SXVR-M26C handbook.pdf - Starlight Xpress

Handbook for the SXVR-M26C Issue 1 March 2010 

The SXVR-M26C one-shot colour CCD camera 

Thank you for purchasing a Starlight Xpress CCD camera. We hope that you will be 

very satisfied with the results. 

The SXVR-M26C is an advanced, high-resolution one-shot colour cooled CCD 

camera, especially designed for astronomical imaging. It incorporates a built-in, fully 

programmable, USB 2 super-fast computer interface, an autoguider control port and 

output and optional integrated dual serial ports for filter wheel and telescope control. 

It also includes a CCD temperature monitoring circuit which provides regulated setpoint 

cooling of the chip and a substantial reduction in overall size. 

The SXVR-M26C uses a Sony ICX493AK ‘Super HAD’ interlaced scan CCD, with 

3900 x 2616 x 6.05uM pixels in a 23.5 x 15mm active area. Super HAD devices have 

excellent quantum efficiency, with a broad spectral response peaking at around 60% 

in the green, and an extremely low dark current, well below that of any comparable 

CCD currently available. The ICX493AK has a ‘Bayer Matrix’ of Red, Green and 

Blue filters integrated onto the CCD surface and the colour data that is encoded into 

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the output image, can be used to recreate a high quality colour picture when processed 

by suitable software. 

The full-frame download time is approximately 10 seconds and a binned 4x4 

download takes only 3 seconds, so finding and centring are very quick and easy in this 

mode. 

Please take a few minutes to study the contents of this manual, which will help you to 

get the camera into operation quickly and without problems. I am sure that you want 

to see some results as soon as possible, so please move on to the ‘Quick Start’ section, 

which follows. A more detailed description of imaging techniques will be found in a 

later part of this manual. 

‘Quick Starting’ your SXVR-M26C system 

In the shipping container you will find the following items: 

1) The SXVR-M26C camera head. 

2) A universal AC power supply module. 

3) A USB camera cable. 

4) An adaptor for 2” drawtubes and M42 Pentax thread lenses. 

5) A guider output to guider port lead. 

6) A disk with the SXVR-M26C control software and this manual. 

Optional extra items include: 

1) A serial port adaptor and cable. 

2) An add-on guide camera head. 

You will also need a PC computer with Windows 7 or Windows XP installed. This 

machine must have at least one USB 2.0 port available and at least 256 Mbytes of 

memory. If you intend to view the finished images on its screen, then you will also 

need a graphics card capable of displaying an image with a minimum of 1024 x 768 

pixels and 65,000 colours. A medium specification 2 core Pentium with between 

1GHz and 4GHz processor speed is ideal. Please note that USB 2.0 operates at a very 

high speed and cannot operate over very long cables. Five metres of good quality 

cable is the maximum normally possible without boosters or extra powered hubs. 

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Installing the USB system: 

First, find a free USB socket on your PC and plug in the USB cable (do not connect 

the camera at this time). If you do not have a USB2 capable computer, it is normally 

possible to install a USB 2 card into an expansion slot. 

The next operation is to run the software installer from the CD ROM provided. Insert 

the CD into the computer and wait for Windows Explorer to open with the list of 

folders on the ROM. Now find the SXVR-M26C folder and run the SETUP.EXE file 

that it contains – this will initiate the self-install software which will guide you 

through the process of installing the SX camera software (SXV_M26C_usb.exe) onto 

your computer. 

Now connect the USB cable to the socket on the camera rear panel. 

Windows will report ‘Found new hardware’ and will ask for the location of the 

drivers. Point the installer at your CD ROM and the driver installation should proceed 

smoothly. (Ignore any warnings about the driver having not been tested by Microsoft). 

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At the end of this process, the USB interface will be installed as a ‘BlockIOClass 

device’ and the camera software will be able to access it. You can confirm that the 

installation is complete by checking the status of the USB devices in the Windows 

‘Device Manager’ (see above). Start up the Windows ‘Control Panel’ and select 

‘System’. Now click on the tab labelled ‘Device Manager’, ‘Hardware’, and all of the 

system devices will be displayed in a list (see above). If the installation is successful, 

there will be a diamond shaped symbol labelled ‘BlockIOClass’ and clicking on the 

‘+’ sign will reveal it to be a ‘Starlight Xpress USB 2.0 SXV-M26C BlockIO camera 

driver’. If this device shows as faulty, try clicking on it and selecting ‘properties’ and 

then ‘update driver’. Following the on screen instructions will allow you to re-select 

the correct inf file (SXVIO_M26C_325.inf) and driver files (SXVIO.sys and 

generic.sys), which should fix the problem. 

Now connect up the power supply and switch it on. The supply is a very efficient 

‘switch mode’ unit, which can operate from either 110v or 220v AC via an 

appropriate mains power cable (supplied). You can now start the ‘SXV_M26C_usb’ 

software by double clicking on the icon when you should see the main menu and 

image panel appear. If this is the first time that it has been run, you will receive a 

warning about the lack of an ‘ini’ file – just click on ‘OK’ and then open ‘Set program 

defaults’ from the ‘File’ menu. In the bottom right hand corner of this box, click on 

‘Save’ and the ini file will be created and the software set up for your camera. 

Now click on the camera icon at the top of the screen. If the USB connection is OK, a 

message box will inform you of the ‘Handle’ number for the SXVIO interface and 

various other version details etc. Click ‘OK’ and the main camera control panel will 

now be seen. 

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As can be seen above, there is a CCD temperature monitoring window at the right 

hand side of the panel. At switch-on, this will default to full power cooling with an 

end point of -40C and, needless to say, this is rather extreme. I recommend changing 

the set point to about -10C for normal use, but you can go much colder if you are 

imaging during the winter months. Under indoor conditions, the low airflow will limit 

the cooling capability, and you should use a set point of no lower than -5C for stable 

cooling. You can determine the optimum settings for your camera and ambient 

conditions when you have some experience of using the system, but do not try to 

operate at extreme cooling when the air temperature is high or the flow is poor. 

Recording your first image: 

We now have the camera and computer set up to take pictures, but an optical system 

is needed to project an image onto the CCD surface. You could use your telescope, 

but this introduces additional complications, which are best avoided at this early 

stage. There are two simple options, one of which is available to everyone with a 

sheet of aluminium baking foil: 

1) Attach a standard ‘M42’ SLR camera lens to the SXVR-M26C, using the 26mm 

spacer to achieve the correct focal distance. 

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Or 

2) Create a ‘Pin hole’ lens by sticking a sheet of aluminium baking foil over the end 

of the adaptor and pricking its centre with a small pin. 

