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 situation, the headquarters of the ecu Southern Observatory in Garching, Germany. We wish to consider this workshop as a "meeting of friends", who got here to Garching to go to ESO and to give their paintings, instead of a proper assembly. in response to our adventure with the 1996 ESO CCO workshop, we intentionally placed emphasis on growing an atmosphere that inspired the members to stick jointly and informally trade rules. those casual occasions begun with a travel of the BWM vehicle 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 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 quarter, used to be an everyday assembly aspect. the outcome was once a great mix of very good shows and posters, accumulated in those lawsuits, and plenty of events for individuals to get involved and to celebrate jointly, as witnessed via the choice of workshop images that we randomly put among papers. This booklet includes a targeted contribution.
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Extra resources for Optical Detectors For Astronomy II: State-of-the-Art at the Turn of the Millennium
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5 mm. 7 mm in the vertical direction in the mosaic. 1 27 Noise performances Table 1 lists the noise performance achieved with the EEV44-82 at different readout speeds and conversion factors (eo/ADD). The noise was measured with the instrument under full operations at the telescope. Table 1. 7 Instrument UVESNIMOS UVESNIMOS WFI VLT test Camera 2 (Full array, 1 port The noise figures may vary slightly (-10%) for different devices. Conversion factors less than 1 eO/ADD are mainly used for spectroscopy applications, whereas, higher conversion factors are used for imaging applications.
Although a 2-day hold time is attractive, even better is to be able to hook up a 160 liter tank of liquid nitrogen to a cryostat, only replacing the tank every few weeks. This version of cryostat is called "continuous flow" and it works by passing nitrogen gas (just above temperature of the liquid) through capillary tubes in the cryostat. The continuous flow cryostat (CFC) is fundamentally different than the "continuous fill" cryostats that are popular at other observatories. ) The CFC is becoming very popular with both optical and infrared detector systems at ESO, and it will be the most used cryostat for future instruments.
The dark current is negligible at this temperature. The quantum efficiency for the devices is thought to be the same as for the CCD44 large format CCD but this has been not yet verified. 3 electrons/ADU, for brighter objects to 2 electrons/ADD. The readout noise is 3 electrons at 50 kps and 6 electrons at 635 kps. 3 MIT CCD performance overview ESO and MITILL are part of the University of Hawaii consortium for the MITILL 2Kx4K 15~m CCID-20. One of these devices is implemented in the red arm mosaic of the UVES \,spectrograph [6].