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Exoplanet atmospheres and demographics in the 2040s

Jens Kammerer, Sydney Vach, Sylvestre Lacour, Mathias Nowak, Thomas Winterhalder, Antoine Mérand, Akke Corporaal, Guillaume Bourdarot, Stefan Kraus, Sasha Hinkley

TL;DR

The paper argues that combining Gaia's upcoming discoveries of nearby young exoplanets with long-baseline interferometry (VLTI, GRAVITY, MATISSE) can yield a statistically meaningful sample of benchmark planets with precise dynamical masses and rich atmospheric data, enabling multi-angle constraints on giant-planet formation. It outlines the achievements of the current VLTI era and presents a roadmap for future facilities (VLTI+, kilometric baseline interferometry) to extend to iceline-scale separations and even younger, primordial atmospheres, while leveraging Gaia DR4 and Roman for expanded demographics and complementary measurements. The proposed approach promises to tighten atmospheric retrievals, trace isotopic abundances, and connect dynamical histories to formation environments, significantly advancing our understanding of planet formation mechanisms. This framework establishes a path toward a comprehensive, physics-driven census of exoplanet atmospheres and demographics in the 2040s.

Abstract

Direct observations of exoplanets probe the demographics and atmospheric composition of young self-luminous companions, yielding insight into their formation and early evolution history. In the near future, Gaia will reveal hundreds of nearby young exoplanets amenable to direct follow-up observations. Long-baseline interferometry with current and future facilities is best capable of exploiting this unique synergy which is poised to deliver a statistical sample of benchmark planets with precise dynamical masses and in-depth atmospheric characterization. This will enable tackling the longstanding question of how giant planets form from multiple angles simultaneously, shining light on the complex physical processes underlying planet formation.

Exoplanet atmospheres and demographics in the 2040s

TL;DR

The paper argues that combining Gaia's upcoming discoveries of nearby young exoplanets with long-baseline interferometry (VLTI, GRAVITY, MATISSE) can yield a statistically meaningful sample of benchmark planets with precise dynamical masses and rich atmospheric data, enabling multi-angle constraints on giant-planet formation. It outlines the achievements of the current VLTI era and presents a roadmap for future facilities (VLTI+, kilometric baseline interferometry) to extend to iceline-scale separations and even younger, primordial atmospheres, while leveraging Gaia DR4 and Roman for expanded demographics and complementary measurements. The proposed approach promises to tighten atmospheric retrievals, trace isotopic abundances, and connect dynamical histories to formation environments, significantly advancing our understanding of planet formation mechanisms. This framework establishes a path toward a comprehensive, physics-driven census of exoplanet atmospheres and demographics in the 2040s.

Abstract

Direct observations of exoplanets probe the demographics and atmospheric composition of young self-luminous companions, yielding insight into their formation and early evolution history. In the near future, Gaia will reveal hundreds of nearby young exoplanets amenable to direct follow-up observations. Long-baseline interferometry with current and future facilities is best capable of exploiting this unique synergy which is poised to deliver a statistical sample of benchmark planets with precise dynamical masses and in-depth atmospheric characterization. This will enable tackling the longstanding question of how giant planets form from multiple angles simultaneously, shining light on the complex physical processes underlying planet formation.
Paper Structure (4 sections, 2 figures)

This paper contains 4 sections, 2 figures.

Table of Contents

  1. Introduction
  2. The VLTI era
  3. Expanding horizons
  4. References

Figures (2)

  • Figure 1: ExoGRAVITY Spectral Library from [15] (right panel) showing the GRAVITY K-band spectra of 22 observed substellar companions sorted by spectral type, from M-type at the top to T-type at the bottom. On the left, zooms on $\beta$ Pic b (L0 spectral type) and AF Lep b (T2 spectral type) are shown, highlighting the chemical features detectable in their spectra.
  • Figure 2: Currently known exoplanet population color-coded by detection technique in the companion mass vs. semi-major axis plane. The detection limits of various facilities are overlaid with solid lines. The boundary between giant planets and brown dwarfs is highlighted by a dotted red line and the boundary between brown dwarfs and stars is highlighted by a dashed red line. VLTI+ is an upgraded VLTI and KPI stands for Kilometric Baseline Interferometry.