The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
EXES operated in the 4.5 - 28.3 um wavelength region, at high (R ~ 50,000 - 100,000), medium (R ~ 5000 - 20,000) and low (R . 1000 - 3000) spectral resolution.
FIFI-LS was an integral field, far-infrared spectrometer. The instrument included two independent grating spectrometers sharing a common field of view (FOV). The short wavelength spectrometer (blue channel) operated in the 51 - 120 um wavelength region, and the long wavelength spectrometer (red channel) covered 115 - 200 um. The spectral resolution ranged from 600 to 2,000 dependent on the observed wavelength, with higher values towards the long wavelength ends of each spectrometer.
FLITECAM was an infrared camera operating in the 1.0 - 5.5 um waveband. It consisted of a 1024x1024 InSb detector with 0.475"x0.475" pixels and used refractive optics to provide an 8' diameter field of view. The instrument had a set of filters for imaging, and grisms for moderate resolution spectroscopy. The filter suite consisted of standard Barr filters used for imaging at J, H, K, L and M in one filter wheel. A second filter wheel held a selection of narrow-band imaging filters including Pa-alpha, Pa-alpha continuum, 3.07 um H2O ice, 3.3 um PAH, L-narrow and M-narrow. Additionally there were order sorting filters for use with the grisms. A selection of three grisms was available to provide medium resolution (R ~ 1500) spectra over the entire wavelength range.
FLITECAM was an infrared camera operating in the 1.0 - 5.5 um waveband. It consisted of a 1024x1024 InSb detector with 0.475"x0.475" pixels and used refractive optics to provide an 8' diameter field of view. The instrument had a set of filters for imaging, and grisms for moderate resolution spectroscopy. The filter suite consisted of standard Barr filters used for imaging at J, H, K, L and M in one filter wheel. A second filter wheel held a selection of narrow-band imaging filters including Pa-alpha, Pa-alpha continuum, 3.07 um H2O ice, 3.3 um PAH, L-narrow and M-narrow. Additionally there were order sorting filters for use with the grisms. A selection of three grisms was available to provide medium resolution (R ~ 1500) spectra over the entire wavelength range.
FORCAST was a dual-channel mid-infrared camera and spectrograph sensitive from 5 - 40 um. Spectroscopy was also possible using a suite of grisms, which provided coverage from 5 - 40 um with a low spectral resolution of R ~ 200.
FORCAST was a dual-channel mid-infrared camera and spectrograph sensitive from 5 - 40 um. Spectroscopy was also possible using a suite of grisms, which provided coverage from 5 - 40 um with a low spectral resolution of R ~ 200.