If you use a normal lens, then stop it down to the smallest aperture number possible, 

(usually F22), as this will minimise focus problems and keep the light level 

reasonable for daytime testing. The pin hole needs no such adjustments and will work 

immediately, although somewhat fuzzily! It is also helpful to use an infrared blocking 

filter, if you have one. This gives much better daylight colour rendering. 

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Point the camera + lens or pinhole towards a well-lit and clearly defined object some 

distance away. Now enter the ‘File’ menu in the SXV_M26C software and click on 

‘SX camera interface’. Select ‘High Resolution’ mode and an exposure time of 0.1 

seconds, then press ‘Take Photo’. 

After the exposure and download have completed (about 10 seconds) an image of 

some kind will appear on the computer monitor. It will probably be poorly focused 

and incorrectly exposed, but any sort of image is an indication of success! In the case 

of the pinhole, all that you can experiment with is the exposure time, but a camera 

lens can be adjusted for good focus and so you might want to try this to judge the high 

image quality that it is possible to achieve. 

Various other exposure options are available, as can be seen in the picture above. For 

example, you can ‘Bin’ the download 2x2, or more, to achieve greater sensitivity and 

faster download, or enable ‘Continuous mode’ to see a steady stream of images. 

‘Focus mode’ downloads a 128 x 128 segment of the image at high speed. The initial 

position of the segment is central to the frame, but can be moved by selecting ‘Focus 

frame centre’ in the ‘File’ menu and clicking the desired point with the mouse. The 

focus window has an adjustable ‘contrast stretch’, controlled by the 12-16 bit slider. 

The image will be ‘normal’ if 16 bits is selected, while setting lower values will 

increase the image brightness in inverse proportion. 

If you cannot record any kind of image, please check the following points: 

1) Ensure that the power indicator lamp is on and that the cables are properly home 

in their sockets. 

2) If the screen is completely white, the camera may be greatly overexposed. Try a 

shorter exposure time, or stop down your lens. See if covering the lens causes the 

image to darken. 

3) If the USB did not initialise properly, the camera start-up screen will tell you that 

the connection is defective. Try switching off the power supply and unplugging the 

USB cable. Now turn the power supply on and plug in the USB cable. This will reload 

the USB software and may fix the problem after restarting the 

SXV_M26C_usb program. Otherwise, check the device driver status, as previously 

described, and re-install any drivers which appear to be defective. You might also 

try checking the ‘Ignore VID/PID’ box in ‘Set program defaults’. 

4) If you cannot find any way of making the camera work, please try using it with 

another computer. This will confirm that the camera is OK, or faulty, and you can 

then decide how to proceed. Our guarantee ensures that any electrical faults are 

corrected quickly and at no cost to the customer. 

Converting your images to colour: 

The images from your camera are monochrome at the moment and they need to be 

converted into true colour before enhancing them. Any processing of the image, other 

than calibration with dark frames etc., will distort the colour rendering of the result 

and so the conversion needs to be done before proceeding. Important! please note 

that you cannot sum frames together before colour conversion. This must be done 

after the images have been colour converted. 

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Here is a small enlarged section of a daylight image which may be similar to your test 

image taken with a 50mm camera lens 

The visible grid encodes the colour information within the image data and will now be 

used to decode the red, green and blue image planes into a colour picture. To do this, 

open the ‘Colour’ header tag where you will see the ‘Synthesize colour image’ option. 

Click on this to open the colour synthesis control panel. 

The synthesis control panel contains several options for correcting colour bias and 

noise. 

1) Daylight Image? – If an unfiltered lens is used, the infra-red content of the 

light will tend to produce a Green – Blue shift in the balance. A partial 

correction of this bias is provided by selecting this option, but the best option 

is to use an infra-red blocking filter when taking daylight shots (see 5 below). 

2) Light Pollution Correction: - This option is for deep sky colour images, 

where a strong colour bias is often present in the sky background. This option 

attempts to return the background colour to a neutral grey. 

3) Colour Smoothing Filter: - Applies a low pass filter to the colour data to 

smooth out colour noise. 

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4) Apply Anti-Alias: - Runs a special filter over the colour data to remove 

coloured artefacts around sharp edges. This is especially useful for cleaning up 

erratically coloured star images. 

5) IR Filter Used? – Sets the colour balance to allow for the loss of infra-red 

content when using an IR blocking filter. 

6) Stretching: - A selection of contrast-boosting options which are preset for 

various subjects. 

7) Remove Background: - This option will adjust the sky background brightness 

to give an optimum background level. 

8) High Pass filters: - Automatically sharpen the luminance data to emphasise 

fine details. Most useful for sharpening planetary images but will also increase 

the noise content. 

I suggest that you switch on the Colour smoothing filter and the Anti-alias filter – you 

can experiment with the other options as you gain more experience. Now click on 

‘Create image’ and you should see that the grid pattern disappears and is replaced by 

colour image data. 

If the colour is roughly correct, then all is well. However, the colour decoding is 

reliant on the filter pattern being properly registered with the processing software and 

this can vary. If the colour is badly wrong, try opening the ‘Set program defaults’ 

dialog box and altering the ‘Pixel’ and ‘Line’ offsets. Reload the raw file and try 

synthesis again. If it’s still not right, experiment with just a pixel offset or just a line 

offset until the colour is good. 

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There is every reason to expect that the image will be reasonably well colour 

balanced, but if it is not, you can adjust the colour in the ‘Set Colour Balance’ dialog 

box (Under ‘Colour’ in the main menu). 

The colour balance controls seem complex, but are really quite easy to use. The most 

useful controls are the ‘Start’ and ‘Saturation Factor’ settings. Saturation factor will 

simply vary the colour intensity, without any alteration of the colour balance, but the 

‘Start’ settings for each colour will alter the colour rendering of the dimmer parts of 

the image. As most astronomical images are badly affected by light pollution, which 

affects the dimmer background colours in particular, the start point settings are 

particularly helpful for correcting this. If you move the start point of the Red 

histogram a few points to the right and click on ‘Apply’, the new image will have 

LESS red in the background and will appear more Cyan. Similarly, if you move the 

Green start point to the right, the image will appear more Magenta and moving the 

blue start point will turn it more Yellow. Do not move the start points beyond the start 

of the main burst of histogram data, or you will introduce colour errors into low 

saturation parts of the image. Just move the sliders by small amounts in the clear area 

below the main peak, until the background is nicely balanced. 

