Large multichip arrays for close-abutted CCDs (charged-coupled devices) are needed for surveillance applications in the visible band and for X-ray astronomy missions such as the Advanced X-ray ...Astrophysics Facility and the ASTRO-D satellite. A 420*420 pixel frame-transfer CCD imager which is designed to be abutted to other imagers on three sides so that arrays of 2*N chips can be constructed has been developed. A three-phase, triple-poly, buried-channel process is used, and the die size is 12 mm*20 mm. The arrays provide low-noise readout circuitry and high charge-transfer efficiency at low charge levels, critical requirements for both of the above applications. The device has also been shown to be suitable as a soft X-ray imager operating in a spectroscopic mode.< >
We are constructing a Ring Imaging Cherenkov detector (RICH) for the CLEO III
upgrade for precision charged hadron identification. The RICH uses plane and
sawtooth LiF crystals as radiators, MWPCs as ...photon detectors with TEA as the
photo-sensitive material, and low-noise Viking readout electronics. Results of
a beam test of the first two out of total 30 sectors are presented.
Joint-gate, vertically stacked CMOS (JCMOS) inverters have been fabricated by a process which utilizes a multilayer substrate consisting of an oxidized n-type silicon wafer upon which are deposited ...two uniformly p-doped polysilicon films separated by a thermally grown (gate quality) oxide. The upper polysilicon film is re crystallized by a scanning CW argon laser and serves as the nMOS substrate. The lower film is the joint polysilicon gate and is heavily doped p-type rather than n-type in order to allow fabrication of enhancement-mode nMOS devices with reduced vertical electric field after threshold voltage adjustment by ion implantation. Fabrication proceeds using a six-mask, self-aligned, top-down process. The W/L ratio was 88 µm/38 µm for the nMOS upper device and 88 µm/60 µm for the pMOS lower device. By virtue of the self-aligned process, both devices can be scaled to smaller dimensions, yielding approximately a 40 × 8 µm inverter in 4 µm channel length technology.
The CLEO detector has been upgraded to include a state of the art particle identification system, based on the Ring Imaging Cherenkov Detector (RICH) technology, in order to take data at the upgraded ...CESR electron positron collider. The expected performance is reviewed, as well as the preliminary results from an engineering run during the first few months of operation of the CLEO III detector.
A 100ns 16-point CCD cosine transform processor Chiang, A.; Bennett, P.; Kosicki, B. ...
1987 IEEE International Solid-State Circuits Conference. Digest of Technical Papers,
1987, Letnik:
XXX
Conference Proceeding
A CCD based on the vector matrix product algorithm, that has been implemented using 256 fixed weight four-quadrant multipliers will be described. 1.5 billion operations/s 40dB dynamic range and 1% ...accuracy have been demonstrated at a 3.3 MHz clock rate. The chip size is 4mm square and it dissipates 720mW.
What are the faintest distant galaxies we can see with the Hubble Space Telescope (HST) now, before the launch of the James Webb Space Telescope? This is the challenge taken up by the Frontier ...Fields, a Director's discretionary time campaign with HST and the Spitzer Space Telescope to see deeper into the universe than ever before. The Frontier Fields combines the power of HST and Spitzer with the natural gravitational telescopes of massive high-magnification clusters of galaxies to produce the deepest observations of clusters and their lensed galaxies ever obtained. Six clusters-Abell 2744, MACSJ0416.1-2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063, and Abell 370-have been targeted by the HST ACS/WFC and WFC3/IR cameras with coordinated parallel fields for over 840 HST orbits. The parallel fields are the second-deepest observations thus far by HST with 5 point-source depths of ∼29th ABmag. Galaxies behind the clusters experience typical magnification factors of a few, with small regions magnified by factors of 10-100. Therefore, the Frontier Field cluster HST images achieve intrinsic depths of ∼30-33 mag over very small volumes. Spitzer has obtained over 1000 hr of Director's discretionary imaging of the Frontier Field cluster and parallels in IRAC 3.6 and 4.5 m bands to 5 point-source depths of ∼26.5, 26.0 ABmag. We demonstrate the exceptional sensitivity of the HST Frontier Field images to faint high-redshift galaxies, and review the initial results related to the primary science goals.
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