Virtis : an imaging spectrometer for the rosetta mission

Coradini, A.; Capaccioni, F.; Drossart, P.; Sémery, Alain; Arnold, Gabriele; Schade, U.; Angrilli, Francesco; Barucci, Maria Antonietta; Bellucci, G.; Bianchini, G.; Bibring, Jean‐Pierre; Blanco, A.; Błęcka, M. I.; Bockelée‐Morvan, Dominique; Bonsignori, Roberto; Bouyé, M.; Bussoletti, E.; Capria, M. T.; Carlson, R. W.; Carsenty, U.; Cerroni, P.; Colangeli, L.; Combes, M.; Combi, M. R.; Crovisier, J.; Dami, Michele; Desanctis, M.C.; DiLellis, A. M.; Dotto, E.; Encrenaz, Th.; Epifani, E. Mazzotta; Erard, S.; Espinasse, S.; Fave, Agnès; Federico, C.; Fink, Uwe; Fonti, S.; Formisano, V.; Hello, Y.; Hirsch, H.; Huntzinger, G.; Knoll, R. H.; Kouach, Driss; Ip, W.-H.; Irwin, P.; Kachlicki, J.; Langevin, Y.; Magni, G.; McCord, T. B.; Mennella, V.; Michaelis, H.; Mondello, Giuseppe; Mottola, S.; Neukum, G.; Orofino, V.; Orosei, R.; Palumbo, P.; Peter, G.; Pforte, B.; Piccioni, G.; Réess, Jean-Michel; Ress, E.; Saggin, Bortolino; Schmitt, Bernard; Stefanovitch, D.; Stern, Alan; Taylor, F. W.; Tiphéne, D.; Tozzi, G. P.

doi:10.1016/s0032-0633(98)00025-7

Cited by 60 publications

(17 citation statements)

References 18 publications

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“…It is derived from the previous VIRTIS-M aboard Rosetta (Coradini et al 1998(Coradini et al , 1999Reininger et al 1994Reininger et al , 1996Filacchione 2006) and VenusExpress missions; all these instruments are based on the optical layout introduced for the first time in Cassini/VIMS-V (Brown et al 2004;Filacchione 2006).…”

Section: Vir Descriptionmentioning

confidence: 99%

The VIR Spectrometer

Sanctis¹,

et al. 2010

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The Dawn spectrometer (VIR) is a hyperspectral spectrometer with imaging capability. The design fully accomplishes Dawn's scientific and measurement objectives. Determination of the mineral composition of surface materials in their geologic context is a primary Dawn objective. The nature of the solid compounds of the asteroid (silicates, oxides, salts, organics and ices) can be identified by visual and infrared spectroscopy using high spatial resolution imaging to map the heterogeneity of asteroid surfaces and high spectral resolution spectroscopy to determine the composition unambiguously. The VIR Spectrometercovering the range from the near UV (0.25 µm) to the near IR (5.0 µm) and having moderate to high spectral resolution and imaging capabilities-is the appropriate instrument for the determination of the asteroid global and local properties. VIR combines two data channels in one compact instrument. The visible channel covers 0.25-1.05 µm and the infrared channel covers 1-5.0 µm. VIR is inherited from the VIRTIS mapping spectrometer (Coradini et al. on board the ESA Rosetta mission. It will be operated for more than 2 years and spend more than 10 years in space.

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Section: Vir Descriptionmentioning

confidence: 99%

The VIR Spectrometer

Sanctis¹,

et al. 2010

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“…The VIRTIS spectral imager is described in detail by Coradini et al [1998]. Here we describe the characteristics of the H‐channel that are relevant to our analysis.…”

Section: Observationsmentioning

confidence: 99%

A latitudinal survey of CO, OCS, H₂O, and SO₂ in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS‐H

