The Titan 14N/15N and 12C/13C isotopic ratios in HCN from Cassini/CIRS

We report the detection of H13CN and HC15N in mid-infrared spectra recorded by the Composite Infrared Spectrometer (CIRS) aboard Cassini, along with the determination of the 12C/13C and 14N/15N isotopic ratios. We analyzed two sets of limb spectra recorded near 13–15◦ S (Tb flyby) and 83◦ N (T4 flyby) at 0.5 cm−1 resolution. The spectral range 1210–1310 cm−1 was used to retrieve the temperature profile in the range 145–490 km at 13◦ S and 165–300 km at 83◦ N. These two temperature profiles were then incorporated in the atmospheric model to retrieve the abundance profile of H12C14N, H13CN and HC15N from their bands at 713, 706 and 711 cm−1, respectively. The HCN abundance profile was retrieved in the range 90–460 km at 15◦ S and 165–305 km at 83◦ N. There is no evidence for vertical variations of the isotopic ratios. Constraining the isotopic abundance profiles to be proportional to the HCN one, we find 12C/13C = 89+22 −18 at 15◦ S, and 68+16 −12 at 83◦ N, two values that are statistically consistent. A combination of these results yields a 12C/13C value equal to 75±12. This global result, as well as the 15◦ S one, envelop the value in Titan’s methane (82.3 ± 1) [Niemann, H.B., and 17 colleagues, 2005. Nature 438, 779–784] measured at 10◦ S and is slightly lower than the terrestrial inorganic standard value (89). The 14N/15N isotopic ratio is found equal to 56+16 −13 at 15◦ S and 56 +10 −9 at 83◦ N. Combining the two values yields 14N/15N = 56 ± 8, which corresponds to an enrichment in 15N of about 4.9 compared with the terrestrial ratio. These results agree with the values obtained from previous ground-based millimeter observations [Hidayat, T., Marten, A., Bézard, B., Gautier, D., Owen, T., Matthews, H.E., Paubert, G., 1997. Icarus 126, 170–182; Marten, A., Hidayat, T., Biraud, Y., Moreno, R., 2002. Icarus 158, 532–544]. The 15N/14N ratio found in HCN is ∼3 times higher than in N2 [Niemann, H.B., and 17 colleagues, 2005. Nature 438, 779–784], which implies a large fractionation process in the HCN photochemistry. © 2007 Elsevier Inc. All rights reserved.