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

By Paola Amico, James W. Beletic

th The four ESO CCO Workshop, Optical Detectors for Astronomy, used to be held in the course of September 13-16, 1999 at its traditional place, the headquarters of the eu Southern Observatory in Garching, Germany. We like to have in mind this workshop as a "meeting of friends", who got here to Garching to go to ESO and to provide their paintings, instead of a proper assembly. in line with our adventure with the 1996 ESO CCO workshop, we intentionally placed emphasis on developing an atmosphere that inspired the individuals to stick jointly and informally alternate principles. those casual occasions started with a journey of the BWM automobile manufacturing facility and persevered with a reception at "SchloB Beletic", the convention dinner at a true SchloB of the Bavarian overseas tuition (where the members loved basket, baseball, desk football, mountaineering and at last dancing) and concluded with a travel of the Paulaner Brewery and dinner on the Seehaus within the Englisher Garten. The lunch "Biergarten", adjoining to the poster consultation sector, was once an everyday assembly element. the end result used to be a very good mix of first-class displays and posters, amassed in those court cases, and plenty of events for individuals to get in contact and to have a good time jointly, as witnessed by way of the choice of workshop photographs that we randomly put among papers. This booklet incorporates a exact contribution.

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M), should be less affected by it, we measure the same amount of PRNU for both devices. However, the MIT device has a higher spatial frequency of fringing, which means that the surface of the CCD is flatter and its parallelism is improved (see fIgure 16, left). .............. '~ -----. " 40 Cyril Cavadore, Reinhold J. -.. ~ ( Figure 16. Left: typical image of a NIR (850 nm) fringing pattern (bandwidth=5nm). 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).

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.

32 Cyril Cavadore, Reinhold J. 8 Days Figure 6. Remanence/residual image effect after flat field taken at t=O . .. ~ ~ ... Figure 7. Top: 2048x5I2 pixel subframe, one hour exposure dark frame, just after a flat field. The dark current is 43e-/pixel/hour and it is caused by the blue diamond pattern. Center: 2nd I-hour dark frame, the diamond pattern is fainter, IOe-/pixel/hour of dark-current. The overscan and prescan areas are visible. Bottom: 28 th I-hour dark frame, dark current has reached the minimum value (4e-/pixlhour) for the operating temperature of 160 K.

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