3. Connect a web-cam with a normal lens on it that lets you see around the room. The camera can be either usb or firewire, but must provide 640x480 output. It can also be a video camera like a PC164C connected through a video2usb converter

4. Launch MetaGuide

5. If you see an error about io.sys, just start it again

6. If you get a box showing several camera options – choose the one for your camera

7. You should now see the MetaGuide interface, with a camera view

8. Aim the camera at the room around you. Note that the brightest spot is selected automatically and marked by the crosshairs. This will act as a “star”

9. The spot is also visible in the lower right corner, where a zoomed, stacked view is shown

10. As you move the camera around, the crosshairs track the star and the zoomed in view remains steady as long as no brighter spot appears in the view

11. Note also that the profile of the spot in the view on the lower left

12. Focus on the red buttons. They are the main ones to work with at first

13. Select VidProps to adjust the camera – brightness, gamma, etc. For a sharp view of the spot, make sure the exposure is short enough that the spot is saturated

14. Select Setup and enter data for your telescope and camera. Also name and location would be good. Fill in the red items. Don’t worry about the others until later

15. Don’t connect to the telescope just yet

16. Leave setup and do File->Save As and save it as ScopeSetup.mg, or whatever you like – but use the .mg extension

17. At this point, you can use MG to collimate, or make XY plots of periodic error with a telescope. You don’t need to have a connection to the telescope mount

CONNECTING TO THE TELESCOPE

There are three ways to connect MetaGuide to the telescope mount for control: ASCOM, GPUSB, and LPT. ASCOM requires the latest installation of the ASCOM environment, plus a driver for your particular mount. You also need a physical connection to the mount – usually via a serial (COM) port. GPUSB requires the GPUSB electronics interface over a USB port, feeding into the ST4 port on your mount. LPT requires either a GPINT interface or a home-made cable to connect an LPT port to the ST4 input.

Note that collimation can be done with no connection to the mount at all – but if you want mount control for collimation or autoguiding, you must set up one of these connections.

ASCOM has many advantages with MetaGuide. With GPUSB or LPT, all MetaGuide can do is move the mount N/E/W/S at autoguide rates. With ASCOM, MetaGuide can query the declination, right ascension, and other properties of the mount such as the actual autoguide rates. This is particularly helpful during calibration. Nonetheless, autoguiding should work well using any of these connections – the user just needs to enter the Declination and exact autoguide rates if calibrating without ASCOM.

ASCOM stands for Astronomy Common Object Model and allows plug-and-play connection between astronomical applications and devices. For more details, and to download the latest version and drivers, see http://ascom-standards.org/.

ASCOM

1. Be sure to install the latest ASCOM environment, plus the latest driver for your mount

2. Open Setup and select ASCOM in the ASCOM/USB/LPT drop-down selector

3. Press the Chooser button and select your mount’s driver. Then select Properties and set the COM port. If you have done this before in a different application, it may already be set for you

4. Then press OK and the mount should be connected

5. Try pressing the N/E/W/S buttons and see if the mount responds by reading its RA/Dec. values. Note that each press of a button will move the mount for 1 second at autoguide rate, which may not be noticeable without reading the display of the mount’s RA/Dec coordinates

6. You can practice all this with the ASCOM telescope simulator, without any connection to a telescope. You can view the simulator display to see changes in RA and Dec.

7. If you need to have several applications connected to the same telescope, you should connect via the ASCOM Hub. Just connect to Hub first, and in the Properties select the driver for your mount. Only one application needs to connect to the mount through the hub; the others can just connect to Hub and they will automatically be connected to the mount. Hub magically lets multiple applications have direct control over the same mount independently.

8. MetaGuide can have trouble with POTH, so use Hub instead, if possible. POTH stands for Plain Old Telescope Hub, and differs from the ASCOM Hub by providing a control panel view of the telescope coordinates. I recommend using Hub rather than POTH if Hub meets your needs

9. MetaGuide requires an ASCOM driver that supports PulseGuide, and also supports the “V5 early binding” drivers. If the driver for your mount has trouble with a direct connection – try connecting through Hub first. If your driver does not support PulseGuide (MetaGuide should indicate this when it tries to connect) see if there is a newer or different driver for your mount that does support PulseGuide

10. You should enter the desired autoguide rates for RA and Dec. in Setup. After you enter them, MetaGuide will try to apply those rates to the mount, and the mount will use the best available values that match those rates and return them. If the values in Setup don’t match your request exactly, it is because the ASCOM driver has chosen the best match instead.

MetaGuide shown connecting to the telescope simulator directly via ASCOM

MetaGuide connected to the simulator via Hub. ASCOM Chooser->Generic Hub->Properties->Choose Scope->Simulator

GPUSB

1. Connect the GPUSB box to your computer via USB cable, and to the mount via the ST4 cable

2. Select USB from the ASCOM/GPUSB/LPT selector

3. You should be able to move the mount with the N/E/W/S buttons as described for ASCOM

4. Note that with GPUSB, all you can do is move the mount at autoguide rates in each of the 4 directions; you cannot query the mount for RA/Dec or other values such as the actual autoguide rates. You must make sure the autoguide rates entered in Setup match the rates in use by the mount. 0.5x sidereal is a common rate – but whatever the mount’s values are should match those shown in Setup

LPT

1. LPT is identical to GPUSB except you must provide a GPINT device or equivalent that allows a direct connection from your LPT port to the ST4 input of the mount. You must also select a port number matching your LPT port – which can be found in Device Manager/Ports on your computer

5. Autoguiding

Once you have a connecton to the mount that appears functional, enter the declination of the star you are observing, and the RA/Dec autoguide rates. (ASCOM will set the declination automatically, and will override the guide rates with values from the driver.) Then approximately center the star in the field and press FullCalibrate to calibrate the view orientation and scale. A dialog and progress bar will appear in the upper left. Do not interact with the telescope or the application until the calibration completes. The star should never leave the view; if it does, cancel the calibration. Make sure the telescope is not bumped or leaned on during this procedure, and that it goes to completion.

If you have just one bright star in the view, the crosshairs should stay on it steadily – but if there are other bright stars that pull the crosshairs away, simply press Lock and the crosshairs will turn red, indicating they are locked on to that one star. The star may drift about and the crosshairs will track – but abrupt motion may lose the lock. In most cases, it is best to lock the star during calibration.

If you are unable to lock onto a star due to hot pixels, see the section below on hot pixel removal.

The calibration process moves the mount in a ‘+’ pattern to determine both the scale and orientation of the guide camera. The guide camera need not be aligned in any particular way. There is a quicker calibration, QuickCal, described below – but this one should take about 1-5 minutes on a typical mount – mainly slowed by declination backlash. QuickCal avoids this delay and can be much faster.

Note that the calibration procedure will set the calibration factor so the image scale is exact. Furthermore, it will determine the orientation of the E/W direction in the field, and whether the N/S direction is inverted. Although the E/W and N/S alignment of the view does not matter for the calibration, it is convenient to have RA motion nearly along the horizontal axis so that drift in Y corresponds to N/S drift.

