Zenith camera

A zenith camera combines an optical lens (about 10–20 cm aperture) with a digital image sensor (CCD) in order to image stars near the zenith. Electronic levels (tilt sensors) serve as a means to point the lens towards zenith. Zenith cameras are generally mounted on a turnable platform to allow star images to be taken in two camera directions (two-face-measurement). Because zenith cameras are usually designed as non-tracking and non-scanning instruments, exposure times are kept short, at the order of few 0.1 s, yielding rather circular star images. Exposure epochs are mostly recorded by means of the timing-capability of GPS-receivers (time-tagging).

Depending on the CCD sensor - lens combination used, few tens to hundreds of stars are captured with a single digital zenith image. The positions of imaged stars are measured by means of digital image processing algorithms, such as image moment analysis or point spread functions to fit the star images. Star catalogues, such as Tycho-2 or UCAC-3 are used as celestial reference to reduce the star images. The zenith point is interpolated into the field of imaged stars, and corrected for the exposure time and (small) tilt of the telescope axis to yield the direction of the plumb line.

If the geodetic coordinates of the zenith camera is known or measured, e.g., with a GPS-receiver, vertical deflections are obtained as result of the zenith camera measurement. Zenith cameras deliver astronomical coordinates and vertical deflections accurate to about 0.1 seconds of arc. Zenith cameras with CCD image sensors are efficient to collect vertical deflections at about 10 field stations per night. Zenith cameras have been used for accurate local surveys of Earth's gravity field (geoid, quasigeoid).

• Geodetic astronomy
• Geoid
• IERS
• Zenith telescope

• Hirt, C.; Seeber, G. Accuracy analysis of vertical deflection data observed with the Hannover Digital Zenith Camera System TZK2-D. Journal of Geodesy 82(6): 347-356. doi:10.1007/s00190-007-0184-7. (PDF).