Limits on the Post-eclipse Emission Spectrum of HD 80606 b From High-Resolution Spectroscop

TL;DR

This study uses high-resolution spectroscopy to investigate the post-eclipse atmosphere of the eccentric exoplanet HD 80606 b, providing tentative detection and constraints on atmospheric composition and thermal structure, consistent with JWST findings.

Contribution

First high-resolution spectroscopic analysis of HD 80606 b's post-eclipse atmosphere, offering tentative detection and atmospheric constraints aligned with JWST results.

Findings

Tentative detection of HD 80606 b with SNR~4.

Rejection of strong thermal inversions near periastron.

Evidence for absorption features from CH₄ and CO.

Abstract

We present Keck/NIRSPEC $K$-band observations of HD 80606 b, one of the most eccentric known exoplanets. HD 80606 b was observed after secondary eclipse, close to periastron, when the planet passes within 0.03 AU of HD 80606 and the rapid heating of the atmosphere may lead to extreme chemical changes and a temporary thermal inversion. The rapid change in the planetary radial velocity near periastron is sufficient to enable high-resolution cross-correlation spectroscopy (HRCCS) analysis, which produces a tentative detection ($\rm SNR\sim4$) of HD 80606 b. Injection-recovery tests appear to reject strong thermal inversions near periastron, consistent with recent results from JWST. We also perform atmospheric retrievals with free parameters for the Pressure-Temperature ($P-T$) profile and with a profile matched to the JWST results, which suggest the presence of absorption features from CH$_4$ and CO. While HD 80606 b is not definitively detected in these data, these results are consistent with JWST observations, which found the post-eclipse atmosphere of HD 80606 b shows weak absorption features from these species. Future observations with higher spectral resolution and/or wider wavelength coverage are needed for a confident atmospheric detection of HD 80606 b via high-resolution spectroscopy alone, but such observations are a challenge to schedule due to the 111-day orbital period.