In some cases, the histograms may all start a long way above zero (usually in astro. 

images with a lot of light pollution). In this case, slide the start point settings for all 

colours until they are equally distant from the beginning of the colour data, but quite 

close to it. This will both correct the colour balance (apart from any fine tweaks) and 

increase the colour saturation. 

In some images, the colour data may be balanced differently in the highlights and 

shadows. For example, the dark areas may be quite neutral in colour, but the 

highlights may be bluish in tint. This indicates a ‘slope error’ in one or more colours 

and, in this example it is caused by the blue data increasing too quickly when 

compared with the red and green data. To correct for this, the other histogram sliders 

may be used as slope adjusters. In the case of the excess blue, try increasing the top 

end (Max) value to greater than 255 (300 max is allowed). This will reduce the blue 

slope and result in a more yellowish rendition. Alternatively, you can increase both 

the red and green slopes by setting the upper red and green sliders below 255. 

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Image enhancements: 

Your first image may be satisfactory, but it is unlikely to be as clear and sharp as it 

could be. Improved focusing and exposure selection may correct these shortcomings, 

and you may like to try them before applying any image enhancement with the 

software. However, there will come a point when you say, “That’s the best that I can 

get” and you will want to experiment with the effects of image processing. In the case 

of daylight images, the processing options are many, but there are few that will 

improve the picture in a useful way. The most useful of these are the ‘Normal 

Contrast Stretch’ and the ‘High Pass Low Power’ filter. The high pass filter gives a 

moderate improvement in the image sharpness, and this can be very effective on 

daylight images. 

Too much high pass filtering results in dark borders around well-defined features and 

will increase the noise in an image to unacceptable levels, but the Low Power filter is 

close to optimum and gives a nicely sharpened picture. 

The ‘Contrast’ routines are used to brighten (or dull) the image highlights and 

shadows. A ‘Normal’ stretch is a simple linear operation, where two pointers (the 

‘black’ and ‘white’ limits) can be set at either side of the image histogram and used to 

define new start and end points. The image data is then mathematically modified so 

that any pixels that are to the left of the ‘black’ pointer are set to black and any pixels 

to the right of the ‘white’ pointer are set to white. The pixels with values between the 

pointers are modified to fit the new brightness distribution. Try experimenting with 

the pointer positions until the image has a pleasing brightness and ‘crispness’. 

At this point, you will have a working knowledge of how to take and process an 

SXVR-M26C image. It is time to move on to astronomical imaging, which has its 

own, unique, set of problems! 

********************************************************************* 

Astronomical Imaging with the SXVR-M26C 

1) Getting the image onto the CCD: 

It is fairly easy to find the correct focus setting for the camera when using a standard 

SLR lens, but quite a different matter when the SXVR-M26C is attached to a 

telescope! The problem is that most telescopes have a large range of focus adjustment 

and the CCD needs to be quite close to the correct position before you can discern 

details well enough to optimise the focus setting. An additional complication is the 

need to add various accessories between the camera and telescope in order that the 

image scale is suitable for the subject being imaged and (sometimes) to include a ‘flip 

mirror’ finder unit for visual object location. 

A simple, but invaluable device, is the ‘par-focal eyepiece’. This is an eyepiece in 

which the field stop is located at the same distance from the barrel end, as the CCD is 

from the camera barrel end. 

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When the par-focal eyepiece is fitted into the telescope drawtube, you can adjust the 

focus until the view is sharply defined and the object of interest is close to the field 

centre. On removing the eyepiece and fitting the CCD camera, the CCD will be very 

close to the focal plane of the telescope and should record the stars etc. well enough 

for the focus to be trimmed to its optimum setting 

Several astronomical stores sell adjustable par-focal eyepieces, but you can also make 

your own with a minimum of materials and an unwanted Kellner or Plossl ocular. 

Just measure a distance of 22mm from the field stop of the eyepiece (equivalent to the 

CCD to adaptor flange distance of the camera) and make an extension tube to set the 

field stop at this distance from the drawtube end. Cut-down 35mm film cassette 

containers are a convenient diameter for making the spacer tube and may be split to 

adjust their diameter to fit the drawtube. 

It is necessary to set up a good optical match between your camera and the telescope. 

Most SCTs have a focal ratio of around F10, which is too high for most deep sky 

objects and too low for the planets! This problem is quite easy to overcome for small 

CCDs, if you have access to a focal reducer (for deep sky) and a Barlow lens for 

planetary work. However, the CCD in the M26C is too large to be fully illuminated 

by most standard SCT scopes, and you may not be able to take satisfactory images 

with such an instrument. One very successful option that may be open to you is to fit a 

‘Hyperstar’ lens (supplied by ‘Starizona’) in place of the secondary mirror. The 

hyperstar turns your SCT into an F2 wide field astrograph and the latest versions (type 

III at the time of writing) will fully illuminate the chip of the SXVR-M26C. The 

hyperstar optic creates a very fast, wide-field system which is ideal for large nebulae 

and star fields etc. Another very good option is to use a well-corrected refractor, such 

as an FSQ106. These superb instruments give pin-point stars over a very wide field 

and are an ideal match to the M26C. 

As a general guide, most CCD astronomers try to maintain an image scale of about 2 

arc seconds per pixel for deep sky images. This matches the telescope resolution to 

the CCD resolution and avoids ‘undersampling’ the image, which can result in square 

stars and other unwanted effects. To calculate the focal length required for this 

condition to exist, you can use the following simple equation: 

F = Pixel size * 205920 / Resolution (in arc seconds) 

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In the case of the SXVR-M26C and a 2 arc seconds per pixel resolution, we get 

F = 0.00605 * 205920 / 2 = 622mm 

For a 200mm SCT, this is an F ratio of 622 / 200 = F3.11, which is rather less than 

can be achieved with a standard converter and appropriate extension tube. However, 

moderate deviations from this focal length will not have a drastic effect and so any F 

ratio from about F4.5 to F6.3 will give good results. 

The same equation can be used to calculate the amplification required for good 

planetary images. However, in this case, the shorter exposures allow us to assume a 

much better telescope resolution and 0.25 arc seconds per pixel is a good value to use. 

The calculation now gives the following result: 

F = 0.00605 * 205920 / 0.25 = 4976mm 

This is approximately F27 when used with a 200mm SCT and so we will need a 2.5x 

Barlow lens and the common 3x version will be good enough for all practical 

purposes. Barlow lenses are less critical than focal reducers and most types can be 

used with good results. However, if you are buying one especially for CCD imaging, I 

recommend getting a 3x or 5x amplifier, or the planets will still be rather small in 

your images. 

