During the past year, the SLD Collaboration completed construction and began operation of a new vertex detector (VXD3) with 307,000,000 CCD pixels. This upgrade will improve the SLD measurement of the polarization-enhanced forwardbackward asymmetry for band cquarks and the precision of the measurement of the b-fraction in hadronic Z decays and opens the possibility to observe ~~-m.ixing. Full s...

This paper presents a new approach for measuring physical variables on micro-electronic components. An optical system is used to simultaneously quantify the surface temperature of a component and its expansion. This double acquisition is realized by a Michelson interferometer coupled with a Charge Coupled Device (CCD) line device. To validate this method, the temperature measurements were direc...

Currently the creation of textures for construction of Visually Realistic Models (VRMs) of buildings is a time consuming manual process involving the use of a number of separate software applications and substantial skill by the user. This paper presents the development of a novel procedure for the semi-automatic construction of textures, which makes use of a Charge Coupled Device (CCD) camera ...

A charge-coupled device (CCD) capable of 200 Mpixels/s readout has been designed and fabricated on thick, high-resistivity silicon. The CCDs, up to 600 microm thick, are fully depleted, ensuring good infrared to x-ray detection efficiency, together with a small point spread function. High readout speed, with good analog performance, is obtained by the use of a large number of parallel output po...

Calibration procedures are described for use with electronic x-ray detectors, with an emphasis on detectors based on fiber-optically coupled charge-coupled devices. Methods are detailed for removing spurious events, pixel pedestals, dark-current, spatial distortion, and intensity response variations for both small-angle and wide-angle applications. The accuracy of the calibration procedures is ...

Comet P/Halley has been observed during its approach to perihelion at heliocentric distances R = I 1.0 AU and R = 8.2 AU. No extended coma is seen and limits can be placed on the fraction of the total light contributed by coma. The brightness of the comet varies on a short time scale. The variations may be due to transient activity or to rotation of the irregular nucleus. ,. 1984 Academic Pre',...