ASCOM is able to deduce much more information from the calibration process than GPUSB or LPT because it can tell which whether guide commands move the telescope north or south. This is described in more detail later.

Once the telescope is calibrated, the guiding-related features such as Guide and Center will be enabled.

If you ever exit MetaGuide and return to it with no changes at all to the telescope and camera, you may recover the previous calibration by selecting UsePrevCal in the Setup dialog. You must manually save the setup values in a .mg file using Save or Save As, otherwise the session values will be lost.

To center a star approximately in the field, just press the Center button. This may take some time if the declination backlash is large. This behaves differently when guiding, as described below.

To begin guiding, just select Guide and the star location will be stored and maintained. The location of the star in the field does not matter at the time Guide is pressed. You should probably Lock the star also.

The Center button takes on a different meaning during guiding. Instead of simply bringing the star near the center, during guiding, Center will make the target location be the center of the screen. This will slowly bring the star to the exact center of the screen and keep it there.

Note that once you press Guide, the guide error plot starts scrolling – showing errors in E/W (white) and N/S (red) on a +/- 4” scale. This plot is updated every 0.5 seconds, independent of the video rate.

There are many ways to tune guiding, including the usual RA and Dec. aggressiveness (here on a scale to 1.0 rather than 10), along with NFrames, which is the number of frames to use in calculating a star location; AccepFrac, which is the fraction of frames that are actually used in the average (the rest of them are lower quality and not included in the centroid calculation); and GuidePeriod, which is the time between corrections. These and more parameters are described in detail below – but the basic idea is to set aggressiveness so that corrections are made quickly, but do not overshoot and cause oscillations. GuidePeriod is related, and should neither be too fast nor too slow. For my CGE I correct every second and typically use a frame rate of 8 fps and NFrames=5. This amounts to approximately 5/8s “exposure” and a correction every second. The total integration time (NFrames/FrameRate) should not exceed the guide period.

Since MetaGuide relies on small corrections, it may be best to set the RA guide rate on the mount to a small value around 0.25x sidereal. On the other hand, Dec. motion may be limited by backlash, so its guide rate may be best set at 0.9x sidereal – along with tuning Dec. backlash so that it is somewhat responsive in both directions, but does not overshoot. But starting values of 0.5 and 0.5 should work.

To summarize, autoguiding just requires connecting to the mount, finding and focusing a guidestar, entering the declination (if not using ASCOM), pressing FullCalibrate, then pressing Guide. Note that you never click on the star itself.

6. Collimation

Collimation involves adjusting the mirrors of a telescope so that everything is aligned well and stars become nice, round dots rather than flared, comatic smudges. A very good telescope, when slightly out of collimation, can give horrible views - but after a slight adjustment can show a dramatic improvement. This is particularly true with high power views of planets, where details of Jupiter’s bands or Saturn’s rings will suddenly pop out with greater clarity.

Collimation is not something to be feared. It is important to do regularly, and it is much easier with a web-cam and MetaGuide.

The first step in collimation is to view a bright star overhead at prime focus with the telescope – i.e. with no Barlows to magnify the image. I recommend working with the actual configuration you intend to use, and not make changes to the components for the sake of collimation. So – if you intend to view with a star diagonal in place, then leave it there and insert the web-cam in the diagonal where the eyepiece would go. If you intend to image with no diagonal – then insert the web-cam with no diagonal.

With an SCT or Newtonian, the star will appear as an out of focus blobby donut. The first step in collimation is to get this donut round and uniformly illuminated. As you change focus and the donut gets larger or smaller, you will need to change the gain/exposure of the web-cam to keep it from saturating. You may want to put “star-stacking,” in the menu->settings, on Centroid to keep the zoomed in view from jumping around. (Peak stacking, as described below, will center on the bright part of the donut – which may move around.)

Try adjusting the collimation screws to make the donut fairly concentric. It need not be perfect because, as described below, best collimation may in fact occur when the donut is off center. Once the donut is fairly centered, you want to move to high power and focus on the Airy pattern itself – perhaps with auto-centering of the star by the mount.

A detailed view of the Airy pattern requires a high effective f/number, which usually means the field of the camera is very small and the mount must be very stable. Typical f/numbers for a good view of the Airy pattern are in the 25-50 range, and may require a Barlow. If you have some experience with planetary imaging and your mount is stable at high power, this may pose no difficulties. Otherwise, you may want to start at lower magnification.

Find a bright star near the zenith – the brighter the better, but it should also be very high up to improve seeing. Center it with an eyepiece, then substitute the web-cam and focus. For imaging the diffraction pattern the star must not be saturated, which means extremely short exposures are not only possible, but required. For an 11” aperture, the exposure may be 1/200 to 1/1000 second. Once the star is in the field of the web-cam, its zoomed in view should be immediately visible in the lower right, along with its radial profile in the lower left. You do not need to select the star with a bounding box or click on it – it is found automatically. Carefully adjust focus and exposure so that the profile height is about 2/3 maximum and as narrow as possible. Note the FWHM plot on the lower right for reference. Note that for best results with the in-focus star appearance, you should set Star-Stacking to ‘Peak’ instead of ‘Centroid.’

Other video settings may be adjusted, but frames per second should be 10-20 and gamma should be 1.0 so that the radial profile corresponds to linear intensity. Use the gain setting to place the peak height about 2/3 of maximum.

Superimposed on the image of the star in the lower right is a red dot. If the star is flared at all due to coma or other aberrations of miscollimation, the dot will be offset in the direction of the flare. To collimate, carefully adjust the collimation screws so that the red dot moves toward the center of the star. If the star easily goes out of the field, try working without a Barlow – which is fine as long as the magnification is large enough that you can still see the elongation of the star. Note that the direction of the flare in the zoom view matches it in the wide view. With an SCT, you typically want to move the star in the direction of the flare itself – and re-center the star to see if the flare is reduced. Repeated motions like this should center the dot on the star when collimation is achieved.

One of the goals of MetaGuide is the auto-centering of the star during high-power collimation, which requires that guiding be enabled as described in the next section.

View of comatic star with coma dot in the upper left, in the direction of the flare

View of coma dot when in collimation – also showing the Airy pattern. This is only possible at high f/ratio with a Barlow – in this case a 12.5” cdk with 3x Barlow. Note that the first Airy ring has appeared, and is in roughly the correct location based on diffraction theory.

For an excellent write-up on the strange appearance of stars away from the zenith, see http://www.paquettefamily.ca/astro/star_study/. This is a wonderful example of the power in combining empirical results with simulation to document a phenomenon that is largely unknown, regarding the wedge-shape appearance of stars. This effect could greatly confuse collimation efforts if not taken into consideration.

7. Collimation with Automatic Re-Centering

MetaGuide not only lets you see the diffraction-limited performance of your telescope in a live view, but the autoguiding features can automatically keep the star centered as you adjust collimation. This means that as long as you can see the computer screen, you can focus on adjusting the collimation screws and not have to worry about recentering the star. This requires you have set up guiding and have the cable connected to the printer port as described in Chapter 4, and calibrate the camera orientation.

