About Telescopes

There are three basic types of telescope design (refracting, reflecting, and catadioptric),
and the Robert Ferguson Observatory operates
all three types.

Size refers to the primary mirror or refracting glass used in the telescope–not the length of the telescope or the magnification.

The larger the primary mirror or refracting glass, the more light is gathered. The "object"—a galaxy, for example—appears brighter to the observer.

Magnification is dependent on the focal length of the telescope and the specific eyepiece used.

Filters of various types can be used to help emphasize certain features of the object being observed. Oddly enough, a green filter can bring out surface features of the red planet Mars.

Other devices attached to a telescope may include one or more "spotting scopes"—smaller telescopes that provide a wider field of view to assist the operator in finding objects.

Telrads are devices which generate a red laser ring "target." When the operator moves the telescope so that the desired object is centered in the target, it will also be visible in the telescope's eyepiece.




RFO Telescopes and Equipment

Reflector Telescope
The West Wing houses a 24" reflecting telescope. This telescope's focal ratio is f/5, with a focal length of 274cm. The entire telescope weighs about one third of a ton. It is supported below the building by three concrete piers.

24-inch ReflectorMounted on the side of the giant 24" scope is an 8" reflecting spotting scope which also functions for observing. There are two other spotting scopes and a Telrad finder.

This telescope is on loan from Bill Russell, board member and docent, and will be replaced with an even bigger one in 2015 (see Project 40)

How it works: The light from an object enters at one end of the telescope and travels the length of the tube where it is reflected off a 24" diameter parabolic mirror. The light then travels back in the opposite direction where it hits a secondary mirror near the end where the light first entered. The secondary is set at an angle of 45º. The light then exits the telescope through a hole in the side of the telescope to an eyepiece.

Refractor Telescope
8" ScopeThe white dome houses a two-meter-long refractor. Attached to the side of the telescope are a spotting scope and a Telrad finder. A tracking motor moves the telescope to counteract the Earth's rotation, so that an object in the eyepiece will stay there over a period of time as the Earth moves. This telescope made its way to RFO from Dominican University in San Rafael.

How it works: Light enters at one end of the telescope through an 8" piece of refracting glass which slightly bends the light. The light rays converge together at the opposite end of the telescope where a small 45º mirror directs the light out to an eyepiece.

Refractor Diagram


Robotic (CCD) Telescope
The East Wing houses a 14" Celestron Schmidt-Cassegrain telescope, a type of catadioptric telescope that "folds" the light path. This telescope is unique Telescopes-CCDat RFO for two reasons: First, it is the only telescope where visual observation is not done. Instead of an eyepiece on the back, a scientific-grade camera is attached for astrophotography and research. Second, the entire system—tracking mount, camera, focuser, and filters—is computer controlled.

This sensitive camera system (called a "CCD" for charge-coupled device, referring to the camera’s chip) is capable of imaging objects hundreds of millions of light-years away. It can also image asteroids and comets to help ascertain their positions and orbits, and can provide data on a star's light, giving astronomers insight into the star's physical properties. Contributions to professional research projects are made with data generated from image analysis. Take a look at our Astrophotography and Research projects.

Mount: Paramount ME
Camera: Apogee U47
Autoguider: Orion Star Shooter
Filters: Optec (LRGB and photometric filter wheels)
Focuser: Optec TCF-5

Sky6 Professional with Tpoint
(planetarium and mount control)
CCD Soft (image acquisition)
PHD Guiding
CCD Stack
AIP (image processing and data analysis)

SCT DiagramHow it works: Light enters at one end and passes through a piece of glass, travels to the other end where it is reflected off of a 14" mirror. The light then travels back up the tube where it is reflected back again with a smaller secondary mirror. The 14" primary mirror has a small hole in its center: the light at this point travels through the hole and out the back of the telescope.

The CCD telescope was made possible by a major donation from philanthropist Rob Cook.

Solar Telescopes
RFO has two methods for observing the Sun—safe direct observation through heavily filtered telescopes, and radio antennae which record fluctuations in activity.

The telescope at right rear is a powerful 80mm Lunt refractor with a red hydrogen-alpha filter. It images the solar chromosphere (atmosphere) and shows prominences, filaments and granules.

The nearer scope is an 80mm Orion refractor with a neutral density filter. It images the solar photosphere (surface) and shows sunspots in high detail. Our "Sun Spotter" apparatus is in the center.

How they work: The light path diagram for our 8" Refractor applies to both these refractors.

Funds for the Lunt telescope were provided by the California State Parks Foundation and private donations. The telescope was dedicated in memory of beloved observatory docent and solar astronomer Merlin Combs.

The Radio Telescope consists of antennae attached to the Observatory's walls which feed radio and audio signals to the indoor classroom computers.

We can hear the Sun's activity,
and see radio graphs projected onto an indoor screen for public observing. Radio astronomer Dean Knight examines the fluctuations appearing on today's graph.

Next: Project 40—Building a Bigger Telescope

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