# Polarimetry microlensing of close-in planetary systems

## TL;DR

This paper explores the potential of using gravitational microlensing to detect and analyze the weak polarization signals from close-in giant planetary systems, which are otherwise too faint to observe directly.

## Contribution

It introduces a simulation framework for polarimetric observations of microlensed CGP systems and assesses the detectability of polarization signals with current and future instruments.

## Key findings

- Current instruments have less than 0.1% detection efficiency.
- Next-generation polarimeters could detect these signals under favorable conditions.
- Microlensing can magnify polarization signatures, aiding in planetary detection.

## Abstract

A close-in giant planetary (CGP) system has a net polarization signal whose value varies depending on the orbital phase of the planet. This polarization signal is either caused by the stellar occultation or by reflected starlight from the surface of the orbiting planet. When the CGP system is located in the Galactic bulge, its polarization signal becomes too weak to be measured directly. One method for detecting and characterizing these weak polarization signatures due to distant CGP systems is gravitational microlensing. In this work, we focus on potential polarimetric observations of highly-magnified microlensing events of CGP systems. When the lens is passing directly in front of the source star with its planetary companion, the polarimetric signature caused by the transiting planet is magnified. As a result some distinct features in the polarimetry and light curves are produced. In the same way microlensing amplifies the reflection-induced polarization signal. While the planet-induced perturbations are magnified, whenever these polarimetric or photometric deviations vanish for a moment the corresponding magnification factor or the polarization component(s) is equal to the related one due to the planet itself. In order to evaluate the observability of such systems through polarimetric or photometric observations of high-magnification microlensing events, we simulate these events by considering confirmed CGP systems as their source stars and conclude that the efficiency for detecting the planet-induced signal with the state-of-the-art polarimetric instrument (FORS2/VLT) is less than 0.1 %. Consequently, these planet-induced polarimetry perturbations can likely be detected under favorable conditions by high-resolution and short-cadence polarimeters of the next generation.