To collimate precisely, first make sure you are roughly collimated using standard procedures – then aim at a bright star high overhead as described above. Adjust the brightness and gamma so that you can see the shape of the star – particularly any comatic or oblong appearance.

Now, center the star and press Guide to begin guiding. As long as you don’t let the star leave the field, you may now make adjustments to collimation and the mount will recenter the star in response to changes. With practice this feels natural, and allows you to get immediate feedback on the changes made by a turn of a collimation screw. If the red dot, indicating coma, is consistently off center of the star, adjust until it is centered. It is much easier to keep track of the changes and their effects since the star is automatically centering itself after changes.

8. Feature Details

MetaGuide has many features to learn, but some are more advanced than others. In order to focus new users on the key features, MetaGuide has an Advanced and Beginner mode. Beginners should start in Beginner mode, but can switch to Advanced mode through Menu->Settings. In either mode, every GUI item has flyover text to provide helpful hints. Just pause the mouse over an item to get a hint of its purpose and usage. To read this help document, go to Help->Help or press the F1 key.

DESCRIPTION OF MAIN METAGUIDE SCREEN CONTROLS

Setup Access the control panel for describing the optics, camera pixel size, and for connection to the mount. Also allows specifying the desired camera frame rate

VidProps Control the camera brightness, gamma, etc.

FullCalibrate Do a full calibration of the guide camera, with a ‘+’ pattern

QuickCal Do a quick calibration with motion only in RA. This requires proper setting of NSInvert and ViewParity, as described below

Calibrated This is a readonly indication that the mount has been calibrated and now Guide can be pressed to begin autoguiding. Note that you can recalibrate any time – even though the mount is already calibrated

LockStar Lock onto the current selected star so that other stars are not selected if they come into view

GuidePeriod The time, in seconds, between corrections sent to the mount. Too fast can lead to oscillations, and too slow can result in poor tracking. This tends to be faster for mounts with imperfect gears, but adequate response time to corrections

FrameRate This is the actual frame rate of the camera. The desired frame rate is entered in the Setup dialog, but the true frame rate provided by the camera is shown here

NFrames The number of video frames used in calculating the star centroid. This results in an effective exposure time given by FrameRate/NFrames. The effective exposure time should not exceed the GuidePeriod

StarThresh This value helps select stars in challenging conditions. The star detection algorithm works very well, so this may never need changing – but if stars are visible yet not detected, try changing this

SaveImage Save annotated images of the zoomed in star, plus the main screen. These are PNG files in the output directory specified in Setup. This will document the appearance, profile, and fwhm of the star, both to document your ‘scope’s performance, and to share with others

Flexure Opens the flexure dialog for measuring flexure with another instance of MetaGuide – as described below

ZeroDelta The drift of the star is constantly being measured, and the motion is shown in dEW, dNS, Distance, Rate, and Drift PA. ZeroDelta lets you reset the calculation of this drift. dEW, dNS, and Distance indicate the current displacement from the start, while Rate and PA indicate the rate of drift and its direction, respectively. This can be helpful when drift aligning. Note that since it uses the EW/NS directions, the mount must be calibrated for these to operate.

Upper/Lower These control the appearance of the zoomed in star, to help show the shape and structure of the comatic outer region. Reset will restore them to default values

MetaGuide MetaGuiding is different from normal guiding because it locks onto a specific gear period, measures its amplitude and phase, and corrects for it in realtime. This is useful for fast gearbox terms and terms that are not harmonics of the worm period and therefore cannot be fixed by PEC. The desired period is entered in Setup, and the MetaGuide checkbox causes corrections to be made. As you guide, MetaGuide tracks the corrections and determines the amplitude and phase of the specified period. If something changes about the guiding, press Reset to start a fresh calculation of the phase. Once you see the amplitude and phase stabilize, and while already guiding, press MetaGuide to begin preemptive corrections for the specified term

ShiftRate Described below, these values allow for “shifted” guiding to track a comet or asteroid. Just enter the E and N rates, in “/minute, and press Shift while guiding to begin tracking the guide star, but with the specified drift

Center This button does two different things depending on whether or not you are guiding. If you are not guiding, but you have calibrated, Center will just move the star to near the center of the screen and stop. If you are guiding, Center will set the target location in the center of the screen permanently. This is useful during collimation to force re-centering of the star as you adjust

Dither Every time you press Dither while guiding, the target x/y location of the star will be moved by two pixels in a spiral pattern. This is useful to reduce background noise and avoid hot pixels. Note that it should be done between exposures and not during. This can be controlled remotely, as described below

GuideXY GuideXY allows you to enter a specific x/y coordinate for the guidestar, and guiding will keep it near there. The actual location may be different by +/- 1 pixel or so. Whenever you press Guide, the x/y location are placed there and stored with the .mg file so the exact same camera framing is repeated. This is particularly useful when continuing an exposure run of the same object on multiple nights. Be careful to press GuideXY if you want to use the specified x/y values, because pressing Guide will overwrite those values with the current star position

x, y Pixel coordinates of the currently selected star – also shown in the adjacent plot

East/North East/North coordinates of the star relative to the center of the screen, in arc-seconds. Note that any value involving East/North requires a prior calibration

RA/Dec Drift Drift rate as measured over previous several minutes, in “/minute. This is useful for drift aligning the mount. Note that periodic error can make the RA rate very misleading, since it tends not to be a linear motion but somewhat oscillatory

FWHM This is a very important item indicating the Diffraction Full-Width at Half-Maximum based on the optics, including the secondary obstruction. This can be quite different from the True FWHM, which is measured directly from the live, stacked star profile. Note that the measured FWHM does not represent a measurement of “seeing” because the video images are aligned and stacked prior to the measurement. Furthermore, small f/ratio systems on large pixels will tend to have much larger FWHM’s than expected by diffraction. This is why a view of the Airy pattern usually requires a Barlow to get to around f/30 for the Airy pattern to appear. But when guiding, FWHM should be as small as possible to guarantee good centroid accuracy. Ideally it should be in the 2-4” range if possible

Log Log starts multiple logs of the star location and guide corrections. If the mount is not calibrated, a simple x,y log of the star location is output. If the mount is calibrated, many more quantities are output for use in studying the guiding quality and the periodic error of the mount. More details of the log format are below. The log prompts for a comment each time, but this can be turned off by directly editing the .mg file. Comments can be very helpful to understand what the log captured when viewed much later

MENU ITEMS

File-Save Save the current configuration and guiding parameters in a .mg file. This .mg file will be used by default the next time MetaGuide starts

StarStacking StarStacking determines the type of centroid used for the star position. Centroid is the usual center-of-gravity calculation, while Peak uses a windowed centroid around the point of peak brightness. This avoids biasing the centroid by noise and turbulence in the outer region of the star spot. Peak is the recommended mode, but there is a more extreme version, Point, that uses a very small window around the brightest pixel of the star

