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NOAO Newsletter - Kitt Peak National Observatory - September 1999 - Number 59


KPNO CCD Mosaic Imager Update

The CCD Mosaic Imager is being used almost every night for science; in Semester 1999A, Mosaic was used for 132 nights (48 on the Mayall 4-m telescope, 84 on the 0.9-m), with 121 nights scheduled for Semester 1999B (61 4-m nights, 60 0.9-m nights). In this article, we provide a few updates since our last Newsletter contribution (December 1998). These updates are in the areas of usage, filters, and electronic cross-talk. Please see the article in the CTIO section on the recent commissioning of Mosaic II, a twin of the KPNO Mosaic, at the Blanco 4-m Telescope. Also see the Massey and Slesnick article on photometry with Mosaic.

image
Caption: This Mosaic image of the field of M81 and M82 by G. Jacoby and P. Massey illustrates the power of Mosaic to observe the sky on a scale formerly available only through large photographic plates, but with over 100 times the efficiency of photon detection and greater accuracy of measurement. This 60' × 40' R-band image was taken at the KPNO 0.9-m telescope during bright time. It is a dithered sequence of five 300s exposures using Mosaic I, processed with the IRAF Mosaic package MSCCRED.

Two new Mosaic filters have been commissioned: Washington M and DDO 51. These allow luminosity discrimination between late-type dwarf and giant stars (Geisler 1984, PASP, 96, 723). The ongoing U filter construction saga that we reported in the last Newsletter article has been completed successfully. A liquid copper sulfate U filter, with transmission properties nearly identical to our standard 4-inch U filters, has been in use since January 1999. Please see the Mosaic Web page for a complete list of supported filters (http://www.noao.edu/kpno/mosaic).

There is some low-level electronic cross-talk between pairs of CCDs in the Mosaic that are attached to the same controller. The cross-talk is not bidirectional. For example, a bright star on CCD[2] produces a "ghost" on CCD[1], but the converse does not occur. The strength of the cross-talk ghosts appears to be directly proportional to the input signal on the "contaminating" chip, with scaling coefficients of order 1/1000. The coefficients have been measured for the science-grade Mosaic I camera, and can be used to remove cross-talk ghosts within the IRAF MSCRED package, applied as the first data processing step in CCDPROC. The residuals from this correction are less than or approximately equal to 1 ADU, even for saturated objects. Within the accuracy of the measurements, the coefficients have remained stable from January through June 1999. Cross-talk correction is now included in the default Mosaic data reduction procedures of IRAF V2.11.2's mscred.ccdproc task.

Taft Armandroff, George Jacoby, James Rhoads


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