Achieving a good focus: 

Your starting point will depend on the focus aids, if any, which you are using. With 

the par-focal eyepiece, you should slip the eyepiece into the drawtube and focus 

visually on a moderately bright star (about 3 rd magnitude). Now withdraw the 

eyepiece and carefully insert the camera nosepiece, until it is bottomed against the 

drawtube end, and then lock it in place. 

SXV_M26C_usb.exe has a focus routine that will repeatedly download and display a 

128 x 128 pixel segment of the image at relatively high speed. This focus window 

may be positioned anywhere in the camera field and can be displayed with an 

adjustable degree of automatic contrast stretching (for focusing on faint stars). To use 

this mode, start up the software and select the SXV camera interface (File menu). Set 

the camera mode to Binned 1x1 and select an exposure time of 1 second. Press ‘Take 

Picture’ and wait for the image to download. There is a good chance that your 

selected star will appear somewhere within the image frame and it should be close to 

a sharp focus. If the focus is still poor, then it may appear as a pale disk of light, often 

with a dark centre (the secondary mirror shadow in an SCT, or Newtonian). Now 

select the ‘File’ menu again and click on ‘Focus frame centre’; you can now use the 

mouse pointer to click on the star image and the new focus frame co-ordinates will be 

displayed. Now return to the camera interface window and click on ‘Start’ in the 

Focus frame. The computer will now display a continuous series of 128 x 128 pixel 

images in the focus window and you should see your selected star appear somewhere 

close to the centre. A ‘peak value’ (the value of the brightest pixel) will also be shown 

in the adjacent text box and this can be used as an indication of the focus accuracy. 

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Although the peak value is sensitive to vibration and seeing, it tends towards a 

maximum as the focus is optimised. Carefully adjust the focus control on your 

telescope until the image is as sharp as possible and the peak value reaches a 

maximum. Wait for any vibration to die down before accepting the reading as reliable 

and watch out for bursts of bad seeing, which reduce the apparent focus quality. Quite 

often, the peak value will increase to the point where it is ‘off scale’ at 4095 and in 

this case you must halt the focus sequence and select a shorter exposure if you wish to 

use the peak value as an indicator. Once you are happy with the focus quality 

achieved, you might like to trim the settings of your par-focal or flip mirror eyepiece 

to match the current camera position. 

Although you can reach a good focus by the above method, many observers prefer to 

use additional aids, such as Hartmann or Bahnitov masks (an objective cover with 

several spaced holes) or diffraction bars (narrow parallel rods across the telescope 

aperture). These make the point of precise focus easier to determine by creating 

‘double images’ or bright diffraction spikes around stars, which merge at the setting 

of exact focus. The 12-16 bit slider control allows you to adjust the contrast of the 

focus frame for best visibility of the star image. It defaults to maximum stretch (12 

bits), which is generally ideal for stars, but a lower stretch value is better for focusing 

on planets. 

Taking your first astronomical image: 

I will assume that you are now set up with a focused camera attached to a telescope 

with an operating sidereal drive. If so, you are now in a position to take a moderately 

long exposure of some interesting deep-sky astronomical object (I will deal with 

planets later). As most drives are not very accurate beyond a minute or two of 

exposure time, I suggest that you find a fairly bright object to image, such as M42, 

M13, M27 or M57. There are many others to choose from, but these are good 

examples. 

Use the finder to align on your chosen object and then centre accurately by using the 

focus frame and a short exposure of between 1 and 5 seconds. The ’12-16 bit’ slider 

in the focus frame allows you to adjust the image contrast if you find that the object is 

too faint with a short exposure. Once properly centred and focused, take an exposure 

of about 60 seconds, and observe the result. Initially, the image may appear rather 

barren and show only a few stars, however, there is a great deal of data hidden from 

view. You can get to see a lot of this, without affecting the image data, if you go to 

the ‘View’ menu and select ‘Auto Contrast Stretch Image’. The faint image data will 

then appear in considerable detail and I think that you will be impressed by the result! 

If you are happy with the image, go to the ‘File’ menu and save it in a convenient 

directory. 

Most competitive brands of CCD camera require a ‘dark frame’ to be subtracted from 

your images to achieve the best results. A dark frame is simply a picture which was 

taken with the same exposure as your ‘light frame’, but with the telescope objective 

covered, so that no light can enter. It records only the ‘hot pixels’ and thermal 

gradients of your CCD, so that these defects are largely removed when the dark frame 

is subtracted from the light frame. The SXVR-M26C CCD is quite different from 

those used in other brands of camera and generates an extremely low level of dark 

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noise. Indeed, it is so low that subtracting a dark frame can actually INCREASE the 

noise in your images! This is because the statistical noise of the dark frame can 

exceed the ‘pattern noise’ from warm pixels and hence add to that of the subtracted 

result. If your test pictures have an exposure time of less than about 10 minutes (as 

above), then don’t bother with a dark frame, just ‘kill’ any hot pixels with your 

processing software. In SXVR-M26C, the ‘Median filter’ can do this, but other 

software (e.g. Maxim DL) will provide a ‘hot pixel killer’ that can be mapped to 

specific locations in the image, or methods such as ‘Sigma combine’ may be used. 

In the unlikely event that you feel that dark frame really is necessary, please proceed 

as follows: 

To take a dark frame, just cover the telescope objective with the lens cap and take 

another exposure with the same length as that of the light frame. This image will be a 

picture of the dark signal generated during your exposure and it should be saved with 

your image for use in processing the picture. If many such darks are recorded and 

averaged together, the statistical noise will be reduced, but the gains to be had are 

rather small compared with the effort involved. 

As variations in ambient temperature will affect the dark signal, it is best to take the 

dark frames within a few minutes of capturing your images. For the same reason, it is 

not wise to use ‘old’ dark frames if you want the best possible results, however, some 

software allows you to scale library dark frames to match the image (e.g. AstroArt) 

and this can be useful as a time saver. 

‘Bias frames’ are somewhat more useful than dark frames when using the SXVR- 

M26C. A bias frame is essentially a zero exposure dark frame and records any minor 

readout defects that the CCD may possess, so a ‘bias frame subtraction’ can clean up 

any ‘warm columns’ or shadings that are created during readout. To record a bias 

frame, cover the camera aperture and take a 1000 th of a second exposure. If you take 

at least 10 such frames and average them together, the resulting ‘master bias’ can be 

used to clean up readout defects for many months before CCD ageing changes require 

another set to be recorded. 

