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CAMERA AND TRIPOD
One of the easiest ways to enter the field of astrophotography is to mount a camera and lens on a tripod and take a brief time exposure. The camera should be set in Manual mode. This will allow you to keep the shutter open with a remote release. A remote timer release is essential even if you are taking shorter exposures as it is almost impossible to manually release the shutter without causing the telescope to shake, degrading the image. One possible solution would be set set a time delay before the shutter releases. This would give the tripod a chance to stop vibrating.
Using a camera and tripod, you can record far more stars than are visible with the naked eye. However, there are distinct limits to how long your exposure can be before the stars begin to look like streaks rather than points of light. This is due to the rotation of the earth on its axis. The length of time that you could expose the film before trails start to appear depends on the focal length of the lens you are using. The section of the sky you are photographing is also a factor. Over the same period of time, stars near the celestial pole move a much shorter distance than do stars near the celestial equator.
The Rule of 500 is a classic and easy way to calculate exposure time. This is simply: 500 / Focal Lenght of Lens. For example, using a 50mm lens, you should be able to take a 10 second exposure without seeing any star trailing. However, this method has its limitations. It was originally based on full-frame cameras using high ISO film. Today's digital cameras have much higher resolution and a 10 second exposure with a 50mm lens may produce stars trails. It may be more helpful to use a 'Rule of 400' when calculating your exposure time. That is, divided 400 by the focal length of the lens you are using.
A much more accurate formula is the NPF rule. In addition to the focal lenght
of the lenss, this formula includes the pixel size of your camera and aperture
of the lens what aperture you are shooting at.
The NPF formula is: (35 x lens aperture) + (35 x pixel pitch) / Lens focal length. Not everyone readily knows the pixel pitch/size of their camera. This can be easily obtained if you do a search on the specs of your camera. Most range from 4 to 8 microns. A simpler option would be to use an app such as PhotoPills. This has a drop down menu of the most common cameras. You simply select your camera and the app inputs the data into the program. This app also makes adjustments for the location of the sky you are shooting. In a pinch, it never hurts to get a rough estimate using the Rule of 400 and bracketing your exposures. Star trailing is often not even noticeable unless you zoom in on a section of the image (or print/post a very large image). The important thing is that you are shooting under dark, clear skies.
There may be times when you want to capture the long-term effect of star trails. Such photos can be very dramatic (http://astronomyphotos.com/StarTrails.htm). In this case, it is best to use a low ISO setting and leave the shutter open for many minutes, even hours. Also, star trails are not a problem when you are attempting to capture meteors or aurora. In any case, do not be too quick to overlook this method. You can obtain some nice shots with little effort or expense.
The piggyback method of astrophotography is so named because you attach your camera atop a telescope that is clock driven on an equatorial mount. This technique allows you to take longer exposures (e.g., 5-10 minutes), capturing much fainter stars and deep-sky objects than would not be possible with a simple camera and tripod. It is still very easy to accomplish. Several types of mounting brackets are commercially available to fit most telescope tubes. Many telescope tube rings already come with a 1/4-20 threaded bolt to hold a camera body. You should be cautious using this method with lenses that exceeds 300mm focal length. Beyond this (unless you have an exceptional mount), additional guiding would be necessary.
Several stand-alone tracing mounts are available on the market. These include the Sky-Watcher Star Adventurer, Vixen Polaire, and iOptron Skytracker. Of course, these will be an additional expense but the results can be exceptional.
Features in the foreground tends to become blurred during piggyback exposures. While the telescopeís clock drive keeps the stars from trailing on the film, it causes any fixed objects to gradually distort. The longer the exposure, the more noticeable the distortion. Some people overcome this problem by layering a still shot of the background onto the night skyline.
Most of the images contained in this site were obtained through the prime focus method. In this technique, the camera body is directly attached to the rear of telescope tube. Many types of telescopes are suited for prime focus shots and camera adapters are available for each of them. The telescope essentially acts as a camera lens. The image size and field of view are determined by the focal length of the telescope. The f/ratio of your setup is simply the diameter of your telescopeís objective lens divided by its focal length. Occasionally, one may use a focal reducer to provide a wider field of view as well as allow for shorter exposure times.
This method requires additional guiding of the telescope during long exposures. We cannot just trip the shutter and sit back because no clock drive is totally accurate. There is periodic error in the gears that drive the shaft. This causes the drive to run a bit slower or faster than ideal. Even if a perfect clock drive existed, atmospheric refraction would cause a shift in the apparent location of an object over time.
Accurate polar alignment is essential before any time exposure can begin. If the mount is not aligned properly, the star field would appear to rotate around the object you are photographing, regardless of how well your mount's clock drive works. The results would look similar to those you would obtain by taking a long exposure of Polaris with a camera and tripod.
Once you have polar aligned your telescope mount, you are ready for prime focus astrophotography. There are basically two methods used to make fine tuning in our guiding: 1) a separate guidescope or, 2) an off-axis guider. Each has its merits and problems. A separate guidescope makes it much easier to locate a suitalbe guide star. But the guidescope must be securely attached to the main telescope or mount. Otherwise, differential flexure will likely occur. This means that gravity will pull the various components on the mount unevenly. Although the guide star may not move as viewed by the guidescope, it would move in relation to the main scope. Isolating the source of flexure can be difficult. An off-axis guider avoids this problem. It is inserted between the telescope and the camera and a small prism deflects a portion of light from the edge of the telescopeís actual field of view. Guiding is much more accurate with this approach. However, it does make acquiring a guide star more difficult, particularly if you are imaging an object that is far from the galactic equator.
There will be times when you will want to obtain a larger image size than is possible through prime focus photography. This is most often the case in planetary or lunar photography. Eyepiece projection is the preferred method in these situations. This method requires a fairly inexpensive camera adapter that allows you to place an eyepiece (or barlow lens) between the telescope and camera. The image is projected onto the film plane. This drastically increases the f/ratio of the system and is therefore not typically suitable for deep sky photography. To determine the effective f/ratio or overall focal length of your system, use the following formulae:
|Effective f/ratio = f/ratio of telescope x [(d - FL of eyepiece)/ FL of eyepiece]|
|Effective FL = FL of telescope x [(d - FL of eyepiece)/ FL of eyepiece]|
where d is the distance between the field stop of the eyepiece and the sensor
plane. For example, using an f/8 1200mm FL scope with a 12mm eyepiece that is
70mm from the focal plane:
|f/ratio = 8 x [(70 - 12)/12] = 8 x (58 /12)|
|= 8 x 4.83|
|The effective FL would therefore be 1200 x 4.83 = 5796mm|
You can also use a barlow lens for what is called negative projection. The formula for figuring out the effective f/ratio is identical to that used with eyepiece projection except for the fact that a barlow lens has a negative focal length; thatís why itís called negative projection.
Many people use the camera on their phone to capture images through a telescope. While these cameras are generally not suited for astrophotography, you can capture some nice images of the moon and planets using eyepiece projection. There are several fairly inexpensive adapters that allows one to attach their phone to a telescope's eyepiece.
Photographing the sun allows us to use a variation of the eyepiece projection technique. This involves attaching a white card on a dowel and placing it approximately one foot away from the eyepiece. The projected image readily show sunspots and transits of the inner planets across the sun's disk. It also allows us to photography various phases of a solar eclipse. You can simply photograph the projected image with a hand-held camera. Needless to say, never look at the sun through a telescope unless you have a solar filter on it.
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