You should use the procedure below if your mount is one of these types:. This degradation is caused by statistical errors in reading out the number of electrons per pixel photosite. There is also a download area with some documentation there. More details to be filled in later. Using a DSLR at the prime focus of a Schmidt-Cassegrain scope, with its length of cm, we immediately note that its position just in front of the corrector plate creates an important obstruction, specially in scopes below mm of aperture.

Uploader: Kagatilar
Date Added: 13 August 2006
File Size: 19.55 Mb
Operating Systems: Windows NT/2000/XP/2003/2003/7/8/10 MacOS 10/X
Downloads: 93120
Price: Free* [*Free Regsitration Required]

What are Fastar and HyperStar?

CCDSoft autoguiding question – Software Bisque

At last, there is a tendency vsi CCD cameras using larger array sizes. Click Start when ready. In one generation, technology available to talented amateurs has done a giant leap! To set the active curve click the combo box and select the curve type: This allows you to see the raw data and motor indices in the curve.

At left, the increase of thermal noise with temperature of a CCD.

Not only CCDs are more efficient and larger but they also include automatic functions: If you want to refine again go back to step 3.

The purpose of PEC is to compensate for the mechanical imperfections in the RA motion of the telescope caused by imperfections in the drive. It is the subject of the next ccdsooft. Then the system let you select the the most sharp image.


If you have Upload changes immediately to mount checked then the active curve will be automatically sent whenever a change is made. Verify PE has been corrected by acquiring PE data again. These images are usually exposed about 1 s for bright objects and 10 s for the dimmer. Once the focus is achieved, remains to center the object, either in low resolution to increase de sensitivity or in full mode.

Polar Alignment Wizard Quickly, accurately, and easily helps you dial in polar alignment.

Shoestring Astronomy Support

So, use this feature at your own risk! Proceed with the installation.

Whenever you start Acquiring PE data PEMPro automatically re-synchronizes to the mount so this allows you the freedom to move the mount around without needing to re-synchronize. Backlash Exerciser Checks the backlash of your mount.

Software/hardware troubleshooting and workarounds

If seeing is bad dai can use longer exposures 2 seconds to tame the seeing. As explained previously, using such an accurate device as a CCD camera, you dramatize the stability of the instrument and it is mandatory to use a sturdy mount. On this tab you can make some useful modifications to the Active curve.

There is one to use multiple stars, and another to set the guiding parameters based on a plate-solved guider image.

That means that you need to take a dark frame at each ambient temperature level each time you use it. The mount must be well polar aligned and driven by an accurate system which errors are limited to a pixel.


No extra software is required. Its total length is cm depending on whether the accessories are thin or large. So prior taking your first CCD pictures of celestial bodies, a short calculation will be useful to check the accuracy of your CCD camera in combination with your optical system. Available for completeness but probably not useful unless using a Northern Hemisphere curve in the Southern Hemisphere or vice versa because the mount movement direction gets reversed in that case.

This is for this reason and for an image quality question too that the usage wants that amateurs work from LRGB images to get color composites instead of using color cameras. It allows you to assess the state of backlash of your mount. Click Create Refinement Curve. Using PEMpro to do periodic error correction turned out to be not as simple as it should be. For more details check out this section. If you are using the Video Interface then you must calibrate by clicking the Calibrate button.