Performance results from in-flight commissioning of the Juno Ultraviolet Spectrograph (Juno-UVS)

T. K. Greathouse; G. R. Gladstone; M. W. Davis; D. C. Slater; M. H. Versteeg; K. B. Persson; B. C. Walther; G. S. Winters; S. C. Persyn; J. S. Eterno

doi:10.1117/12.2024537

26 September 2013 Performance results from in-flight commissioning of the Juno Ultraviolet Spectrograph (Juno-UVS)

T. K. Greathouse, G. R. Gladstone, M. W. Davis, D. C. Slater, M. H. Versteeg, K. B. Persson, B. C. Walther, G. S. Winters, S. C. Persyn, J. S. Eterno

Author Affiliations +

Proceedings Volume 8859, UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XVIII; 88590T (2013) https://doi.org/10.1117/12.2024537
Event: SPIE Optical Engineering + Applications, 2013, San Diego, California, United States

Abstract

We present a description of the Juno ultraviolet spectrograph (Juno-UVS) and results from its in-flight commissioning performed between December 5^th and 13^th 2011 and its first periodic maintenance between October 10^th and 12^th 2012. Juno-UVS is a modest power (9.0 W) ultraviolet spectrograph based on the Alice instruments now in flight aboard the European Space Agency’s Rosetta spacecraft, NASA’s New Horizons spacecraft, and the LAMP instrument aboard NASA’s Lunar Reconnaissance Orbiter. However, unlike the other Alice spectrographs, Juno-UVS sits aboard a spin stabilized spacecraft. The Juno-UVS scan mirror allows for pointing of the slit approximately ±30° from the spacecraft spin plane. This ability gives Juno-UVS access to half the sky at any given spacecraft orientation. The planned 2 rpm spin rate for the primary mission results in integration times per 0.2° spatial resolution element per spin of only ~17 ms. Thus, for calibration purposes, data were retrieved from many spins and then remapped and co-added to build up exposure times on bright stars to measure the effective area, spatial resolution, scan mirror pointing positions, etc. The primary job of Juno-UVS will be to characterize Jupiter’s UV auroral emissions and relate them to in-situ particle measurements. The ability to point the slit will make operations more flexible, allowing Juno-UVS to observe the atmospheric footprints of magnetic field lines through which Juno flies, giving a direct connection between energetic particle measurements on the spacecraft and the far-ultraviolet emissions produced by Jupiter’s atmosphere in response to those particles.

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T. K. Greathouse, G. R. Gladstone, M. W. Davis, D. C. Slater, M. H. Versteeg, K. B. Persson, B. C. Walther, G. S. Winters, S. C. Persyn, and J. S. Eterno "Performance results from in-flight commissioning of the Juno Ultraviolet Spectrograph (Juno-UVS)", Proc. SPIE 8859, UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XVIII, 88590T (26 September 2013); https://doi.org/10.1117/12.2024537

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