Color This mode sets the color of the zoomed in star view in the lower right. Some users may prefer a simple gray scale vs. the colored version

IsoLines This is a simple way to show Isolines in the zoomed in star, to help reveal its shape

Gamma This alters the view of the zoomed in star and can also help reveal its shape. Note that when measuring the fwhm and comparing to the diffraction plot, use Gamma=1

Advanced Advanced/Beginner mode displays or hides more advanced features from the main MetaGuide panel and the Setup dialog. This setting is saved in the .mg configuration file

Simulate If you have a video camera hooked up, Simulate will show the theoretical appearance of the star along with its diffraction pattern. Note that this will tend to be MUCH smaller than the actual star spot unless you are at high f/ratio through Barlowing

Integrate Integrate does two things: it stacks the main camera view to give it a cleaner and lower noise long exposure mode. In addition, this stacked image is used for the centroid calculation rather than centroiding each frame individually. This is useful for viewing faint objects and for guiding on stars that are too faint for detection without integration. But note that integration may lose accuracy compared to live video of a brighter guide star

Help Help should bring up this document in pdf form, but it requires the Adobe Acrobat reader to be installed

About Shows the MetaGuide version number

SETUP DIALOG

Username, Scope Description, and Location are provided for documentation purposes. Log files include the user name and scope description in the file name for convenience

Aperture, Prime FNumber, and Barlow/Reducer magnification help define the image scale and predict how quickly calibration should succeed.

CalFactor can be entered by the user, but its value is normally set by the calibration process after the true image scale is determined. This factor results in the calibrated FNumber and the calibrated focal length

Sec. Obs Secondary Obstruction should be entered as percent of diameter. For an SCT it is typically around 34%, while for a refractor it is 0. This value affects the diffraction pattern – in particular the brightness of the surrounding rings

Frame Rate This is the desired frame rate of the camera. The actual frame rate may be different, and is shown in the main MetaGuide screen. For faint guide stars, use a low frame rate and a small value of NFrames to keep the total time less than the guide period. For bright guide stars or collimation with a bright star, use a high frame rate and large value for NFrames. Examples would be: faint star use 7 fps and NFrames = 5; bright star use 30 fps and NFrames=20

Declination With an ASCOM connection this is filled in automatically, but with other connections you must enter the declination of the current object during calibration and guiding. This value is not very critical, but should be accurate to at least 5 degrees or so. You should set it every time you change declination significantly to calibrate or guide

RA/Dec Rate These are the current autoguide rates set in the mount. For ASCOM, enter desired values and the true values of the mount will be determined automatically. For non-ASCOM connections, you must enter the actual values set in the mount. Typical values are 0.5x sidereal. The RA guide rate should always be <1 to avoid backlash, but the Dec guide rate could be more than 1 if it seems to work better. These values require tuning and experimentation to determine optimal values

WAngleXAxis This value indicates the direction of West relative to the X axis. This is determined by the calibration process and normally the user does not modify it

RA/Dec Agg Aggression determines how much of a correction should be made based on the measured guide error of the star. A responsive mount under good seeing may benefit from a high aggression value of 0.9 or so, while poor seeing may benefit from lower values around 0.5. These values require tuning, and optimal values may vary from night to night

Dec Lash This is a form of software backlash correction. When the guide error of the star reverses direction from N to S, a long pulse of this duration, in milliseconds, is added in to help kick the mount the other direction, taking up backlash. With imbalance in the dec. axis, the optimal pulse time may be greater in one direction than the other. Typical values are 200 ms. This may be used in concert with the mount’s built-in backlash correction

Dec. Reverse This specifies how far the star must drift in the opposite direction in Dec. before corrections are sent, with corresponding backlash pulses. If the value is 0”, then every time the star changes from N to S the mount will react with backlash correction. A value of 0.2-0.5” will reduce how often this kick occurs, and avoid oscillations

Block Corr Corrections can be blocked in any of the directions with these checkboxes. Some people like to offset the polar alignment so a star drifts only one direction, allowing them to disable corrections in the other direction. You can also disable corrections in E/W – for whatever reason

ViewParity This indicates whether the camera view is correct in terms of handedness – i.e. rotation doesn’t matter, but the E direction must be counter-clockwise of the N direction for ViewParity to be false. If it is a mirror image, ViewParity will be checked

NSReversed This indicates whether guide corrections to the mount in the N direction actually move the mount north. Some mounts, such as the CGE, will change the direction in which N moves the mount on a meridian flip. This is described in more detail below

KillHotPixels If the camera view has hot pixels that distract the star detection algorithm, cover the scope and press KillHotPixels. The hot pixels will be identified and removed. This can be very effective both in finding stars well and removing distracting spots from the view

Occultation This is an experimental mode in which the selected star is measured for each frame and dumped to a log with approximate timings. It is not intended for actual occultation timing, but for general experimental needs where a star and/or seeing are monitored at high speed

PixelSize Enter the pixel size in microns, for proper image calibration. Typical values are 5.6um for a Toucam Pro, 7.4um for a SKYnyx 2-0m, etc.

Pixels/Arc-sec, Arc-Sec/Pixel, Field Width, Airy FWHM: These values are all based on the calibrated focal length and on the theoretical diffraction pattern, including the effect of the secondary obstruction

Manual Control These buttons move the mount for one second at guide rate in each of the directions. Holding a button down does not maintain motion – each press is only for one second. This is largely for diagnostics and testing the connection to the mount

UsePrevCal This is an important button that lets you recover a previous calibration as long as nothing has changed in the camera or mount. After you calibrate, press Save or SaveAs and the calibration info will be stored with the mount. On restarting MetaGuide, connect to the mount and press UsePrevCal and the mount will immediately be calibrated and ready to guide on a star. If the camera has rotated at all since the calibration was saved, a fresh calibration should be performed

MeridFlip This is an important button for equatorial mounts after a meridian flip, where the guide camera view may rotate 180 degrees. See below for more details on how to use this feature. You may also need to press NSReversed on a meridian flip

ASCOM/USB Make the correct selection for your mount as described above

ASCOM Chooser If guiding by ASCOM, press this button to select your mount driver and connect to the mount

ScopeName If using ASCOM, this is the ASCOM name of the mount driver, including connections via Hub. This value is saved in the .mg file and reloaded automatically

OutputDir This is the directory in which logs and images are saved automatically. It may be desirable to store a .mg file and logs along with images in the same directory to keep track of the session information, and to compare results and guide parameters later

MetaPeriod Desired period in seconds of the periodic error term to be removed by realtime, phase-locked MetaGuiding. This is different from autoguiding because the single frequency will be preemptively removed while guiding, rather than reactively. The term need not be a harmonic of the worm period – it can be any problematic period

MetaLeadTime This is the time in seconds by which to advance MetaGuide corrections related to the given MetaPeriod. This only applies to MetaGuiding – not normal autoguiding

9. Video Tips and Advantages

Video has an undeserved poor reputation for autoguiding, but it has many advantages both for advanced users and beginners. The key advantage is that everything appears in real time, with no latency or pauses. This lets you catch guide stars when they appear in the view, and lets you see first hand the fine motion of the mount that lead to guiding problems. Video at 8 fps with a SKYnyx 2-0m camera allows my C11 to see guidestars down to about mag. 10. There is no need for the user to squint at the screen to see guidestars since MetaGuide finds even faint stars automatically and places crosshairs on them.

