Information AboutOsiris |
| CATEGORIES ABOUT OSIRIS | |
| agricultural gods | |
| death gods | |
| underworld gods | |
| egyptian gods | |
| fertility gods | |
| health gods | |
| life-death-rebirth gods | |
| nature gods | |
| primordial teachers | |
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OSIRIS is the name of two entirely separate astronomical instruments. The duplication of names is coincidental, though partly driven by two teams trying to make acronyms using similar words. OSIRIS ('''OH-Suppressing Infrared Integral Field Spectrograph''') is an Integral Field Spectrograph for the Keck II Telescope in Hawaii . As an integral field spectrograph, it can obtain many spectra simultaneously covering a small region of the sky. As such, it combines the capabilities of a traditional Spectrograph and a regular imaging Camera . The 'OH suppressing' portion of the name refers to the fact that OSIRIS has sufficient Spectral Resolution that Sky Glow from OH molecules can be separated and removed from the spectra of the science targets. OSIRIS covers the wavelength range from 1 to 2.5 micrometres with a spectral resolution of about 3800. Combined with the Keck Laser Guide Star Adaptive Optics system, it can obtain Diffraction-limited observations on extremely faint targets. OSIRIS was developed by the UCLA Infrared astronomy lab under Prof. James Larkin and achieved First Light on February 22 , 2005 . OSIRIS ('''Optical System for Imaging and low Resolution Integrated Spectroscopy''') is the Spanish Day One instrument for the Gran Telescopio Canarias (GTC) . Sensitive in the wavelength range from 365 through 1000 nm, OSIRIS is a multiple purpose instrument for imaging and low-resolution long slit and multiple object Spectroscopy (MOS). Imaging can be done using broad band filters or narrow band Tunable Filters with FWHM ranging from 0.2 to 1.3 nm at 365 nm, through 0.9 to 5.4 nm at 1000 nm. OSIRIS observing modes include also fast photometry and spectroscopy. OSIRIS field of view is of 8.5x8.5 arcminutes and the maximum nominal spectral resolution is of 5000 for a slit width of 0.6 arcsec. MOS incorporates detector charge shuffling co-ordinated with telescope nodding for an excellent sky subtraction. The use of tunable filters is a completely new feature in 8 to 10 m class Telescope s that will allow observing the very faint and distant emission line objects. The OSIRIS scientific Key Project is OTELO . EXTERNAL LINKS |
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