Analysis of Titan CH4 3.3μm upper atmospheric emission as measured by Cassini/VIMS

García‐Comas, M.; López‐Puertas, M.; Funke, B.; Dinelli, B. M.; Moriconi, M. L.; Adriani, A.; Molina, A.; Coradini, A.

doi:10.1016/j.icarus.2011.03.020

Cited by 24 publications

(37 citation statements)

References 49 publications

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“…spectral and radiometric calibrations have been discussed in detail by García-Comas et al [2011]. In this spectral region, the spectral calibration error is smaller than 0.1% [Cruikshank et al, 2010].…”

Section: Analysis Of the "Unidentified" Emissionmentioning

confidence: 97%

“…These large intensities can only be explained by invoking non-LTE effects, e.g., species that are pumped by solar radiation near 3.3 m and then fluoresce [López-Puertas and Taylor, 2001;García-Comas et al, 2011]. Without that pumping, the emission at the cold typical temperatures of Titan's upper atmosphere, 150 K, would be several orders of magnitude weaker.…”

Section: The Measurementsmentioning

confidence: 99%

“…[9] Simulations of the observed spectra with a sophisticated CH 4 non-LTE model and the CH 4 densities derived from the Q and P branches [García-Comas et al, 2011] show that the CH 4 emission alone cannot reproduce the excess of emission of the R branch. The model (dashed line in Figure 1) predicts very well the measured radiance (black solid line) at wavelengths larger than 3.3 m, but it clearly underestimates the emission at wavelengths shorter than 3.3 m. We subtracted the simulated CH 4 emission from the measured radiance and isolated the spectral feature shown in Figure 3, the "unidentified" emission (UnE).…”

Section: The Measurementsmentioning

confidence: 99%

“…They were previously studied by García-Comas et al (2011) to derive CH 4 densities. Here, we report an unidentified emission peaking around 3.28 m, hidden under the methane R branch.…”

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confidence: 99%

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1] We have analyzed limb daytime observations of Titan's upper atmosphere at 3.3 m, acquired by the visual-infrared mapping spectrometer (VIMS) on Cassini. They were previously studied by García-Comas et al (2011) to derive CH 4 densities. Here, we report an unidentified emission peaking around 3.28 m, hidden under the methane R branch.

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mentioning

confidence: 99%

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An unidentified emission in Titan's upper atmosphere

Dinelli

López‐Puertas

Adriani

et al. 2013

Geophysical Research Letters

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[1] We have analyzed limb daytime observations of Titan's upper atmosphere at 3.3 m, acquired by the visual-infrared mapping spectrometer (VIMS) on Cassini. They were previously studied by García-Comas et al. (2011) to derive CH 4 densities. Here, we report an unidentified emission peaking around 3.28 m, hidden under the methane R branch. This emission is very strong, with intensity comparable to the CH 4 bands located in the same spectral region. It presents a maximum at about 950 km and extends from 600 km up to 1250 km. It is definitely pumped by solar radiation since it vanishes at night. Our analysis shows that neither methane nor the major hydrocarbon compounds already discovered in Titan's upper atmosphere are responsible for it. We have discarded many other potential candidates and suggest that the unidentified emission might be caused by aromatic compounds. Citation:

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Section: Analysis Of the "Unidentified" Emissionmentioning

confidence: 97%

Section: The Measurementsmentioning

confidence: 99%

Section: The Measurementsmentioning

confidence: 99%

“…They were previously studied by García-Comas et al (2011) to derive CH 4 densities. Here, we report an unidentified emission peaking around 3.28 m, hidden under the methane R branch.…”

mentioning

confidence: 99%

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confidence: 99%

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