@prefix skos: . @prefix ns0: . skos:changeNote """2018-07-05 14:24:13.0 [mmorahan] Insert Concept add broader relation (OSIRIS [598b6dc4-aff0-4e14-b7b7-039e58560dd0,367787] - Profilers/Sounders [4190ebdc-e89a-4f3f-bc74-b2af4c68d009,346931]); """, """2018-07-05 14:25:41.0 [mmorahan] insert AltLabel (id: null category: primary text: Optical Spectrograph and Infrared Imaging System language code: en); insert Definition (id: null text: OSIRIS is a Canadian sensor (CSA, NSERC) built by Routes AstroEngineering Ltd. of Ottawa, Ontario. OSIRIS has a dual-purpose objective of detecting aerosol layers and to detect abundances of species such as O3, NO2, OClO, and BrO (retrieval of altitude profiles of terrestrial atmospheric minor species by observing limb-radiance profiles). The instrument is a UV/VIS/IR limb sounder, in effect a double instrument, mounted in a common optical housing and supported by common electronics. The UV/VIS imaging spectrograph uses compact reflective optics (off-axis system, folded design, aperture = 36 mm x 36 mm) and an aspherical ruled grating along with UV-enhanced CCD arrays. The IR imager consists of three infrared telescopes (co-aligned single-lens imagers operating at 1263, 1273, and 1530 nm). The CCD detector, a 1353 x 286 array, is operated in a frame transfer MPP (Multi-Pin-Phase) mode with only 32 rows of the imaging section of the array illuminated by the slit image. Radiation detected outside the slit image provides information on the internal scattering properties of the spectrograph. The detector is passively cooled through a radiator. As OSIRIS is pointed at the limb, the entrance slit to the spectrograph subtends a region 30 km long by 1 km high. Scattered light has been reduced through the use of a beam-fold mirror that is located between the telescope mirror and the entrance slit. The optical spectrograph (grating spectrometer type) measures species in the altitude range from 15 to 80 km (measurement of atmospheric airglow as well as utilization of the DOAS (Differential Optical Absorption Spectroscopy) technique on scattered and subsequently absorbed moonlight). The FOV of the UV/VIS and the IR channels are aligned (and co-aligned with SMR) to produce simultaneous measurements. Instrument mass = 12 kg, power=20W. On-orbit spectral calibration for the UV/VIS instrument is done by observing artificial sources emanating from the Earth, such as discrete lines produced by mercury and sodium street lights. Radiometric calibration is not provided internally. For the IR imager, the IR shutter assembly contains a built-in incandescent lamp providing the radiometric calibration signal. UV/VIS Spectrograph Wavelength 280 - 800 nm Wavelength resolution 1 nm from 300-450 nm, < 2nm from 450-800 nm Slit orientation perpendicular to the orbit plane (horizontal) FOV 0.02º (vertical) x 0.75º (horizontal) corresponding to 1 km x 40 km on Earth Spatial resolution 1 km at the limb Pointing direction aligned with SMR boresight AD converter 14 bit Detector type Si CCD array (1353 x 286 pixels) Species to be detected O3, NO2, BrO, OCLO, O2, aerosols IR Imager Bandpass filter center wavelengths 1.263 µm, 1.273 µm, 1.520 µm Bandwidth (FWHM) 10 nm (1.263 and 1.273), 40 nm (1.520) FOV 118 km (vertical) x 2 km (horizontal) Spatial resolution 1 km in the vertical direction Telescope aperture 23 mm diameter Detector type (linear arrays with hybrid multiplexers) 3 InGaAs, each detector has 128 pixels Detector pointing direction in the orbit plane (vertical) Detector temperature -40ºC (or less) Temperature stability during exposure ±0.1ºC language code: en); """, """2019-02-22 08:45:17.0 [mmorahan] insert WeightedRelation (id: null related concept uuid: 1f7c6ae3-d38e-42b7-a874-60298b0fcfa1 relationship type: null relationship value: null generated by: null); """ ; ns0:altLabel [ ] ; skos:definition """OSIRIS is a Canadian sensor (CSA, NSERC) built by Routes AstroEngineering Ltd. of Ottawa, Ontario. OSIRIS has a dual-purpose objective of detecting aerosol layers and to detect abundances of species such as O3, NO2, OClO, and BrO (retrieval of altitude profiles of terrestrial atmospheric minor species by observing limb-radiance profiles). The instrument is a UV/VIS/IR limb sounder, in effect a double instrument, mounted in a common optical housing and supported by common electronics. The UV/VIS imaging spectrograph uses compact reflective optics (off-axis system, folded design, aperture = 36 mm x 36 mm) and an aspherical ruled grating along with UV-enhanced CCD arrays. The IR imager consists of three infrared telescopes (co-aligned single-lens imagers operating at 1263, 1273, and 1530 nm). The CCD detector, a 1353 x 286 array, is operated in a frame transfer MPP (Multi-Pin-Phase) mode with only 32 rows of the imaging section of the array illuminated by the slit image. Radiation detected outside the slit image provides information on the internal scattering properties of the spectrograph. The detector is passively cooled through a radiator. As OSIRIS is pointed at the limb, the entrance slit to the spectrograph subtends a region 30 km long by 1 km high. Scattered light has been reduced through the use of a beam-fold mirror that is located between the telescope mirror and the entrance slit. The optical spectrograph (grating spectrometer type) measures species in the altitude range from 15 to 80 km (measurement of atmospheric airglow as well as utilization of the DOAS (Differential Optical Absorption Spectroscopy) technique on scattered and subsequently absorbed moonlight). The FOV of the UV/VIS and the IR channels are aligned (and co-aligned with SMR) to produce simultaneous measurements. Instrument mass = 12 kg, power=20W. On-orbit spectral calibration for the UV/VIS instrument is done by observing artificial sources emanating from the Earth, such as discrete lines produced by mercury and sodium street lights. Radiometric calibration is not provided internally. For the IR imager, the IR shutter assembly contains a built-in incandescent lamp providing the radiometric calibration signal. UV/VIS Spectrograph Wavelength 280 - 800 nm Wavelength resolution 1 nm from 300-450 nm, < 2nm from 450-800 nm Slit orientation perpendicular to the orbit plane (horizontal) FOV 0.02º (vertical) x 0.75º (horizontal) corresponding to 1 km x 40 km on Earth Spatial resolution 1 km at the limb Pointing direction aligned with SMR boresight AD converter 14 bit Detector type Si CCD array (1353 x 286 pixels) Species to be detected O3, NO2, BrO, OCLO, O2, aerosols IR Imager Bandpass filter center wavelengths 1.263 µm, 1.273 µm, 1.520 µm Bandwidth (FWHM) 10 nm (1.263 and 1.273), 40 nm (1.520) FOV 118 km (vertical) x 2 km (horizontal) Spatial resolution 1 km in the vertical direction Telescope aperture 23 mm diameter Detector type (linear arrays with hybrid multiplexers) 3 InGaAs, each detector has 128 pixels Detector pointing direction in the orbit plane (vertical) Detector temperature -40ºC (or less) Temperature stability during exposure ±0.1ºC"""@en ; skos:prefLabel "OSIRIS"@en ; skos:inScheme ; skos:broader ; a skos:Concept . skos:prefLabel "Profilers/Sounders"@en ; a skos:Concept ; skos:narrower .