitat amb <b>-localasnet</b>).
Les següents opcions s'apliquen només a la resolució de plaques de Siril.
La magnitud límit d'estels utilitzades per resoldre astronòmicament es calcula automàticament a partir de la mida del camp de visió, però es pot modificar passant un valor d'offset positiu o negatiu a <b>-limitmag=</b>, o simplement un valor positiu absolut per a la magnitud límit.
La selecció del catàleg d'estrelles és automàtica llevat que es passi l'opció <b>-catalog=</b>: si es tenen instal·lats catàlegs locals, s'utilitzen; en cas contrari, la selecció es basa en el camp de visió i la magnitud límit. Si es passa l'opció, es força l'ús del catàleg remot donat en argument, amb valors possibles: tycho2, nomad, gaia, ppmxl, brightstars, apass
This command evaluates the expression given in argument as in PixelMath tool. The full expression must be between double quotes and variables (that are image names, without extension, located in the working directory in that case) must be surrounded by the token $, e.g. "$image1$ * 0.5 + $image2$ * 0.5". A maximum of 10 images can be used in the expression.
Image can be rescaled with the option <b>-rescale</b> followed by <b>low</b> and <b>high</b> values in the range [0, 1]. If no low and high values are provided, default values are set to 0 and 1. Another optional argument, <b>-nosum</b> tells Siril not to sum exposure times. This impacts FITS keywords such as LIVETIME and STACKCNT
 
Generates an intensity profile plot between 2 points in the image, also known as a <i>cut</i>. The arguments may be provided in any order. The arguments <b>-to=x,y</b> and <b>-from=x,y</b> are mandatory.

The argument <b>-layer=<i>{red | green | blue | lum | col}</i></b> specifies which channel (or luminance or colour) to plot if the image is color. This can be used in conjunction with spectrometric options. It may also be used with the <b>-tri</b> option, which generates 3 parallel equispaced profiles each separated by <b>-spacing=</b> pixels, but note that for tri profiles the <i><b>col</b></i> option will be treated the same as <i><b>lum</b></i>.

The option <b>-cfa</b> selects CFA mode, which generates 4 profiles: 1 for each CFA channel in a Bayer patterned image. This option cannot be used with color images or mono images with no Bayer pattern, and cannot be used at the same time as the <b>-tri</b> option.

The option <b>-arcsec</b> causes the x axis to display distance in arcsec, if the necessary metadata is available. This option is overridden if spectrometric options are provided. If not provided or if metadata is not available, distance will be shown in pixel units.

The argument <b>-savedat</b> will cause the data files to be saved: the filename will be written to the log. Alternatively the argument <b>-filename=</b> can be used to specify a filename to write the data file to. (The <b>-filename=</b> option implies <b>-savedat</b>.)

<b>Spectrometric Options</b>

If spectrometric options are provided, all of the following must be provided: <b>-wavenumber1=</b> / <b>-wavelength1=</b> and <b>-wavenumber2=</b> / <b>-wavelength2=</b> specify 2 wavenumbers in cm<sup>-1</sup> / wavelengths in nm, and <b>-wn1=x,y</b> and <b>-wn2=x,y</b> specify points in the image corresponding to those wavenumbers. As a convenience, <b>-wavelength1=</b> and <b>-wavelength2=</b> may be used instead to provide wavelengths in nm. The following optional spectrometric arguments may be provided: <b>-width=</b>, which specifies how many pixels should be averaged perpendicular to the profile line, and one of <b>-xaxis=wavelength</b> or <b>-xaxis=wavenumber</b>, which set the units for the x axis (the default is wavelength).

The argument <b>"-title=<i>My Title"</i></b> sets a custom title "My Title"
 

Loading…

User avatar None

String updated in the repository

  1. Siril
  2. Siril Application
  3. Catalan
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>.
9 months ago
Browse all string changes

Things to check

Mismatched full stop

Source and translation do not both end with a full stop

Reset

XML syntax

The translation is not valid XML

Reset

Glossary

English Catalan
Pixel Size Siril
stars estels Siril
wavelength Siril

String information

Source string location
src/core/command_def.h:93
String age
9 months ago
Last updated
3 months ago
Source string age
9 months ago
Translation file
po/ca.po, string 2734