Optical Detectors For Astronomy II: State-of-the-Art at the by Paola Amico, James W. Beletic PDF

By Paola Amico, James W. Beletic

ISBN-10: 9401058768

ISBN-13: 9789401058766

ISBN-10: 9401143617

ISBN-13: 9789401143615

th The four ESO CCO Workshop, Optical Detectors for Astronomy, used to be held in the course of September 13-16, 1999 at its ordinary situation, the headquarters of the ecu Southern Observatory in Garching, Germany. We like to bear in mind this workshop as a "meeting of friends", who got here to Garching to go to ESO and to offer their paintings, instead of a proper assembly. in keeping with our adventure with the 1996 ESO CCO workshop, we intentionally placed emphasis on developing an atmosphere that inspired the contributors to stick jointly and informally trade principles. those casual occasions started with a journey of the BWM car manufacturing unit and persisted with a reception at "SchloB Beletic", the convention dinner at a true SchloB of the Bavarian foreign university (where the individuals loved basket, baseball, desk football, mountain climbing and finally dancing) and concluded with a journey of the Paulaner Brewery and dinner on the Seehaus within the Englisher Garten. The lunch "Biergarten", adjoining to the poster consultation region, used to be a regular assembly aspect. the outcome was once a very good mix of first-class shows and posters, amassed in those lawsuits, and plenty of events for individuals to get involved and to rejoice jointly, as witnessed by means of the choice of workshop photos that we randomly positioned among papers. This e-book encompasses a specified contribution.

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Extra info for Optical Detectors For Astronomy II: State-of-the-Art at the Turn of the Millennium

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Right: typical image with a brickwall pattern visible at 350 nm (bandwidth=5nm) In figure 17, the high PRNU in the wavelength range 300-400nrn (up to 40%) for the MITILE device is related to the backside laser annealing process (see also the "brick wall" pattern in figure 16 right). The next MITILL devices have been manufactured with an enhanced laser annealing process and the brickwall pattern should be reduced. 60 ~ 50 40 ~ \ I~EEVI ~MIT / 20 1\ 10 o 300 '\ '-400 ~ 500 ~ 600 700 800 Wavelength (nm) V 900 /V1000 1100 Figure 17.

In addition the QE curve for the most sensitive device in the ultraviolet is shown. This CCD was then selected for the blue arm of the UVES instrument. All the QE curves have been obtained with the ESO CCD Testbench [1]. Cyril Cavadore, Reinhold J. Dom and James W. a ~ "- . J. '1 VI 50 40 ~ '\{ "- ~ 30 20 ~ 10 a 300 ~ 400 500 600 . 700 800 900 r--. 1000 1100 Wavelength Figure 1. Average QE of 12 EEV44·82 devices. Error bars show the QE standard deviation. 3 Photo Response Non Uniformity (PRNU) Fringing patterns in a CCD image make the flat-fielding process of the image difficult, especially for images taken with a spectrograph.

W. Beletic, (2000). "Computer simulation of CCDs and APDs for curvature wavefront sensing. In: Adaptive Optical System Technology", SPIE Proceedings, vol. 4007. 5m Telescope T. Fechner, D. M. Roth Astrophysikalisches lnstitut Potsdam Abstract: PMAS, the Potsdam Multi-Aperture Spectrophotometer. 5m telescope, under development at the Astrophysical Institute Potsdam. With kind permission of the ESO Optical Detector Group, ESO designs for the CCD detector heads and controllers have been employed. We will describe the current status of the project and report on the performance of the 2 CCD systems that are built into PMAS.

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Optical Detectors For Astronomy II: State-of-the-Art at the Turn of the Millennium by Paola Amico, James W. Beletic

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