‘Flat fields’ are often recommended for optimising the results from your CCD 

camera, but these are generally less important than dark frames, especially if you 

make sure that the optical window of the camera is kept dust-free. The purpose of a 

flat field is to compensate for uneven illumination and sensitivity of the CCD and it is 

better to avoid the need for one by keeping the optics clean and unvignetted. I will 

ignore flat fielding for current purposes and describe the process in detail at a later 

stage. 

Processing a deep-sky image: 

Your raw image may look something like the one shown below – a 20 minute 

exposure of the region of the Rosette, taken through a 100mm F5 refractor with an 

IDAS light-pollution rejection filter. 

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Relatively little nebulosity is visible at this time, but it will be revealed later. If you 

zoom in on the raw image, you will see that it has the regular grid of brighter and 

darker pixels, caused by the Bayer matrix filter grid on the CCD. 

Now apply the colour synthesis routine, using the same offsets that gave good results 

with the daylight image tests. 

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The image should now look quite impressive and I hope that you are pleased with 

your first efforts! 

In many cases, a ‘Normal’ contrast stretch will give a good result, but may ‘burn out’ 

the bright regions and leave the faint parts of the image rather lacking in brightness. 

To combat this, many imagers will use a combination of ‘Normal’ and ‘Non-linear’ 

contrast stretches. The best settings are different for different objects, but performing 

a non-linear or power law stretch, followed by normalising the background to black 

with a normal stretch, is the usual procedure. 

Further small refinements are usually possible and you will become expert at judging 

the best way to achieve these as your experience increases. As a rough guide, the 

‘Filters’ menu can be used to sharpen, soften or noise reduce the image. Strong ‘High 

Pass’ filters are usually not a good idea with deep sky images, as the noise will be 

strongly increased and dark rings will appear around the stars, but a ‘Median’ filter 

can remove odd speckles and a mild ‘Unsharp Mask’ (Radius 3, Power 1) will 

sharpen without too much increase in noise. 

Other things to try include summing several images for a better signal to noise ratio. 

Summing can be done in the ‘Merge’ menu and involves loading the first processed 

image, selecting a reference point (a star) then loading the second image and finding 

the same star with the mouse. Once the reference is selected, you can either add 

directly, or average the images together. Averaging is generally better, as you are less 

likely to saturate the highlights of the picture. The signal-to-noise ratio will improve 

at a rate proportional to the square root of the number of summations (summing 4 

images will double the signal-to-noise), but different exposures must be used. 

Summing an image with itself will not improve the S/N ratio! 

Although I have concentrated on the use of a telescope for deep-sky imaging, do not 

forget that you have the option of using an ordinary camera lens for impressive wide- 

17


field shots! A good quality 200mm F3.5 lens with an infrared blocking filter will yield 

very nice images of large objects, such as M31, M42, M45 etc. If you cannot obtain a 

large IR blocker for the front of the lens, it is quite acceptable to place a small one 

behind the lens, inside the adaptor tube. You can even try using a hydrogen-alpha 

filter to bring out nebulae, reduce light pollution and sharpen the star images to pinpoints, 

although the results will be monochrome red! 

Taking pictures of the planets: 

The SXVR-M26C has a large CCD with 10 million pixels and so it is not well suited 

to planetary imaging, where a small CCD is ideal. However, it can be used if you 

accept the relatively large amount of wasted image area, or use a sub-frame 

download. 

Planetary imaging is in many ways quite different from deep sky imaging. Most deep 

sky objects are faint and relatively large, so a short focal length and a long exposure 

are needed, while planets are bright and very small, needing long focal lengths and 

short exposures. High resolution is critical to achieving good results and I have 

already shown how a suitable focal length can be calculated and produced, using a 

Barlow lens. 

Many camera users comment on the difficulty of finding the correct focus when 

taking pictures of Jupiter etc. This is usually due to poor seeing conditions, which are 

only too common, but may also be due in part to poor collimation of your telescope. 

Please ensure that the optics are properly aligned as shown by star testing, or by using 

one of the patent collimation aids that are widely available. It is also better to use a 

star for initial focusing, as planetary detail is difficult to judge in bad seeing. Although 

the star will also suffer from blurring, the eye can more easily gauge when the most 

compact blur has been achieved! 

You could begin by imaging lunar craters, or the planets, Jupiter, Saturn or Mars. The 

rapid variations of seeing which accompany planetary imaging, will ruin the 

definition of about 95% of your images and so I recommend setting the camera to run 

in ‘Autosave’ mode. This will automatically take a sequence of images and save them 

with sequential file names in your ‘Autosave’ directory. Dozens of images will be 

saved, but only one or two will be satisfactory for further processing. The ‘Subframe’ 

mode of the SXVR may be found useful for limiting the wasted area and reducing the 

download time of small planetary images. 

To start the Autosave process, call up the SXVR Camera Interface and select the 

‘Continuous Mode’ check box at the top (make sure the rest are unchecked). Now 

check the ‘Autosave Image’ checkbox near the bottom of the window. If you now 

click on ‘Take Picture’ the automatic sequence will begin and will not stop until you 

press a computer key. The images will be saved in FITs format with sequential names 

such as ‘Img23, Img24….’ and will be found in the ‘Autosave’ directory (or a subdirectory 

of Autosave, set up in the program defaults menu). 

The exposure time needed for good planetary images is such that the image histogram 

has a peak value at around 200 and does not extend much above 220 (Ignore the 

major peak near zero, due to the dark background). If you use too short an exposure 

18


time, the image noise level will be increased, and if too long a time is used you will 

saturate the highlights and cause white patches on the image. With the recommended 

focal length, Jupiter and Mars will both need an exposure time of between 0.1 and 1 

seconds and Saturn will need between 0.5 and 2 seconds. 

Processing a planetary image: 

Planetary images have one major advantage over deep sky images, when you come to 

process them – they are MUCH brighter, with a correspondingly better signal to noise 

ratio. This means that aggressive sharpening filters may be used without making the 

result look very noisy and so some of the effects of poor seeing can be neutralised. 

A raw image 

Try applying an ‘Unsharp Mask’ filter with a radius of 5 and a power of 5. This will 

greatly increase the visibility of any detail on the planet, but the optimum radius and 

power will have to be determined by experiment. 

Jupiter after the application of an ‘Unsharp mask’ 

In general terms, the larger the image and the worse the seeing, then the wider the 

radius for best results. My Jupiter shots are usually about one third the height of the 

CCD frame and I find that the ‘radius 5, power 5’ values are good for most average 

seeing conditions. If you have exceptionally good conditions, then a reduction to R=3, 

P=3 will probably give a more natural look to the image, as too large a radius and 

power tends to outline edges with dark or bright borders. 