Even focusing is easier with video because it is so interactive and responsive. This makes it possible to use a simple thumbscrew to focus the guide camera, since slight adjustments of the camera are immediately evident in the live view of the star.

A key problem for beginners is simply focusing the guide camera on a star – any star. A good trick is to adjust gamma so that even a faint “doughnut” of an out-of-focus star appears clearly as a large speckled washer in the view. With gamma=1, nothing may appear – but with higher gamma it is evident. It is good to experiment with all the parameters of your video guide camera to help detect out of focus stars, and to help faint stars show when in focus.

Note that collimation with a bright star may require very short exposures – perhaps 1/5000 second, depending on the f/ratio. The profile of the star, in the lower left view, should not be flat at the top, and should only go up to ½ or ¾ of the plot scale.

10. Understanding the Plots

The plots show two curves, and the first item shown is white; the second is red. For example, in the X/Y plot, X is white and Y is red.

The X/Y plot is normalized in each direction, so it goes from left to right and bottom to top for X and Y respectively.

The next plot shows X/Y drift, and is simply a zoomed in view of the first plot. This takes some getting used to, but it is extremely informative. In order to give a sense of the motion of the star in x,y while still at a magnified scale, the plot “wraps” on itself when it goes off scale. Thus a star with increasing X value will rise up from the middle of the plot to the top of the scale, and then drop down abruptly – then increase again creating a sawtooth pattern. It is essential to realize that the sawtooth has nothing to do with the actual motion of the star, except that it is steadily increasing. The frequency of the sawtooth then corresponds to the rate of motion. This is an unusual way to show drift, but once you get used to it, it is very informative.

The Error E/N plot only applies when guiding, and shows the current guide error in arc-seconds in the east direction (white) and north direction (red). By studying this plot as you adjust parameters such as aggressiveness, you can get a feel for how to keep the errors as small as possible, and to avoid oscillations and overshoot.

The FWHM/Intensity plot shows FWHM (white) and Intensity (red) for the star. For best focus, the white line should be low and the red line should be high.

Since MetaGuide uses a rolling set of frames for its centroiding, these plots are always updated twice per second, regardless of the effective exposure for the centroid. This gives much more consistent feedback on focus and on guide tuning.

11. How MetaGuide Improves Centroid Accuracy

There is much talk of the sub-pixel accuracy of centroiding algorithms, but it is usually based on assumptions of nice, round, Gaussian stars and ccd’s suffering only from read noise. In fact, for short exposure guide images, the guidestars tend to be misshapen blobs with ill-defined centers. A typical center-of-gravity algorithm will find the center of mass of that blob and be heavily biased by whatever strange things are happening near the edge. This can result in completely overlooked errors in the centroid that directly increase the resulting error in the guide corrections. In addition, ccd’s are susceptible to other forms of noise, including pixel crosstalk, that cause guide stars to bloat far beyond the size expected based on diffraction and seeing conditions alone.

MetaGuide uses a novel form of “Lucky Guiding” that directly targets the problems of these misshapen stars. Instead of using the entire star in a 1 second exposure to determine the centroid, which would be biased by edge distortions, MetaGuide finds a windowed centroid around the peak of each video image of the star. These stars are sorted based on quality, and the best fraction, specified by AccepFrac, of those stars are used to determine the full centroid. Each of the accepted frames has its own windowed centroid value, and the centroid of those centroids becomes the final centroid used for guiding.

This improved accuracy and avoidance of star edge distortions directly improves the centroid used for corrections. This, coupled with rapid corrections with low latency video allows tight and aggressive autoguiding even with a mid-range mount.

One example of the benefit of this algorithm is to look at the FWHM of stars stacked by the normal centroiding algorithm, and one stacked using the Peak (recommended) centroid of MetaGuide. The version stacked using Peak will have a smaller FWHM. This is essential to resolving the Airy pattern during collimation also.

12. A New Age of Imaging with Mid-Range Equipment

It used to be that astro-imagers would focus on the optics, with less concern for the mount and camera. This changed recently with better autoguiding when people realized how important the mount is in getting small, round stars. Much of the difference is associated with reduced periodic error – but more important may be better bearings and smoother gearboxes – both of which require much more expense to manufacture to the required tolerances and high quality. The situation went from a $300 film camera on a $500 mount with $1000 optics – for example – to a $1000 camera on a $9000 mount with $2000 optics. Without a good mount, better optics were not a win since the results were limited by noise in the mount.

Although autoguiding software and technology have improved over the years, high-end mounts tend to give much smaller star fwhm’s than mid-range mounts using typical autoguiding setups. Adaptive optics can be a cost-effective way to get high-end results from a mid-range mount, but it is limited by the availability of bright guidestars and added complexity of the autoguding setup. What struck me, though, is that mid-range mounts worked noticeably better even when the adaptive optics were operating as slowly as 1 Hz. To me, this meant that tighter autoguiding at the 1 Hz range without adaptive optics might still show improvement, and the two key issues were to reduce latency, and to improve centroid accuracy. With tight corrections every 1 second, using a video centroid, a mid-range mount can now achieve 2” fwhm or less and yield results that rival high-end mounts. This inverts the priority of cost in an imaging setup - reducing the need for an expensive mount, and instead putting more emphasis on the camera and optics.

13. Collimation at the Diffraction Limit

There are numerous ways to collimate a telescope, but many concentrate on the appearance of the out-of-focus star and ignore the in-focus shape. In fact, complex optical designs with several components may show the best stars when the out-of-focus appearance looks misaligned. Although the out-of-focus appearance (e.g. “centering the donut”) is a good first-step in collimating, it should be followed by careful in-focus collimation at high power. Normally this requires a night of very steady seeing, but with MetaGuide the diffraction pattern is more readily visible and collimation based on the in-focus diffraction pattern is now easier.

Understanding the nature of the diffraction pattern and how it relates to star size and resolution involves distinguishing the physical size of the diffraction pattern on the image plane from the angular size it corresponds to in the sky. The former is determined entirely by the f/number of the telescope, while the latter includes the magnifying effect of the telescope’s focal length.

The size of the Airy pattern is proportional to the f/number of the telescope, and independent of the focal length. Thus the size and appearance of the spot formed on a Toucam Pro will be the same for a 5” f/10 as it would be for a 50” f/10 telescope. Only the irradiance would be different, with the 50” concentrating 100 times as much power into the same size disk.

The angular size of these disks will be quite different, however, and will be 10x smaller, in arc-seconds, for the 50” than for the 5”.

