ALICE: The Ultraviolet Imaging Spectrograph Aboard the New Horizons Pluto–Kuiper Belt Mission

Stern, S. A.; Slater, D. C.; Scherrer, J.; Stone, John Marshall; Dirks, Greg; Versteeg, M. H.; Davis, Michael W.; Gladstone, G. Randall; Parker, J. W.; Young, L. A.; Siegmund, Oswald H. W.

doi:10.1007/s11214-008-9407-3

Cited by 119 publications

(72 citation statements)

References 15 publications

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“…The excitation of the N 2 Rydberg-valence states responsible for these emissions occurs in the short wavelength portion of the EUV between 800 and 1000 Å. This excitation, emission, and associated dissociation and ionization play a role in establishing the physical composition of the N 2 -bearing atmospheres of Earth (Meier et al 2005;Meier & Picone 1994;Knight et al 2008;Strickland et al 1999Strickland et al , 2004aStrickland et al , 2004b, Titan (Ajello et al 2007(Ajello et al , 2011bStevens et al 1994Stevens et al , 2011Stevens 2001;Broadfoot et al 1981;Fulchignoni et al 2005), Triton (Broadfoot et al 1989;Summers & Strobel 1991), and Pluto (Zhu et al 2014;Stern et al 2008;Bagenal et al 1997), and in interstellar clouds and extrasolar protoplanetary disks (Maret et al 2006;Pascucci et al 2009;Li et al 2013).…”

Section: Introductionmentioning

confidence: 99%

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

Heays

Ajello

Aguilar

et al. 2014

ApJS

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We have analyzed high-resolution (FWHM = 0.2 Å) extreme-ultraviolet (EUV, 800-1350 Å) laboratory emission spectra of molecular nitrogen excited by an electron impact at 20 and 100 eV under (mostly) optically thin, singlescattering experimental conditions. A total of 491 emission features were observed from N 2 electronic-vibrational transitions and atomic N i and N ii multiplets and their emission cross sections were measured. Molecular emission was observed at vibrationally excited ground-state levels as high as v = 17, from the a 1 Π g , b 1 Π u , and b 1 Σ u + excited valence states and the Rydberg series c n+1 1 Σ u + , c n 1 Π u , and o n 1 Π u for n between 3 and 9. The frequently blended molecular emission bands were disentangled with the aid of a sophisticated and predictive quantummechanical model of excited states that includes the strong coupling between valence and Rydberg electronic states and the effects of predissociation. Improved model parameters describing electronic transition moments were obtained from the experiment and allowed for a reliable prediction of the vibrationally summed electronic emission cross section, including an extrapolation to unobserved emission bands and those that are optically thick in the experimental spectra. Vibrationally dependent electronic excitation functions were inferred from a comparison of emission features following 20 and 100 eV electron-impact collisional excitation. The electron-impact-induced fluorescence measurements are compared with Cassini Ultraviolet Imaging Spectrograph observations of emissions from Titan's upper atmosphere.

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Section: Introductionmentioning

confidence: 99%

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

Heays

Ajello

Aguilar

et al. 2014

ApJS

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“…The photon-counting LAMP imaging spectrograph is closely based on the Pluto Alice (P-Alice) instrument design (Stern et al , 2008 which is, in turn, based largely on the Rosetta Alice (R-Alice) instrument design Slater et al 2001), with only relatively minor changes in baffling, software, and the addition of a lunar terminator sensor (see below). In this section we provide a description of the instrument, concentrating on the differences with the P-Alice design.…”

Section: Overviewmentioning

confidence: 99%

“…The LAMP instrument is a "close cousin" of the sensitive (∼1 Rayleigh level), lightweight (∼4 kg), low-power (∼4 W) Alice imaging ultraviolet spectrograph (UVS) currently in flight on the ESA/NASA Rosetta comet orbiter Slater et al 2001) and NASA New Horizons missions (Stern et al , 2008. LAMP will be the first UVS to operate in lunar orbit since that on the Apollo 17 mission in 1972.…”