As a finishing touch, the application of a Median filter or a Weighted Mean Low Pass 

filter can be useful to smooth out the high frequency noise after a strong Unsharp 

Mask. 

As with deep-sky images, it is advantageous to sum planetary images together to 

improve the signal to noise ratio. In this case, the ‘averaging’ option should always be 

used, or the result is likely to exceed the dynamic range of the software and saturate 

19


the highlights. Aligning the images is always something of a problem, as there are 

rarely any stars to use when imaging the planets, but Jupiter’s satellites can be useful 

reference points. Otherwise, you will have to find a well-defined feature on the planet, 

or estimate where the centre of the disk is located. Some more sophisticated software 

can automatically align planetary images and you may find these programs (e.g. 

‘Registax’) to be very useful. 

********************************************************************* 

Using the add-on autoguider: 

A very useful accessory is the add-on autoguider head, which takes its power and 

control signals directly from the SXVR camera, via the 18 way socket on its rear 

panel. The autoguider is only 1.25” in diameter and has a video style ‘CS’ mount 

thread in its nose, so video lenses may be attached. The guider may be used with 

either an off-axis prism assembly mounted in front of the SXVR camera, or with a 

separate guide telescope, rigidly mounted alongside your imaging telescope. I 

personally use it with a 70mm aperture, F10, inexpensive refractor as a guide ‘scope, 

but a shorter focal length lens will make more guide stars available in any given 

region of sky (See the picture below). 

To use the autoguider, first orient it so that the connector plug is roughly parallel to 

the declination axis of your mount. This is not absolutely essential, as the training 

routine will learn the angle of the head and compensate for it, but it is easier to 

understand the motion of the guide star if the guider frame is aligned with the RA and 

Dec axes. Now connect the head to the camera, using the 18 way connector lead, 

including the port divider box, if it is to be used. 

The recommended way of connecting the autoguider output to the mount is to use an 

RJ11 telephone lead between the socket on the SXV camera and the autoguider input 

of your mount. This output is ‘active low’ (i.e. the control relays pull the guider inputs 

down to zero volts when applying a guide correction) and matches most of the 

autoguider inputs on commercial mounts. If ‘active high’ inputs are needed, or a very 

low control voltage drop is essential, then you will need to add a Starlight Xpress 

‘relay box’ between the guider output and the input to the mount. Please contact your 

local distributor if a relay box is required. Some mounts (Vixen, for example) use a 

similar guider input socket, but have re-arranged connections. Details are given on our 

web pages at the end of the ‘STAR2000’ section. 

20


The autoguider installed on a 70mm refractor guide ‘scope in the author’s garden (the 

camera shown is the older SXVF version, but the connections are the same). 

To use the autoguider, please proceed as follows: 

1) Having started the SXVR-M26C software, open the autoguider control panel 

by clicking on the autoguider menu button. 

21


The autoguider control panel with a guide star selected 

2) Press the ‘Start’ button and a series of 1 second exposure guider images will 

begin to appear in the picture frame. If the images look too dim, use the 

‘Stretch Image’ slider to increase its contrast and brightness until the noise 

begins to be visible. 

3) If you haven’t focused the guider lens or ‘scope, move the mount until a bright 

star is visible on the guider image and then adjust the focus until it is as sharp 

as possible. 

4) At this point, you may want to test the guiding control by pressing the manual 

‘Move Telescope’ buttons at the bottom left corner of the control panel. You 

can watch the position of any stars in the guider image and confirm that they 

move in response to the buttons. The movement should be slow if the correct 

guiding rate is selected on your mount (typically 2x sidereal). Adjust this, if 

necessary. 

5) Move the mount until the required object for imaging is properly framed in the 

main CCD image (leave the guider menu and use the main camera control 

panel, as necessary). 

6) Re-open the guider control panel, start imaging and try to locate a clearly 

visible guide star. If necessary, make adjustments to the guide telescope or offaxis 

guider until one is found. 

7) Press ‘Stop’ and then press ‘Select Guide Star’. Use the mouse to left click on 

the selected star and a green cross will highlight it and the co-ordinates will 

appear in the text boxes above the image window. 

8) The various guiding rate defaults, listed on the right-hand side of the control 

panel, are unlikely to be perfect for your particular telescope and mount. You 

have the option of manually selecting values, or asking the software to attempt 

to determine what they should be. This is done by pressing the ‘Train’ button 

and waiting for the software to complete a sequence of automatic moves and 

calculations. The training will also determine the angle at which the guide 

camera is oriented with respect to the RA and Dec axes. If you do not wish to 

train the system at this time, the default values of 6 pixels per second will 

serve as a starting point. 

22


9) Now press ‘Go to main camera’ and the guider control panel will be replaced 

by the camera control panel. Set the required exposure time for the image (say 

5 minutes) and press the ‘Autoguide next image’ button. The autoguider 

window will reappear and, after a few seconds, you should see error values 

appearing in the text windows at the top. The guide star will be fairly close to 

the green cross, although not necessarily accurately centred, and you should 

see the power/ guide LED on the rear of the camera brighten and change 

colour with each correction. 

10) If the star begins to drift away from the cross, despite the corrections being 

made, the chances are that the N/S and/or E/W directions are set wrongly. 

Judge which axis is incorrectly set by observing the direction of the drift and 

then stop the exposure by pressing ‘Esc’. Open the guider control panel and 

check the appropriate swap box(es). After this operation, you will probably 

need to find the guide star again by taking a guider image and reselecting the 

star, as before. Now return to the main camera menu and try the ‘Autoguide 

next image’ button again. 

11) Once guiding is taking place without problems, the main exposure can be 

allowed to finish and, if all is well, you should see an image with tiny circular 

stars. 

If the stars are not circular, you may need to alter the guiding parameters, or 

investigate the rigidity and drive performance of your mount. A lot of information 

can be deduced by watching the behaviour of the guide star in the guider frame. If 

it is continually moving between two locations, either side of the green cross, then 

the RA or Dec pixels per second value is set too low. The higher these values are 

set, the gentler the guiding becomes. Too low a value will cause an overaggressive 

correction to be made and result in oscillation of the star position 

between two points. 

Another source of guiding errors can be an accurately balanced telescope mount! 

Good balance can result in the telescope mount ‘bouncing’ between the gear teeth 

as corrections are made. A simple fix is to add a weight of about 0.5kg (1 pound) 

on the eastern end of the declination axis, so that there is always some pressure 

acting against the gear teeth. 