In short, the physical size of the Airy pattern depends only on the f/number, while its angular size depends only on the diameter of the telescope.

For some concrete examples:

The angular resolution of a 6” telescope is twice as good as for a 3”, regardless of focal length.

A 3” f/10 will have the same size (in micrometers) Airy pattern as a 6” f/10.

If you have a 3” f/10 and you replace it with a 6” f/5, which has the same focal length, you will quadruple the light-gathering, and you will halve the size of the Airy pattern. This means that for the same detector, the gain in ADU of the central pixel will be roughly a factor of 4x4 = 16!

Of course, this all assumes the seeing and imaging are “diffraction limited” when in fact the measured FWHM of deep sky images is typically much larger due to seeing.

MetaGuide lets you see how your telescope is performing at the diffraction level so that you can collimate it optimally, reduce guiding errors, and keep the net FWHM as low as possible in your final image.

NOTE! You must use a high enough f/ratio for the Airy pattern to be large enough to be resolved with a web-cam’s resolution. This may require a Barlow, and an effective f/ratio of 20-50. At lower f/ratios, the star spot is blurred by the bleeding and crosstalk of the pixels and will be artificially much larger than the diffraction limit. See the examples at the end of this document.

14. The Importance of Saving Images and Tracking FWHM

The SaveImage button creates two .png image files with annotations. One is a small image that shows the raw view of the star, along with the stacked view and the radial profile; the other is the wide view of the camera itself. These images are annotated with many of the optical parameters and capture a great deal of information about your telescope, collimation quality, and seeing.

The images are also annotated with UserName+ScopeDescription on one line, and Location on the next. These lines are truncated to 30 characters, so keep them succinct so they will appear in the PNG dump. The image files are named and indexed automatically based on the date.

People often talk about how great their optics are, and how they saw several rings in the Airy pattern, but until MetaGuide there has been no easy way to document this performance and it is left as a subjective anecdote. MetaGuide allows people to document their seeing with the push of a button, as shown in the examples at the end of this document. This is the first tool that makes it easy to document and compare their star images, with much of the atmospheric effect removed. If someone is boasting about their optics and the diffraction rings – why not push a button and share the result with the world?

15. Pre-Emptive Corrections by MetaGuiding

MetaGuiding refers to dynamically recognizing patterns in the guiding corrections to the mount and locking onto and correcting them in a pro-active rather than reactive manner. This reduces the amount of reactive guiding corrections, with the potential to produce tighter tracking with more optimally tuned guide parameters. This does not require any sort of index as with PEC, but it does require that the user know and provide the frequency of interest.

Currently the mount locks onto a single drive period that the user specifies (in seconds) in the Scope Setup Dialog. A future version will allow the specification of several frequency terms to track.

When guiding is enabled, the RA and Dec. drift rates will be shown, along with an Amplitude and Phase display corresponding to the frequency being monitored. Once the Amp. and phase values appear stable, you may enable MetaGuiding in the Setup dialog, and that frequency term will be proactively corrected.

In addition to the MetaGuide frequency, there is a MetaAggression parameter, along with an Input Lag time that can be adjusted. MetaAggression is the same as Dec. and RA aggression, but refers to the proactive corrections at the specified frequencies. The lag time accommodates the time that the proactive corrections must be applied in advance in order for them not to apply too late. Typical values for MetaAggression and Lag time are 0.9 and 2.0 respectively.

The desired frequency can be determined from an examination of PE logs taken at intervals of 1 second or so to avoid smoothing out high frequency periodic noise. MetaGuide is good for creating such logs, by passively logging the star position in time without guiding enabled. Careful study of the plots may reveal a term in the 5-50 second period range that, if periodic enough, may be removed proactively.

You may need to tune the guide parameters when MetaGuide is enabled.

It may also be beneficial to combine MetaGuiding with PEC. The combination of PEC with proactive correction of a fast term has the potential greatly to reduce the work done by the autoguider.

The proactive MetaGuiding method is novel, but I mainly did it as an experiment to see if it would be a big help in reducing the gear noise that causes hard to correct guide errors that cannot be addressed by PEC. In practice, MetaGuiding may not help much as long as you have PEC enabled and you guide aggressively, with corrections every second and an accurate, tight centroid at long focal length, as provided by off-axis guiding. I encourage additional experimentation with it to see if it helps or not for different mounts.

16. Launching MetaGuide from an Icon

The MetaGuide installation package associates the setup files with .mg extension with MetaGuide, so that launching from an icon will restore the full session settings of that setup. It may be beneficial to store a .mg setup file with each imaging session to keep track of what settings you used each time. Alternatively you can have a single folder with several setup files in it – corresponding to different OTA’s, different cameras, and different reducer/Barlow combinations. You can also launch MetaGuide from a command line, with the .mg file as a parameter.

17. Equipment Tips for Better Autoguiding

Have imbalance both in RA and Dec. for better response

Polar align well so there is minimal dec. drift, and chase dec. errors aggressively

Study the plots to tune the guide parameters so there are no oscillations and no long periods with constant error

Have a good, well-aligned finder scope with crosshairs oriented NS and EW to help center on stars and focus well

RoboFocus is great since it provides absolute focus positioning – allowing you to make changes to the focal train and recover a previous focus set position

I much prefer off-axis guiding with stars at long focal length, rather than a small guidescope. But MetaGuide should work fine at guiding either way

For Off-Axis guiding, get a compact OAG and keep the distance from the pickoff mirror/prism to the guide chip as short as possible. This gives the guide chip a wider view of the light cone and increases the guide star intensity – while also minimizing aberrations. If you have spacers both in the guide path and in the imaging path – try to remove them so spacers are only required in one path

I use a driveway setup, and one thing that improved my productivity enormously is a TeleGizmos 365 series Scope Cover. This allows me to leave equipment set up and aligned even in bad weather, so I can start imaging effortlessly compared to lugging equipment out and setting up each time. Just beware of spiders and wasp nests.

In cold weather I control everything with a Tripp-Lite 36’ USB cable, direct to a powered hub. This is documented at: http://www.astrogeeks.com/Bliss/MetaGuide/images/MultiObjectNight.html

18. Good Vs. Great Autoguiding: Know Your FWHM

I often see people talk about how ‘great’ their autoguiding is with particular equipment – but without quantitative information, it is hard to know just what that means. Some people cite the displayed error of their guidestar while autoguiding, perhaps with values like 0.1” rmsd - but what does this have to do with the size of stars in the image, particularly when flexure may be producing oblong stars?

To me, the best measure of autoguide quality is the roundness and smallness, in arc-seconds, of stars in long exposure images – at least as long as one full worm period. An autoguide setup may be keeping the star roughly centered and even display excellent values for the guide error – but this can all be misleading if the centroid is not accurate or if there is flexure between the guide and imaging chips.

Stars may appear round and small, but when measured they may actually be 6” in diameter, instead of a more desirable 2”. Without measuring the FWHM of stars in 10-20 minute raw exposures (no processing other than calibration with bias, flats, darks) it is hard to know just from appearance just how good the guiding really is.

