Model-free inverse method for transit imaging of stellar surfaces: Using transit surveys to map stellar spot coverage

TL;DR

This paper introduces a model-free technique for mapping stellar surface brightness variations using transit light curves, enabling large-scale stellar spot coverage surveys without relying on stellar atmosphere models or limb-darkening assumptions.

Contribution

The method uniquely derives stellar surface maps directly from transit data without assumptions about spot size, shape, or contrast, suitable for large exoplanet transit surveys.

Findings

Successfully mapped synthetic stellar disks.

Validated method with archive VLT data.

Produced high-quality brightness variation maps.

Abstract

Context. We present a model-free method for mapping surface brightness variations. Aims. We aim to develop a method that is not dependent on either stellar atmosphere models or limb-darkening equation. This method is optimized for exoplanet transit surveys such that a large database of stellar spot coverage can be created. Methods. The method uses light curves from several transit events of the same system. These light curves are phase-folded and median-combined to for a high-quality light curve without temporal local brightness variations. Stellar specific intensities are extracted from this light curve using a model-free method. We search individual light curves for departures from the median-combined light curve. Such departures are interpreted as brightness variations on the stellar surface. A map of brightness variations on the stellar surface is produced by finding the brightness distribution that can produce a synthetic light curve that fits observations well. No assumptions about the size, shape, or contrast of brightness variations are made. Results. We successfully reproduce maps of stellar disks from both synthetic data and archive observations from FORS2, the visual and near UV FOcal Reducer and low dispersion Spectrograph for the Very Large Telescope (VLT).