Getting a good result from an autoguider will often entail a lot of detective work 

to eliminate the sources of gear error, telescope flexure, mirror shift etc., but the 

final result is well worth the effort! 

********************************************************************* 

Using the built-in serial ports 

The SXVR-M26C incorporates two fast serial ports for use with external accessories. 

The ports are available on 5 pins of the 18 way connector that is provided for the 

autoguider and may be accessed by plugging in a ‘serial port divider box’. The divider 

box and cables are available as an accessory and may be chained in series with the 

autoguider cable, when the guider is in use, or may be used on its own. 

23


The two serial connections are in the form of standard RS232 PC style plugs and 

provide TX, RX and Ground connections at RS232 levels. Access is via commands 

sent through the USB connection and, at the time of writing, is limited to any serial 

controls that are provided by the SXV software. It is expected that many more 

functions will be added as the software is upgraded. 

********************************************************************* 

Other features of the SXVR-M26C hardware and software 

Using the ‘Binned’ modes: 

Up to this point, I have assumed that the full resolution imaging mode is being used. 

Binned 2x2 mode sums groups of 4 pixels into one output pixel, thus creating a 1516 

x 1008 pixel image with 4 times the effective sensitivity. Using 2x2 binning, you can 

considerably improve the sensitivity of the SXVR-M26C without losing a great deal 

of resolving power, so you may like to use this mode for finding faint deep-sky 

objects. Because of the unique readout system of the M26C camera, your 2x2 binned 

images can still be decoded to colour frames. This is unusual, as binning will 

normally destroy the colour data. At the time of writing, binned 4x4 is not available, 

but may be included in later versions of the software. 

Taking and using a flat field: 

Flat fields are images, which display only the variations of illumination and 

sensitivity of the CCD and are used to mathematically modify a wanted image in such 

a way that the errors are removed. Common flat field errors are due to dust motes on 

the camera window and vignetting effects in the optical system of the telescope. Dust 

motes act as ‘inverse pinholes’ and cast out-of-focus images of the telescope aperture 

onto the CCD chip, where they appear as shadow ‘do-nuts’. Most optical systems 

show some vignetting at the edges of the field, especially when focal reducers are 

used. This causes a brighter centre to show in images, especially when there is a lot of 

sky light to illuminate the field. 

If dust motes are your main problem, it is best to clean the camera window, rather 

than to rely on a flat field to remove the do-nuts. Flat fields always increase the noise 

in an image and so physical dust removal is the best option. If you have serious 

vignetting, first check whether the optical system can be improved. The most likely 

cause of this problem is trying to use too powerful a degree of optical compression 

with a focal reducer and you might want to try moving the camera closer to the 

reducer lens. 

If you really do need to use a flat field for image correction, then it must be taken with 

care. It is most important that the optical system MUST NOT be disturbed between 

taking your original images and taking the flat field. Any relative changes of focus 

and rotation etc. will upset the match between flat field and image and the result will 

be poor correction of the errors. The other necessity for recording a good flat field is a 

source of very even illumination of the telescope field. This is surprisingly difficult to 

achieve and many designs of light source have appeared in the literature and on the 

24


Web. These usually consist of a large wooden box, containing several lamps and an 

internal coating of matt white paint, which is placed over the objective of the 

telescope to provide an evenly illuminated surface. These can work well, but I prefer a 

simpler method, as follows: 

Most imaging sessions begin or end in twilight and so the dusk or dawn sky can 

provide a distributed source of light for a flat field. However, using the sky directly is 

likely to result in recording many unwanted stars, or patches of cloud etc., so a 

diffuser needs to be added to the telescope. An ideal material is Mylar plastic drafting 

film, obtained from an office supplies warehouse. It is strong and water resistant and 

can be easily replaced if damaged. Stretch a piece of the film loosely across the 

aperture of your telescope and point the instrument high in the sky, to avoid any 

gradient in the light near the horizon. Now take several images with exposure times 

adjusted to give a bright, but not overloaded, picture. A histogram peaking at around 

128 is ideal. Averaging flat fields together is a good way to reduce their noise 

contribution and so recording 4, or more, images is a good idea. 

To use your flat fields, they must first have a dark frame subtracted. Although this 

may appear to be unimportant with such brightly lit and short exposures, there is the 

‘bias offset’ of the camera in each image and this can produce an error in the final 

correction. As we are mainly interested in the bias, any very short exposure dark 

frame will give a good result. The dark subtracted images should then be averaged 

together before use. 

After the above procedures have been executed, the flat field will be ready for use. 

Load up your image for processing, subtract the dark frame and then select ‘Apply 

flat field’ in the ‘Merge’ menu. The result should be an image with very few signs of 

the original artefacts and you can then process it in the normal way. 

********************************************************************* 

The SXVR-M26C accessory ports 

25


The SXVR-M26C is provided with two ports for use with accessories. The 

Autoguider output port is a 6 way RJ11 socket, which is compatible with the standard 

autoguider input of most telescope mounts. It provides 4 active-low opto-isolator 

outputs and a common return line, capable of sinking a minimum of 5mA per output. 

This socket may be used for telescope control if the SXVR-M26C is employed as an 

autoguider, but is primarily intended to be the control output for the optional add-on 

autoguider camera head, available for use with the SXVR-M26C. 

The high density parallel port socket provides both control and power for the add-on 

autoguider, but also includes a pair of serial ports for use with other devices. 

********************************************************************* 

Camera maintenance: 

Very little maintenance is needed to keep the SXVR-M26C in excellent operating 

order, however two problems, which are common to all CCD equipment, might show 

up on occasion. These are dust and condensation. 

Removing Dust: 

26


1) Dust can be deposited on either the optical window (not a big problem to cure), or 

on the CCD faceplate (very difficult to eliminate entirely). When small particles 

collect on the window they may not be noticed at all on deep sky (small F ratio) 

images, as they will be very much out of focus. However, if a powerful contrast boost 

of the image is carried out, they may well begin to show as the shadow ‘Do-nuts’ 

mentioned earlier. Images taken with a large F ratio optical system are more likely to 

be affected by such dirt, owing to the smaller and sharper shadows that they cast. A 

light polluted sky will also make these marks much more obvious. There is no great 

difficulty in removing such particles on the outside surface by the careful use of a lens 

cleaning cloth, ‘lens pen’, or ‘air duster’ and so you should have little trouble with 

this aspect of maintenance. Dust on the CCD faceplate is a much greater nuisance, as 

it casts very sharply defined and dark shadows and it entails dismantling the camera to 

get rid of it! To clean the CCD you will need a good quality lens cloth (no silicone) or 

tissues and some high-grade acetone or isopropyl alcohol. A very suitable cloth is the 

‘Micro-Fibre’ type marketed by PENTAX etc., and suitable alcohol is available from 

Maplin or Radio Shack etc. as tape head cleaning fluid. Most pharmacist shops will 

have small bottles of pure acetone. A bright light and a strong watchmakers eyeglass 

will also be found to be essential. 