Marcq¹,

Bézard²,

Drossart³

et al. 2008

J. Geophys. Res.

102

114

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The high‐resolution channel (R ≃ 2000) of the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument (VIRTIS‐H) aboard Venus Express has provided numerous spectra of the nightside infrared thermal emission in the 2.3‐μm window. Mixing ratios of various minor species in the 30–40 km range could therefore be inferred using this spectral window at higher latitudes accessible to the spacecraft but which cannot be observed from Earth. The previously known enhancement in carbon monoxide (CO) toward high latitudes is confirmed and extended up to 60° with a mixing ratio varying from 24 ± 3 to 31 ± 2 ppmv at 36 km. Measurements of carbonyl sulfide (OCS) also agree with the previously suspected latitudinal variations that are anticorrelated with those of CO, ranging between 2.5 ± 1 and 4 ± 1 ppmv at 33 km. New constraints were also derived on the mean abundance of water vapor (H2O, 31 ± 2 ppmv) and sulfur dioxide (SO2, 130 ± 50 ppmv) in the probed altitude range. CO and OCS variations are interpreted as caused by large‐scale vertical motions, an explanation under current testing by various chemical and dynamical modeling. In such a case, these variations may help constrain the chemical time scale of those species in the lower troposphere.

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“…Onboard are seven science instruments devoted to observing the atmosphere and surface of Venus from UV to infrared and radio wavelengths. Visible and Infrared Thermal Imaging Spectrometer (VIRTIS), which is also flying on the Rosetta mission [ Coradini et al , 1998], is one of these instruments. Covering wavelengths from 0.27 to 5.19 μ m, VIRTIS is divided into two subsystems; the nonimaging H channel covering the spectral ranges from 1.84 to 4.99 μ m, with a spectral resolution of 1nm, and the imaging M channel, which is further divided into two channels.…”

Section: Venus Express/virtis‐m Observationsmentioning

confidence: 99%

Tropospheric carbon monoxide concentrations and variability on Venus from Venus Express/VIRTIS‐M observations

Tsang¹,

Irwin²,

Wilson³

et al. 2008

J. Geophys. Res.

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[1] We present nightside observations of tropospheric carbon monoxide in the southern hemisphere near the 35 km height level, the first from Venus Express/Visible and Infrared Thermal Imaging Spectrometer (VIRTIS)-M-IR. VIRTIS-M data from 2.18 to 2.50 mm, with a spectral resolution of 10 nm, were used in the analysis. Spectra were binned, with widths ranging from 5 to 30 spatial pixels, to increase the signal-to-noise ratio, while at the same time reducing the total number of retrievals required for complete spatial coverage. We calculate the mean abundance for carbon monoxide at the equator to be 23 ± 2 ppm. The CO concentration increases toward the poles, peaking at a latitude of approximately 60°S, with a mean value of 32 ± 2 ppm. This 40% equator-to-pole increase is consistent with the values found by Collard et al. (1993) from Galileo/NIMS observations. Observations suggest an overturning in this CO gradient past 60°S, declining to abundances seen in the midlatitudes. Zonal variability in this peak value has also been measured, varying on the order of 10% ($3 ppm) at different longitudes on a latitude circle. The zonal variability of the CO abundance has possible implications for the lifetime of CO and its dynamics in the troposphere. This work has definitively established a distribution of tropospheric CO, which is consistent with a Hadley cell circulation, and placed limits on the latitudinal extent of the cell.

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Virtis : an imaging spectrometer for the rosetta mission

Cited by 60 publications

References 18 publications

The VIR Spectrometer

The VIR Spectrometer

A latitudinal survey of CO, OCS, H₂O, and SO₂ in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS‐H

Tropospheric carbon monoxide concentrations and variability on Venus from Venus Express/VIRTIS‐M observations

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Virtis : an imaging spectrometer for the rosetta mission

Cited by 60 publications

References 18 publications

The VIR Spectrometer

The VIR Spectrometer

A latitudinal survey of CO, OCS, H2O, and SO2 in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS‐H

Tropospheric carbon monoxide concentrations and variability on Venus from Venus Express/VIRTIS‐M observations

Contact Info

Product

Resources

About

A latitudinal survey of CO, OCS, H₂O, and SO₂ in the lower atmosphere of Venus: Spectroscopic studies using VIRTIS‐H