Widish field imaging with refractors can produce impressive, sharp stars across the field – but due to the short f.l. of the imager, those stars tend to bloat and mask underlying guide errors. This makes for a much easier setup with which to autoguide and image, particularly since refractors can be guided well with guidescopes, but the resulting stars may have FWHM in the 4-6” range, which is much easier to achieve than 2” FWHM with a long focal length SCT. The latter really does require good guiding. For this reason, I recommend noting and tracking the FWHM in your images. This will not only allow you to document and improve your autoguiding results, but you can share them with others in a quantitative way that can be understood and compared. When you get long exposure images in the 2” FWHM realm, you really are starting to guide well.

19. Analog Video Cameras Like the PC164C

There are several very sensitive NTSC/PAL analog video cameras used for astronomical applications such as meteor imaging and occultation timing. Although they are sensitive, they suffer a loss of resolution due to the analog nature of the signal, compression used to encode the signal, and the conversion of the raster scan to a rectangular pixel array in the image. Nonetheless, they can be used with MetaGuide if a suitable video2USB converter is available that outputs 640x480 as needed by MetaGuide.

I have a Dazzle DVC-90 capture device that works with my PC164C. The main problems are numerous hot pixels, that must be removed using the hot pixel remover in MetaGuide, and the fixed video imaging rate. In addition, the more recent version of the PC164C, the PC164C-EX2, is more sensitive but has greatly distorted stars as shown in: http://www.astrogeeks.com/Bliss/OccultVideo/PC164C_EX_Compare.html.

Given these concerns, analog video cameras may not be ideal for collimation or autoguding – but they may work allright. One way to reduce the effect of pixel bloating and compression artifacts is to guide at long focal length – so the angular size of pixel-scale effects is reduced.

20. Usage with NexRemote, TheSky, and Other Applications

NexRemote and MetaGuide work well together with or without ASCOM. First connect NexRemote to the mount, and specify a virtual port for use by other applications – say COM 10. NexRemote should connect to the telescope over a real COM port, nowadays usually a USB2Serial converter. Let’s call that “real” port COM 5.

Once NR is connected to the scope and the mount is aligned, connect MetaGuide to the mount either via ASCOM, USB, or LPT. If you use ASCOM, you should select the celestron driver and connect through the NR virtual port, in this case COM 10.

If you are using ASCOM and you want other apps such as TheSky to connect also, first connect MetaGuide to the ASCOM Hub, and then to the mount as described above. Then use TheSky to connect via the Telscope API to Hub also – at which point all apps should have access to the mount.

If you do not have the Telescope API in TheSky, download it from the ASCOM site.

21. Polar Alignment Using Quick Drift Measurements for Drift Alignment

Drift alignment is a standard method for polar alignment of a mount. It has a bad reputation for being time consuming and difficult, but is well known for the resulting accuracy. MetaGuide makes drift alignment much easier by providing quick feedback on the declination drift of a star as you adjust the mount.

Details of drift alignment can be found at many sites on the web, so I will summarize here how to incorporate MetaGuide in the process.

First, find a brightish star near the meridian and near the equator, and calibrate the mount with it. (You should only have to calibrate the guider once during this whole process.) Do not press guide, but let the mount stabilize for several seconds so the drift plot of the star looks steady. Now press ZeroDelta to reset the measurement of the drift rate of the star. After several seconds, you can read the Dec. Drift rate just left of the plot showing X/Y drift rate. Although the RA drift rate may oscillate due to periodic error, the dec. drift rate should be fairly steady. (I recommend using Periodic Error Correction, PEC, for this process if it is available on your mount – but it is not essential). Note the sign and magnitude of the dec. drift and adjust the mount azimuth control a bit (by physically rotating the mount head – not using direction controls) while keeping the star in view. You may not need to recenter the star as long as it stays on screen, and you definitely do not need to recalibrate the guider (only the mount has changed – not the relationship of the guider to the mount). Press ZeroDelta again and watch the new value of the dec. drift. If it is worse, you know you went the wrong way in your azimuth adjustment. If it is better, you are now on track to get the drift close to zero.

Once the drift of the low star near the meridian is minimal, move to a star low in the east or west and near the equator but probably on the same side of the meridian so you don’t have to meridian flip. Repeat the dec. drift measurement above, but this time adjust the mount in altitude, changing the up/down angle of the polar axis to zero out the dec. drift.

You may iterate this if you like, but just one iteration with an East/West star and a meridian star should get you well polar aligned with much less effort than squinting in an eyepiece trying to gauge star drift.

22. QuickCal, Meridian Flip, View Parity, and NSReverse

FullCalibration will always work to find the orientation of the guide camera, but the added time it takes to move in declination is undesirable. QuickCal does a calibration based on motion only in RA, but you must have ViewParity and NSReverse set correctly or else the N/S corrections will be backwards. You could do QuickCal and press guide – and see if the N/S guiding is centering the star or pushing it away. If it pushes the star away, just press NSReverse and it should then work fine.

A more systematic way to do this is to use ASCOM to do a full calibration, and then make note of the values it finds for ViewParity and NSReverse. An equatorial mount may have different values of NSReverse on either side of the meridian. ViewParity, however, should depend only on the camera and number of mirrors. Normally, ViewParity is OFF if the number of mirrors in the optic path is even – i.e. a refractor or an SCT. But OAG introduces an additional mirror, so ViewParity should be ON with OAG.

The other thing that happens on a meridian flip is the 180 degree rotation of the scene. The Meridian Flip button allows you to do a meridian flip and immediately resume guiding without recalibrating.

To make this concrete, here is how it works for me with my cge:

With OAG, ViewParity is ON because the number of mirrors is ODD.

When imaging in the East, NSReverse is FALSE.

With OAG, when I do a meridian flip, I must also rotate the OAG to recover the guidestar. Thus the view in the guide camera does not change at all – but NSReverse does turn ON in the west, so I must turn it on.

On the other hand, if I guided on my cge with a separate guidescope, I would have:

ViewParity is OFF because it is a simple refractor

Imaging in the east, NSReverse is FALSE

When I do a meridian flip, the view rotates 180 degrees, so I must press Meridian Flip

For my cge, in the west I must set NSReverse to TRUE

This may take some getting used to, but it greatly expedites and simplifies the meridian flip process – which often happens in the middle of the night when people need all the help they can get. If in doubt, do a QuickCal or FullCalibration.

23. Shift Guiding for Comets and Asteroids

The Shift button allows tracking a comet or asteroid that moves slowly relative to the stars. Enter the rate of motion, from a planetarium program, for the object and guide on a star as usual, but with Shift enabled. The guide star will be tracked as usual, but with a growing offset that tracks the comet. If the motion rates are set correctly, the comet can be exposed longer and reveal sharp detail that would otherwise be lost.

