hvb356 (at) hotmail.de
NEW - Jan 2018
Ab nun können die Skripte von Hartmut Bornemann direkt in PixInsight geladen bzw. akualisiert werden.
Zurzeit funktioniert das Repository nur für das Betriebssystem Windows und OS X .
Für Linux/... Rechner können die Skripts händisch installiert werden. Eine Anleitung befindet sich am Anfang der Seite.
A new repository with PixInsight-scripts from Hartmut Bornemann ist ready. This repository keeps his scripts in your system automatically up to date.
Currently the repository works only under OS Windows/OS X.
Linux/... users can install the scripts manually. Please follow my instructions:
Install Scripts in PixInsight - Instruction - PDF - en
Im Folgenden wird beschrieben, wie man den Link zu diesem Repository in die Liste der vorinstallierten Repository einfügt. Bitte beachten Sie, dass der Verzeichnisname Groß- und Kleinschreibung unterscheidet.
The following describes, how to add the link to this repository into the list of pre-installed repositories. Please note, that that the Directory Name is case sensitive.
1) Add the link
http://www.skypixels.at/HVB_Repository/ to RESOURCES / Updates / Manage Repositories.
2) Schließe und öffne PixInsight um das automatische Update zu aktivieren oder gehe zu:
RESOURCES / Updates / Check for Updates.
Close and restart PixInsight to start the automatic update or go to:
RESOURCES / Updates / Check for Updates.
3. Die Skripte von Hartmut Bornemann sind somit installiert bzw. aktualisiert. Bei jedem Start von PixInsight wird automatisch auf aktuelle Versionen geprüft.
The scripts from Hartmut Bornemann are now up to date in your system. Every time you start PixInsight, it automatically checks for updates.
Liste der Skripte von Hartmut Bornemann. Die Skripte können auch einzeln installiert werden.
List of the Scripts by Hartmut Bornemann. The scripts can also be installed individually.
MaskGen creates binary masks with the Gaia catalog. The script requires a template as an astrometred image.
PSFImage can replace DynamicPSF and automate the creation of a PSF profile. The script is applied to a view or preview and generates a profile image for use in deconvolution. The criteria are the Moffat functions, the limitation of the amplitude and a setting for the sensitivity of the StarDetector.
All settings are saved. The result is displayed in the TextBox and commented on in the FITS header.
RGB color calibration
RGB color calibration of filtered CCD images is best done with a comparison of measured intensities of each frame to their band magnitude equivalent derived from magnitudes in photometric star catalogues. The calibration is finally expressed as the relation of the weights between R, G and B. The process therefore uses a reference channel (R) and calculates G and B relative weights, which are finally normalized to 1.The Script includes the PixInsight ColorCalibration process. Use with a linear RGB.
FitsDataView generates a table with FITS keys and statistical values from any number of FITS files. The table can be viewed with Preview. Via "Write csv-file" the table is stored as a file for further processing. With a double-click on the filename an image is created.
Narrow-band filters see use in astronomy to measure the intensity of emission
emitters. Since these filters have a range of bandwidth of around a few
nanometers (nm), errors from neighbouring sources will accumulate. For example,
a H-alpha-filter with 6nm bandwidth is receptive to the NII line with a
wavelength distance of 2nm. This is where the continuum subtraction (CS) helps
filter the emission out of the continuum. The resulting data can be used to
calculate the intensity of an object. In astro-photography, the addition of
the difference image onto a broadband channel generates a noticeable
amplification of the objects.
Updating JPEG metadata stored as Exif tags. For Exif see also Exchangeable Image File Format in public sources.
AdvStarmask is a suitable alternative to the PI-process StarMask. The script works without any parameter.
GAME ist ein grafisch interaktiver Editor für die Erstellung von elliptischen Abbildungen zur Maskierung von Galaxien. Die Maske kann beliebig viele Ellipsen verwalten. Sie wird aus dem aktiven Bild gewonnen. Jede Ellipse wird durch 5 Ankerpunkte bestimmt. Der zentrale Punkt dient zur Verschiebung und mit den peripheren Punkte kann die Kontur gedreht und gestreckt werden.
