The astro-photographic capability of the telescope is based on the style, stability, and accuracy of the mount and tripod. Telescopes on either very lightweight mounts or non tracking mounts (such as Dobsonians) are capable of only very short exposures such as lunar photographs. If a motor drive is attached to an equatorial mount, even a small lightweight mount is capable of capturing some planetary detail. Larger EQ mounts that utilize very precise tracking and excellent stability are capable of longer exposure deep-sky photography.

The weight rating is a measure of how much the mount can handle before vibration become excessive. This specification is dependent on the shape of the telescope. For example, if you have two telescopes that both weigh 15 lbs., but one is a Cassegrain with a very short tube and the other is a very long focal length refractor, the Cassegrain will be more stable due to the fact that the tube itself is much shorter. The extra length of the refractor tube acts as a "lever arm" and vibrations become much more prominent. So be careful as you approach the weight capacity limit that you don't overload the mount with a very long tube.

A universal attachment system for holding the optical tube onto the tripod. A dovetail bar is attached to the tube rings, then it slides onto the mount itself, making for quick assembly and disassembly.

A motor drive automatically moves the telescope in right ascension at the same rate as the east-west drift of the stars so stars can be continuously tracked in the eyepiece without manual adjustment. Motor drives are usually equipped with a hand control that allows the telescope's tracking speed to be slightly increased or decreased, which is particularly critical when taking long-exposure astro-images.

Some mounts are compatible with a motorized Go-To system for fully automated computer finding of objects in the night sky. Other mounts are compatible with computer finding systems which require the user to manually move the mount to the object's position as indicated by the computer finder.

Periodic errors are inherent in almost all worm gears due to slight eccentricities and misalignments. PEC (Periodic Error Correction) training function provides a manual correcting method to reduce the amplitude of the worm gear errors. By recording a full cycle of guiding actions, the mount can compensate for drifting in the R.A. sidereal tracking caused by periodic errors. The PEC training function is recommended for advanced users with interest in long-exposure astrophotography. Standard sidereal tracking is sufficient for all casual visual applications, and PEC training is not required. Also, PEC is typically not used in conjunction with an auto-guider.

A GPS module automatically sets the date, time and location for the mount, relieving the user from the need to look up coordinates on a map or manually enter perfect time. This can be very beneficial when traveling with the scope as locations can quickly be automatically entered into the hand control.

The latitude range refers to the usable range on the EQ mount's latitude axis. If you live above or below the latitude specified, the mount may not be able to polar align properly because of interference with the counterweight shaft or the polar axis housing.

Ports allow the mount to connect to devices such as autoguiders (for long exposure photography without tedious manual guiding), PC's running planetarium software (via the RS-232 port) and GPS receivers (through the Aux port).

The height range specification is a measure of the tripod itself - not the eyepiece height. Since telescopes come in all shapes and sizes, the eyepiece height will vary, even when using the same tripod. For an EQ tripod the mount is set up so the counterweight shaft is horizontal, and then the height is measured from the ground to the center of the mounting plate.