High end mounts can track at different rates directly, without the need for autoguiding, but this would not work for mid-range mounts because of periodic error and dec. drift, plus gearbox and bearing noise in both axes. The shift mode of guiding combines the precision of autoguiding with a reference star, plus the accurately know rate of motion of the comet or asteroid. Slow comets can be exposed much longer with no loss of detail, and fast comets remain sharp even though they might be noticeably blurred in a 30 second exposure without shift guiding.

Shift guiding on a fast comet requires some effort because the guidestar will appear to move off the guide chip over time, while the comet remains fixed on the imaging chip (as desired). This means you need to leapfrog from one guidestar to the next as the comet moves along. This requires pre-planning with a planetarium program. It’s important to know the orientation of the tail in order to frame the imaging camera and then choose good guide stars.

This image was guided with Shift enabled, using E/N motion rates read from TheSky. Shift allowed longer sub-exposures while still capturing the sharp edge of the tail. This is comet C/2006 VZ13, and this is a very sharp image of the tail that can be compared favorably with others on the web. This used 2m sub-exposures, which would have been greatly blurred without shift-guiding.

24. Remote Operation with Windows Messages

MetaGuide is aware of numerous messages from other applications on a PC that allow it to work in concert with imaging software such as Astro Art. Astro Art supports a command of the form:

System.Broadcast(message$, wparam, lparam)

MetaGuide supports the following messages – all of which except SHIFT ignore the values of wparam and lparam (so values of 0, 0 are recommended)

MG_RemoteLock	Lock on current star
MG_RemoteUnLock	Disable lock, allowing lock on current brightest star
MG_RemoteGuide	Start guiding
MG_RemoteUnGuide	Stop guiding
MG_RemoteDither	Dither once
MG_RemoteLog	Start Logging
MG_RemoteUnLog	Stop Logging
MG_RemoteSetShift	Set shift rates via wparam, lparam (details below)
MG_RemoteShift	Enable shift guiding
MG_RemoteUnShift	Disable shift guiding
MG_RemoteMeridianFlip	Do meridian flip – rotate guide camera view 180 degrees
MG_RemoteNSReversed	Reverse N/S directions, as for equatorial mount on merid flip
MG_RemoteNSUnReversed	Disable N/S reversal

Remote commands allow scripted autoguiding sessions with a guidescope, as long as the guidescope is guaranteed to find a guideable star wherever it points. You would move the scope to the next object, lock on the brightest guidestar in view, begin guiding, and in between each exposure you would dither. If you move to an object that requires a meridian flip, then the appropriate flip commands should be sent.

A simpler cooperative application is to dither the guidestar between exposures, which must be driven by the imaging application since it knows when the camera is not exposing.

All commands can be sent with wparam = lparam = 0, except for MG_RemoteSetShift. For that command, wparam and lparam map an unsigned integer to a signed, float value corresponding to the shift rates in “/minute. The mapping is:

float ewrate = (wparam-10000)/100.0;

float nsrate = (lparam-10000)/100.0;

The system broadcast command in Astro Art corresponds to the following code that applies to many programming environments:

UINT handle = RegisterWindowMessage("MG_RemoteSetShift");

WinSendMessage(HWND_BROADCAST, handle, wparam, lparam);

25. Off-Axis Guiding with MetaGuide

The high accuracy of the MetaGuide centroiding works best when the guidestar is imaged at long focal length, and there is little flexure in the optics. This is the case with off-axis guiding. Off-axis guiding has a bad reputation due to people years ago randomly searching for a guidestar. This is all different nowadays with planetarium programs that allow custom field-of-view indicators (FOVI’s) that let you pre-plan the best guidestar near your object. If the OAG is calibrated and has direct readout of angles, then the guidestar can be literally dialed in prior to imaging. Instead of hunting for the guidestar, you just hunt for the object itself and roughly frame it – which will then make the guidestar appear on the guide video view. You can then calibrate using that guidestar and commence guiding after optimally framing the target object. Note that the guidestar should be well focused and not too bright or faint – based on studying its intensity profile and fwhm. If the guidestar is too faint, try using Integrate mode.

Off-axis guiding setup showing simple degree indicators.

FOVI view in TheSky showing selected guidestar and corresponding angle.

26. Log Formats

The Logging button starts logging in two separate files. Each file is given a unique name that combines the user name, scope description, date, and an index. One log, MG_XXX_XXX.log, is a simple log of 3 columns containing time, NS, EW (pixels) if not guiding, or time, sumE, sumN if guiding. The former is for passive logging of the star, e.g. for periodic error measurement; the latter can also be used for PE measurement, but is based on the actual autoguider response. The other log file, MG_Full_XXX_XXX.log, is a very detailed listing of values associated with the star, including the MetaGuide phase, amplitude, and corrections. The file has a header line at the top describing the contents in each column.

Note that units of arc-seconds are associated with NS/EW measurements, and units of pixels are used for X/Y screen coordinates.

The PECPrep log is for the EQMOD PECPrep utility, which allows diagnostics of the periodic error and more.

27. Flexure Measurement

MetaGuide can measure small flexure and flop between two mounted telescopes by looking at drift and shift at the sub-pixel level. To do this, start two copies of MG on the same computer and associate each with a different camera. Under the covers the two copies will be communicating with each other. Then select the copy that goes with the longer focal length telescope, connect it to the mount, and calibrate it. The other MG need not be associated with the mount or calibrated.

Then press the Flexure button and a screen will appear as below

Now press Calibrate in the flexure dialog and follow the directions to move the telescope a small amount N/S and E/W. When the flexure dialog is calibrated, begin guiding using the long focal length MG that has already been calibrated and wait a bit as the flexure rate is measured. The radial dial indicates the instantaneous and averaged flexure rates.

To measure flop, place a star in the center of the field and zero the flexure measurement. Then either move the telescope and return to the star, or move to a different star and begin guiding again with the star in the center. The delta value shown, in arc-seconds, corresponds to the flop that has occurred.

Flexure measurement in realtime is particularly challenging since the slow motion on the sub-pixel scale is difficult to measure without noise. MetaGuide displays both the instantaneous values of displacement, along with a linear fit to the past several minutes of motion. Pressing reset will restart this calculation, and over time the flexure rate should stabilize.

It is very important to have the star autoguided and centered during the measurement, due to the precision required in measuring these small drift rates.

MetaGuide is a multi-function telescope tool based on real-time image processing of a video stream.

All it takes is a web-cam that outputs 640x480 video, or a video camera connected to a video2usb converter that outputs 640x480. For guiding, you need either an ASCOM connection, GPUSB, or LPT port interface.

Note that collimation can be done with no connection to the mount at all – but if you want mount control for collimation or autoguiding, you must set up one of these connections.

ASCOM stands for Astronomy Common Object Model and allows plug-and-play connection between astronomical applications and devices. For more details, and to download the latest version and drivers, see http://ascom-standards.org/.

22. QuickCal, Meridian Flip, View Parity, and NSReverse

The following images were all taken with a C11 on CGE, using Off-Axis-Guiding with an SXVF-h9 CCD.