Radiometric performance results of the Juno ultraviolet spectrograph (Juno-UVS)

Davis, Michael W.; Gladstone, G. Randall; Greathouse, Thomas; Slater, D. C.; Versteeg, M. H.; Persson, Kristian; Winters, Gregory S.; Persyn, Steven C.; Eterno, John S.

doi:10.1117/12.894274

Cited by 16 publications

(14 citation statements)

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“…With a 2 rpm spin rate and a 1 hour integration time, Figure 8 represents the signal to noise one can expect from summing 120 spins worth of data. From The left hand plot in Figure 9 shows that on axis (0° along the slit) the image is best at the shortest wavelengths and degrades slightly as you move to longer wavelengths, similar to radiometric ground calibration 6 . This is a result of the optimization of the grating blaze and curvature for ~90 nm light.…”

Section: Spatial Point Spread Functionmentioning

confidence: 85%

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

et al. 2013

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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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Section: Spatial Point Spread Functionmentioning

confidence: 85%

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

et al. 2013

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“…ESCAPE utilizes an electronics package with flight heritage on numerous missions, including ICON-EUV, JUNO-UVS, JUICE-UVS, EUROPA-UVS and EMM-EMUS. [104][105][106][107] This package utilizes low-power amplifiers / discriminators for the start and stop signals of each axis of the XDL, followed by time to digital conversion, and an FPGA (ACTEL AX/RT family) to convert the raw event time of arrival differences into x, y and signal amplitudes outputted as 32-bit LVDS (13-bit X, 12-bit Y, 7-bit pulse height). Maximum global count rates for primary science targets, including airglow contributions, are less than 1000 Hz, posing no counting rate challenges for the detector system.…”

Section: Escape Spectrographmentioning

confidence: 99%

The extreme-ultraviolet stellar characterization for atmospheric physics and evolution (ESCAPE) mission concept

Fleming

Drake

Mason

et al. 2019

UV, X-Ray, and Gamma-Ray Space Instrumentation for Astronomy XXI

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“…Seen from the Earth, Juno travels clockwise around the planet while it spins counterclockwise twice per minute. The Juno‐UVS (ultraviolet spectrograph) instrument is a UV photon‐counting imaging spectrograph operating in the 68 to 210 nm range [ Gladstone et al , ; Greathouse et al , ; Davis et al , ]. It is equipped with a scan mirror that allows it to look up to ±30° perpendicular to the Juno spin plane.…”

Section: Juno‐uvs Auroral Observationsmentioning

confidence: 99%

Morphology of the UV aurorae Jupiter during Juno's first perijove observations

Bonfond

Gladstone

Grodent

et al. 2017

Geophysical Research Letters

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On 27 August 2016, the NASA Juno spacecraft performed its first close‐up observations of Jupiter during its perijove. Here we present the UV images and color ratio maps from the Juno‐UVS UV imaging spectrograph acquired at that time. Data were acquired during four sequences (three in the north, one in the south) from 5:00 UT to 13:00 UT. From these observations, we produced complete maps of the Jovian aurorae, including the nightside. The sequence shows the development of intense outer emission outside the main oval, first in a localized region (255°–295° System III longitude) and then all around the pole, followed by a large nightside protrusion of auroral emissions from the main emission into the polar region. Some localized features show signs of differential drift with energy, typical of plasma injections in the middle magnetosphere. Finally, the color‐ratio map in the north shows a well‐defined area in the polar region possibly linked to the polar cap.

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Radiometric performance results of the Juno ultraviolet spectrograph (Juno-UVS)

Cited by 16 publications

References 0 publications

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

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

The extreme-ultraviolet stellar characterization for atmospheric physics and evolution (ESCAPE) mission concept

Morphology of the UV aurorae Jupiter during Juno's first perijove observations

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