Detection of C3 in Titan with VLT-ESPRESSO

TL;DR

This study reports the first ultra high resolution optical detection of C3 molecules in Titan's atmosphere, confirming their presence with high confidence and demonstrating the application of exoplanet spectroscopy techniques to Solar System objects.

Contribution

It provides the highest spectral resolution optical detection of C3 in Titan, using VLT ESPRESSO, and validates the method with Bayesian analysis, advancing atmospheric composition studies.

Findings

Eight sigma detection of C3 in Titan's atmosphere.

Estimated C3 column density of approximately 1.5E13 cm-2.

Results consistent with photochemical model predictions.

Abstract

Titan is regarded as a natural laboratory in the Solar System for studying atmospheric photochemistry and the abiotic production of organic molecules on cold small exoplanets. Since the end of the Cassini-Huygens mission, telescope observations have enabled new detections of increasingly complex carbon-based molecules at infrared and sub-millimetre wavelengths, while the optical regime has been largely overlooked. Following a recent tentative detection of the 405 nm absorption band of C3 in Titan in archived optical VLT UVES spectra at resolving power R = 60000, this work reports an eight sigma detection of the C3 405 nm absorption band in Titan using dedicated ultra high resolution VLT ESPRESSO observations at R = 190000, the highest spectral resolution optical observations of Titan to date. The VLT ESPRESSO spectrum is compared to model spectra of Titan with varying C3 abundances. A chi squared analysis is used to assess the agreement between non solar spectral features and C3 absorption as the C3 abundance is varied, and a Bayesian Markov Chain Monte Carlo fit between model and observed spectra is performed. The chi squared analysis yields an eight sigma detection of C3, consistent with a C3 column density of approximately 1.5E13 cm-2, while the MCMC fit retrieves a C3 column density of 1.47E13 cm-2 at five sigma. These values are consistent with the order of magnitude predicted by photochemical models, which reach parts per million levels in the Titan mesosphere. This work demonstrates the usefulness of instruments and techniques originally developed for exoplanet research when applied to Solar System targets.