An empirical line list for methane in the 1.26–1.71μm region for planetary investigations (T=80–300K). Application to Titan

Campargue, A.; Wang, Le; Mondelain, D.; Kassi, S.; Bézard, Bruno; Lellouch, E.; Coustenis, A.; Bérgh, C. de; Hirtzig, M.; Drossart, P.

doi:10.1016/j.icarus.2012.02.015

Cited by 65 publications

(74 citation statements)

References 57 publications

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“…Correlated-k values (Lacis and Oinas, 1991) for CH 4 and CH 3 D are calculated for 390 combinations of temperature and pressure that have been used in the literature, e.g., by Sromovsky et al (2012) and Irwin et al (2014). CH 4 and CH 3 D lines are from the HITRAN 2012 database (Rothman et al, 2013), which include the WKMC-80K methane line data of Campargue et al (2012) that are relevant to this spectral region.…”

Section: Ch 4 and Ch 3 D Opacitiesmentioning

confidence: 99%

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Meridional variation in tropospheric methane on Titan observed with AO spectroscopy at Keck and VLT

Ádámkovics

Mitchell

Hayes

et al. 2016

Icarus

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The spatial distribution of the tropospheric methane on Titan was measured using near-infrared spectroscopy. Ground-based observations at 1.5 µm (H-band) were performed during the same night using instruments with adaptive optics at both the W. M. Keck Observatory and at the Paranal Observatory on 17 July 2014 UT. The integral field observations with SINFONI on the VLT covered the entire H-band at moderate resolving power, R = λ/∆λ ≈ 1, 500, while the Keck observations were performed with NIRSPAO near 1.5525 µm at higher resolution, R ≈ 25, 000. The moderate resolution observations are used for flux calibration and for the determination of model parameters that can be degenerate in the interpretation of high resolution spectra. Line-by-line calculations of CH 4 and CH 3 D correlated k distributions from the HITRAN 2012 database were used, which incorporate revised line assignments near 1.5 µm. We fit the surface albedo and aerosol distributions in the VLT SINFONI observations that cover the entire H-band window and used these quantities to constrain the models of the high-resolution Keck NIRSPAO spectra when retrieving the methane abundances. Cassini VIMS images of the polar regions, acquired on 20 July 2014 UT, are used to validate the assumption that the opacity of tropospheric aerosol is relatively uniform below 10 km. We retrieved methane abundances at latitudes between 42 • S and 80 • N. The tropospheric methane in the Southern mid-latitudes was enhanced by a factor of ∼10-40% over the nominal profile that was measured using the GCMS on Huygens. The Northern hemisphere had ∼90% of the nominal methane abundance up to polar latitudes (80 • N). These measurements suggest that a source of saturated polar air is equilibrating with dryer conditions at lower latitudes.

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Section: Ch 4 and Ch 3 D Opacitiesmentioning

confidence: 99%

“…Various prescriptions for χ are in the literature and we use the sub-Lorenztian line shape of Campargue et al (2012) that is determined from laboratory data. The following notation is used to describe the Voigt profile when determining line shape:…”

Section: Ch 4 and Ch 3 D Opacitiesmentioning

confidence: 99%

Meridional variation in tropospheric methane on Titan observed with AO spectroscopy at Keck and VLT

Ádámkovics

Mitchell

Hayes

et al. 2016

Icarus

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show abstract

“…While this estimate may be biased by the use of older methane absorption coefficients less appropriate for Uranus' atmospheric conditions, Irwin et al (2011Irwin et al ( , 2012b derived comparable values based on Uranus' H-band spectra, using the updated methane coefficients of Karkoschka and Tomasko (2010) and the recent line data from Campargue et al (2012). The simplest distribution of particle sizes is a delta function at a specific particle radius.…”

Section: Particle Scattering Propertiesmentioning

confidence: 99%

Clouds and aerosols on Uranus: Radiative transfer modeling of spatially-resolved near-infrared Keck spectra

Kleer

Luszcz‐Cook

Pater

et al. 2015

Icarus

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“…In some cases, the lower state energy of the transitions could not be determined and so these line data cannot be extrapolated to conditions much different from 80 K. However, as shown in Fig. 13 of Campargue et al (2012), these transitions, which, in the H-band, are located essentially around 1.53 and 1.61 lm, contribute at most to 20% of the absorption at 80 K. Furthermore, as for Uranus (and Titan) the temperatures are close to 80 K, temperature extrapolation errors should be very small. The WKC -80K line parameters do not include line broadening coefficients, for which we had to turn to other sources.…”

Section: Measurement and Modelling Of Uranus' Near-infrared Spectrummentioning

confidence: 99%

The application of new methane line absorption data to Gemini-N/NIFS and KPNO/FTS observations of Uranus’ near-infrared spectrum

Irwin

Bérgh

Courtin

et al. 2012

Icarus

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An empirical line list for methane in the 1.26–1.71μm region for planetary investigations (T=80–300K). Application to Titan

Cited by 65 publications

References 57 publications

Meridional variation in tropospheric methane on Titan observed with AO spectroscopy at Keck and VLT

Meridional variation in tropospheric methane on Titan observed with AO spectroscopy at Keck and VLT

Clouds and aerosols on Uranus: Radiative transfer modeling of spatially-resolved near-infrared Keck spectra

The application of new methane line absorption data to Gemini-N/NIFS and KPNO/FTS observations of Uranus’ near-infrared spectrum

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