Correction factor Barlow/Reducer
Seeing values FWHM
Focal length Guidescope

Binning Camera - Binning Guidecam

Focal length mm
Apparent field of view in degrees
Field apperture in mm

Vignetting calculation formula
Blend Simulation Graphics J/N


Focal length / Aperture Telescope
Aperture ratio without corrector

Main camera pixels x/y - Pixelsize x/y

Mag factor - FoV arcmins
Exit pupil

Current filter distance to chip
Diameter of filter or bottleneck

Effective focal length Telescope
Aperture ratio with corrector

Main camera pixel values with binning

Min. useful magnification
Max. useful magnification

Illumination of the corners in %
FoV & Illumination Preview

Useful focal length - Aperture ratio - Barlow
for planetary imaging

Target image scale range for act. seeing
Sampling for actual setup

min. useful wide-angle EP
max. useful tele-EP

Max. distance of bottleneck to
avoid vignetting on image

Telescope aperture in inch
Resolution of Telescope in arcsecs

Guide camera pixels x/y - Pixelsize x/y

Limiting magnitude of Telescope
Max imaging time without tracking

Guide camera pixel values with binning

Field Cam Rotation - Sim Cam Rotation
Field Orientation from Image

Opt. focal length of Guidescope
Max. focal length of Telescope

Mega-Pixel Maincam - Guidecam
Subpixel correction value

FoV Width  Height  Diagonal arcmins

Chip Width  Height  Diagonal mm

Implications of under-/over-sampling:

undersampling reduces the influence of guiding errors and improves signal to noise at the expense of finest detail

oversampling will require a good mount and careful guiding. OK for high magnification solar, lunar or planetary imaging. Might cause signal to noise issues with wide-field imaging

It is important to find a good balance between over- and undersampling. Namely so, that the camera still works as sensitive as possible, but the images are good shaded. The following figure illustrates graphically this relationship.


On the left the undersampling shows almost only square stars. On the right oversampling shows many shades of gray, but the light of the stars is smeared over many pixels.

Center of the picture is an example of good sampling. For deep sky imaging, the rule of thumb for the image scale is to achieve a value of about 1.5 arcsecs to 2 arcsecs per pixel. In this rule of thumb, the normal local seeing should be included. The seeing value is simply divided by 2.67 (low) or 2 (high) if you have local seeing on average of 4 arcseconds.



Yellow rectangle = FoV of selected chhip
Red outline = Vignetting
Green outline = FoV of selected eyepiece on telescope
White circle = Apparent moon size


1 = FWHM 0-1 Dream
2 = FWHM 1-2 Perfect
3 = FWHM 2-3 Very good
4 = FWHM 3-4 Good
5 = FWHM 4-5 Average
6 = FWHM 5-6 Average
7 = FWHM 6-7 Moderate
8 = FWHM 7-8 Bad
9 = FWHM 8-9 Very bad
10 = FWHM 9-10 Unusable
Camera Rotation by 90 degrees

AstroVis_Guide Donationware

The software can still be used without restrictions, but the author would be happy to receive a donation of any amount if you find the program useful. But also as compensation for the costs arising from the further development and hosting of the software.

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