The 12CO/13CO isotopologue ratio of a young, isolated brown dwarf. Possibly distinct formation pathways of super-Jupiters and brown dwarfs

TL;DR

This study measures the 12CO/13CO isotopologue ratio in a young, isolated brown dwarf to explore its formation pathway, revealing potential differences from super-Jupiters despite similar atmospheric features.

Contribution

It provides the first measurement of the 12CO/13CO ratio in an isolated brown dwarf, suggesting distinct formation processes from super-Jupiters based on isotopic evidence.

Findings

Detected 13CO at ~8.4 S/N in the brown dwarf atmosphere.

Measured 12CO/13CO ratio of approximately 97, slightly above the local interstellar standard.

Indicates possible different formation pathways for brown dwarfs and super-Jupiters.

Abstract

Linking atmospheric characteristics of planets to their formation pathways is a central theme in the study of extrasolar planets. Although the 12C/13C isotope ratio shows little variation in the solar system, the atmosphere of a super-Jupiter was recently shown to be rich in 13CO, possibly as a result of dominant ice accretion beyond the CO snowline during its formation. In this paper we aim to measure the 12CO/13CO isotopologue ratio of a young, isolated brown dwarf. While the general atmospheric characteristics of young, low mass brown dwarfs are expected to be very similar to those of super-Jupiters, their formation pathways may be different, leading to distinct isotopologue ratios. We analyse archival K-band spectra of the L dwarf 2MASS J03552337+1133437 taken with NIRSPEC at the Keck telescope. A free retrieval analysis is applied to the data to determine the isotopologue ratio 12CO/13CO in its atmosphere. The isotopologue 13CO, is detected in the atmosphere through the cross-correlation method at a signal-to-noise of ~8.4. The detection significance is determined to be ~9.5 sigma using Bayesian model comparison between two retrieval models. We retrieve an isotopologue ratio 12CO/13CO of 97(+25/-18), marginally higher than the local interstellar standard. Its C/O ratio of ~0.56 is consistent with the solar value. Although only one super-Jupiter and one brown dwarf have now a measured 12CO/13CO ratio, it is intriguing that they are different, possibly hinting to distinct formation pathways. Albeit spectroscopic similarities, isolated brown dwarfs may experience a top-down formation via gravitational collapse, which resembles star formation, while giant exoplanets favorably form through core accretion, which potentially alters isotopologue ratios in their atmospheres depending on the material they accrete from protoplanetary disks. (abridged)