Astrometry with Optic at WIYN

Astronomy and Astrophysics – Astronomy

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Scientific paper

The astrometric precision of Orthogonal Transfer CCDs (OTCCDs) is investigated, using the OPTIC camera at WIYN 3.5-m telescope. The precision of the positions, determined with the Yale image-centering code, was used to establish astrometric design requirements for the anticipated WIYN One Degree Imager camera that will use similar technology.
OTCCDs are able to electronically compensate for real-time image motion, providing tip/tilt corrections without additional optics or moving parts (Tonry et al. 1997, PASP, 109, 1154). The Orthogonal Parallel Transfer Imaging Camera (OPTIC) consists of two 2K by 4K OTCCDs arranged in a single dewar mounted adjacent to each other with a small gap between the chips. Each chip is electronically divided into two regions, and each of these is further subdivided into two parts: a guide region and a science region. When mounted on WIYN, the camera has a scale of 0.14 arcsec/pixel, and a 10 × 10 arcmin field of view. OPTIC has a read noise of < 4 electrons when read at 160 kpix/sec and a nominal gain of 1.45 e^-/ADU.
To test the astrometric performance of OPTIC, we imaged the open cluster NGC 188, during 7 nights in october 2003, using Johnson-V and Gunn-i filters ranged from 0.6 arcsec to 3 arcsec, but only frames with < 2 arsec were considered for this study. After a careful internal astrometric reduction, we estimate that OPTIC achieves a precision of 2 milliarseconds over the dynamical range of the CCDs. This precision is obviously affected by the stability of the atmosphere, so these results demonstrate that the unique charge tranfer donde by OPTIC, which tracks the motion of a guide star, is able to stabilize the field within the atmospheric isokinetic region to the level of a few milli-arcseconds.

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