The NEMESIS planetary atmosphere radiative transfer and retrieval tool by Irwin, P, Teanby, N, de Kok, R, Fletcher, L, Howett, C, Tsang, C, Wilson, C, Calcutt, S, Nixon, C, Parrish, P

Atmospheric composition and cloud structure in Jovian 5-mu m hotspots from analysis of Galileo NIMS measurements by Nixon, C, Irwin, P, Calcutt, S, Taylor, F, Carlson, R

“…The first is a full-scattering radiative transfer forward model that is slow but accurate. …”

ALMA detection and astrobiological potential of vinyl cyanide on Titan by Palmer, M, Cordiner, M, Nixon, C, Charnley, S, Teanby, N, Kisiel, Z, Irwin, P, Mumma, M

“…We detect the three strongest rotational lines of C2H3CN in the frequency range of 230 to 232 GHz, each with >4σ confidence. Radiative transfer modeling suggests that most of the C2H3CN emission originates at altitudes of ≳200 km, in agreement with recent photochemical models. …”

Isotopic ratios of carbon and oxygen in Titan's co using ALMA by Serigano, J, Nixon, C, Cordiner, M, Irwin, P, Teanby, N, Charnley, S, Lindberg, J

“…Molecular abundances and the vertical atmospheric temperature profile were derived by modeling the observed emission line profiles using NEMESIS, a line-by-line radiative transfer code. We present the first spectroscopic detection of 17O in the outer solar system with C17O detected at >8σ confidence. …”

Measurement of CH3D on Titan at submillimeter wavelengths by Thelen, A, Nixon, C, Cordiner, M, Charnley, S, Irwin, P, Kisiel, Z

“…These two lines were modeled using the Non-linear optimal Estimator for MultivariatE spectral analySIS (NEMESIS) radiative transfer code to determine the disk-averaged CH3D volume mixing ratio = 6.157 × 10−6 in Titan's stratosphere (at altitudes >130 km). …”

Spatial and temporal variations in Titans surface temperatures from Cassini CIRS observations by Cottini, V, Nixon, C, Jennings, D, De Kok, R, Teanby, N, Irwin, P, Flasar, F

“…We begin by modeling Cassini Composite Infrared Spectrometer (CIRS) far infrared spectra collected in the period 20042010, using a radiative transfer forward model combined with a non-linear optimal estimation inversion method. …”

Gas phase dicyanoacetylene (C4N2) on Titan: New experimental and theoretical spectroscopy results applied to Cassini CIRS data by Jolly, A, Cottini, V, Fayt, A, Manceron, L, Kwabia-Tchana, F, Benilan, Y, Guillemin, J, Nixon, C, Irwin, P

“…We have also improved the analysis of the complex rotational and hot band structure of C4N2 in order to obtain the first line lists for both bending modes ν8 and ν9. Using our radiative transfer code including the new line list of the strong ν9 band, we have searched for the signature of C4N2 at 107cm-1 in the atmosphere of Titan utilizing Titan CIRS far infrared spectra. …”

Water vapor in Titan's stratosphere from Cassini CIRS far-infrared spectra by Cottini, V, Nixon, C, Jennings, D, Anderson, C, Gorius, N, Bjoraker, G, Coustenis, A, Teanby, N, Achterberg, R, Bezard, B, de Kok, R, Lellouch, E, Irwin, P, Flasar, F, Bampasidis, G

“…CIRS senses water emissions in the far infrared spectral region near 50μm, which we have modeled using two independent radiative transfer codes (NEMESIS (Irwin, P.G.J. et al. [2008]. …”

Spatial variations in Titan’s atmospheric temperature: ALMA and Cassini comparisons from 2012 to 2015 by Thelen, A, Nixon, C, Chanover, N, Molter, E, Cordiner, M, Achterberg, R, Serigano, J, Irwin, P, Teanby, N, Charnley, S

“…Temperature profiles retrieved by the NEMESIS radiative transfer code are compared to Cassini Composite Infrared Spectrometer (CIRS) and radio occultation science results from similar latitude regions. …”

The composition of Titan's stratosphere from Cassini/CIRS mid-infrared spectra by Coustenis, A, Achterberg, R, Conrath, B, Jennings, D, Marten, A, Gautier, D, Nixon, C, Flasar, F, Teanby, N, Bezard, B, Samuelson, R, Carlson, R, Lellouch, E, Bjoraker, G, Romani, P, Taylor, F, Irwin, P, Fouchet, T, Hubert, A, Orton, G, Kunde, V, Vinatier, S, Mondellini, J, Abbas, M, Courtin, R

“…We have used temperature profiles retrieved from the inversion of the emission observed in the methane ν4 band at 1304 cm-1 and a line-by-line radiative transfer code to infer the abundances of the trace constituents and some of their isotopes in Titan's stratosphere. …”