Trade-offs in high-contrast integral field spectroscopy for exoplanet detection and characterisation: Young gas giants in emission

TL;DR

This study explores the trade-offs in high-contrast integral field spectroscopy for exoplanet detection and characterization, emphasizing optimal spectral resolution and wavelength coverage to maximize detection and atmospheric analysis of young gas giants.

Contribution

It provides a comprehensive analysis of instrument design trade-offs, validated with real data, to optimize exoplanet detection and atmospheric characterization using high-contrast integral field spectroscopy.

Findings

Moderate spectral resolutions (R>300) are effective for molecule mapping.

Optimal spectral resolution is around R~2,000 before maximizing bandwidth.

High spectral resolution (R~10,000) is needed for radial velocity and spin measurements.

Abstract

Context: Combining high-contrast imaging with medium- or high-resolution integral field spectroscopy has the potential to boost the detection rate of exoplanets, especially at small angular separations. Furthermore, it immediately provides a spectrum of the planet that can be used to characterise its atmosphere. The achievable spectral resolution, wavelength coverage, and FOV of such an instrument are limited by the number of available detector pixels. Methods: The trade-offs are studied through end-to-end simulations of a typical high-contrast imaging instrument, analytical considerations, and atmospheric retrievals. The results are then validated with archival VLT/SINFONI data of the planet beta Pictoris b. Results: We show that molecular absorption spectra generally have decreasing power towards higher spectral resolution and that molecule mapping is already powerful for moderate resolutions (R>300). When choosing between wavelength coverage and spectral resolution for a given number of spectral bins, it is best to first increase the spectral resolution until R~2,000 and then maximise the bandwidth within an observing band. We find that T-type companions are most easily detected in the J/H band through methane and water features, while L-type companions are best observed in the H/K band through water and CO features. Such an instrument does not need to have a large FOV, as most of the gain in contrast is obtained in the speckle-limited regime close to the star. We show that the same conclusions are valid for the constraints on atmospheric parameters such as the C/O ratio, metallicity, surface gravity, and temperature, while higher spectral resolution (R~10,000) is required to constrain the radial velocity and spin of the planet.