| 28 | 28 | || '''23.09.2016''' || '''Anna Boehle (UCLA)''' || '''Upgrade of the detector in the integral field spectrograph OSIRIS[[BR]]'''[[BR]]OSIRIS is a near-infrared (1 - 2.5 microns) integral field spectrograph (IFS) on the Keck I 10-meter telescope in Hawaii. This adaptive-optics-fed instrument uses an array of small lenses to sample a rectangular section of the focal plane, producing up to 3,000 spectra simultaneously with a spectral resolution of ~3,800 and diffraction-limited spatial resolution. The unique capabilities of this IFS have allowed it to contribute to a variety of science programs since its commissioning in 2005, such as characterizing the atmospheres of extrasolar planets and tracing the motions of gas and stars at the centers of the Milky Way and other galaxies.[[BR]][[BR]]In January 2016, the detector in OSIRIS was upgraded from the original Rockwell Hawaii-2 to a Teledyne Hawaii-2RG with lower read noise, lower dark current, and higher quantum efficiency. In addition to the upgraded detector, the detector head was also mounted on a linear stage, allowing the position of the detector to be accurately adjusted along the optical path when the instrument is at cryogenic temperatures (~80 K). This linear stage greatly reduced the number of cool downs required to put the detector image plane at the spectrograph camera focus and adjust any residual tip/tilt of the detector image plane. [[BR]][[BR]]In this talk, Anna Boehle will give a brief overview of integral field spectroscopy and its advantages and challenges and also present the details and the results of the upgrade of the OSIRIS detector.[[BR]][[BR]]Presentation: English[[BR]][https://svn.mpia.de/trac/gulli/att/raw-attachment/wiki/AlteVortraege2016S2/2016-09-23_OSIRIS.pdf Slides: English][[BR]]Questions: German, English || |
