H18 windows

Versa H18 Window Micro Case. The image is for reference only. One standard mm rear fan is included. Built for Gamers. Easy Cable Management. Wiring tangled problem no longer exists with the cable routing gap, hiding cables behind motherboard tray to ensure smoothness for building the system as well as better airflow.

Significant faster. Main features: Native astrometric solver, command line compatible with PlateSolve2. Stacking astronomical images including dark frame and flat field correction. Filtering of deep sky images based on HFD value and average value. Alignment using an internal star match routine, internal astrometric solver.

Background equalizing. FITS thumbnail viewer. Results can be saved to 16 bit or float FITS files. FITS header edit. FITS crop function. Some pixel math functions and digital development process Can display images and tables from a multi-extension FITS. Blink routine. Stacking of images: Stacking of astronomical images is done to achieve a greater signal to noise ratio, prevent sensor saturation and correct the images for dark current and flat field. Additional imperfect images due to guiding, focus problems or clouds can be removed.

This is a screen short of the stack menu. It contains several tabs for the file list and settings. File can be sorted on quality and values. The image can be visually inspected in the viewer by a double click on the file or using the pop-up menu. Stacking methods: average and sigma-clipping-average.. Internal calculation using floating point numbers. Simple and intuitive user interface. Automatic saving of selected options and files.

Limited memory use, independent of the number of images stacked. Astrometric Solving: ASTAP can be used as astrometric solver to synchronise the telescope mount position with center position of an image taken with the telescope. Existing images can be solved to annotate, for photometry or the measure positions of unknown objects. The solution is not corrected for optical distortion, refraction, proper motion of stars and other minor effects all to be very minor.

The process astrometric solving is often referred to as a "plate solve". That was a correct description in the past, but in modern times there are no photographic plates involved in the process.

But they can be placed anywhere as long all files are in the same directory. The program is also a rpm package is available. The program and star databases are are provide as pkg file. The best stack option is "Sigma clip average". For only 2 or 3 images or when you are in a hurry or for testing "average"will do. Satellite tracks will not be removed. Astrometric image stitching mode Mosaic This will stitch astrometric tiles. Prior to this stack the images to tiles and check for clean edges.

If not use the "Crop each image function". For flat background apply artificial flat in tab pixel math 1 in advance if required. Adapt the mosaic canvas height and width if required, default is 2. Calibration and alignment of the files only Darks and flats will be applied. The images will be aligned to the reference image.

Calibration of the files only Darks and flats will be applied. Stacks based on filter will not be combined to RGB. This converson is called demosaic or debayer. First set Bayer pattern correctly by loading a raw image grayscale in the viewer and try one of the bayer patterns till the image colours match in viewer. Select the range which matches with the value of brightest stars. AstroM, white stars , as bilinear method but if there is an unbalance between the 4 red, 4 blue or 2 green pixels it uses luminance only.

Effective for unsampled images and stacks of a few images only. Star colour is lossed if undersampled but star will become white. Simple but very effective for astro images. Works best for a little oversampled images. Stars have very few artifact if any. Bilinear , a basic demosaic method using the colour information from a 3x3 pixel range. Star centering Comet centering No alignment. This can be done using the "calibration only"option in tab "stack method" and then executing the regular stack procedure.

Note that the measured star flux is compared and calibrated with the star database. For most cases you should install the V17 star database containing the Johnson-V magnitudes.

After stopping the cycle it is possible to measure any object using the mouse pointer. So the Gaia database should be the V17 which contains the calculated Johnson-V magnitudes.

The three stars are just measured against the Gaia Johnson-V database. Only two are required for the report. The you just need to select the variable star and a check star.

The third star 3 is just a bonus. From the up to calibration stars any outlier star is removed if it deviates more then 1. For the remaining stars the factors are averaged and used for flux calibration of the variable and check star..

So it is a different setup then usual but there is never lack of calibration stars. The curve area has a pop-up menu to save it to file or copy it to the clipboard. Inspector tab. It's done by calculating the best focus position for each image area. To do this it requires a series of images taken at several focuser positions. The routine will calculate from these images the best focus point of each area.

It will measure the median HFD values of each image and area and build a table HFD as function of the focuser position. Form this data, curve fitting will give the transfer fucntion and the best focus position expressed in focuser steps.

The focus point differences between the image areas will indicate the tilt of each area. The difference between the centrum and outer areas focus point will indicate the curvature. The usage is as follows: Prepare a series of short exposure images with different focuser positions and a lot of stars. Exposure time a few seconds.

Move for each image the focuser a small fixed step but only in one way to prevent backlash problems. Images with stars having an hfd above 20 will not be analysed correctly. Press curve fitting. The difference between the focus point of each image area will be reported in focuser steps.

The reported hfd values can be selected and copied for further analysis in a spreadsheet. Live stacking tab. All file s in the specified directory will be stacked live. If it is finished it will wait for new file s.

If a file is detected which is 0. You can save the stack results from the viewer menu. You can rename them back with the button at the bottom. Note there is no rejection of poor images.

Viewer, file menu If the program is associated with FITS image files or any other format, it will show the image as soon you click image file. If the program is started without parameters, you can open more instances.

Images can be loaded from the file menu or can be drag dropped on the main form. The images of MEF can be saved as a single image. The MEF tables can copied into the clipboard and paste to a spreadsheet.

Use the arrow key to move up or down or just click on the image. The current zoom and position is maintained so you could study the corner of a series images on image quality. This could be useful to browse your FITS files. By clicking on the thumbnail it will be opened in the viewer. The thumbnail size is depending on the form size. Make it larger, the thumbnails will follow. So the thumbnails are pretty big by purpose.

The images are fully loaded in memory so it will consume some memory and time. So don't try get thumbnails of images. Viewer popup menu: Add annotation, free text label at a x,y position. It can be connected via a line by first holding the right mouse button and moving the mouse away. See sample above. Persistent by annotation keyword in the FITS header. The annotation can be switched off in pulldown menu "View".

Remove by removing the annotation line in the header. If a is added to the text, the annotation is written persistent in the image data. So the image will be permanently altered after saving.

Adding two or more will increase the font size. Add marker, rectangle marker at x,y position. Draw the rectangle first by holding the right mouse button down and moving the mouse away. Add object position , Enabled after astrometric solve. Orange if a lock is possible, see above sample, red if not. Not persistent after image clean up. See above sample for orange star.

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