Procedure: 

1) Disconnect the lead from the camera head and remove it from the telescope. Place 

it on a table with the optical window facing downward. 

2) Remove the two M3 screws and the M8 nut from the camera back plate and ease 

the plate out of the camera body. Unplug the fan lead from the camera PCB. 

3) Withdraw the body cylinder and unscrew the two top spacer pillars from the PCB. 

Now gently lift the PCB off the 20 way connector NOTING THE ORIENTATION 

OF THE BOARD for correct replacement later. Now remove the lower two spacers 

from the heat sink plate assembly. 

4) The camera heat sink assembly can now be lifted away from the camera front 

barrel and the CCD will be exposed. Note that a layer of white heat-sink compound is 

applied to the periphery of the heat sink disc and this should be left undisturbed by 

subsequent operations. 

5) You can now closely examine the CCD faceplate under the spotlight using the 

watchmaker's glass when any dust motes will show clearly. If there is only an odd 

particle or two and the CCD is otherwise clean, carefully brush away the dust with a 

corner of your lens cloth. A smeared or very dusty CCD will need a few drops of 

alcohol to clean thoroughly and you may have to make several attempts before the 

surface is free of contamination. One gentle wipe from one end to the other, with no 

return stroke, will be found to be the most effective action. DO NOT rub vigorously 

and be very careful to avoid scratching the window. 

6) Before re-assembly, make certain that the inside surface of the front window is also 

clean, and then carefully replace the camera front barrel and screw it into place. (If the 

heat sink seal is disturbed, renew it with fresh compound before reassembling). 

7) Replace all the camera parts in reverse order and the job is done. 

Dealing with condensation: 

27


The SXVR-M26C is designed to avoid condensation by minimising the volume of air 

trapped within the CCD cavity and by preventing moisture ingress. This normally 

works very well, but storage of the camera in a humid location can lead to the trapped 

air becoming moist by diffusion through the optical window mounting thread etc. and 

can result in condensation on the CCD window. If this becomes a problem, try storing 

the camera in a warm, dry place, or in a plastic lunch box containing a sachet of silica 

gel desiccant. If this is not effective, try opening the main barrel and loosening the 

stand-offs to allow a gap to form between the heat sink and the front barrel assembly. 

Now put the camera into a desiccator box (as above) or leave it in a warm place for 

several hours before re-sealing it. 

N.B. DO NOT leave the camera switched on for long periods between uses. The 

cold CCD will collect ice by slow diffusion through any small leaks and this will 

become corrosive water on the cooler and CCD pins when the power is removed. If 

substantial amounts of moisture are seen, dismantle the camera and dry it 

thoroughly. 

********************************************************************* 

Alternative Software 

Although we hope that you will be satisfied with our ‘SXV_hmf_usb’ software, other 

companies are offering alternative programs with more powerful processing 

functions. One of these is programs is ‘AstroArt’ by MSB software. You can purchase 

AstroArt from many dealers Worldwide and more information may be obtained from 

their web site at http://www.msb-astroart.com 

‘Maxim DL’ is another popular choice and you can find out more by visiting 

http://www.cyanogen.com 

********************************************************************* 

Some details of the camera and CCD characteristics 

CCD type: 

CCD size: 

Sony ICX493AK ‘Super HAD’ interline Bayer matrix imager. 

Active area 23.4mm x 14.9mm 

CCD pixels: 3900 x 2016 pixel array. Each pixel is 6.05 x 6.05uM 

Well depth: Full res. mode 25,000e. Binned 2x2 mode approx. 30,000e 

Mean visual QE: 60%, 65% at peak (540nM) 

Useful spectral response: 360nM – 1100nM 

Readout noise: Approx. 5e RMS typical, 8e max. 

Back focal distance: The CCD is approximately 17.5mm from the barrel front. 

Camera size: 63mm diameter x 65mm long 

28


29


Dear Observer, 

Thank you for purchasing a Starlight Xpress CCD Imaging System. We are confident that you will gain 

much satisfaction from this equipment, but please read carefully the accompanying instruction manual 

to ensure that you achieve the best performance that is capable of providing. 

As with most sophisticated equipment a certain amount of routine maintenance is necessary to keep the 

equipment operating at its optimum performance. The maintenance has been kept to a minimum, and is 

fully described in the manual. 

In the unfortunate instance when the equipment does not perform as expected might we recommend 

that you first study the fault finding information supplied. If this does not remedy the problem, then 

contact Starlight Xpress for further advice. Our message board service on the Starlight Xpress web site 

will often provide solutions to any problems. 

The equipment is covered by a 12-month guarantee covering faulty design, material or workmanship in 

addition to any statutory Consumer Rights of Purchasers. 

CONDITIONS OF GUARANTEE 

1) The equipment shall only be used for normal purposes described in the standard operating 

instructions, and within the relevant safety standards of the country where the equipment is used. 

2) Repairs under guarantee will be free of charge providing proof of purchase is produced, and that the 

equipment is returned to the Service Agent at the Purchaser’s expense and risk, and that the equipment 

proves to be defective. 

3) The guarantee shall not apply to equipment damaged by fire, accident, wear an tear, misuse, 

unauthorised repairs, or modified in any way whatsoever, or damage suffered in transit to or from the 

Purchaser. 

4) The Purchaser’s sole and exclusive rights under this guarantee is for repair, or at our discretion the 

replacement of the equipment or any part thereof, and no remedy to consequential loss or damage 

whatsoever. 

5) This guarantee shall not apply to components that have a naturally limited life. 

6) Starlight Xpress’s decision in all matters is final, and any faulty component which has been replaced 

will become the property of Starlight Xpress Ltd. 

For further info. or advice, please call: 

Mr Michael Hattey, 

Starlight Xpress Ltd., 

The Offices, Foxley Green Farm, 

Ascot Road, Holyport, 

Berkshire, 

England. SL6 3LA 

Tel: 01628 777126 

Fax: 01628 580411 

Email: michael.hattey@starlight-xpress.co.uk 

Web site: http://www.starlight-xpress.co.uk 

30

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