Section: Introductionmentioning

confidence: 99%

LAMP: The Lyman Alpha Mapping Project on NASA’s Lunar Reconnaissance Orbiter Mission

et al. 2009

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The Lyman Alpha Mapping Project (LAMP) is a far-ultraviolet (FUV) imaging spectrograph on NASA's Lunar Reconnaissance Orbiter (LRO) mission. Its main objectives are to (i) identify and localize exposed water frost in permanently shadowed regions (PSRs), (ii) characterize landforms and albedos in PSRs, (iii) demonstrate the feasibility of using natural starlight and sky-glow illumination for future lunar surface mission applications, and (iv) characterize the lunar atmosphere and its variability. As a byproduct, LAMP will map a large fraction of the Moon at FUV wavelengths, allowing new studies of the microphysical and reflectance properties of the regolith. The LAMP FUV spectrograph will accomplish these objectives by measuring the signal reflected from the night-side lunar surface and in PSRs using both the interplanetary HI Lyman-α sky-glow and FUV starlight as light sources. Both these light sources provide fairly uniform, but faint, illumination. With the expected LAMP sensitivity, by the end of the primary 1-year LRO mission, the SNR for a Lyman-α albedo map should be >100 in polar regions >1 km 2 , providing useful FUV constraints to help characterize subtle compositional and structural features. The LAMP instrument is 162 G.R. Gladstone et al.based on the flight-proven Alice series of spectrographs flying on the Rosetta comet mission and the New Horizons Pluto mission. A general description of the LAMP instrument and its initial ground calibration results are presented here.

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“…The LymanBirge-Hopfield (LBH) band is one of the most important molecular emissions of excited nitrogen in the FUV. It is always found and can be produced due to impact excitation of protons and electrons in the aurora and airglow observations of nitrogen-bearing atmospheres of Earth [e.g., Bishop and Feldman, 2003;Strickland et al, 2001], Titan [e.g., Ajello et al, 2008;Sittler et al, 2009] and Triton [e.g., Broadfoot et al, 1989] and is expected at Pluto [Stern et al, 2008].…”

Section: Introductionmentioning

confidence: 99%

Laboratory studies of UV emissions from proton impact on N₂: The Lyman-Birge-Hopfield band system for aurora analysis

et al. 2011

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[1] We have measured the emission cross sections of the Lyman-Birge-Hopfield (LBH) a 1 P g − X 1 S g + band system and several atomic nitrogen (N I) multiplets (1200, 1243, 1493 Å) by H + (proton) impact on N 2 over an impact energy range of 1-7 keV. The peak proton-impact-induced emission cross section of the LBH band system (1260-2500 Å) was measured to be 5.05 ± 1.52 × 10 −17 cm 2 at 7 keV. To the best of our knowledge, the present LBH emission cross sections are reported for the first time in the far ultraviolet (FUV) wavelength range of 1100-1600 Å. The proton energy range in this study, when coupled with previously published 10-100 keV proton excited emissions of N I multiplets, provides a wide energy range of emission cross sections for proton energy loss transport codes. This energy range includes the peak cross section and the energy range for Born scaling. The reported measurements lead to an important component of monoenergetic yields for proton FUV auroral emission. Such yields, based on emission cross sections and transport modeling, allowed for convenient comparison of emission efficiencies between proton and electron aurora. In addition, we have measured the H Ly a, LBH, and N I multiplet emission cross sections for H 2 + and H 3 + ion impact on N 2 at 5 keV and found that the magnitude of H Ly a emission cross section, s em (Ly a), follows in the order of impact ion mass H 3 + > H 2 + > H + .Citation: Ajello, J. M., R. S. Mangina, D. J. Strickland, and D. Dziczek (2011), Laboratory studies of UV emissions from proton impact on N 2 : The Lyman-Birge-Hopfield band system for aurora analysis,

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ALICE: The Ultraviolet Imaging Spectrograph Aboard the New Horizons Pluto–Kuiper Belt Mission

Cited by 119 publications

References 15 publications

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

LAMP: The Lyman Alpha Mapping Project on NASA’s Lunar Reconnaissance Orbiter Mission

Laboratory studies of UV emissions from proton impact on N₂: The Lyman-Birge-Hopfield band system for aurora analysis

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ALICE: The Ultraviolet Imaging Spectrograph Aboard the New Horizons Pluto–Kuiper Belt Mission

Cited by 119 publications

References 15 publications

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N 2 BY ELECTRON IMPACT

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N 2 BY ELECTRON IMPACT

LAMP: The Lyman Alpha Mapping Project on NASA’s Lunar Reconnaissance Orbiter Mission

Laboratory studies of UV emissions from proton impact on N2: The Lyman-Birge-Hopfield band system for aurora analysis

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Product

Resources

About

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

THE HIGH-RESOLUTION EXTREME-ULTRAVIOLET SPECTRUM OF N ₂ BY ELECTRON IMPACT

Laboratory studies of UV emissions from proton impact on N₂: The Lyman-Birge-Hopfield band system for aurora analysis