GAME is an interactive graphical Editor for the creation of elliptical shapes used for masking galaxies. The mask can handle various ellipsoids. The active window serves as the graphics base. An ellipsoid is defined by 5 anker points. The central point makes the move, while the peripheral points help rotate and scale the object.ContinuumSub.zip (2019)
Narrow-band filters see use in astronomy to measure the intensity of emission emitters. Since these filters have a range of bandwidth of around a few nanometers (nm), errors from neighbouring sources will accumulate. For example, a H-alpha-filter with 6nm bandwidth is receptive to the NII line with a wavelength distance of 2nm. This is where the continuum subtraction (CS) helps filter the emission out of the continuum. The resulting data can be used to calculate the intensity of an object. In astro-photography, the addition of the difference image onto a broadband channel generates a noticeable amplification of the objects.
A mighty utility to "blend" two images with selectable blending modes. Based on PixelMath blending Modes given by Juan Conejero in
( Forum ).
With the latest Formula by Gerald Wechselberger, one can create a perfect starmask. Simply select a view for the upper and lower image and open the "Starmask" overlay mode. Experimental presetting of both thresholds is required.
Advanced image sharpen using the MultiscaleLinearTransform process
1. Active window
2. Some ideas, how to raise or lower the bias in 4 layers
2DPlot draws the intensity of pixel values along a straight line. This imaginary line is made of x and y values which run normally in vertical or horizontal directions through a pixelmatrix of a selected image. Other standard line directions go diagonal up or down and can be chosen by checking the radio buttons in the left navigation window.
The button at the top flips between the curve graphics and a preview of the selected image. In the preview window, one can use a ruler styled 'cutting tool' for a more specific analysis. This ruler can start per mouse click at any location of the image and rotate by turning the wheel. A red line shown in the middle of the ruler marks the line of intersection.
Variations in data scaling help to compare channels in a color image or even different images. The 'Variable Range' checkbox should be deselected for this case.
Press the left mouse button down at any place in the graphics to show pixel coordinates and intensity.
Other options shown are self-explanatory.
For documentation purposes or further analysis of selected data, right click the mouse button. This will pop up a menu with two options Save Graphics and Save Intensities. Save Graphics saves the current graphics as shown while Save Intensities writes a CSV-file containing the index, x- and y-coordinates and the intensity.
Alternatively save the graphics by pressing Ctrl-C.
Copyright Â© Hartmut Bornemann, 2014, mailto:email@example.com
Searches the image with the highest signal-to-noise ratio from a selection of images. The name of the file with the best value can then be selected in the Image Integration as a reference image.
List SNR values of all views using SNREvaluation() - Previews included
Estimation of the signal-to-noise ratio function:
SNR(f,g) = E(f^2) / E((f - g)^2)
where f is a distribution function, g is a sample, and E(.) is the expected value of the argument. The denominator is the mean square error, which we approximate with the variance of the noise.
The SNR measures the power of a signal in relation to the power of noise. The ratio is a quality indicator. SNR calculates the value für the active image as an absolute number and also in decibels (db = 10 * log10(snr)), which is often better readable.
Improving contrast of small structures
SST implements the Section "High-Contrast, Small-Scale Structures" in Vicent Peris' tutorial https://pixinsight.com/tutorials/NGC7023-HDR/#First_Dynamic_Range_Compression
The script needs an existing RAW image, a copy of the linear RGB before delinearization. This RAW image is referenced in the dialog window. Before running SST.js, the active, nonlinear image must be compressed with the HDRWaveletTransform process. The effect of SST is controlled by the number of iterations.
Automatic BackgroundNeutralization and ColorCalibration
AutoColor substitutes the BackgroundNeutralization and ColorCalibration processes in a single step. The channel combined RGB becomes a calibrated image ready for further processing (narrowband, delinearization, luminance, ...).
A simple script to transform the active image into a non-linear form.
This script makes the following steps:
LinLRGB helps to create a linear LRGB. This script extracts a linear RGB into HSI components H and Si. These components are thereafter combined to HSI with the luminance L frame in place of I.
A routine to write a JPEG image without constraint.SwapChannel.zip (2012)
With SwapChannel a simple permutation of the channels is possible. The 3 RGB channels are shown with their indices 0;1;2. Substituting for example, for G the index 0, then green and red are reversed.
The script determines the background better than the Standard formula bg = 3 * median - 2 * mean. The values are listed as normalized and as a 16-bit value (Process Console).