The instrument operates in 5 modes; stellar occultation, echelle, limb, scan, disk mapping, and corona observations. "Our observations place those changes in the context of the whole planet." Navigational & Ancillary Information (NAIF). IUVS captures sharpened ultraviolet view of Mars MAVEN’s Imaging UltraViolet Spectrograph … In the top panel, natural variability of the solar wind results in occasional dense flows of solar wind protons bombarding Mars. The units for such fields, data numbers (DN), may represent ADC counts, encoder steps, discrete time intervals, and so on. "These two scenarios result in very different [deuterium-hydrogen] ratios; in the first case, D/H is much larger than we see at Earth, and in the second, they're about the same."

"As the other instruments measure local conditions around the spacecraft, it's important to know how those compare to the planet as a whole," Schneider said. As MAVEN's instruments work together to fill in the pieces of Mars' atmospheric loss, IUVS will play a key role. To download high-resolution version of this video, visit: svs.gsfc.nasa.gov/goto?11295 Privacy / Copyright The Corona Mode The corona mode consists of data products from the different processing level collections (raw, calibrated, processed, derived) covering coronal scans of the extended Martian atmosphere during the side segments of the MAVEN orbit when IUVS has pointing priority. IUVS is an Imaging UltraViolet Spectrograph Spanning 110-340 nm with two spectral resolution modes with low resolution (180-340 nm, λ/Δλ~400) and high resolution (110-190 nm, λ/Δλ=13,800) to measure the D/H ratio. The MAVEN spacecraft orbiting Mars has obtained a new type of imaging data which reveals the effects of global‐scale winds and waves in the upper atmosphere.

This data would provide important insight into how the Mars atmosphere has changed. MAVEN observations of a proton aurora.

At bottom, observations by MAVEN’s Imaging Ultraviolet Spectrograph show increased ultraviolet emission from the atmosphere when the solar wind is enhanced.

LASP mechanical engineers pose with the MAVEN Remote Sensing Package and its Imaging Ultraviolet Spectrograph (IUVS) shortly before the package was delivered to Lockheed Martin for integration onto the spacecraft. Freedom of Information Act. D/H ratio above the homopause with sufficient accuracy (~30%) to capture spatial/temporal variations (factor of 2) and compare with measured D/H in bulk atmosphere.

The Imaging Ultraviolet Spectrograph, IUVS for short, designed and built at the University of Colorado Boulder's Laboratory for Atmospheric and Space Physics, known as LASP, will measure Mars' global atmosphere to help solve the mystery of how the planet became frozen and barren. Raw = DN/bin + engineering and geometric data. Ultraviolet emissions confirm the expected change of wind patterns with season and pinpoint an unusually bright spot on Mars' nightside.

See section 4.1 of the SIS for processing details. Many fields are direct unconverted copies of telemetry produced by the instrument. The IUVS instrument operates in a number of modes that include using an echelle grating. While the instrument measures the gases in the planet's upper atmosphere, it will also be able to identify changes in the planet's lower atmosphere - like dust storms - below the reach of other MAVEN instruments. MAVEN includes a remote sensing Imaging UltraViolet Spectrograph (IUVS) instrument.

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